Author name code: pasachoff ADS astronomy entries on 2022-09-14 author:"Pasachoff, Jay M." ------------------------------------------------------------------------ Title: The Eclipse Megamovie Project (2017) Authors: Hudson, Hugh S.; Peticolas, Laura; Johnson, Calvin; White, Vivian; Bender, Mark; Pasachoff, Jay M.; Martínez Oliveros, Juan Carlos; Collier, Braxton; Filippenko, Alexei V.; Filippenko, Noelle; Fraknoi, Andrew; Guevara Gómez, Juan Camilo; Koh, Justin; Konerding, David; Krista, Larisza; Kruse, Brian; McIntosh, Scott; Mendez, Brian; Ruderman, Igor; Yan, Darlene; Zevin, Dan Bibcode: 2022arXiv220713704H Altcode: The total solar eclipse of August 21, 2017, crossed the whole width of North America, the first occasion for this during the modern age of consumer electronics. Accordingly, it became a great opportunity to engage the public and to enlist volunteer observers with relatively high-level equipment; our program ("Eclipse Megamovie") took advantage of this as a means of creating a first-ever public database of such eclipse photography. This resulted in a large outreach program, involving many hundreds of individuals, supported almost entirely on a volunteer basis and with the institutional help of Google, the Astronomical Society of the Pacific, and the University of California, Berkeley. The project home page is \url{http://eclipsemegamovie.org}, which contains the movie itself. We hope that our comments here will help with planning for similar activities in the total eclipse of April 8, 2024. Title: Centennial of Definitive Verification of Einstein's GR: 1922-2022 Authors: Pasachoff, Jay Bibcode: 2022AAS...24023601P Altcode: Two years ago, we celebrated (AAS meeting 235 session 001) the centennial of the "Eddington expeditions" whose reports at meetings of the Royal Astronomical Society and the Royal Society in late 1919 brought Einstein's General Theory of the Relativity to the scientific and nonscientific world, and made Einstein a figure not only in science but also in Popular Culture. A Lick Observatory expedition in 1922 led to even better results on the observational agreement with Einstein's theory. We devote this special centennial session to discussing the Lick expedition and the artifacts that survive, to the role of the expedition in scientific history, similar observations made at the 2017 Great American Eclipse and plans for similar eclipse-deflection observations planned for the April 8, 2024, total solar eclipse to be observed probably from Mexico before the eclipse path enters the United States. Title: Preliminary Report on the December 4, 2021, Solar Eclipse Antarctic Expeditions Authors: Pasachoff, Jay; Boris, Theo; Lockwood, Christian; Sliski, David; Voulgaris, Aristeidis; Schneider, Glenn; Knowlton, Peter; Tosolini, Anna; Lu, Muzhou; Economou, Thanasis; Rojo, Patricio Bibcode: 2022AAS...24033209P Altcode: We give a preliminary report on results gathered from our three successful expeditions to the December 4, 2021, total solar eclipse, whose totality passed over Antarctica and adjacent ocean. One of our groups was on a chartered LATAM Boeing 787 Dreamliner that flew eastward from Punta Arenas, Chile at 41,000 ft (a second 787 was 1000 feet lower). Eastward of the Falkland Islands the aircraft turned southwest for a totality run as the upper of two planes with paths plotted by Glenn Schneider to observe totality a few degrees above the horizon out the left-hand windows from near the sunrise point. Our group carried cameras with telephotos and 3 spectrographs from Voulgaris (Icarus Optomechanics), and observed a measured 1 m 52 s of totality (07:22:35.1 to 07:04:26.6 UTC; middle of eclipse: 07:03:30.85 -56.167825°S -45.209159°W). We also worked with four people including Boris, Lockwood, and equipment, who flew to Union Glacier, on the Antarctic continent (Latitude -79.76, Longitude -82.85). In addition to astronomical equipment to image totality at an altitude of about 14° above the horizon, they sent back a livestream to NASA.gov and the NASA YouTube channel. Further, Rojo, a professor of astronomy at the University of Chile, joined the official expedition carried by the Chilean Air Force to spend two weeks on Union Glacier, Antarctica, conducting that expedition's only astronomical observations. He carried Celestron, Sony, Canon, and Nikon telephotos; with Sony, Nikon, and Canon cameras, much of the equipment from Williams College; with filters by Questar and Thousand Oaks Optical; and an Icarus Optomechanics spectrograph from Voulgaris.

In addition, efforts by the AAS Eclipse Task Force's Formal Education working group are on-going, in preparation for the annular 2023 and total 2024 solar eclipses.

JMP's current research about eclipses is sponsored by grant AGS-1903500 of the Solar Terrestrial Program, Atmospheric and Geospace Sciences Division of the NSF, succeeding AGS-1602461 from the period of the 2017 eclipse. We thank Williams College for additional student expeditionary support from the Freeman Foote endowment. We thank Tim Todd of TEI Tours and Travel, for his travel arrangements; John Beattie for on-site arrangements, and Mark Sood of A Classic Tours Collection for additional assistance. Title: A Diligent Analysis of the Flash and Coronal Spectrum of the Total Solar Eclipse of 20 March 2015 Authors: Voulgaris, Aristeidis G.; Mouratidis, C.; Tziotziou, K.; Seiradakis, J. H.; Pasachoff, J. M. Bibcode: 2022SoPh..297...49V Altcode: During totality of the solar eclipse of 20 March 2015, at Svalbard, Norway, the emission spectra of the solar chromosphere and corona were captured with a slitless spectrograph. A very lucky coincidence of a large number of sunspots and Active Regions (ARs) around the solar limb allowed us to observe a number of different spectroscopic effects. This eclipse took place about one year after the second solar maximum of the double-peaked Solar Cycle 24, which produced less activity than the previous stronger solar maxima. The spectra taken during the eclipse show strong and high activity of the green coronal line Fe XIV (5303 Å) and the lower intensity of the red coronal line Fe X (6374 Å). After subtraction of the emitted continuum of K+(F) corona, the detection and identification of several extremely weak emission lines, including the two forbidden emission lines of Ca XV (5694 Å and 5446 Å) and also Ni XIII (5116 Å) and Ni XV (6702 Å), was possible. The large number of ARs also led to the observation of a continuum brightening in ARs and a continuum darkening in surrounding areas. Title: IAU Commission C3 (History of Astronomy): Triennial Report, 2018–2021 Authors: Orchiston, Wayne; Sterken, Christiaan; Schechner, Sara; Sun, Xiaochun; Chinnici, Ileana; Lee, Eun-Hee; Pasachoff, Jay M.; van der Kruit, Pieter C. Bibcode: 2022JAHH...25..138O Altcode: IAU Commission C3 (History of Astronomy) started in 2015 as a natural continuation of the previous IAU Commission 41 for History of Astronomy which was established in 1948 and which was extremely successful in supporting research on the history of astronomy, organizing and sponsoring workshops and conferences, promoting research collaborations, forming specialist working groups and fostering the publication of members' research (see Kochhar et al., 2015). Title: White-Light Coronal Imaging at the 21 August 2017 Total Solar Eclipse Authors: Pasachoff, Jay M.; Rušin, Vojtech Bibcode: 2022SoPh..297...28P Altcode: We describe the solar corona as imaged in the 21 August 2017 total solar eclipse from sites in Oregon and Illinois, USA separated by nearly one hour. Our composite images, each made from dozens of individual frames, show helmet streamers, nearly radially oriented narrow rays, and polar coronal holes filled with polar plumes. The Ludendorff flattening index of 0.24 is compared with measurements from the last two centuries. We discuss the most remarkable coronal dynamics detected over a nearly one-hour interval between the two observing sites. Title: The Fiftieth Anniversary Celebration of the Solar Physics Division of the American Astronomical Society Authors: Pasachoff, Jay M.; Dupree, Andrea K.; Foukal, Peter; Weart, Spencer; Zirker, Jack Bibcode: 2021JAHH...24.1057P Altcode: The fiftieth anniversary celebration of the Solar Physics Division of the American Astronomical Society was held virtually in August 2020 with joint sponsorship from the Historical Astronomy Division, following the COVID-19-forced transformation of the original plan to hold the meeting in Spokane, Washington. The presenters had given papers at the first meeting in Huntsville, Alabama, in 1970, and addressed related fields from the vantage point of fifty years. Title: The eclipse Megamovie Project (2017) Authors: Hudson, Hugh; Peticolas, Laura; Johnson, Calvin; White, Vivian; Bender, Mark; Pasachoff, Jay M.; Oliveros, Juan Carlos Martínez; Filippenko, Alexei V.; et al. Bibcode: 2021JAHH...24.1080H Altcode: The total solar eclipse of August 21, 2017, crossed the whole width of North America, the first occasion for this during the modern age of consumer electronics. Accordingly, it became a great opportunity to engage the public and to enlist volunteer observers with relatively high-level equipment; our program ('Eclipse Megamovie') took advantage of this as a means of creating a first-ever public database of such eclipse photography. This resulted in a large outreach program, involving more than one thousand individuals, supported almost entirely on a volunteer basis and with the institutional help of Google, the Astronomical Society of the Pacific, and the University of California, Berkeley. The project home page at eclipsemegamovie.org contains the finished movie itself. We hope that our comments here will help with planning for similar activities during the total eclipse of 8 April 2024. Title: Total solar eclipses then and now Authors: Pasachoff, Jay M. Bibcode: 2021JAHH...24.1069P Altcode: I describe the new equipment and observations of the major total solar eclipse that passed from Mexico (where we observed it, in Miahuatlán, Oaxaca) on 7 March 1970, to the improved imaging and other capabilities we applied to the recent total solar eclipses of 2 July 2019 (from Chile), and 4 December 2021 (from on and near Antarctica, including airborne observations). Title: Another 6-Inch Brashear Restoration II Authors: Pasachoff, Jay M. Bibcode: 2021S&T...142a...6P Altcode: No abstract at ADS Title: Observational Validation of Predictions for the 2020 Eclipse Corona Authors: Pasachoff, J. M.; Downs, C.; Linker, J.; Caplan, R.; Riley, P.; Lionello, R.; Möller, A.; Rušin, V.; Vanur, R.; Carlos, W. Bibcode: 2021AAS...23822901P Altcode: Using observations from Argentina during the eclipse of 14 December 2020, compare our observations to a prediction simulation of the eclipse corona, developed by Predictive Science Inc. This 2020 prediction was based on a thermodynamic magnetohydrodynamic (MHD) model of the corona with a new two-temperature formulation and updates to a wave-turbulence-driven (WTD) heating and acceleration model. A comparison of the observed and predicted white light morphology is used to assess and inform the WTD model parametrization. Using observations by AM from Piedra del Águila, Argentina, we provided a quick composite by Williams College for comparison with the Predictive Science prediction for a NASA press release the following day (https://www.nasa.gov/feature/goddard/2020/scientists-use-nasa-data-predict-appearance-corona-dec-14-total-solar-eclipse) and a later composite by RV for a NASA press release about a newly discovered sungrazer comet that soon followed (https://www.nasa.gov/feature/goddard/2020/recently-discovered-comet-seen-during-2020-total-solar-eclipse-SOHO). See also Pasachoff, Jay M., 2021, Preliminary Report on the 14 December 2020 Total Solar Eclipse Observations, for International Astronomical Union Symposium 367: Education and Heritage in the Era of Big Data in Astronomy, submitted (Cambridge University Press, 2021); Pasachoff, Jay M., 2021, The 2020 Total Eclipse, Astronomy Magazine, April, pp. 47-51. Acknowledgments: JMP's research for this eclipse was sponsored by grant AGS-1903500 of the Solar Terrestrial Program, Atmospheric and Geospace Sciences Division of the NSF. PSI was supported by AFOSR, NASA, and NSF. VR and RV have been supported by the project VEGA ~ 2/0048/20 (Slovak Academy of Sciences). We thank Lina Tran and Joy Ng of NASA's Goddard Space Flight Center for their work on the prediction/verification and eclipse-comet press releases. Title: High-frequency Forbidden-line Coronal Oscillations As a Test of Coronal Heating Methods Authors: Pasachoff, J. M.; Person, M. J.; Wang, A. Bibcode: 2021AAS...23822902P Altcode: We report on data reduction carried out in 2020 on high-frequency (2 Hz) observations in the coronal green line (Fe XIV, 637.4 nm) and the coronal red line (Fe X, 530.3 nm) at the Williams College solar eclipse expedition to Salem, Oregon, for the August 21, 2017, totality. The observations and analysis followed previous work, testing the predictions of coronal heating from surface Alfvén waves, which would be at much higher frequency than the body waves in coronal loops usually invoked and studied. AW, in his A.B. senior thesis with joint advisors in the Astronomy and Mathematics departments, computed power spectra. He found some excess power at the high frequencies but only in the pixels closest to the solar limb, raising questions of equipment vibrations, raising questions for further observations. Newly designed equipment, with new detectors, was built for the 14 December 2020 total solar eclipse, but COVID-19-related travel bans at Williams College and at MIT prevented us from taking the apparatus. We look forward to using it at the total solar eclipses of 2023 in Australia and 2024 in Mexico/US.

Acknowledgments: Our research has been supported in large part from grant AGS-1903500 from the Solar Terrestrial Program of the Atmospheric and Geospace Sciences Division of the National Science Foundation and prior NSF grants, and from the Committee for Research and Exploration of the National Geographic Society, with additional support from Sigma Xi. Additional support for undergraduate participation came from the NSF, the NASA Massachusetts Space Grant Consortium, and the Clare Booth Luce Foundation, with travel support from the Freeman Foote Fund, the Rob Spring Fund, the Brandi Fund, and other sources at Williams College. Title: The International Astronomical Union's Working Group on Solar Eclipses Authors: Pasachoff, J. M. Bibcode: 2021AAS...23822903P Altcode: The International Astronomical Union's Working Group on Solar Eclipses of Divisions C (Education, Outreach, and Heritage) and E (Sun and Heliosphere) has the following tasks: (a) Working with the general public, providing materials and links to explain why eclipses are interesting to watch, how to observe them safely, and what science is being studied; and (b) Working with professional astronomers from around the world, to help coordinate their expeditions to total solar eclipses, including helping them work with customs in various countries about the temporary importation of scientific equipment. With our especially easy-to-remember website URL of http://eclipses.info, we endeavor to be a one-stop location for a wide variety of observing aids for professional and amateur astronomers. We link, for example, to the major sites for eclipse mapping. For professionals, we hope to be able to advise on the temporary duty-free import of equipment for eclipse observations. We provide links to books and summary articles about solar eclipses, and information about safe observing of solar eclipses (while trying to explain their excitement and value to the general public). • Members: Jay Pasachoff (USA, Chair), Iraida Kim (Russia), Jagdev Singh (India), Vojtech Rusin (Slovakia, through 2021), Yoichiro Hanaoka (Japan), Zhongquan Qu (China), Beatriz Garcia (Argentina), Patricio Rojo (Chile), Xavier Jubier (France), Fred Espenak (US), Jay Anderson (Canada), Glenn Schneider (US), Michael Gill (UK), Michael Zeiler (USA), Bill Kramer (USA); associates: Michael Kentrianakis (USA), and Ralph Chou (Canada). • For the 2019 and 2020 total eclipses in Chile and Argentina, Patricio Rojo (U. Chile) and Beatriz Garcia (Pierre Auger Observatory, Argentina) were added to the Working Group.• For the next triennium, September 2021-September 2024, given visibility of totality from Learmonth, Western Australia in 2023, we propose adding Terry Cuttle (public outreach, Australia) and Michael Wheatland (U. Sydney; an editor of the journal Solar Physics). We also propose adding Andreas Möller (Germany; who will collaborate with Bill Kramer on an archive of eclipse publications and maintain the eclipse-chaser.com website). Prof. Wheatland is an IAU member; Mr. Cuttle and Mr. Möller would be associates. Also we add Costantino Sigismondi (Italy), Robert Walsh (UK), and Kevin Reardon (US National Solar Observatory, USA). For the three eclipses in Spain (two total and one annular) in 2025-2026-2017, we add Mohamad Soltanolkotabi (Spain). We also look ahead to eclipses in Australia in 2028 and 2030. The 2027 eclipse continues from Spain across North Africa. The 2030 eclipse that reaches Australia starts over South Africa. • JMP represents this IAU Working Group on the American Astronomical Society's Solar Eclipse Task Force for the 2023 and 2024 eclipses (see http://eclipse.aas.org): Solar Eclipse Across America. Each year, we provide "Eclipses" for the International Geophysical Calendar (International Space Environmental Service), http://www.spaceweather.org/ISES/info/geocal/geocal.html • Acknowledgment: JMP's current solar eclipse activity is sponsored in large part by grant 1903500 of the Solar Terrestrial Program, Atmospheric and Geospace Sciences Division, NSF. Title: Haze in Pluto's atmosphere: Results from SOFIA and ground-based observations of the 2015 June 29 Pluto occultation Authors: Person, Michael J.; Bosh, Amanda S.; Zuluaga, Carlos A.; Sickafoose, Amanda A.; Levine, Stephen E.; Pasachoff, Jay M.; Babcock, Bryce A.; Dunham, Edward W.; McLean, Ian S.; Wolf, Jürgen; Abe, Fumio; Becklin, E. E.; Bida, Thomas A.; Bright, Len P.; Brothers, Tim; Christie, Grant; Durst, Rebecca F.; Gilmore, Alan C.; Hamilton, Ryan T.; Harris, Hugh C.; Johnson, Chris; Kilmartin, Pamela M.; Kosiarek, Molly; Leppik, Karina; Logsdon, Sarah E.; Lucas, Robert; Mathers, Shevill; Morley, C. J. K.; Nelson, Peter; Ngan, Haydn; Pfüller, Enrico; Natusch, Tim; Sallum, Stephanie; Savage, Maureen L.; Seeger, Christina H.; Siu, Ho Chit; Stockdale, Chris; Suzuki, Daisuke; Thanathibodee, Thanawuth; Tilleman, Trudy; Tristram, Paul J.; Vacca, William D.; Van Cleve, Jeffrey; Varughese, Carolle; Weisenbach, Luke W.; Widen, Elizabeth; Wiedemann, Manuel Bibcode: 2021Icar..35613572P Altcode: On UT 29 June 2015, the occultation by Pluto of a bright star (r‧ = 11.9) was observed from the Stratospheric Observatory for Infrared Astronomy (SOFIA) and several ground-based stations in New Zealand and Australia. Pre-event astrometry allowed for an in-flight update to the SOFIA team with the result that SOFIA was deep within the central flash zone (~22 km from center). Analysis of the combined data leads to the result that Pluto's middle atmosphere is essentially unchanged from 2011 and 2013 (Person et al. 2013; Bosh et al. 2015); there has been no significant expansion or contraction of the atmosphere. Additionally, our multi-wavelength observations allow us to conclude that a haze component in the atmosphere is required to reproduce the light curves obtained. This haze scenario has implications for understanding the photochemistry of Pluto's atmosphere. Title: Preliminary Report on the 14 December 2020 Total Solar Eclipse Observations Authors: Pasachoff, Jay M. Bibcode: 2021IAUS..367...43P Altcode: This paper summarizes preliminary scientific observations from sites in Chile and Argentina from which the totality was observed on 14 December 2020 at the minimum of the solar-activity/sunspot cycle. Title: History of Astronomy: The Voyager Golden Record in Intellectual History Authors: Pasachoff, J. Bibcode: 2021AAS...23722201P Altcode: In this session cosponsored by the American Astronomical Society's History of Astronomy Division, we discuss especially the Golden Record of music, greetings, photographs, and more organized by Jon Lomberg working for Carl Sagan in spring 1977, shortly before the Voyagers' launches. Emer Reynolds will discuss the 2019 documentary — The Farthest — that she directed; we have separately arranged for those attending the meeting to stream the two-hour theatrical version. Sarah May will discuss the legacy of the Golden Record in intellectual history. Nick Oberg will discuss the trajectory of the Voyager spacecraft in the distant future. Supplementally, as three nations' missions travel from Earth to Mars this fall, Lomberg will discuss the disk of greetings and more that was sent to Mars on NASA's Phoenix lander in 2008. Title: Observations of the December 14, 2020, Total Solar Eclipse Authors: Pasachoff, J. M.; Rusin, V.; Vansur, R. Bibcode: 2021AAS...23740502P Altcode: With special arrangements from the Ministry of Science of Chile, arranged through the U.S. Embassy in Santiago, we were able to have a group of about a dozen northern-hemisphere astronomers at our site in Pucón, Chile, near the Villarrica volcano's mid-level ski area, for the total solar eclipse of December 14, 2020. Though the authors could not travel there personally, we had a group of a dozen people there, though that site turned out to be cloudy, and in spite of an attempt to reach clear areas in Argentina, our group was unable to cross the border. We collected observations from a few sites from which the eclipse was visible, as well as space imaging. We worked to analyze the white-light imaging, making composite images that (a) were released to compare with predictions of the coronal streamers made by Predictive Science Inc based on SDO observations of the magnetic field over the preceding weeks; and (b) comparing the position of the eclipse comet. Information is available at my eclipse website at http://totalsolareclipse.org and at the website of the International Astronomical Union's Working Group on Solar Eclipses at http://eclipses.info. JMP's eclipse research receives major support from grant AGS-1903500 from the Solar Terrestrial Program, Atmospheric and Geospace Sciences Division, U.S. National Science Foundation to Williams College. Title: Great Astronomers and their Original Publications Authors: Pasachoff, J. Bibcode: 2021AAS...23754706P Altcode: During fall 2020, I taught a hybrid course on Great Astronomers and their Original Publication, using the first-editions of Copernicus, Galileo, Kepler, Newton and others from my own collection and the collection of the Chapin Library of Williams College. The course's text was the new Cosmos: The Art and Science of the Universe, by Roberta J. M. Olson and me (Reaktion Books, 2019). My own lectures and guest lectures from colleagues around the world were via Zoom, while Williams College's Chapin Librarian Wayne Hammond met small groups of the 24 enrolled students in a library classroom where the students in groups of four or five (plus one remote section) viewed and handled the actual first editions. The course was "writing intensive" in Williams College's system, so required 3 papers in draft and final form as well as reports on individual biographies and other books separately assigned. The course was crosslisted among Astronomy, History of Science, Leadership Studies, and Science & Technology Studies departments/programs. Speakers, all via Zoom, included Dan Falk and Peter Usher (Shakespeare's astronomy), Dava Sobel (Copernicus and Galileo), Robert Littman (Gutenberg), Michael Mendillo (constellation maps), Owen Gingerich (Copernicus and volvelles), Mordechai Feingold (Newton's Principia census), Nick Wilding (Galileo: Sidereus Nuncius forgery), Meg Ford (Christie's London; 2020 De Revolutionibus auction), Thomas Lecky (formerly Christie's New York; now Riverrun Books), James Voelkel '84 (Science History Institute's library, his Kepler biography); Al Van Helden (Galileo), Hanoch Gutfreund and Jurgen Renn (Einstein), David DeVorkin (George Ellery Hale; Cecilia Payne-Gaposchkin, H. N. Russell), and Roberta Olson (related art-history). Wayne Hammond (Chapin Librarian) discussed Caroline Herschel and others. Title: Anomalies and Fluctuations of Near-surface Air Temperature at Tianhuangping (Zhejiang), China, Produced by the Longest Total Solar Eclipse of the 21st Century Under Cloudy Skies Authors: Peñaloza-Murillo, Marcos A.; Roman, Michael T.; Pasachoff, Jay M. Bibcode: 2020PASP..132k4503P Altcode: 2019arXiv190503613P During a total eclipse of the Sun, the solar disk blocked by the lunar disk produces an instant and strong decline of energy at the surface. This loss of energy leads to a decreasing air temperatures near the surface. Anyone under a completely clear sky, with a total solar eclipse (TSE) in progress, feels a cooling, whose minimum is reached a few minutes after totality. This drop in temperature is known as an anomaly and this delay is called thermal lag. During a TSE air temperature changes appreciably not only in magnitude but also in timing, depending on weather and geographical conditions. If the eclipse is partially or totally obscured by clouds, some effects are produced on the thermal lag. Under clear skies, the temperature response lags behind the change in solar flux as one expects in TSE; however, under cloudy skies, the lag can reverse in early and/or late stages of partial phases. The normal heating of the surface by the Sun, which drives turbulent motion in the air layer near the surface, is disrupted during the eclipse. The 2009 TSE in China provided an opportunity to have a look at these kinds of perturbations caused by this eclipse. In this paper, the second of a series of three, we analyze the near-surface air temperature response, at three different heights over the ground, recorded by the Williams College expedition under meteorological conditions characterized by cloudy skies during the longest total solar eclipse of the 21st century on 2009 July 22, at Tianhuangping (Zhejiang), China. An analysis of the relationship between solar radiation and air temperature was made by applying a study previously published in the first paper of this series in which we evaluated the cloudiness contribution in estimating the impact on global solar radiation throughout this phenomenon at that site. The analysis of this response includes linear and absolute negative anomalies as well as fluctuations, which was undertaken through a statistical study to get information on the convection activity produced by the latter. The fluctuations generated by turbulence were studied by analyzing variance and residuals. The results, indicating a steady decrease and recovery of both perturbations, were consistent with those published by other studies for this total solar eclipse. Title: History of Astronomy: The Voyager Golden Record in Intellectual History Authors: Pasachoff, J. M. Bibcode: 2020DPS....5240701P Altcode: In this session cosponsored by the American Astronomical Society's History of Astronomy Division, we discuss especially the Golden Record of music, greetings, photographs, and more organized by Jon Lomberg working for Carl Sagan in spring 1977, shortly before the Voyagers' launches. Emer Reynolds will discuss the 2019 documentary The Farthest that she directed; we have separately arranged for those attending the meeting to stream the two-hour theatrical version. Sarah May will discuss the legacy of the Golden Record in intellectual history. Nick Oberg will discuss the trajectory of the Voyager spacecraft in the distant future. Supplementally, as three nations' missions travel from Earth to Mars this fall, Lomberg will discuss the disk of greetings and more that was sent to Mars on NASA's Phoenix lander in 2008. Title: The Galilean Moons I Authors: Pasachoff, Jay Bibcode: 2020S&T...140c...8P Altcode: No abstract at ADS Title: Compositing Eclipse Images from the Ground and from Space Authors: Lockwood, Christian A.; Pasachoff, Jay M.; Seaton, Daniel B.; Sliski, David H.; Lefaudeux, Nicolas Bibcode: 2020RNAAS...4..133L Altcode: We present composite white-light images of the 2019 July 2, total solar eclipse, from the minimum of the solar-activity cycle. We exhibit high-resolution high dynamic range composites from three observation sites in Chile, including one made of 646 individual ground-based images and with such a wide field it exceeds the field of view of the Naval Research Laboratory's C2 and C3 coronagraphs aboard ESA's Solar and Heliospheric Observatory. We compare the resolution of the coronal streamers and other magnetic phenomena of the corona. We also show continuity of features on the solar surface as observed from NOAA's GOES-16 and GOES-17 Solar Ultraviolet Imager. Title: Total Solar Eclipses Forever Authors: Pasachoff, J. Bibcode: 2020SPD....5110104P Altcode: Fifty years ago, Donald Menzel and I had a major expedition to Miahuatlán, Oaxaca, Mexico (sponsored by National Geographic) for the March 7, 1970, total solar eclipse, whose path extended up the US Eastern Seaboard and out to sea at Nantucket. We had a giant wide-field coronal Littrow spectrograph designed by James G. Baker. We described the coronal configuration, including a paper in Nature about the eclipse. I will discuss science from the series of total solar eclipses since then, including our hopes for observing the 14 December 2020 total solar eclipse whose path of totality will cross southern Chile and Argentina, as did the 2 July 2019 eclipse. I will comment on imaging, spectra, and prediction of both configuration from magnetic field maps and Baily's beads from 3D mapping of the Moon. Over the decades, 14 of my eclipse expeditions were supported by the Committee for Research and Exploration of the National Geographic Society. My recent research on solar eclipses receives major support from (currently grant AGS-1903500) from the Solar Terrestrial Program, Atmospheric and Geospace Sciences Division, U.S. National Science Foundation. Additional student support has recently come from Sigma Xi, NASA's Massachusetts Space Grant Consortium, and The Global Initiative, Freeman Foote, and Brandi Funds of Williams College. Title: Compositing Eclipse Images from the Ground and from Space Authors: Pasachoff, J. M.; Lockwood, C. A.; Seaton, D. B.; Sliski, D.; Lefaudeux, N. Bibcode: 2020AAS...23611204P Altcode: We present composite white-light images of the 2 July 2019 total solar eclipse, from the minimum of the solar-activity cycle. With separate high-resolution ground-based images, one of them made of 646 individual images with such a wide field that it exceeds the fields of view of the Naval Research Laboratory's C2 and C3 coronagraphs aboard ESA's Solar and Heliospheric Observatory, we have composites based on observations from the Cerro Tololo Inter-American Observatory and the centerline of totality at La Higuera in Chile. We compare the resolution of the coronal streamers and other magnetic phenomena of the corona. We also show continuity from features on the solar surface as observed from NASA's Solar Dynamics Observatory and NOAA's GOES-16 Solar Ultraviolet Imager (SUVI). Acknowledgments: JMP's eclipse research receives major support from grant AGS-903500 from the Solar Terrestrial Program, Atmospheric and Geospace Sciences Division, U.S. National Science Foundation. We had additional student support from the Massachusetts NASA Space Grant Consortium; Sigma Xi; the Global Initiatives Fund at Williams College; and the University of Pennsylvania. Title: Size and Shape Constraints of (486958) Arrokoth from Stellar Occultations Authors: Buie, Marc W.; Porter, Simon B.; Tamblyn, Peter; Terrell, Dirk; Parker, Alex Harrison; Baratoux, David; Kaire, Maram; Leiva, Rodrigo; Verbiscer, Anne J.; Zangari, Amanda M.; Colas, François; Diop, Baidy Demba; Samaniego, Joseph I.; Wasserman, Lawrence H.; Benecchi, Susan D.; Caspi, Amir; Gwyn, Stephen; Kavelaars, J. J.; Ocampo Uría, Adriana C.; Rabassa, Jorge; Skrutskie, M. F.; Soto, Alejandro; Tanga, Paolo; Young, Eliot F.; Stern, S. Alan; Andersen, Bridget C.; Arango Pérez, Mauricio E.; Arredondo, Anicia; Artola, Rodolfo Alfredo; Bâ, Abdoulaye; Ballet, Romuald; Blank, Ted; Bop, Cheikh Tidiane; Bosh, Amanda S.; Camino López, Matías Aarón; Carter, Christian M.; Castro-Chacón, J. H.; Caycedo Desprez, Alfonso; Caycedo Guerra, Nicolás; Conard, Steven J.; Dauvergne, Jean-Luc; Dean, Bryan; Dean, Michelle; Desmars, Josselin; Dieng, Abdou Lahat; Bousso Dieng, Mame Diarra; Diouf, Omar; Dorego, Gualbert Séraphin; Dunham, David W.; Dunham, Joan; Durantini Luca, Hugo A.; Edwards, Patrick; Erasmus, Nicolas; Faye, Gayane; Faye, Mactar; Ferrario, Lucas Ezequiel; Ferrell, Chelsea L.; Finley, Tiffany J.; Fraser, Wesley C.; Friedli, Alison J.; Galvez Serna, Julián; Garcia-Migani, Esteban A.; Genade, Anja; Getrost, Kai; Gil-Hutton, Ricardo A.; Gimeno, German N.; Golub, Eli Joseph; González Murillo, Giovanni Francisco; Grusin, Michael D.; Gurovich, Sebastian; Hanna, William H.; Henn, Santiago M.; Hinton, P. C.; Hughes, Paul J.; Josephs, John David, Jr.; Joya, Raul; Kammer, Joshua A.; Keeney, Brian A.; Keller, John M.; Kramer, Emily A.; Levine, Stephen E.; Lisse, Carey M.; Lovell, Amy J.; Mackie, Jason A.; Makarchuk, Stanislav; Manzano, Luis E.; Mbaye, Salma Sylla; Mbaye, Modou; Melia, Raul Roberto; Moreno, Freddy; Moss, Sean K.; Ndaiye, Diene; Ndiaye, Mapathe; Nelson, Matthew J.; Olkin, Catherine B.; Olsen, Aart M.; Ospina Moreno, Victor Jonathan; Pasachoff, Jay M.; Pereyra, Mariana Belen; Person, Michael J.; Pinzón, Giovanni; Pulver, Eduardo Alejandro; Quintero, Edwin A.; Regester, Jeffrey R.; Resnick, Aaron Caleb; Reyes-Ruiz, Mauricio; Rolfsmeier, Alex D.; Ruhland, Trina R.; Salmon, Julien; Santos-Sanz, Pablo; Santucho, Marcos Ariel; Sepúlveda Niño, Diana Karina; Sickafoose, Amanda A.; Silva, José S.; Singer, Kelsi N.; Skipper, Joy N.; Slivan, Stephen M.; Smith, Rose J. C.; Spagnotto, Julio C.; Stephens, Andrew W.; Strabala, Samuel D.; Tamayo, Francisco J.; Throop, Henry B.; Torres Cañas, Andrés David; Toure, Labaly; Traore, Alassane; Tsang, Constantine C. C.; Turner, Jake D.; Vanegas, Santiago; Venable, Roger; Wilson, John C.; Zuluaga, Carlos A.; Zuluaga, Jorge I. Bibcode: 2020AJ....159..130B Altcode: 2020arXiv200100125B We present the results from four stellar occultations by (486958) Arrokoth, the flyby target of the New Horizons extended mission. Three of the four efforts led to positive detections of the body, and all constrained the presence of rings and other debris, finding none. Twenty-five mobile stations were deployed for 2017 June 3 and augmented by fixed telescopes. There were no positive detections from this effort. The event on 2017 July 10 was observed by the Stratospheric Observatory for Infrared Astronomy with one very short chord. Twenty-four deployed stations on 2017 July 17 resulted in five chords that clearly showed a complicated shape consistent with a contact binary with rough dimensions of 20 by 30 km for the overall outline. A visible albedo of 10% was derived from these data. Twenty-two systems were deployed for the fourth event on 2018 August 4 and resulted in two chords. The combination of the occultation data and the flyby results provides a significant refinement of the rotation period, now estimated to be 15.9380 ± 0.0005 hr. The occultation data also provided high-precision astrometric constraints on the position of the object that were crucial for supporting the navigation for the New Horizons flyby. This work demonstrates an effective method for obtaining detailed size and shape information and probing for rings and dust on distant Kuiper Belt objects as well as being an important source of positional data that can aid in spacecraft navigation that is particularly useful for small and distant bodies. Title: Eclipse Tests of General Relativity in the 21st Century Authors: Pasachoff, J. M. Bibcode: 2020AAS...23500101P Altcode: The analysis of the results, and their reception over the years, of the 1919 total solar eclipse observations from Principe by Arthur Eddington and colleague Edwin Cottingham, and from Sobral (Brazil) by Andrew Crommelin and Charles Davidson, all in collaboration with Astronomer Royal Sir Frank Watson Dyson, will be discussed by experts Daniel Kennefick (US) and Jeffrey Crelinsten (Canada). At this Centennial, I will discuss current repetitions of this "Eddington Experiment" and future plans.

JMP's eclipse research receives major support from grant AGS-903500 from the Solar Terrestrial Program, Atmospheric and Geospace Sciences Division, U.S. National Science Foundation. Title: Early Results from the Solar-Minimum 2019 Total Solar Eclipse Authors: Pasachoff, J. M.; Lockwood, C. A.; Inoue, J. L.; Meadors, E. N.; Voulgaris, A.; Sliski, D.; Sliski, A.; Reardon, K. P.; Seaton, D. B.; Caplan, R. M.; Downs, C.; Linker, J. A.; Sterling, A. C. Bibcode: 2020AAS...23535903P Altcode: We report on first results from our observations in Chile on July 2, 2019, that revealed the extreme-solar-minimum corona, with only equatorial streamers and with visible polar plumes. We have observations in clear skies from our three observing sites: (1) The Cerro Tololo Inter-American Observatory, 7,240-foot altitude, 2 min 6 sec; (2) La Higuera, centerline, 2,500-foot altitude, 2 min 35 sec totality; (3) La Serena, sea level, 2 min 15 sec totality. Prominences on the limb provided orientation and coordination with spacecraft observations from NOAA's GOES-R Solar Ultraviolet Imager (SUVI) and the Atmospheric Imaging Assembly (AIA) on NASA's Solar Dynamics Observatory (SDO). The double-diamond ring at second contact will extend our determination of a new IAU-recommended value of the solar diameter through comparison with models taking into account the precise lunar profile. Our coronal spectra from slitless spectrographs, from CTIO, showed the Fe XIV 530.3 nm green line substantially weaker than the Fe X 637.4 nm red line, corresponding to the relatively low coronal temperature at this phase of the solar-activity cycle. On the spectra we also detected the weak coronal emission line of Ar X at 553.3 nm, as we also detected at the previous total solar eclipse of August 21, 2017, in the USA. We show a comparison of the eclipse observation with a prediction of the structure of the corona from an MHD model, carried out by Predictive Science Inc. (PSI). We consider the lines of sight to NASA's Parker Solar Probe at the times of total eclipses, when we can examine the coronal imaging in terms of electron density to compare with the in situ measurements.

We received major support from grant AGS-903500 from the Solar Terrestrial Program, Atmospheric and Geospace Sciences Division, U.S. National Science Foundation. The CTIO site was courtesy of Associated Universities for Research in Astronomy (AURA). We had additional student support from the Massachusetts NASA Space Grant Consortium; Sigma Xi; the Global Initiatives Fund at Williams College; and the University of Pennsylvania. PSI was supported by AFOSR, NASA, and NSF. ACS received support from the NASA/HGI program, and from the MSFC Hinode project. AV thanks the mathematician Christophoros Mouratidis for his help with the data reduction of the spectra. Title: Early results from the solar-minimum 2019 total solar eclipse Authors: Pasachoff, Jay M.; Lockwood, Christian A.; Inoue, John L.; Meadors, Erin N.; Voulgaris, Aristeidis; Sliski, David; Sliski, Alan; Reardon, Kevin P.; Seaton, Daniel B.; Caplan, Ronald M.; Downs, Cooper; Linker, Jon A.; Schneider, Glenn; Rojo, Patricio; Sterling, Alphonse C. Bibcode: 2020IAUS..354....3P Altcode: We observed the 2 July 2019 total solar eclipse with a variety of imaging and spectroscopic instruments recording from three sites in mainland Chile: on the centerline at La Higuera, from the Cerro Tololo Inter-American Observatory, and from La Serena, as well as from a chartered flight at peak totality in mid-Pacific. Our spectroscopy monitored Fe X, Fe XIV, and Ar X lines, and we imaged Ar X with a Lyot filter adjusted from its original H-alpha bandpass. Our composite imaging has been compared with predictions based on modeling using magnetic-field measurements from the pre-eclipse month. Our time-differenced sites will be used to measure motions in coronal streamers. Title: Demonstrating the Cosmic Distance Ladder with Cepheids Authors: Pasachoff, Jay M.; Mativi, Jason W. Bibcode: 2020PhTea..58....6P Altcode: To span the great distance from our solar system to the farthest clusters of galaxies in our universe, astronomers break down the distance indicators into steps. The nearest ones are measured geometrically, with what is known as parallax. Among the objects whose distances are thus directly measured are a rare type of star known as a Cepheid variable. Henrietta Leavitt about a hundred years ago discovered, by looking at a number of such stars in the Small Magellanic Cloud, that the brighter the star, the longer its period. This secondary indicator can be used in nearby galaxies to calibrate as a standard candle a specific type of supernova (Type Ia, from explosions of white-dwarf stars), whose peak intensities are so bright that they can be seen throughout the observable universe. Title: Measuring the Scale of the Solar System through Transits of Mercury Authors: Pasachoff, Jay; Backhaus, Udo; Knülle-Wenzel, Alfred; Zender, Joe J. Bibcode: 2019EPSC...13...62P Altcode: We discuss use of past transits of Venus and Mercury for finding the distance from the Earth to the Sun, and propose a student and citizen-science exercise to make that measurement through simultaneous observations of the 11 November 2019 transit of Mercury from widely separated terrestrial sites. Title: The 1919 Eclipse Expedition Results in the Context of the 2019 Age of LIGO Authors: Pasachoff, Jay; Kennefick, Julia Bibcode: 2019EPSC...13.1951P Altcode: To mark the centennial of the 29 May 1919 total solar eclipse observed from Principe and Brazil from which Eddington, Dyson, Crommelin and others took and/or analyzed data about the deflection of starlight near the Sun, endorsing Albert Einstein's prediction from his General Theory of Relativity, our session includes authors of recent books analyzing the 1919 events and subsequent discussions. Our session also includes astronomers who are working to mark and establish a lasting educational presence at Roça Sundy, Principe. Title: Transits of Mercury and General Relativity from observations, and the 2019 November 11 transit Authors: Sigismondi, Costantino; Bordoni, Luigi; Pasachoff, Jay Bibcode: 2019EPSC...13..993S Altcode: The transit of Mercury of November 11, 2019 provides the opportunity to test a method of measuring the solar diameter and shape (due to the oblateness) better than 0.1", or 70 Km of resolution on the Sun. Beyond the General Relativity implications of Mercury itself, we exploit the most precise ephemerides to achieve 0.1" with ground-based instruments of the solar diameter, of which monitoring the secular variations (related to our climate), as well as transient variations as potential proxies of major flares and Coronal Mass Ejections (to predict space weather). Title: Depictions of the Moon in Western Visual Culture Authors: Pasachoff, J. M.; Olson, Roberta J. M. Bibcode: 2019oeps.book...55P Altcode: No abstract at ADS Title: Education and Outreach About Science at the 2017 Eclipse Authors: Pasachoff, J. M. Bibcode: 2019ASPC..516..331P Altcode: When a solar eclipse is visible from a country, especially a total solar eclipse, we astronomers have the attention of the general public in addition to that of scientists and students. At the time of the 2017 solar eclipse whose totality crossed the Continental United States, with a partial eclipse visible from all states, we were able to provide students and the general public, as well as scientists a wide range of substantial scientific information about eclipses, about the Sun, and about the rest of the Universe. For the Working Group on Solar Eclipses of the International Astronomical Union, we also acted as a liaison providing letters of invitation that were useful for foreign colleagues obtaining U.S. visas and helping to arrange observing locations. Title: Eclipse Megamovie 2017 Successes and Potential For Future Work Authors: Peticolas, L.; Hudson, H.; Johnson, C.; Zevin, D.; White, V.; Oliveros, J. C. M.; Ruderman, I.; Koh, J.; Konerding, D.; Bender, M.; Cable, C.; Kruse, B.; Yan, D.; Krista, L.; Collier, B.; Fraknoi, A.; Pasachoff, J. M.; Filippenko, A. V.; Mendez, B.; McIntosh, S. W.; Filippenko, N. L. Bibcode: 2019ASPC..516..337P Altcode: In 2011, an "Eclipse Megamovie" was envisioned for the 2017 total solar eclipse that would be created using the public's photographs of the Sun's corona as frames in a movie illuminating dynamic changes in the chromosphere and corona. On August 21, 2017, our team collected photographs of the total solar eclipse from thousands of volunteers with telescopes, DSLR (Digital Single-Lens Reflex) cameras, and mobile device cameras setup across the path of totality. Our efforts resulted in 1,190 photographers contributing 50,016 DSLR photographs in a final open-source, public archive that is 766 GB in size. All photographs in this archive are Creative Commons zero (CC0), making them freely available for public use. From mobile devices, we obtained an archive of 60,000 images, 211 GB in size. The first Eclipse Megamovie video was compiled and made available to the public a few hours after the Moon's shadow left the U.S. East Coast. For two weeks, additional images were added to this video, as volunteers uploaded them to the project server. The project also resulted in a comprehensive website with 12,749 users sufficiently interested in the project to each create a user profile on the website, several short documentaries, 190 articles and press releases, open-source code for use in future related efforts, and hundreds of public presentations across the country prior to the eclipse. Information on how to access these resources is included in this paper. Title: Transit of Mercury and General Relativity from Observations, and the 2019 November 11 Transit Authors: Sigismondi, C.; Bordoni, L.; Pasachoff, J. Bibcode: 2019JOA.....9c...8S Altcode: The transit of Mercury of November 11 2019, provides the opportunity to test a method of measuring the solar diameter and shape (due to the oblateness) better than 0.1", or 70 km of resolution on the Sun. Beyond the General Relativity implications of Mercury itself, we exploit the most precise ephemerides to achieve 0.1" with ground-based instruments of the solar diameter, of which monitoring the secular variations (related to our climate), as well as transient variations as potential proxies of major flares and Coronal Mass Ejections (to predict space weather). Title: Solar Seeing Authors: Pasachoff, Jay M. Bibcode: 2019S&T...137f...8P Altcode: No abstract at ADS Title: The IAU and Solar Eclipses Authors: Pasachoff, Jay M.; Hiei, Eijiro; Perez, Cielo Bibcode: 2019IAUS..349..459P Altcode: We describe the history of solar-eclipse supervision since the formation of the International Astronomical Union, as the supervising body morphed from a full commission to a subcommission to its current status as an Inter-Divisional Working Group of the Education, Outreach and Heritage Division and the Sun and Heliosphere Division. Title: Book Review: The Sun Authors: Golub, Leon; Pasachoff, Jay M. Bibcode: 2018JAHH...21..241C Altcode: No abstract at ADS Title: Images and Spectra of the 2017 Total Solar Eclipse Corona From Our Oregon Site Authors: Pasachoff, Jay M.; Lockwood, Christian; Meadors, Erin; Yu, Ross; Perez, Cielo; Peñaloza-Murillo, Marcos A.; Seaton, Daniel B.; Voulgaris, Aris; Dantowitz, Ron; Rušin, Vojtech; Economou, Thanasis Bibcode: 2018FrASS...5...37P Altcode: No abstract at ADS Title: Airborne and Ground Observations of the Stellar Occultation by Triton on 5 October 2017 Authors: Person, Michael J.; Schindler, Karsten; Bosh, Amanda S.; Wolf, Juergen; Levine, Stephen E.; Zuluaga, Carlos A.; Pfueller, Enrico; Caton, Daniel; Patton, Alexander; Pasachoff, Jay; Oswalt, Terry; von Hippel, Ted; Brothers, Timothy; Operations Tea, Sofia; Lincoln Labs Firepond Observations Team; Triton Occultation Observation Team Bibcode: 2018DPS....5041610P Altcode: On 5 October 2017, Triton occulted the 13th magnitude star UCAC4 410-143659 as seen from the Eastern US, North Atlantic, and Europe. Our collaboration observed this event from the Stratospheric Observatory for Infrared Astronomy (SOFIA) aircraft, as well as numerous (over two dozen) ground stations throughout the US and Europe. Here, we present the preliminary results of analyzing this dataset and highlight a number of features of Triton's atmosphere. Initial reduction of the data indicates that the atmospheric pressure increases seen throughout the 90's have stabilized or perhaps begun to reverse, as the current pressures are more comparable to those measured during the earlier occultations of the 1990's than the later ones, although still greater than the pressure observed by Voyager 2 in 1989. Careful calibration of the multi-wavelength observations made from SOFIA indicates a clear atmosphere at the levels to which we are sensitive (>35 km), with no signs of the various particulate dust plumes or cloud-like structures seen by Voyager 2 below 8 km altitude. Data reduction is progressing and a final report is in preparation. Title: Who named the largest moons of Jupiter? Johannes Kepler contributed Authors: Pasachoff, Jay M. Bibcode: 2018iau3.book...38P Altcode: It is little known that one day after Galileo discovered what are generally called the Galilean moons of Jupiter (which is very well visible in the evening sky this month), Simon Marius of Nuremberg independently discovered them, if we go by written notes. (If we go by verbal accounts, Marius may well have seen them first.) In his book Mundus Iovialis (1614) Marius credits Kepler for giving him the idea to name the moons Io, Europa, Ganymede, and Callisto, the names that have stuck, even if the set of moons are known as the Galilean moons. Galileo took strong objection to Marius's report of independent discovery but historical verification favors Marius's claim.

At the Smithsonian Institution's National Air and Space Museum, two audio clips (#3 and #48) about Kepler's work (51 seconds and 2 minutes 41 seconds, respectively) recorded by Pasachoff are available to visitors; they are available also at https://airandspace.si.edu/explore-universe-audio-tour Title: Science at the Great American Eclipse Authors: Pasachoff, Jay M. Bibcode: 2018A&G....59d4.19P Altcode: Jay Pasachoff rounds up observations made by citizen scientists, individuals, groups and an array of spacecraft. Title: Das Beispiel Hilmar und Waltraut - Ehepaare am Himmel der Kleinen Planeten Authors: Schmadel, Lutz D.; Pasachoff, Jay M.; Ting, Peter M. Bibcode: 2018AcHA...64..281S Altcode: The names of the minor planets are not just arabesques of its discoverers, but they also reflect the ever-changing zeitgeist of more than two centuries. Increasingly, the list of names is no longer to be regarded as merely an inventory of deceased astronomers or a list of mythological figures. More and more not only prominent figures in the history of astronomy but also their spouses have given their names to minor planets. In grateful memory of our colleagues Hilmar Duerbeck and Waltraut Seitter, we introduce a new catalog listing pairs (or triples) of married couples after whom minor planets have been named. Title: Predicting the corona for the 21 August 2017 total solar eclipse Authors: Mikić; , Zoran; Downs, Cooper; Linker, Jon A.; Caplan, Ronald M.; Mackay, Duncan H.; Upton, Lisa A.; Riley, Pete; Lionello, Roberto; Török, Tibor; Titov, Viacheslav S.; Wijaya, Janvier; Druckmüller, Miloslav; Pasachoff, Jay M.; Carlos, Wendy Bibcode: 2018NatAs...2..913M Altcode: 2018NatAs.tmp..120M The total solar eclipse that occurred on 21 August 2017 across the United States provided an opportunity to test a magnetohydrodynamic model of the solar corona driven by measured magnetic fields. We used a new heating model based on the dissipation of Alfvén waves, and a new energization mechanism to twist the magnetic field in filament channels. We predicted what the corona would look like one week before the eclipse. Here, we describe how this prediction was accomplished, and show that it compared favourably with observations of the eclipse in white light and extreme ultraviolet. The model allows us to understand the relationship of observed features, including streamers, coronal holes, prominences, polar plumes and thin rays, to the magnetic field. We show that the discrepancies between the model and observations arise from limitations in our ability to observe the Sun's magnetic field. Predictions of this kind provide opportunities to improve the models, forging the path to improved space weather prediction. Title: Configuration of and Motions in the Solar Corona at the 2017 Total Solar Eclipse Authors: Pasachoff, Jay M.; Rusin, Vojtech; Vanur, Roman; Economou, Thanasis; Voulgaris, Aristeidis; Seiradakis, John H.; Seaton, Daniel; Dantowitz, Ronald; Lockwood, Christian A.; Nagle-McNaughton, Timothy; Perez, Cielo; Meadors, Erin N.; Marti, Connor J.; Yu, Ross; Rosseau, Brendan; Ide, Charles A.; Daly, Declan M.; Davis, Allen Bradford; Lu, Muzhou; Steele, Amy; Lee, Duane; Freeman, Marcus J.; Sliski, David; Rousseva, Ana; Greek Salem (Oregon) Team; Voulgaris, Aristeidis; Seiradakis, John Hugh; Koukioglou, Stavros; Kyriakou, Nikos; Vasileiadou, Anna; Greek Carbondale (Illinois) Team; Economou, Thanasis; Kanouras, Spyros; Irakleous, Christina; Golemis, Adrianos; Tsioumpanika, Nikoleta; Plexidas, Nikos; Tzimkas, Nikos; Kokkinidou, Ourania Bibcode: 2018AAS...23232510P Altcode: We report on high-contrast data reduction of white-light images from the August 21, 2017, total solar eclipse. We show the configuration of the solar corona at this declining phase of the solar-activity cycle, with the projection onto the plane of the sky of the three-dimensional coronal streamers plus extensive polar plumes. We discuss the relation of the white-light coronal loops visible in our observations with extreme-ultraviolet observations from NASA’s Solar Dynamics Observatory Atmospheric Imaging Assembly (AIA) and NOAA’s GOES-16 Solar Ultraviolet Imager (SUVI). We show differences and motions over a 65-minute interval between observations from our main site at Willamette University in Salem, Oregon, and a subsidiary site in Carbondale, Illinois. We discuss, in particular, a giant demarcation about 1 solar radius outward in the southwest that crosses the radial streamers.Our observations of the eclipse were sponsored in large part by the Committee for Research and Exploration of the National Geographic Society and by the Solar Terrestrial Program of the National Geographic Society. Additional support was received from the NASA Massachusetts Space Grant Consortium, the Sigma Xi honorary scientific society, the University of Pennsylvania (for DS), the Slovak Academy of Sciences VEGA project 2/0003/16, and the Freeman Foote Expeditionary and Brandi funds at Williams College. We thank Stephen Thorsett, Rick Watkins, and Honey Wilson of Willamette University for their hospitality. See http://totalsolareclipse.org or http://sites.williams.edu/eclipse/2017-usa/. Title: Simon Marius's Mundus Iovialis and the Discovery of the Moons of Jupiter Authors: Pasachoff, Jay M. Bibcode: 2018smhr.book..191P Altcode: Though the details of who was first to see the four major satellites of Jupiter are obscured by the mists of time, it seems that Simon Mayr (Marius) nearly simultaneously and independently discovered them and noted the discovery only 1 day after Galileo similarly discovered and noted it. The twin discoveries were confused by the use of different calendars by Marius and by Galileo, the former using the Julian calendar then still in use in Protestant regions and the latter using the new Gregorian calendar that was adopted in Catholic regions. Galileo was particularly sensitive to his priority, and the use of 1609 by Marius in the title of his Mundus Iovialis of 1614 raised particular ire, though adding the required 10 days for the conversion from O.S. to N.S. brought Marius's discovery into early 1610. In the long run, we now use the names that Marius gave—Io, Europa, Ganymede, and Callisto—to what are called the Galilean satellites. Title: Preparing a Nation for the Eclipse of a Generation - Authors: Speck, Angela; Habbal, Shadia; Tresch Fienberg, Richard; Kentrianakis, Michael; Fraknoi, Andrew; Nordgren, Tyler; Penn, Matthew; Pasachoff, Jay M.; Bakich, Michael; Winter, Henry; Gay, Pamela; Motta, Mario Bibcode: 2018AAS...23122002S Altcode: On August 21st 2017, there was a total solar eclipse visible from a vast swath of the US.In preparation for that event, the American Astronomical society created a taskforce charged with planning for the eclipse for the entire nation. The preparations included interfacing with the public, the media, non-profit organizations and governmental organizations. Preliminary data suggests that nearly 90% of American adults watched the eclipse either directly or via live streams. Moreover, there were no major problems associated with the event, in spite of valiant attempts from, e.g. imprope solar viewing materials. The eclipse offered opportunities for many scientific experiments within and ebyond astronomy. Here we present on the work of the taskforce, and the lessons learned as well as lesser known science experiments undertaken during the eclipse. Title: Early Science Results from the Williams College Eclipse Expedition Authors: Pasachoff, Jay M.; Person, Michael J.; Dantowitz, Ron; Lockwood, Christian A.; Nagle-McNaughton, Tim; Meadors, Erin N.; Perez, Cielo C.; Marti, Connor J.; Yu, Ross; Rosseau, Brendan; Daly, Declan M.; Ide, Charles A.; Davis, Allen B.; Lu, Muzhou; Sliski, David; Seiradakis, John; Voulgaris, Aris; Rusin, Vojtech; Peñaloza-Murillo, Marcos A.; Roman, Michael; Seaton, Daniel B.; Steele, Amy; Lee, Duane M.; Freeman, Marcus J. Bibcode: 2018AAS...23122006P Altcode: We describe our first cut of data reduction on a wide variety of observations of the solar corona and of the effect of the penumbra and umbra on the terrestrial atmosphere, carried out from our eclipse site on the campus of Willamette University in Salem, Oregon. Our team of faculty, undergraduate students, graduate students, and other colleagues observed the eclipse, taking images and spectra with a variety of sensors and telescopes. Equipment included frame-transfer cameras observing at 3 Hz in 0.3 nm filters at the coronal green and red lines to measure the power spectrum of oscillations in coronal loops or elsewhere in the lower corona; 3 spectrographs; a variety of telescopes and telephotos for white-light imaging; a double Lyot system tuned at Fe XIV 530.3 nm (FWHM 0.4 nm) and Fe X 637.4 nm (FWHM 0.5 nm); and a weather station to record changes in the terrestrial atmosphere. We are comparing our observations with predictions based on the previous mapping of the photospheric magnetic field, and preparing wide-field complete coronal imaging incorporating NOAA/NASA GOES-16 SUVI and NRL/NASA/LASCO for the corona outside our own images (which extend, given the completely clear skies we had, at least 4 solar radii), and NASA SDO/AIA and NOAA/NASA GOES-16 SUVI for the solar disk. One of our early composites appeared as Astronomy Picture of the Day for September 27: https://apod.nasa.gov/apod/ap170927.htmlOur expedition was supported in large part by grants from the Committee for Research and Exploration of the National Geographic Society and from the Solar Terrestrial Program of the Atmospheric and Geospace Sciences Division of the National Science Foundation, with additional student support from the STP/AGS of NSF, the NASA Massachusetts Space Grant Consortium, the Sigma Xi honorary scientific society, the Clare Booth Luce Foundation studentship and the Freeman Foote Expeditionary Fund at Williams College, other Williams College funds, and U. Pennsylvania funds. Title: First 2017-total-eclipse results from the Williams College team Authors: Pasachoff, J.; Dantowitz, R.; Rusin, V.; Seiradakis, J. H.; Voulgaris, A.; Seaton, D. B.; Davis, A. B.; Lu, M.; Sliski, D.; Ladd, E. F.; Economou, T.; Peñaloza-Murillo, M. A.; Nagle-McNaughton, T. Bibcode: 2017AGUFMSH13B2476P Altcode: We report on a wide range of observations we carried out during the total solar eclipse of August 21, 2017. Our main site was on the campus of Willamette University, Salem, Oregon, at which we had a variety of telescopes, spectrographs, cameras, a grism, and terrestrial-atmospheric measuring devices. Our goals included differentiating between models of coronal heating through measuring power-spectra of coronal loops in the [Fe XIV] and [Fe X] emission lines at multi-Hertz cadence with a frame-transfer CCD and otherwise; following coronal structure over the solar-activity cycle; comparing the results of a full-MHD prediction with actual coronal streamers; studying the dynamics of coronal plumes given the minimum phase of the solar-activity cycle; measuring the variation of the corona over the solar-activity cycle from our continuing measurements of the green-line/red-line intensity ratio; studying a variety of additional coronal emisson lines; high-resolution coronal imaging compared with overlapping images from space coronagraphs aboard SoHO and STEREO; comparing with AIA/SDO, HMO/SDO, SUVI/GOES-16, and SWAP/PROBA2 space images; and more. Our research has been supported in large part by grants from the Committee for Research and Exploration of the National Geographic Society and from the Solar Terrestrial Program of the Atmospheric and Geospace Sciences Division of the National Science Foundation, with additional support from Sigma Xi. Additional support for undergraduate participation came from the NSF, the NASA Massachusetts Space Grant Consortium, and the Clare Booth Luce Foundation, with travel support from the Freeman Foote Fund, the Rob Spring Fund, the Brandi Fund, and other sources at Williams College. Title: Pluto occultation on 2015 June 29 UTC with central flash and atmospheric spikes just before the New Horizons flyby Authors: Pasachoff, Jay M.; Babcock, Bryce A.; Durst, Rebecca F.; Seeger, Christina H.; Levine, Stephen E.; Bosh, Amanda S.; Person, Michael J.; Sickafoose, Amanda A.; Zuluaga, Carlos A.; Kosiarek, Molly R.; Abe, Fumio; Nagakane, Masayuki; Suzuki, Daisuke; Tristram, Paul J.; Arredondo, Anicia Bibcode: 2017Icar..296..305P Altcode: We observed the occultation by Pluto of a 12th magnitude star, one of the two brightest occultation stars ever in our dozen years of continual monitoring of Pluto's atmosphere through such studies, on 2015 June 29 UTC. At the Univ. of Canterbury Mt. John Observatory (New Zealand), under clear skies throughout, we used a POETS frame-transfer CCD at 10 Hz with GPS timing on the 1-m McLellan telescope as well as an infrared camera on an 0.6-m telescope and three-color photometry at a slower cadence on a second 0.6-m telescope. At the Auckland Observatory, we used a POETS and a PICO on 0.5-m and 0.4-m telescopes, with 0.4 s and 2 s cadences, respectively, obtaining ingress observations before clouds moved in. The Mt. John light curves show a central flash, indicating that we were close to the center of the occultation path. Analysis of our light curves show that Pluto's atmosphere remains robust. The presence of spikes at both sites in the egress and ingress shows atmospheric layering. We coordinated our observations with aircraft observations (Bosh et al., 2017) with the Stratospheric Observatory for Infrared Astronomy (SOFIA). Our chords helped constrain the path across Pluto that SOFIA saw. Our ground-based and airborne stellar-occultation effort came only just over two weeks of Earth days and two Pluto days before the flyby of NASA's New Horizons spacecraft. Title: Solar-system Education for the 2017 Total Solar Eclipse Authors: Pasachoff, Jay M. Bibcode: 2017DPS....4910103P Altcode: I describe an extensive outreach program about the Sun, the silhouette of the Moon, and the circumstances both celestial and terrestrial of the August 21, 2017, total solar eclipse. Publications included a summary of the last decade of solar-eclipse research for Nature Astronomy, a Resource Letter on Observing Solar Eclipses for the American Journal of Physics, and book reviews for Nature and for Phi Beta Kappa's Key Reporter. Symposia arranged include sessions at AAS, APS, AGU, and AAAS. Lectures include all ages from pre-school through elementary school to high school to senior-citizen residences. The work, including the scientific research about the solar corona that is not part of this abstract, was supported by grants from the Solar Terrestrial Program of the Atmospheric and Geospace Sciences Division of NSF and from the Committee for Research and Exploration of the National Geographic Society. Additional student support was received from NSF, NASA's Massachusetts Space Grant Consortium, the Honorary Research Society Sigma Xi, the Clare Booth Luce Foundation, and funds at Williams College. Title: Syzygy Information: Lunar Limb Profiles at Total Eclipses of the Decade Authors: Pasachoff, Jay M.; Jubier, Xavier; Wright, Ernest Bibcode: 2017DPS....4941717P Altcode: The topographic 3D mapping of the lunar surface by the Japanese Kaguya and NASA's Lunar Reconnaissance Orbiter has led to greatly improved predictions of Baily's beads at total solar eclipses. This information has been included in the program Solar Eclipse Maestro. Matching the predictions with observations of Baily's beads made at total solar eclipses, including the 21 August 2017 eclipse as well as previous total and annular eclipses, may even improve the accuracy of the solar diameter used as a standard by the International Astronomical Union. Title: The 2016 Transit of Mercury and the Solar Parallax Authors: Pasachoff, Jay M.; Backhaus, Udo; Gährken, Bernd; Schneider, Glenn Bibcode: 2017DPS....4920004P Altcode: We observed the 9 May 2016 transit of Mercury with the 1.6-m New Solar Telescope of the Big Bear Solar Observatory of the New Jersey Institute of Technology in California and with smaller telescopes in Germany. The solar granulation behind the silhouette of Mercury can be aligned, showing Mercury's parallax. From these observations, the value of the solar parallax can be determined, showing historical parallels. As a second method of making the parallactic shift of Mercury visible and the distance to the sun measurable, we aligned photos taken with telescopes of shorter focal lengths, for instance, by using the prominent sunspots. Title: Heliophysics at total solar eclipses Authors: Pasachoff, Jay M. Bibcode: 2017NatAs...1E.190P Altcode: Observations during total solar eclipses have revealed many secrets about the solar corona, from its discovery in the 17th century to the measurement of its million-kelvin temperature in the 19th and 20th centuries, to details about its dynamics and its role in the solar-activity cycle in the 21st century. Today's heliophysicists benefit from continued instrumental and theoretical advances, but a solar eclipse still provides a unique occasion to study coronal science. In fact, the region of the corona best observed from the ground at total solar eclipses is not available for view from any space coronagraphs. In addition, eclipse views boast of much higher quality than those obtained with ground-based coronagraphs. On 21 August 2017, the first total solar eclipse visible solely from what is now United States territory since long before George Washington's presidency will occur. This event, which will cross coast-to-coast for the first time in 99 years, will provide an opportunity not only for massive expeditions with state-of-the-art ground-based equipment, but also for observations from aloft in aeroplanes and balloons. This set of eclipse observations will again complement space observations, this time near the minimum of the solar activity cycle. This review explores the past decade of solar eclipse studies, including advances in our understanding of the corona and its coronal mass ejections as well as terrestrial effects. We also discuss some additional bonus effects of eclipse observations, such as recreating the original verification of the general theory of relativity. Title: First Results from the August 21, 2017, Total Solar Eclipse Authors: Pasachoff, Jay M. Bibcode: 2017SPD....4820803P Altcode: I report on the observations planned and, weather permitting, made from our site in Salem, Oregon, at the August 21, 2017, total solar eclipse. I also give a first report on collaborators' successes, including Megamovie and simultaneous space observations. We also describe our participation in PBS's NOVA on the eclipse that was to be aired on public television on eclipse night. Our eclipse expedition is supported in large part by grants from the Solar Terrestrial Program of the Atmospheric Sciences Division of NSF and by the Committee for Research and Exploration of the National Geographic Society. Title: Results from and Plans for the Two 2017 Solar Eclipses Authors: Pasachoff, Jay M.; Seaton, Daniel; Kentrianakis, Michael; Fischer, Daniel Bibcode: 2017AAS...23030106P Altcode: At this writing fresh from observing the 26 February 2017 annular solar eclipse in exceptionally clear sky from sites in Patagonia, Argentina, we show images from the centerline near Facundo showing Baily's beads and central annularity of the magnitude 99.3% eclipse. From close to the edge of the path from sites north of Facundo within the northern limit (images by Daniel Fischer) and north of Sarmiento at the southern limit (images by Jörg Schoppmeyer), we show unfiltered images that show substantial solar chromosphere with innermost corona above it. We also show SWAP and SDO eclipse images.For the 21 August 2017 total solar eclipse, we describe our plans for observing coronal structure above the limb from the ground in Oregon and for ultraviolet imaging on the solar disk at the time of the terrestrial eclipse through six filters using the new Solar Ultraviolet Imager (SUVI) on the National Oceanic and Atmospheric Administration's GOES-16 spacecraft, planned along with three similar spacecraft for coronal coverage for the next two decades. SUVI has the biggest overlapping field of view, 53 arcmin square, of any multi-channel space-based EUV imager.Our research on the 2017 total solar eclipse is supported by grants from the Committee for Research and Exploration of the National Geographic Society and from the Solar Terrestrial Program of the Atmospheric and Geospace Sciences Division of the National Science Foundation. NOAA NCEI are the acronyms for the National Oceanic and Atmospheric Administration's National Centers for Environmental Information. Title: Books and Other Resources for Education about the August 21, 2017, Solar Eclipse Authors: Pasachoff, Jay M.; Fraknoi, Andrew; Kentrianakis, Michael Bibcode: 2017AAS...23010804P Altcode: As part of our work to reach and educate the 300+ million Americans of all ages about observing the August 21 solar eclipse, especially by being outdoors in the path of totality but also for those who will see only partial phases, we have compiled annotated lists of books, pamphlets, travel guides, websites, and other information useful for teachers, students, and the general public and made them available on the web, at conferences, and through webinars. Our list includes new eclipse books by David Barron, Anthony Aveni, Frank Close, Tyler Nordgren, John Dvorak, Michael Bakich, and others. We list websites accessible to the general public including those of the International Astronomical Union Working Group on Eclipses (http://eclipses.info, which has links to all the sites listed below); the AAS Eclipse 2017 Task Force (http://eclipse2017.aas.org); NASA Heliophysics (http://eclipse.nasa.gov); Fred Espenak (the updated successor to his authoritative "NASA website": http://EclipseWise.com); Michael Zeiler (http://GreatAmericanEclipse.com); Xavier Jubier (http://xjubier.free.fr/en/site_pages/solar_eclipses/); Jay Anderson (meteorology: http://eclipsophile.com); NASA's Eyes (http://eyes.nasa.gov/eyes-on-eclipse.html and its related app); the Astronomical Society of the Pacific (http://www.astrosociety.org/eclipse); Dan McGlaun (http://eclipse2017.org/); Bill Kramer (http://eclipse-chasers.com). Specialized guides include Dennis Schatz and Andrew Fraknoi's Solar Science for teachers (from the National Science Teachers Association:http://www.nsta.org/publications/press/extras/files/solarscience/SolarScienceInsert.pdf), and a printing with expanded eclipse coverage of Jay Pasachoff's, Peterson Field Guide to the Stars and Planets (14th printing of the fourth edition, 2016: http://solarcorona.com).A version of our joint list is to be published in the July issue of the American Journal of Physics as a Resource Letter on Eclipses, adding to JMP's 2010, "Resource Letter SP-1 on Solar Physics," AJP, 78, September, 890-901. Title: Astronomy: An all-American eclipse Authors: Pasachoff, Jay Bibcode: 2017Natur.545..409P Altcode: Jay Pasachoff enjoys four books heralding this summer's US total solar eclipse. Title: Educating the Public about the 2017 Total Solar Eclipse Authors: Pasachoff, Jay M. Bibcode: 2017AAS...22941103P Altcode: On behalf of the International Astronomical Union's Working Group on Solar Eclipses, I have long worked to bring knowledge about eclipses and how to observe the safely to the people of the various countries from which partial, annular, or total solar eclipses are visible. In 2017, we have first a chance to educate the people of South America on the occasion of the February 26 annular eclipse through southern Chile and Argentina that is partial throughout almost the entire continent (and an eclipse workshop will be held February 22-24 in Esquel, Argentina: http://sion.frm.utn.edu.ar/WDEAII) and then a chance to educate the 300 million people of the United States and others in adjacent countries as far south as northern South America about the glories of totality and how to observe partial phases. Our website, a compendium of links to information about maps, safe observing, science, and more is at http://eclipses.info. We link to important mapping sites at EclipseWise.com, GreatAmericanEclipse.com, and http://xjubier.free.fr/en/site_pages/solar_eclipses/xSE_GoogleMap3.php?Ecl=+20170821&Acc=2&Umb=1&Lmt=1&Mag=1&Max=1, and information about cloudiness statistics at http://eclipsophile.com, as well as simulation sites at https://svs.gsfc.nasa.gov/cgi-bin/details.cgi?aid=4314 and http://eyes.jpl.nasa.gov. The American Astronomical Society's task force on the 2017 eclipse has a website at http://eclipse.aas.org. We are working to disseminate accurate information about how and why to observe the total solar eclipse, trying among other things to head off common misinformation about the hazards of looking at the sun at eclipses or otherwise. About 12 million Americans live within the 70-mile-wide band of totality, and we encourage others to travel into it, trying to make clear the difference between even a 99% partial eclipse and a total eclipse, with its glorious Baily's beads, diamond rings, and totality that on this occasion lasts between 2 minutes and 2 minutes 40 seconds on the centerline. Our research on the 2017 total solar eclipse is supported by grants from the Committee for Research and Exploration of the National Geographic Society and from the Solar Terrestrial Program of the Atmospheric and Geospace Sciences Division of the National Science Foundation. Title: The solar corona through the sunspot cycle: preparing for the August 21, 2017, total solar eclipse Authors: Pasachoff, Jay M.; Seaton, Daniel; Rusin, Vojtech Bibcode: 2017AAS...22932502P Altcode: We discuss the evolution of the solar corona as seen at eclipses through the solar-activity cycle. In particular, we discuss the variations of the overall shape of the corona through the relative proportions of coronal streamers at equatorial and other latitudes vs. polar plumes. We analyze the two coronal mass ejections that we observed from Gabon at the 2013 total solar eclipse and how they apparently arose from polar crown filaments, one at each pole. We describe the change in the Ludendorff flattening index from solar maximum in one hemisphere as of the 2013 eclipse through the 2015 totality's corona we observed from Svalbard and, with diminishing sunspot and other magnetic activity in each hemisphere, through the 2016 corona we observed from Ternate, Indonesia.We discuss our observational plans for the August 21, 2017, total solar eclipse from our main site in Salem, Oregon, and subsidiary sites in Madras, OR; Carbondale, IL; and elsewhere, our main site chosen largely by its favorable rating in cloudiness statistics. We discuss the overlapping role of simultaneous spacecraft observations, including those expected not only from NASA's SDO, ESA's SWAP on PROBA2, and NRL/NASA/ESA's LASCO on SOHO but also from the new SUVI (Solar Ultraviolet Imager) aboard NOAA's GOES-R satellite, scheduled as of this writing to have been launched by the time of this January 2017 meeting.Our research on the 2013 and 2015 total solar eclipses was supported by grants from the Committee for Research and Exploration of the National Geographic Society (NG-CRE). Our research on the 2017 total solar eclipse is supported by both NG-CRE and the Solar Terrestrial Program of the Atmospheric and Geospace Sciences Division of the National Science Foundation. Title: The Astrophysics of the Solar Corona at the August 21, 2017, American Total Solar Eclipse Authors: Pasachoff, Jay Bibcode: 2017APS..APR.Y3008P Altcode: The first total solar eclipse to cross the United States from coast to coast in 99 years will occur on August 21, 2017, with a 70-mile-wide path of totality from Oregon to South Carolina, with cloudiness statistics more favorable in the northwest than in the southeast. I will discuss a series of observations of the solar corona made during recent solar eclipses and related spacecraft observations. I will further discuss plans for using the 2017 eclipse for furthering our studies of the heating of the solar corona to millions of kelvins, of the dynamics of coronal mass ejections and polar plumes, and of the response of the corona to the solar magnetic field. I will conclude by discussing public-education plans for the eclipse, during which the whole U.S., Mexico, Central America, and Canada will enjoy a partial eclipse. My work at solar eclipses has recently been supported by the NSF and the Committee for Research and Exploration of the National Geographic Society, and I thank them both for research grants for our scientific studies of the 2017 total eclipse, including AGS-1602461 from the NSF and 987816 from National Geographic. Title: Measuring Bent Starlight Authors: Pasachoff, Jay Bibcode: 2016S&T...132f...6P Altcode: No abstract at ADS Title: Simon Marius vs. Galileo: Who First Saw Moons of Jupiter? Authors: Pasachoff, Jay M.; Van Helden, Albert Bibcode: 2016DPS....4831206P Altcode: In his almanac for 1612 and book Mundus Iovalis of 1614, Simon Marius in Germany reported his discovery of moons around Jupiter, which he started writing down in late 1609 in the Julian calendar, which translated to 8 January 1610 in the Gregorian calendar in use by Galileo in Italy. Is Marius to be believed? Galileo certainly did not. But a Dutch jury of experts about three hundred years later reported that they validated the claim that Marius independently discovered the moons of Jupiter one day after Galileo first both saw and wrote down his discovery! There is no doubt that the names Io, Europa, Ganymede, and Callisto came from Marius (to whom they were suggested by Kepler). See JMP's Journal for the History of Astronomy article, 46(2), 218-234 (2015).Marius wrote that he had been observing the moons around Jupiter since November 1609 (Julian), using a neighboring nobleman's telescope, which would mean that he actually saw the Jupiter satellites first (though publish or perish). Whether this feat was technically possible comes down to discussions of the capabilities of telescopes in the early 17th century.The quadricentennial of Marius's book was celebrated in Nuremberg with a symposium that is now in press in German with an English translation expected. One of us (AVH) has recently prepared a complete English translation of Marius's book, superseding the partial translation made 100 years ago. There is no evidence that, whether he saw what we now call the Galilean satellites first or not, Marius appreciated their cosmological significance the way that Galileo soon did. And Marius was certainly the first to publish tables of the moons of Jupiter.We thank the Chapin Library of Williams College and the Huntington Library for assistance with first editions of Marius's 1614 book, and we thank Pierre Leich of the Simon Marius Gesellschaft for his consultations. Title: The 2016 Transit of Mercury Observed from Major Solar Telescopes and Satellites Authors: Pasachoff, Jay M.; Schneider, Glenn; Gary, Dale; Chen, Bin; Sterling, Alphonse C.; Reardon, Kevin P.; Dantowitz, Ronald; Kopp, Greg A. Bibcode: 2016DPS....4811705P Altcode: We report observations from the ground and space of the 9 May 2016 transit of Mercury. We build on our explanation of the black-drop effect in transits of Venus based on spacecraft observations of the 1999 transit of Mercury (Schneider, Pasachoff, and Golub, Icarus 168, 249, 2004). In 2016, we used the 1.6-m New Solar Telescope at the Big Bear Solar Observatory with active optics to observe Mercury's transit at high spatial resolution. We again saw a small black-drop effect as 3rd contact neared, confirming the data that led to our earlier explanation as a confluence of the point-spread function and the extreme solar limb darkening (Pasachoff, Schneider, and Golub, in IAU Colloq. 196, 2004). We again used IBIS on the Dunn Solar Telescope of the Sacramento Peak Observatory, as A. Potter continued his observations, previously made at the 2006 transit of Mercury, at both telescopes of the sodium exosphere of Mercury (Potter, Killen, Reardon, and Bida, Icarus 226, 172, 2013). We imaged the transit with IBIS as well as with two RED Epic IMAX-quality cameras alongside it, one with a narrow passband. We show animations of our high-resolution ground-based observations along with observations from XRT on JAXA's Hinode and from NASA's Solar Dynamics Observatory. Further, we report on the limit of the transit change in the Total Solar Irradiance, continuing our interest from the transit of Venus TSI (Schneider, Pasachoff, and Willson, ApJ 641, 565, 2006; Pasachoff, Schneider, and Willson, AAS 2005), using NASA's SORCE/TIM and the Air Force's TCTE/TIM. See http://transitofvenus.info and http://nicmosis.as.arizona.edu.Acknowledgments: We were glad for the collaboration at Big Bear of Claude Plymate and his colleagues of the staff of the Big Bear Solar Observatory. We also appreciate the collaboration on the transit studies of Robert Lucas (Sydney, Australia) and Evan Zucker (San Diego, California). JMP appreciates the sabbatical hospitality of the Division of Geosciences and Planetary Sciences of the California Institute of Technology, and of Prof. Andrew Ingersoll there. The solar observations lead into the 2017 eclipse studies, for which JMP is supported by grants from the NSF AGS and National Geographic CRE. Title: Implications of the Central Flash Analysis from the 2015 Pluto Stellar Occultation Authors: Person, Michael J.; Bosh, Amanda S.; Sickafoose, Amanda A.; Zuluaga, Carlos; Levine, Stephen; Pasachoff, Jay M.; Babcock, Bryce A.; Dunham, Edward W.; McLean, Ian S.; Wolf, Juergen; Abe, F.; Becklin, Eric E.; Bida, Thomas A.; Bright, Leonard P.; Brothers, Tim; Christie, Grant; Collins, Peter; Durst, Rebecca; Gilmore, Alan; Hamilton, Ryan T.; Harris, Hugh C.; Johnson, Christian I.; Kilmartin, Pam; Kosiarek, Molly; Leppik, Karina; Logsdon, Sarah E.; Lucas, Robert; Mathers, Shevill; Morley, Caroline; Natusch, T.; Nelson, P.; Ngan, H.; Pfueller, E.; Roeser, H. -P.; Sallum, Stephanie; Savage, Maureen L.; Seeger, Christina; Chit Siu, Ho; Stockdale, Christopher; Suzuki, D.; Thanathibodee, T.; Tilleman, T.; Tristam, P. J.; Van Cleve, Jeffrey E.; Varughese, C.; Weisenbach, Luke; Widen, E.; Wiedemann, M. Bibcode: 2016DPS....4822404P Altcode: Two weeks before the historic New Horizons flyby of Pluto, a stellar occultation was observed from Australia and New Zealand (Bosh et al., 2016, Pasachoff et al., 2016, Sicardy et al., 2016). Prior to these observations, an extensive astrometric campaign (Bosh et al., this meeting) was conducted to carefully place the SOFIA aircraft within the central flash region of the occultation shadow. Multiple central flash chords were obtained and initial analysis indicated global asymmetry of Pluto's atmosphere (Person et al., 2015).Further analysis of these chords reveals asymmetries in Pluto's atmosphere stronger than those previously observed by either central flash measurements or occultation shadow fitting (Person et al., 2006, Olkin et al., 2014). Here we will discuss this revealed atmospheric asymmetry in terms of the bulk atmospheric movements necessary to cause distortions of this order, given the extreme surface sphericity seen by New Horizons (Nimmo et al., 2016), and its implications for surface ice transport scenarios (Hansen et al., 2015), and Pluto's seasonal evolution (Earle et al., 2015). Title: The thermal field of the terminator mesosphere of Venus using solar transit data Authors: Tanga, Paolo; Widemann, Thomas; Pere, Christophe; Babcock, Brice A.; Berthier, Jerome; Pasachoff, Jay M.; Roos-Serote, Maarten Bibcode: 2016DPS....4811509T Altcode: We exploit the solar transits of Venus in 2004 and 2012, to derive useful constraints on the mesosphere of the planet by the observation of the so-called "aureole" resulting from direct sunlight refraction. In 2012 we organized an extensive campaign, involving observations through both space- and ground- based telescopes. A specific design adapted from the Lyot coronograph was developed and replicated in several copies to improve the SNR in proximity of the solar disk (Venus Twilight Experiment).we report on the different data sets collected during the 2012 transit, and present lightcurve analyses based on imaging from NASA's Solar Dynamic Observatory (SDO), JAXA's Hinode, and by the instruments of the Venus Twilight Experiment.We explored different approaches to model the variation of the aureole brightness, ranging from simple isothermal modeling to multi-layer.Although less resolved than the local measurements obtained by Venus Express (SOIR experiment), aureole modeling has the advantage of being able to cover simultaneously a wide range of latitudes. We were able to compare the aureole-derived vertical refractivity profiles to density profiles obtained simultaneously by SOIR during the transit itself. Our inverse model, constraining the vertical temperature profiles at all latitudes, detects a cold layer (at ~86-94 km altitude on average) whose vertical extent depends on latitude (thicker towards the N pole than at the Equator), and a latitude-dependent aerosol slanted-opacity altitude (τ=1).Eventually our model shows that a relevant contribution to the aureole flux comes from deep layers where aerosol absorption cannot be neglected, allowing us to put some constraints on the scale height of aerosol dispersion. Title: First Report on the 2016 March 9 Total Solar Eclipse Observations Authors: Pasachoff, Jay M. Bibcode: 2016AAS...22831105P Altcode: Totality swept across Indonesia and into the Pacific on 2016 March 9, lasting up to 2 min 45 s on Ternate in the Spice Islands (Malukus). I provide a first report on our observations. Our scientific goal is to follow changes in the corona over the solar-activity cycle, now past its 2012 and 2014 double peak, and to measure temporal changes in the corona on the scale of minutes or hours by comparing eclipse observations made at several sites along the path. I also discuss the near-simultaneous coronal observations made with SOHO/LASCO, SDO/AIA, STEREO/SECCHI, PROBA2/SWAP, and Hinode XRT.For the forthcoming 2017 eclipse, we acknowledge grants to JMP and Williams College from the Solar Terrestrial Program of the Atmospheric and Geospace Sciences Division of the National Science Foundation and from the Committee for Research and Exploration of the National Geographic Society. Title: Public Education Plans for the 2017 August 21 Total Solar Eclipse Authors: Pasachoff, Jay M. Bibcode: 2016AAS...22811201P Altcode: A total solar eclipse will cross the continental United States on 2017 August 21, the first such in 99 years and the first whose path of totality on land is entirely in the United States since 1776. People in the rest of the United States-as well as in Canada, Central America, and northern South America-will have a partial solar eclipse. Totality will range up to about 70 km in diameter, and will be visible from a path that extends from Oregon to South Carolina. Cloudiness statistics based on decades on satellite infrared imaging are more favorable for western sites. The sun's diameter will be 80% covered in Miami (south of totality) and New York (north of totality), and 70% covered in Los Angeles (south of totality). For the Working Group on Solar Eclipses of the International Astronomical Union, I maintain a website at http://eclipses.info that provides links to a wide variety of eclipse-related material and to useful websites run by others.Prior to this total eclipse, annular eclipses will cross Africa (from Gabon to Tanzania and Madagascar) and Isle de la Réunion on 2016 September 1, and Chile and Argentina on 2017 February 26, at which time we plan an eclipse workshop in Esquel, Argentina.For the forthcoming 2017 eclipse, we acknowledge grants to JMP and Williams College from the Solar Terrestrial Program of the Atmospheric and Geospace Sciences Division of the National Science Foundation and from the Committee for Research and Exploration of the National Geographic Society. Title: Early Evaluation of the Corona at the 2016 March 9 Total Solar Eclipse Authors: Pasachoff, Jay M.; Seaton, Daniel B.; Sterling, Alphonse C. Bibcode: 2016SPD....47.0326P Altcode: We observed the corona on 2016 March 9 with a variety of assets on the ground and in space. The umbra of the total eclipse swept across Indonesia and into the Pacific, with totality at our Indonesian observation sites lasting 2 min 45 s at Ternate in the Spice Islands (Malukus) and 2 min 10 at Belitung. We compare our ground-based results with the coronal configurations observed with PROBA2/SWAP and Hinode XRT. One of our scientific goals is to follow the coronal configuration over the solar-activity cycle, with the sunspot number now half its maximum of either its 2012 or 2014 peak. We are evaluating temporal changes by comparing eclipse observations made at several ground-based sites along the path, with the longest span being 75 min from Belitung to the Woleia atoll in mid-Pacific, 1:25 UTC to 2:40 UTC; we are evaluating whether the airborne observations made at 3:35 UTC on March 8 (across the International Dateline) are of suitable quality to provide further comparison at high spatial resolution. We also compare our images with the near-simultaneous coronal observations made with SOHO/LASCO, SDO/AIA, STEREO-A/SECCHI, and the Mauna Loa Solar Observatory's K-cor coronagraph. ACS received support for image analysis from the Hinode project. Title: C46 `ASTRONOMY Education and Development': a Peculiar Commission Authors: de Greve, Jean-Pierre; García, Beatriz; Gerbaldi, Michèle; Ferlet, Roger; Guinan, Edward; Hearnshaw, John; Jones, Barrie; Marschall, Laurence; Miley, George; Pasachoff, Jay; Ros, Rosa; Stavinschi, Magda; Torres-Peimbert, Silvia Bibcode: 2016IAUTA..29..205D Altcode: C46 was a Commission of the Executive Committee of the IAU under Division XII (Union-Wide Activities), then after 2012 under Division C (Education, Outreach, and Heritage). It was the only commission dealing exclusively with astronomy education; a previous Commission 38 (Exchange of Astronomers), which allocated travel grants to astronomers who needed them, and a Working Group on the Worldwide Development of Astronomy, have been absorbed by Commission 46. Title: Trio of Stellar Occultations by Pluto One Year Prior to New Horizons' Arrival Authors: Pasachoff, Jay M.; Person, Michael J.; Bosh, Amanda S.; Sickafoose, Amanda A.; Zuluaga, Carlos; Kosiarek, Molly R.; Levine, Stephen E.; Osip, David J.; Schiff, Avery; Seeger, Christina H.; Babcock, Bryce A.; Rojo, Patricio; Servajean, Elise Bibcode: 2016AJ....151...97P Altcode: We observed occultations by Pluto during a predicted series of events in 2014 July with the 1 m telescope of the Mt. John Observatory in New Zealand. The predictions were based on updated astrometry obtained in the previous months at the USNO, CTIO, and Lowell Observatories. We successfully detected occultations by Pluto of an R = 18 mag star on July 23 (14:23:32 ± 00:00:04 UTC to 14:25:30 ± 00:00:04 UTC), with a drop of 75% of the unocculted stellar signal, and of an R = 17 star on July 24 (11:41:30 ± 00:00:08 UTC to 11:43:28 ± 00:00:08 UTC), with a drop of 80% of the unocculted stellar signal, both with 20 s exposures with our frame-transfer Portable Occultation, Eclipse, and Transit System. Since Pluto had a geocentric velocity of 22.51 km s-1 on July 23 and 22.35 km s-1 on July 24, these intervals yield limits on the chord lengths (surface and lower atmosphere) of 2700 ± 130 km and 2640 ± 250 km, respectively, indicating that the events were near central, and therefore provide astrometric constraints on the prediction method. Our coordinated observations with the 4 m AAT in Australia on July 23 and the 6.5 m Magellan/Clay on Las Campanas, the 4.1 m Southern Astrophysical Research Telescope on Cerro Pachön, the 2.5 m DuPont on Las Campanas (LCO), the 0.6 m SARA-South on Cerro Tololo of the Southeastern Association for Research in Astronomy (SARA), the MPI/ESO 2.2 m on La Silla, and the 0.45 m Cerro Calán telescope and 0.36 telescope in Constitución in Chile on July 27 and 31, which would have provided higher-cadence observations for studies of Pluto’s atmosphere, were largely foiled by clouds, but led to detection with the LCO Magellan/Clay and DuPont Telescopes on July 31 of the grazing occultation of a previously unknown 15th-magnitude star, completing the trio of occultations successfully observed and reported in this paper. Title: The Solar Eclipse Mural Series by Howard Russell Butler Authors: Pasachoff, J. M.; Olson, R. J. M. Bibcode: 2016ASPC..501...13P Altcode: There is a rich trove of astronomical phenomena in works of art by artists from the greater New York area, a trend that is even more pronounced in the oeuvres of New York City residents through the present day. A case in point is the trio of oil paintings by artist (and former physics professor) Howard Russell Butler depicting total solar eclipses in 1918, 1923, and 1925 that are based on his own observations. They were long displayed in the former art-deco building of the Hayden Planetarium of the American Museum of Natural History, the location of this conference. (The Museum also has nine other Butler paintings, none of which are currently exhibited.) Since the eclipse paintings have been in storage for many years, these once famous works are now virtually forgotten. Based on our research as an astronomer who has seen sixty-two solar eclipses and an art historian who has written extensively about astronomical imagery, we will discuss Butler's Solar Eclipse Triptych to explore its place in the history of astronomical imaging. Title: Structure, Dynamics, and Spectra of the Solar Corona at the 2013 and 2015 Total Eclipses and Plans for 2017's American Totality Authors: Pasachoff, Jay M.; Dantowitz, Ronald; Voulgaris, Aristeidis Bibcode: 2016AAS...22712502P Altcode: We observed the total solar eclipses of 3 November 2013 from Gabon and of 20 March 2015 from Svalbard in clear skies with cameras to image the solar corona at high resolution and with spectrographs for coronal emission lines. We report on the composite images showing coronal structure and (in comparison with other sites' images) dynamics, as well as the relation of our inner- and middle-corona composite images with surface EUV images from SDO and SWAP and with the outer-corona images from the coronagraphs on SOHO/LASCO. Our spectra show not only the common forbidden lines of Fe XIV (green line) and Fe X (red line) but also rarer species such as Ca XV. Finally, we describe our planned suite of observations for the 21 August 2017 solar eclipse, whose path of totality will cross the United States from Pacific to Atlantic, with more-favorable cloudiness statistics for western sites.Our Gabon and Svalbard expeditions were supported by grants from the Committee for Research and Exploration of the National Geographic Society. Title: Occultation Evidence for Haze in Pluto's Atmosphere in 2015 at the New Horizons Encounter Authors: Bosh, A. S.; Person, M. J.; Zuluaga, C.; Sickafoose, A. A.; Levine, S. E.; Pasachoff, J. M.; Babcock, B. A.; Dunham, E. W.; McLean, I.; Wolf, J.; Abe, F.; Becklin, E.; Bida, T. A.; Bright, L. P.; Brothers, T.; Christie, G.; Collins, P. L.; Durst, R. F.; Gilmore, A. C.; Hamilton, R.; Harris, H. C.; Johnson, C.; Kilmartin, P. M.; Kosiarek, M. R.; Leppik, K.; Logsdon, S.; Lucas, R.; Mathers, S.; Morley, C. J. K.; Natusch, T.; Nelson, P.; Ngan, H.; Pfüller, E.; Röser, H. P.; Sallum, S.; Savage, M.; Seeger, C. H.; Siu, H.; Stockdale, C.; Suzuki, D.; Thanathibodee, T.; Tilleman, T.; Tristram, P. J.; Van Cleve, J.; Varughese, C.; Weisenbach, L. W.; Widen, E.; Wiedemann, M. Bibcode: 2015AGUFM.P54A..07B Altcode: On UT 29 June 2015, the occultation by Pluto of a bright star (r'=11.9) was observed from the Stratospheric Observatory for Infrared Astronomy (SOFIA) as well as several ground-based stations in New Zealand and Australia. Pre-event astrometry allowed for an in-flight update to the SOFIA team with the result that SOFIA was deep within the central flash zone. Combined analysis of the data sets leads to the result that Pluto's middle atmosphere is essentially unchanged from 2011 and 2013 (Person et al. 2013; Bosh et al. 2015); there has been no significant expansion or contraction of the atmosphere. Additionally, we find that a haze component in the atmosphere is required to reproduce the light curves obtained. This haze scenario has implications for understanding the photochemistry of Pluto's atmosphere. This work was supported by NASA grants NNX15AJ82G (Lowell Observatory), NNX10AB27G (MIT), and NNX12AJ29G (Williams), and by the National Research Foundation of South Africa. Co-authors were visiting observers on SOFIA, at the Keck Observatory, the Magellan Observatory, the SARA-CT Observatory, the Mt. John University Observatory, and the Auckland Observatory. Title: Ground-based Light Curves Two Pluto Days Before the New Horizons Passage Authors: Bosh, A. S.; Pasachoff, J. M.; Babcock, B. A.; Durst, R. F.; Seeger, C. H.; Levine, S. E.; Abe, F.; Suzuki, D.; Nagakane, M.; Sickafoose, A. A.; Person, M. J.; Zuluaga, C.; Kosiarek, M. R. Bibcode: 2015AGUFM.P51A2048B Altcode: We observed the occultation of a 12th magnitude star, one of the two brightest occultation stars ever in our dozen years of continual monitoring of Pluto's atmosphere through such studies, on 29 June 2015 UTC. At Canterbury University's Mt. John University Observatory on the south island of New Zealand, in clear sky, we used our POETS frame-transfer CCD at 10 Hz with GPS timing on the 1-m McLellan telescope as well as an infrared camera on an 0.6-m telescope and three-color photometry at a slower cadence on a second 0.6-m telescope. The light curves show a central flash, indicating that we were close to the center of the occultation path, and allowing us to explore Pluto's atmosphere lower than usual. The light curves show that Pluto's atmosphere remained robust. Observations from 0.5- and 0.4-m telescopes at the Auckland Observatory gave the first half of the occultation before clouds came in. We coordinated our observations with aircraft observations with NASA's Stratospheric Observatory for Infrared Astronomy (SOFIA) and its High Speed Imaging Photometer for Occultations (HIPO). Our ground-based and airborne stellar-occultation effort came only just over two weeks of Earth days and two Pluto days (based on Pluto's rotational period) before the flyby of NASA's New Horizons spacecraft, meaning that the mission's exquisite snapshot of Pluto's atmosphere can be placed in the context of our series of ground-based occultation observations carried out on a regular basis since 2002 following a first Pluto occultation observed in 1988 from aloft. Our observations were supported by NASA Planetary Astronomy grants NNX12AJ29G to Williams College, NNX15AJ82G to Lowell Observatory, and NNX10AB27G to MIT, and by the National Research Foundation of South Africa. We thank Alan Gilmore, Pam Kilmartin, Robert Lucas, Paul Tristam, and Carolle Varughese for assistance at Mt. John. Title: Investigation of particle sizes in Pluto's atmosphere from the 29 June 2015 occultation Authors: Sickafoose, Amanda A.; Bosh, A. S.; Person, M. J.; Zuluaga, C. A.; Levine, S. E.; Pasachoff, J. M.; Babcock, B. A.; Dunham, E. W.; McLean, I.; Wolf, J.; Abe, F.; Bida, T. A.; Bright, L. P.; Brothers, T.; Christie, G.; Collins, P. L.; Durst, R. F.; Gilmore, A. C.; Hamilton, R.; Harris, H. C.; Johnson, C.; Kilmartin, P. M.; Kosiarek, M. R.; Leppik, K.; Logsdon, S.; Lucas, R.; Mathers, S.; Morley, C. J. K.; Natusch, T.; Nelson, P.; Ngan, H.; Pfüller, E.; de, H. -P.; Sallum, S.; Savage, M.; Seeger, C. H.; Siu, H.; Stockdale, C.; Suzuki, D.; Thanathibodee, T.; Tilleman, T.; Tristam, P. J.; Van Cleve, J.; Varughese, C.; Weisenbach, L. W.; Widen, E.; Wiedemann, M. Bibcode: 2015DPS....4710504S Altcode: The 29 June 2015 observations of a stellar occultation by Pluto, from SOFIA and ground-based sites in New Zealand, indicate that haze was present in the lower atmosphere (Bosh et al., this conference). Previously, slope changes in the occultation light curve profile of Pluto’s lower atmosphere have been attributed to haze, a steep thermal gradient, and/or a combination of the two. The most useful diagnostic for differentiating between these effects has been observing occultations over a range of wavelengths: haze scattering and absorption are functions of particle size and are wavelength dependent, whereas effects due to a temperature gradient should be largely independent of observational wavelength. The SOFIA and Mt. John data from this event exhibit obvious central flashes, from multiple telescopes observing over a range of wavelengths at each site (Person et al. and Pasachoff et al., this conference). SOFIA data include Red and Blue observations from the High-speed Imaging Photometer for Occultations (HIPO, at ~ 500 and 850 nm), First Light Infrared Test Camera (FLITECAM, at ~1800 nm), and the Focal Plan Imager (FPI+, at ~ 600 nm). Mt. John data include open filter, g', r', i', and near infrared. Here, we analyze the flux at the bottom of the light curves versus observed wavelength. We find that there is a distinct trend in flux versus wavelength, and we discuss applicable Mie scattering models for different particle size distributions and compositions (as were used to characterize haze in Pluto's lower atmosphere in Gulbis et al. 2015).SOFIA is jointly operated by the Universities Space Research Association, Inc. (USRA), under NASA contract NAS2-97001, and the Deutsches SOFIA Institut (DSI) under DLR contract 50 OK 0901 to the University of Stuttgart. Support for this work was provided by the National Research Foundation of South Africa, NASA SSO grants NNX15AJ82G (Lowell Observatory), PA NNX10AB27G (MIT), and PA NNX12AJ29G (Williams College), and the NASA SOFIA Cycle 3 grant NAS2-97001 issued by USRA. Title: The Lunar Profile and Baily's Beads at Solar Eclipses Authors: Pasachoff, Jay M.; Wright, Ernest T. Bibcode: 2015DPS....4710707P Altcode: The lunar mapping from NASA's Lunar Reconaissance Orbiter and JAXA's Kaguya has provided information that allows calculation of the lunar limb profile whose low points at total solar eclipses provides the Baily's Beads. Preparations for the forthcoming August 21, 2017, total solar eclipse (lunar occultation) whose totality crosses the continental United States from northwest to southeast (http://eclipses.info for the International Astronomical Union Working Group on Solar Eclipses) has led to new calculations of the Baily's Beads and of comparisons of the totality duration between predictions and observations for historical events.JMP's research on the annular and total solar eclipses of 2012 was supported in part by the Solar-Terrestrial Program of the Atmospheric and Geospace Sciences Division of the National Science Foundation through grant AGS-1047726. His observations of the 2013 and 2015 total solar eclipses were supported by grants 9327-13 and 9616-14, respectively, from the Committee for Research and Exploration of the National Geographic Society, with additional support from Williams College. Title: Preparing for and Observing the 2017 Total Solar Eclipse Authors: Pasachoff, J. Bibcode: 2015ASPC..500...43P Altcode: I discuss ongoing plans and discussions for EPO and scientific observing of the 21 August 2017 total solar eclipse. I discuss aspects of EPO based on my experiences at the 60 solar eclipses I have seen. I share cloud statistics along the eclipse path compiled by Jay Anderson, the foremost eclipse meteorologist. I show some sample observations of composite imagery, of

spectra, and of terrestrial temperature changes based on observations of recent eclipses, including 2012 from Australia and 2013 from Gabon. Links to various mapping sites of totality,

partial phases, and other eclipse-related information, including that provided by Michael Zeiler, Fred Espenak (retired from NASA) and Xavier Jubier can be found on the website I run

for the International Astronomical Union's Working Group on Eclipses at http://www.eclipses.info. Title: Aeolus: A Markov Chain Monte Carlo Code for Mapping Ultracool Atmospheres. An Application on Jupiter and Brown Dwarf HST Light Curves Authors: Karalidi, Theodora; Apai, Dániel; Schneider, Glenn; Hanson, Jake R.; Pasachoff, Jay M. Bibcode: 2015ApJ...814...65K Altcode: 2015arXiv151004251K Deducing the cloud cover and its temporal evolution from the observed planetary spectra and phase curves can give us major insight into the atmospheric dynamics. In this paper, we present Aeolus, a Markov chain Monte Carlo code that maps the structure of brown dwarf and other ultracool atmospheres. We validated Aeolus on a set of unique Jupiter Hubble Space Telescope (HST) light curves. Aeolus accurately retrieves the properties of the major features of the Jovian atmosphere, such as the Great Red Spot and a major 5 μm hot spot. Aeolus is the first mapping code validated on actual observations of a giant planet over a full rotational period. For this study, we applied Aeolus to J- and H-band HST light curves of 2MASS J21392676+0220226 and 2MASS J0136565+093347. Aeolus retrieves three spots at the top of the atmosphere (per observational wavelength) of these two brown dwarfs, with a surface coverage of 21% ± 3% and 20.3% ± 1.5%, respectively. The Jupiter HST light curves will be publicly available via ADS/VIZIR. Title: Central Flash Analysis of the 29 June 2015 Occultation Authors: Person, Michael J.; Bosh, A. S.; Sickafoose, A. A.; Zuluaga, C. A.; Levine, S. E.; Pasachoff, J. M.; Babcock, B. A.; Dunham, E. W.; McLean, I.; Wolf, J.; Abe, F.; Becklin, E.; Bida, T. A.; Bright, L. P.; Brothers, T. C.; Christie, G.; Collins, P. L.; Durst, R. F.; Gilmore, A. C.; Hamilton, R.; Harris, H. C.; Johnson, C.; Kilmartin, P. M.; Kosiarek, M. R.; Leppik, K.; Logsdon, S. E.; Lucas, R.; Mathers, S.; Morley, C. J. K.; Natusch, T.; Nelson, P.; Ngan, H.; Pfueller, E.; Roeser, H. -P.; Sallum, S.; Savage, M.; Seeger, C. H.; Siu, H.; Stockdale, C.; Suzuki, D.; Thanathibodee, T.; Tilleman, T.; Tristram, P. J.; Van Cleeve, J.; Varughese, C.; Weisenbach, L. W.; Widen, E.; Wiedemann, M. Bibcode: 2015DPS....4710505P Altcode: After an extensive prediction effort, the 29 June 2015 occultation by Pluto was observed from both airborne (Stratospheric Observatory for Infrared Astronomy - SOFIA) and numerous ground-based telescopes (Bosh et al. - this meeting). Real-time prediction updates allowed placement of the SOFIA telescope with its four detectors deep within the central-flash region of the atmospheric occultation. Fortuitously, the Mount John University Observatory (Lake Tekapo, New Zealand) was also within the central-flash region (Pasachoff et al. - this meeting). This happenstance resulted in multiple central-flash detections in several colors from each facility allowing direct comparison of different areas of the central-flash evolute.Here we examine and discuss the central-flash signatures from the highest signal-to-noise light curves from each facility. The relative orientations and asymmetries in the central flashes allow us to use them to tightly constrain the lower atmospheric ellipticity and orientation of likely winds with respect to Pluto’s figure. The ratio of the two separate central flashes is also a strong constraint on the geometric solution for the full occultation data set, and the absolute height of the central flashes with respect to those expected for a clear isothermal atmosphere places constraints on haze densities and thermal gradients in Pluto’s lower atmosphere. We can also compare the central-flash signatures in several colors (similar to Sickafoose et. al - this meeting) to establish bounds on haze-particle sizes in the lower atmosphere.SOFIA is jointly operated by the Universities Space Research Association, Inc. (USRA), under NASA contract NAS2-97001, and the Deutsches SOFIA Institut (DSI) under DLR contract 50 OK 0901 to the University of Stuttgart. Support for this work was provided, in part, by NASA grants SSO NNX15AJ82G (Lowell Observatory), PA NNX10AB27G (MIT), and PA NNX12AJ29G (Williams College), as well as the National Research Foundation of South Africa, and the NASA SOFIA Cycle 3 grant NAS2-97001 issued by USRA. Title: Haze in Pluto's atmosphere: Results from SOFIA and ground-based observations of the 2015 June 29 Pluto occultation Authors: Bosh, A. S.; Person, M. J.; Zuluaga, C. A.; Sickafoose, A. A.; Levine, S. E.; Pasachoff, J. M.; Babcock, B. A.; Dunham, E. W.; McLean, I.; Wolf, J.; Abe, F.; Becklin, E.; Bida, T. A.; Bright, L. P.; Brothers, T.; Christie, G.; Collins, P. L.; Durst, R. F.; Gilmore, A. C.; Hamilton, R.; Harris, H. C.; Johnson, C.; Kilmartin, P. M.; Kosiarek, M. R.; Leppik, K.; Logsdon, S. E.; Lucas, R.; Mathers, S.; Morley, C. J. K.; Nelson, P.; Ngan, H.; Pfüller, E.; Natusch, T.; Röser, H. -P.; Sallum, S.; Savage, M.; Seeger, C. H.; Siu, H.; Stockdale, C.; Suzuki, D.; Thanathibodee, T.; Tilleman, T.; Tristram, P. J.; Van Cleve, J.; Varughese, C.; Weisenbach, L. W.; Widen, E.; Wiedemann, M. Bibcode: 2015DPS....4710503B Altcode: We observed the 29 June 2015 occultation by Pluto from SOFIA and several ground-based sites in New Zealand. Pre-event astrometry (described in Zuluaga et al., this conference) allowed us to navigate SOFIA into Pluto's central flash (Person et al., this conference). Fortuitously, the central flash also fell over the Mt. John University Observatory (Pasachoff et al., this conference). We combine all of our airborne and ground-based data to produce a geometric solution for the occultation and to investigate the state of Pluto's atmosphere just two weeks before the New Horizons spacecraft's close encounter with Pluto. We find that the atmosphere parameters at half-light are unchanged from our observations in 2011 (Person et al. 2013) and 2013 (Bosh et al. 2015). By combining our light-curve inversion with recent radius measurements from New Horizons, we find strong evidence for an extended haze layer in Pluto's atmosphere. See also Sickafoose et al. (this conference) for an evaluation of the particle sizes and properties.SOFIA is jointly operated by the Universities Space Research Association, Inc. (USRA), under NASA contract NAS2-97001, and the Deutsches SOFIA Institut (DSI) under DLR contract 50 OK 0901 to the University of Stuttgart. Support for this work was provided by NASA SSO grants NNX15AJ82G (Lowell Observatory), NNX10AB27G (MIT), and NNX12AJ29G (Williams College), and by the National Research Foundation of South Africa. Title: A Central Flash at an Occultation of a Bright Star by Pluto Soon Before New Horizons' Flyby Authors: Pasachoff, Jay M.; Babcock, Bryce A.; Durst, Rebecca F.; Seeger, Christina H.; Levine, Stephen E.; Bosh, Amanda S.; Sickafoose, Amanda A.; Person, Michael J.; Abe, Fumio; Suzuki, Daisuke; Nagakane, Masayuki; Tristam, Paul J. Bibcode: 2015DPS....4721012P Altcode: From the Mt. John Observatory, New Zealand, we were so close to the center of the occultation path on 29 June 2015 UTC that we observed a modest central flash from the focusing of starlight from a 12th-magnitude star. The star was one of the brightest ever in our years of continual monitoring that started in 2002. At the time of Pluto's perihelion in 1989, it was feared from models that Pluto's atmosphere might collapse by now, a motivation for the timely launch of New Horizons; some models now allow Pluto to retain its atmosphere throughout its orbit.We used our frame-transfer CCD at 10 Hz with GPS timing on the 1-m McLellan telescope of Canterbury U. We also observed with a Lowell Obs. infrared camera on the "AAVSO" 0.6-m Optical Craftsman telescope; and obtained 3-color photometry at a slower cadence on a second 0.6-m telescope. We coordinated with the overflight of SOFIA and its 2.5-m telescope, which benefited from last-minute astrometry, and the Auckland Observatory's and other ground-based telescopes.Our light curves show a modest central flash; our tentative geometrical solution shows that we were only about 50 km from the occultation path's centerline. The flash is from rays lower than otherwise accessible in Pluto's atmosphere. Our light curves, at such high cadence that we see spikes caused by atmospheric effects that we had not seen so well since our 2002 Mauna Kea occultation observations, show that Pluto's atmosphere had not changed drastically since our previous year's observations. Our data provide a long-term context for New Horizon's highly-detailed observations of Pluto's atmosphere in addition to providing a chord for the geometrical solution that includes SOFIA's observations.Our observations were supported by NASA Planetary Astronomy grants NNX12AJ29G to Williams College, NNX15AJ82G to Lowell Observatory, and NNX10AB27G to MIT, and by the National Research Foundation of South Africa. We are grateful to Alan Gilmore, Pam Kilmartin, Robert Lucas, and Carolle Varughese for assistance at Mt. John. We thank the AAVSO for use of the AAVSOnet 0.6-m telescope and Arne Henden for assistance. Title: Report of the IAU Working Group on Solar Eclipses Authors: Pasachoff, Jay M. Bibcode: 2015IAUGA..2254605P Altcode: The Working Group on Solar Eclipses coordinates scientists and information in the study of the Sun and the heliosphere at solar eclipses. Our Website at http://eclipses.info has a wide variety of information, including links to maps and other websites dealing with solar eclipses, as well as information on how to observe the partial-phases of solar eclipses safely and why it is interesting for not only scientists but also for the public to observe eclipses and to see how we work to uncover the mysteries of the sun's upper atmosphere. In the last triennium, there were total eclipses in Australia and the Pacific in 2012; in an arc across Africa from Gabon to Uganda and Kenya in 2013; and in the Arctic, including Svalbard and the Faeroes plus many airplanes aloft, in 2015. In the coming triennium, there will be total solar eclipses in Indonesia and the Pacific in 2016 and then, on 21 August 2017, a total solar eclipse that will sweep across the Continental United States from northwest to southeast. Mapping websites, all linked to http://eclipses.info, include Fred Espenak's http://EclipseWise.com; Michael Zeiler's http://GreatAmericanEclipse.com and http://eclipse-maps.com; Xavier Jubier's http://xjubier.free.fr; and (with weather and cloudiness analysis) Jay Anderson's http://eclipser.ca. Members of the Working Group, chaired by Jay Pasachoff (U.S.), include Iraida Kim (Russia), Kiroki Kurokawa (Japan), Jagdev Singh (India), Vojtech Rusin (Slovakia), Zhongquan Qu (China), Fred Espenak (U.S.), Jay Anderson (Canada), Glenn Schneider (U.S.), Michael Gill (U.K.), Xavier Jubier (France), Michael Zeiler (U.S.), and Bill Kramer (U.S.). Title: Public Education and Outreach for Observing Solar Eclipses and Transits Authors: Pasachoff, Jay M. Bibcode: 2015IAUGA..2254684P Altcode: The general public is often very interested in observing solar eclipses, with widespread attention from newspapers and other sources often available only days before the events. Recently, the 2012 eclipse's partial phases in Australia and the 2015 eclipse's partial phases throughout Europe as well as western Asia and northern Africa, were widely viewed. The 21 August 2017 eclipse, whose totality will sweep across the Continental United States from northwest to southeast, will have partial phases visible throughout the U.S., Canada, Mexico, Central America, and into South America. The 2019 and 2020 partial phases of total eclipses will be visible throughout South America, and partial phases from annular eclipses will be visible from other parts of the world. The 9 May 2016 transit of Mercury will be best visible from the Western Hemisphere, Europe, and Africa. Many myths and misunderstandings exist about the safety of observing partial phases, and it is our responsibility as astronomers and educators to transmit accurate information and to attempt the widest possible distribution of such information. The Working Group on Public Education at Eclipses and Transits, formerly of Commission 46 on Education and Development and now of New Commission 11, tries to coordinate the distribution of information. In collaboration with the Solar Division's Working Group on Solar Eclipses, their website at http://eclipses.info is a one-stop shop for accurate information on how to observe eclipses, why it is interesting to do so, where they will be visible (with links to online maps and weather statistics), and how encouraging students to observe eclipses can be inspirational for them, perhaps even leading them to realize that the Universe can be understood and therefore renewing the strength of their studies. Links to information about transits of Mercury and Venus are also included. Title: Division XII: Commission 46: Education & Development of Astronomy Authors: Ros, Rosa M.; Hearnshaw, John; Stavinschi, Magda; Garcia, Beatriz; Gerbaldi, Michele; de Greve, Jean-Pierre; Guinan, Edward; Haubold, Hans; Jones, Barrie; Marshall, Laurence A.; Pasachoff, Jay Bibcode: 2015IAUTB..28..137R Altcode: C46 is a Commission of the Executive Committee of the IAU under Division XII Union-Wide Activities. Aiming at improvement of astronomy education and research at all levels worldwide (through the various projects it initiates),maintains, develops, as well as through the dissemination of information. C46 has 332 members and it was managed by the Organizing Committee, formed by the Commission President (Rosa M. Ros, from Spain), the Vice-Presiden (John Hearnshaw, from New Zealand), the Retiring President (Magda Stavinschi, from Romania), the Vice-President of the IAU (George Miley, from Netherland) and the PG chairs: • Worldwide Development of Astronomy WWDA: John Hearnshaw • Teaching Astronomy for Development TAD: Edward Guinan and Laurence A. Marshall • International Schools for Young Astronomers ISYA; chair: Jean-Pierre de Greve • Network for Astronomy School Education NASE: Rosa M. Ros and Beatriz Garcia • Public Understanding at the times of Solar Eclipses and transit Phenomena PUTSE: Jay Pasachoff • National Liaison and Newsletter: Barrie Jones • Collaborative Programs: Hans Haubold Title: Book review: Nearest Star: The surprising science of our Sun (Golub & Pasachoff) Authors: Smith, L.; Golub, L.; Pasachoff, J. M. Bibcode: 2015JBAA..125..183S Altcode: No abstract at ADS Title: Simon Marius's Mundus Iovialis: 400th Anniversary in Galileo's Shadow Authors: Pasachoff, Jay M. Bibcode: 2015JHA....46..218P Altcode: No abstract at ADS Title: The Solar Corona at the 2015 Total Solar Eclipse Authors: Pasachoff, Jay M.; Carter, Allison L. Bibcode: 2015TESS....120319P Altcode: We report on our successful observations of the solar corona at the 20 March 2015 total solar eclipse from our site at a latitude of about 78° on the Svalbard archipelago, and related observations by colleagues aloft. Our equipment included cameras for imaging at a variety of scales for use in making high-contrast composites, as reported our Astrophysical Journal article (2015) about our 2012 total solar eclipse observations and similar articles about the corona and changes in it at previous total eclipses. Our Svalbard equipment also included a spectrograph, with which we continued our monitoring of the ratio of the Fe XIV and Fe X coronal lines, which has recently been >1 with the solar maximum, a reversal from <1 at earlier eclipses closer to the last solar minimum. Our 2013 observations from Gabon showed two coronal mass ejections and an erupting prominence; the 2015 eclipse showed an erupting prominence and some unusual coronal structure in an overall coronal shape typical of solar maximum. We use our ground-based eclipse observations to fill the gap in imaging between the SDO and SWAP (17.4 nm) EUV observations on the solar disk and the inner location of the LASCO C2 occultation disk, with STEREO observations providing the possibility of three-dimensional interpretations. Our expedition was supported by a grant (9616-14) from the Committee for Research and Exploration of the National Geographic Society. Title: Air-cooling mathematical analysis as inferred from the air-temperature observation during the 1st total occultation of the Sun of the 21st century at Lusaka, Zambia Authors: Peñaloza-Murillo, Marcos A.; Pasachoff, Jay M. Bibcode: 2015JASTP.125...59P Altcode: We analyze mathematically air temperature measurements made near the ground by the Williams College expedition to observe the first total occultation of the Sun [TOS (commonly known as a total solar eclipse)] of the 21st century in Lusaka, Zambia, in the afternoon of June 21, 2001. To do so, we have revisited some earlier and contemporary methods to test their usefulness for this analysis. Two of these methods, based on a radiative scheme for solar radiation modeling and that has been originally applied to a morning occultation, have successfully been combined to obtain the delay function for an afternoon occultation, via derivation of the so-called instantaneous temperature profiles. For this purpose, we have followed the suggestion given by the third of these previously applied methods to calculate this function, although by itself it failed to do so at least for this occultation. The analysis has taken into account the limb-darkening, occultation and obscuration functions. The delay function obtained describes quite fairly the lag between the solar radiation variation and the delayed air temperature measured. Also, in this investigation, a statistical study has been carried out to get information on the convection activity produced during this event. For that purpose, the fluctuations generated by turbulence has been studied by analyzing variance and residuals. The results, indicating an irreversible steady decrease of this activity, are consistent with those published by other studies. Finally, the air temperature drop due to this event is well estimated by applying the empirical scheme given by the fourth of the previously applied methods, based on the daily temperature amplitude and the standardized middle time of the occultation. It is demonstrated then that by using a simple set of air temperature measurements obtained during solar occultations, along with some supplementary data, a simple mathematical analysis can be achieved by applying of the four methods reviewed here. Title: Book Review: Eclipses, Transits, and Comets of the Nineteenth Century: How America's Perceptions of the Skies Changed Authors: Pasachoff, Jay M. Bibcode: 2015JAHH...18..112P Altcode: No abstract at ADS Title: Structure and Dynamics of the 2012 November 13/14 Eclipse White-light Corona Authors: Pasachoff, J. M.; Rušin, V.; Saniga, M.; Babcock, B. A.; Lu, M.; Davis, A. B.; Dantowitz, R.; Gaintatzis, P.; Seiradakis, J. H.; Voulgaris, A.; Seaton, D. B.; Shiota, K. Bibcode: 2015ApJ...800...90P Altcode: 2014arXiv1412.1155P Continuing our series of observations of coronal motion and dynamics over the solar-activity cycle, we observed from sites in Queensland, Australia, during the 2012 November 13 (UT)/14 (local time) total solar eclipse. The corona took the low-ellipticity shape typical of solar maximum (flattening index ɛ = 0.01), a change from the composite coronal images we observed and analyzed in this journal and elsewhere for the 2006 and 2008-2010 eclipses. After crossing the northeast Australian coast, the path of totality was over the ocean, so further totality was seen only by shipborne observers. Our results include velocities of a coronal mass ejection (CME; during the 36 minutes of passage from the Queensland coast to a ship north of New Zealand, we measured 413 km s-1) and we analyze its dynamics. We discuss the shapes and positions of several types of coronal features seen on our higher-resolution composite Queensland coronal images, including many helmet streamers, very faint bright and dark loops at the bases of helmet streamers, voids, and radially oriented thin streamers. We compare our eclipse observations with models of the magnetic field, confirming the validity of the predictions, and relate the eclipse phenomenology seen with the near-simultaneous images from NASA's Solar Dynamics Observatory (SDO/AIA), NASA's Extreme Ultraviolet Imager on Solar Terrestrial Relations Observatory, ESA/Royal Observatory of Belgium's Sun Watcher with Active Pixels and Image Processing (SWAP) on PROBA2, and Naval Research Laboratory's Large Angle and Spectrometric Coronagraph Experiment on ESA's Solar and Heliospheric Observatory. For example, the southeastern CME is related to the solar flare whose origin we trace with a SWAP series of images. Title: 400th Anniversary of Marius's Book with the First Image of an Astronomical Telescope and of Orbits of Jovian Moons Authors: Pasachoff, Jay M.; Leich, Pierre Bibcode: 2015AAS...22521505P Altcode: Simon Mayr's (Marius's) Mundus Iovialis Anno M·DC·IX Detectus Ope Perspicilli Belgici (The World of Jupiter...) was published in Nuremberg in 1614; Marius was the Ansbach court mathematician. The frontispiece includes not only a portrait of Marius (1573-1624) himself but also, in the foreground, a long tube labelled "perspicillum," the first known image of a telescopic device used for astronomy; the name "telescope" came later. A schematic diagram of Jupiter with four moons orbiting appears at upper left; Marius, following a suggestion from Kepler, gave these Galilean satellites the names now still in use: Io, Europa. Ganymede, and Callisto. The title continues Hoc est, Quatuor Joviali cum Planetarum, cum Theoria, tum Tabulae, Propriis Observationibus Maxime Fundate.... A pair of conferences was held in Germany in 2014 to commemorate the 400th anniversary of Marius's book and to discuss Marius's work and its relation to Galileo's work (http://www.simon-marius.net; http://www.simon-marius.net/index.php?lang=en&menu=1 28 languages are available). Marius (Mayr) had independently discovered the four satellites of Jupiter, apparently one day after Galileo, on December 29 O.S., 1609; by the time he published his work four years later (a local-circulation publication had appeared in Nuremberg in 1611 in Prognosticon Astrologicum auf das Jahr 1612), Galileo had gained fame and priority, and Galileo accused Marius of plagiarism in Il Saggiatore (1623). With his Belgian telescope, Marius also noted the tilt of the orbital plane of Jupiter's moons, sunspots (1611), and the Andromeda Nebula (1612). He claimed to have worked out a system of cosmology similar to the Tychonic system in 1596, contemporaneously to Kepler's Mysterium Cosmographicum. A crater, the Marius Hills, and the Rima Marius on the Moon are named for him by the I.A.U., as well as, to celebrate the quadricentennial, a main-belt asteroid, now (7984) Marius. Acknowledgment: JMP thanks Seth Fagen, PRPH Books in New York, for introducing him to Marius's book 18 years ago. Title: Trio of stellar occultations by Pluto One Year Prior to New Horizons' Arrival Authors: Pasachoff, Jay M.; Person, Michael J.; Bosh, Amanda S.; Gulbis, Amanda A. S.; Zuluaga, Carlos A.; Levine, Stephen; Osip, David J.; Schiff, Adam R.; Seeger, Christina H.; Babcock, Bryce A.; Rojo, Patricio; Kosiarek, Molly R.; Servajean, Elise Bibcode: 2015AAS...22513715P Altcode: Our campaign in July 2014 yielded three successful stellar occultations (~m=15, 17, and 18) of Pluto (~m=14), observed from telescopes in New Zealand, Australia, and Chile. Telescopes involved included Chile: Magellan's Clay (6.5 m), SOAR (4.1 m), Carnegie's DuPont (2.4 m); Australia: AAT (4 m); and Canterbury's Mt. John McLellan (1-m); as well as various smaller telescopes in Australia and Chile. One of the events was also observed, with negative results, from GROND on La Silla (2.2 m) and SMARTS's ANDICAM at CTIO (1.3 m). Though our observations were coordinated across continents, each successfully observed event was seen from only one site because of bad weather at the other sites. Two of the events were uniquely observed from Mt. John (Pasachoff et al., DPS 2014) and one, with only Chile sites in the predicted path, from the Clay (Person et al., DPS 2014). This last event was expected to be of the brightest star with the largest telescope we have ever observed for a Pluto occultation, but clouds arrived at the 6.5-m Clay 90 s before the predicted time; a 1% occultation was nonetheless seen and eventually, confirmed by Keck AO observations, to be of a 15th magnitude star previously hidden in the brightness of the 12th mag star. Our scientific conclusion is that as of these observations, one year before New Horizons' passage of Pluto, the atmosphere of Pluto remained robust and of the same size. Details on our analysis of the three events will be presented.Acknowledgments: This work was supported in part by NASA Planetary Astronomy grants to Williams College (NNX12AJ29G) and to MIT (NNX10AB27G), as well as grants from USRA (#8500-98-003) and Ames Research (#NAS2-97-01) to Lowell Observatory. A.R.S. was supported by NSF grant AST-1005024 for the Keck Northeast Astronomy Consortium REU, with partial support from U.S. DoD's ASSURE program. P.R. acknowledges support from FONDECYT through grant 1120299. J.M.P. thanks Andrew Ingersoll and Caltech Planetary Astronomy for hospitality. Title: Observations of a successive stellar occultation by Charon and graze by Pluto in 2011: Multiwavelength SpeX and MORIS data from the IRTF Authors: Gulbis, A. A. S.; Emery, J. P.; Person, M. J.; Bosh, A. S.; Zuluaga, C. A.; Pasachoff, J. M.; Babcock, B. A. Bibcode: 2015Icar..246..226G Altcode: Pluto's lower atmosphere has been observed to evolve since the first definitive occultation detection in 1988. Possibilities for explaining the lower atmospheric structure include a steep thermal gradient and/or extinction, the latter of which can be characterized as a dependence between occultation flux and wavelength. On 2011 June 23, a 14.43 UCAC magnitude star (R = 13.64) was occulted by Pluto as observed from multiple sites. Observations made at NASA's 3-m Infrared Telescope Facility (IRTF) on Mauna Kea, Hawai'i, showed a full occultation of the star by Charon followed by an atmospheric graze by Pluto. Data were taken simultaneously in visible-wavelength images and low-resolution, near-infrared spectra. This dataset is unique in that (i) the double occultation allows astrometric measurements for Pluto and Charon as well as accurate calibration of the Pluto light curve, and (ii) the wavelength-resolved data serve as a test for atmospheric extinction. The graze reached a minimum normalized flux level of roughly 0.35, serving primarily as a probe of Pluto's upper atmosphere (which is typically defined to be above half-light level in occultation light curves). However, the light curve is well fit by atmospheric models with a power-law thermal gradient, a clear upper atmosphere, and haze in the lower atmosphere. We find a negative dependence between flux and wavelength in the deepest part of Pluto's atmosphere probed by the graze and in a spike during emersion. A simple extinction model for spherical, μm-sized tholins matches the observed spectral trends. While the atmospheric fits cannot rule out a clear atmosphere having a steep thermal gradient at the bottom, the flux-wavelength dependence and the feasibility of our particle-scattering fits suggest that Pluto's lower atmosphere contained haze in 2011. These results provide an important link in monitoring Pluto's dynamic atmosphere. Title: The state of Pluto's atmosphere in 2012-2013 Authors: Bosh, A. S.; Person, M. J.; Levine, S. E.; Zuluaga, C. A.; Zangari, A. M.; Gulbis, A. A. S.; Schaefer, G. H.; Dunham, E. W.; Babcock, B. A.; Davis, A. B.; Pasachoff, J. M.; Rojo, P.; Servajean, E.; Förster, F.; Oswalt, T.; Batcheldor, D.; Bell, D.; Bird, P.; Fey, D.; Fulwider, T.; Geisert, E.; Hastings, D.; Keuhler, C.; Mizusawa, T.; Solenski, P.; Watson, B. Bibcode: 2015Icar..246..237B Altcode: We observed two stellar occultations on UT 4 May 2013 and UT 9 September 2012, with the aim of measuring Pluto's atmospheric parameters. Both of these events were observed by world-wide collaborations of many observers, and both occurred within 1 month of Pluto's stationary points. The PC20120909 event was observed at the McDonald Observatory (MONET 1.2-m), and Olin Observatory (the Ortega 0.8-m); the P20130504 event was observed at the Las Campanas Observatory (du Pont 2.5-m), the Cerro Tololo Inter-American Observatory (SMARTS 1-m), and the Cerro Calán National Astronomical Observatory (Goto 0.45-m). Analysis of the data indicates an atmospheric state similar to that in June 2011. The shadow radius for the event is unchanged from recent events, indicating an atmosphere that is holding stable and not in the midst of global collapse. We discuss the advantages and disadvantages of comparing various atmospheric parameters across events (the shadow radius vs. the pressure at a particular radius). These analyses suggest that Pluto will still have an atmosphere when the New Horizons spacecraft arrives in July 2015. Title: Coronal Dynamics at Recent Total Solar Eclipses Authors: Pasachoff, J. M.; Lu, M.; Davis, A. B.; Demianski, M.; Rusin, V.; Saniga, M.; Seaton, D. B.; Lucas, R.; Babcock, B. A.; Dantowitz, R.; Gaintatzis, P.; Seeger, C. H.; Malamut, C.; Steele, A. Bibcode: 2014AGUFMSH41B4144P Altcode: Our composite images of the solar corona based on extensive imaging at the total solar eclipses of 2010 (Easter Island), 2012 (Australia), and 2013 (Gabon) reveal several coronal mass ejections and other changes in coronal streamers and in polar plumes. Our resultant spatial resolution is finer than that available in imaging from spacecraft, including that from SOHO/LASCO or STEREO. We trace the eruptions back to their footpoints on the sun using imaging from SDO and SWAP, and follow them upwards through the corona, measuring velocities. The high-resolution computer compositing by Miloslav Druckmüller and Hana Druckmüllerová (2010 and 2013) and Pavlos Gaintatzis (2012) allows comparison of our images with those taken at intervals of minutes or hours along the totality path.

Williams College's 2013 eclipse expedition was supported in part by grant 9327-13 from National Geographic Society/Committee for Research and Exploration. Our work on the 2012 eclipse is supported in part by grant AGS-1047726 from Solar Terrestrial Research/NSF AGS. V.R. and M.S. were partially supported by the VEGA grant agency project 2/0098/10 and 2/0003/13 (Slovak Academy of Sciences) and Grant 0139-12 from NG/CRE, and Hana Druckmüllerová by grant 205/09/1469 of the Czech Science Foundation. M.L. was supported by Sigma Xi. C.M. was a Keck Northeast Astronomy Consortium Summer Fellow, supported at Williams College by REU/NSF grant AST-1005024. Partial support was provided by U.S. Department of Defense's ASSURE program. J.M.P. thanks Caltech's Planetary Sciences Department for hospitality. Support for D.B.S. and SWAP came from PRODEX grant C90345 managed by ESA in collaboration with the Belgian Federal Science Policy Office (BELSPO) in support of the PROBA2/SWAP mission, and from the EC's Seventh Framework Programme (FP7/2007-2013) under grant 218816 (SOTERIA project, www.soteria-space.eu). SWAP is a project of the Centre Spatial de Liège and the Royal Observatory of Belgium funded by BELSPO. Title: Coordinated Occultation Observations for Pluto, Nix, and Quaoar in July 2014 Authors: Pasachoff, Jay M.; Schiff, Adam R.; Seeger, Christina H.; Babcock, Bryce A.; Person, Michael J.; Gulbis, Amanda A. S.; Bosh, Amanda S.; Zuluaga, Carlos A.; Levine, Stephen E.; Osip, David J.; Rojo, Patricio; Kosiarek, Molly Bibcode: 2014DPS....4641901P Altcode: We observed Pluto, its moon Nix, and Quaoar during a predicted series of occultations in July 2014 with the 1-m telescope of the Mt. John University Observatory in New Zealand. The observations were based on new USNO photometry. We successfully detected occultations by Pluto of an R=18 mag star on 23 July (14:23:30 ± 00:00:10 UTC to 14:25:30 ± 00:00:10 UTC), with a drop of 5%, and of an R=17 star on 24 July (11:41:30 ± 00:00:10 UTC to 11:43:30 ± 00:00:10 UTC), with a drop of 3%, both with 20 s exposures with our frame-transfer POETS. Since Pluto had a geocentric velocity of 22.51 km/s on 23 July and 22.35 km/s on 24 July, these intervals yield limits on the chord lengths (surface + lower atmosphere) of 2700 ± 130 km and 2640 ± 250 km respectively, indicating that the events were near central, and provide astrometric data. Our coordinated observations with the 4-m AAT in Australia on 23 July and the 6.5-m Magellan/Clay, the 4.1-m SOAR, the 2.5-m DuPont, the 0.6-m SARA South, and the 0.45-m Cerro Calán telescopes in Chile on July 27 and 31, which would have provided higher-cadence observations for studies of Pluto’s atmosphere, were largely foiled by clouds.This work was supported in part by NASA Planetary Astronomy grants to Williams College (NNX12AJ29G) and to MIT (NNX10AB27G), as well as grants from USRA (#8500-98-003) and Ames Research (#NAS2-97-01) to Lowell Observatory. A.R.S. was supported by NSF grant AST-1005024 for the Keck Northeast Astronomy Consortium REU, with partial support from U.S. DoD's ASSURE program. P.R. acknowledges support from FONDECYT through grant 1120299. Title: Evidence of Haze in Pluto’s Lower Atmosphere in 2011 Authors: Gulbis, Amanda; Emery, Joshua P.; Person, Michael J.; Bosh, Amanda S.; Zuluaga, Carlos A.; Pasachoff, Jay M. Bibcode: 2014DPS....4640101G Altcode: Based on stellar occultation observations since 1988, Pluto’s lower atmosphere has been evolving (e.g., Elliot et al. 2007, AJ, 134, 1; Young et al. 2008, AJ, 136, 1757; Bosh et al. 2014, Icarus, in press). The structure of the lower atmosphere is likely due to a steep thermal gradient and/or extinction, the latter of which can be characterized as a dependence between observed occultation flux and wavelength. On 2011 June 23, a 13.64 R-magnitude star was occulted by Pluto as observed from multiple sites (Person et al. 2013, AJ, 146, 83). Observations made at NASA’s 3-m Infrared Telescope Facility (IRTF) on Mauna Kea, Hawai’i, showed a full occultation of the star by Charon followed by an atmospheric graze by Pluto. Data were taken simultaneously in visible-wavelength images and low-resolution, near-infrared spectra. This unique, wavelength-resolved dataset serves as a test for atmospheric extinction. The graze primarily probed Pluto’s upper atmosphere. The upper atmosphere is typically defined to be above half-light level in occultation light curves (approximately three pressure scale heights above the surface), and the graze reached a minimum of roughly 0.35 flux. However, the light curve is well matched by an atmospheric model with a power-law thermal gradient, a clear upper atmosphere, and haze in the lower atmosphere. Furthermore, there is a negative dependence between flux and wavelength in the deepest part of the atmosphere probed by the graze, as well as in an emersion spike. We find that a simple extinction model for spherical, micron-sized tholins matches the observed spectral trends (Gulbis et al. 2014, Icarus, in press). While the atmospheric fits cannot rule out a clear atmosphere having a steep thermal gradient at the bottom, the flux-wavelength dependence and the feasibility of our particle-scattering fits suggest that Pluto’s lower atmosphere contained haze in 2011. These results provide an important link in monitoring Pluto’s dynamic atmosphere, especially placed in context of the imminent arrival of the New Horizons spacecraft. Title: Venus' thermospheric temperature field using a refraction model at terminator : comparison with 2012 transit observations using SDO/HMI, VEx/SPICAV/SOIR and NSO/DST/FIRS Authors: Widemann, Thomas; Jaeggli, Sarah; Reardon, Kevin; Tanga, Paolo; Père, Christophe; Pasachoff, Jay M.; Vandaele, Ann Carine; Wilquet, Valerie; Mahieux, Arnaud; Wilson, Colin Bibcode: 2014DPS....4630206W Altcode: The transit of Venus in June 2012 provided a unique case study of the Venus' atmosphere transiting in front of the Sun, while at the same time ESA's Venus Express orbiter observed the evening terminator at solar ingress and solar egress.We report on mesospheric temperature at Venus' morning terminator using SDO/HMI aureole photometry and comparison with Venus Express. Close to ingress and egress phases, we have shown that the aureole photometry reflects the local density scale height and the altitude of the refracting layer (Tanga et al. 2012). The lightcurve of each spatially resolved aureole element is fit to a two-parameter model to constrain the meridional temperature gradient at terminator. Our measurements are in agreement with the VEx/SOIR temperatures obtained during orbit 2238 at evening terminator during solar ingress (46.75N - LST = 6.075PM) and solar egress (31.30N - LST = 6.047PM) captured from the Venus Express orbiter at the time Venus transited the Sun.We also performed spectroscopy and polarimetry during the transit of Venus focusing on extracting signatures of CO2 absorption. Observations were taken during the first half of the transit using the Facility InfraRed Spectropolarimeter (FIRS) on the Dunn Solar Telescope (DST). Although the predicted CO2 transmission spectrum of Venus was not particularly strong at 1565 nm, this region of the H-band often used in magnetic field studies of the Sun's photosphere provides a particularly flat solar continuum with few atmospheric lines. Sun-subtracted Venus limb observations show intensity distribution of vibrational CO2 bands 221 2v+2v2+v3 at 1.571μm and 141 v1+4v2+v3 at 1.606μm. Title: Recreating Galileo's 1609 Discovery of Lunar Mountains Authors: Pasachoff, Jay M.; Needham, Paul S.; Wright, Ernest T.; Gingerich, Owen Bibcode: 2014DPS....4610606P Altcode: The question of exactly which lunar features persuaded Galileo that there were mountains on the moon has not yet been definitively answered; Galileo was famously more interested in the concepts rather than the topographic mapping in his drawings and the eventual engravings. Since the pioneering work of Ewen Whitaker on trying to identify which specific lunar-terminator features were those that Galileo identified as mountains on the moon in his 1609 observations reported in his Sidereus Nuncius (Venice, 1610), and since the important work on the sequence of Galileo's observations by Owen Gingerich (see "The Mystery of the Missing 2" in Galilaeana IX, 2010, in which he concludes that "the Florentine bifolium sheet [with Galileo's watercolor images] is Galileo's source for the reworked lunar diagrams in Sidereus Nuncius"), there have been advances in lunar topographical measurements that should advance the discussion. In particular, one of us (E.T.W.) at the Scientific Visualization Studio of NASA's Goddard Space Flight Center has used laser-topography from NASA's Lunar Reconnaissance Orbiter to recreate what Galileo would have seen over a sequence of dates in late November and early December 1609, and provided animations both at native resolution and at the degraded resolution that Galileo would have observed with his telescope. The Japanese Kaguya spacecraft also provides modern laser-mapped topographical maps. Title: Atmospheric state of Pluto from the 31 July 2014 stellar occultation Authors: Person, Michael J.; Bosh, Amanda S.; Zuluaga, Carlos A.; Kosiarek, Molly; Osip, David J.; Levine, Stephen E.; Pasachoff, Jay M.; Schiff, Adam R.; Seegar, Christina H.; Babcock, Bryce A.; Gulbis, Amanda A.; Rojo, Patricio Bibcode: 2014DPS....4641909P Altcode: On 31 July 2014 (UT), while observing a potential Pluto occultation (m=12, unfortunately obscured by clouds), we imaged a fortuitous occultation by Pluto of a small companion star (m=15) several minutes before the main event (and before the clouds came in) with the 6.5-m Clay telescope at Magellan. The main star’s resulting light curve (essentially flat until the weather intervened) was one of the highest signal-to-noise light curves yet obtained from a Pluto occultation observation. It will be analyzed for possible signatures of dust in the Pluto system (see Levine et al., this meeting). Given the lower signal to noise ratio provided by the secondary star, careful calibration is needed to analyze the atmospheric occultation itself. Several other attempts at observing Pluto occultations in July 2014 were unfortunately clouded out (see Levine et al., Pasachoff et al., this meeting).Using precise astrometry obtained with the 2.5-m DuPont telescope and the 4.3-m Discovery Channel telescope before and after the event, while Pluto and the stars were well-separated, we are able to constrain the closest approach distance of the secondary star occultation event. Using the photometry from these same images, we are also able to characterize the relative brightness of both stars in relation to Pluto (taking care to account for the light from Charon as well). With these two constraints we can analyze the atmospheric signature of the occultation, and provide a current (July 2014) estimate of Pluto’s changing atmospheric diameter. Initial results indicate no large changes in the atmospheric scale height; complete results from the final analysis will be presented with this work.This work was supported in part by NASA Planetary Astronomy grants to MIT (NNX10AB27G) and Williams College (NNX12AJ29G), as well as grants from USRA (#8500-98-003) and Ames Research (#NAS2-97-01) to Lowell Observatory. P.R. acknowledges support from FONDECYT through grant 1120299. Title: The H-R Diagram's 100th Anniversary Authors: Pasachoff, Jay M. Bibcode: 2014S&T...127f..32P Altcode: No abstract at ADS Title: Howard Russell Butler's Oil Paintings of Solar Eclipses and Prominences Authors: Pasachoff, Jay M.; Olson, Roberta J. M. Bibcode: 2014AAS...22420306P Altcode: Howard Russell Butler (1856-1934) was invited to join the US Naval Observatory expedition to the total solar eclipse of 1918 because of his ability to paint astronomical phenomena based on quickly-made notes about spatial and color details. His giant triptych of the total eclipses of 1918, 1923, and 1925 was proposed for a never-built astronomical center at the American Museum of Natural History and wound up at their Hayden Planetarium when it was constructed in the mid-1930s. Half-size versions are installed at the Fels Planetarium at the Franklin Institute in Philadelphia and at the Firestone Library of Princeton University, whose newly conserved canvases were recently hung; the Buffalo Museum of Science has another half-size version in storage. We discuss not only the eclipse triptychs but also the series of large oil paintings he made of solar prominences (in storage at the American Museum of Natural History) and of his 1932-eclipse and other relevant works.JMP was supported for this work in part by Division III Discretionary Funds and the Brandi Fund of Williams College. His current eclipse research is supported by grants AGS-1047726 from the Solar Research Program of the Atmospheric and Geospace Sciences Division of NSF and 9327-13 from the Committee for Research and Exploration of the National Geographic Society. Title: Imaging and Spectra of the Chromosphere and Corona at the 2013 Total Eclipse in Gabon Authors: Pasachoff, Jay M.; Davis, Allen B.; Demianski, Marek; Rusin, Vojtech; Saniga, Metod; Seaton, Daniel B; Gaintatzis, Pavlos; Voulgaris, Aristeidis; Lucas, Robert; Edwards, Zophia; Zeiler, Michael; Kentrianakis, Michael Bibcode: 2014AAS...22432316P Altcode: We successfully observed the 3 November 2013 eclipse's 59 s of totality in clear sky from the centerline of totality where it exited La Lope National Park in Gabon, close to the maximum totality available on land. Our wide-field imaging showed two CMEs and an erupting prominence. We compare our images with those obtained elsewhere in totality to assess motion and dynamics. Our imaging observations are also compared with near-simultaneous observations from SDO/AIA, SDO/HMI, Hinode/XRT, SOHO/LASCO, SOHO/EIT, PROBA2/SWAP, and STEREO/SECCHI. We also have flash and coronal spectra, which continue to show overall warming of the corona in 2012 and 2013 through studies we have made over the solar cycle that include the ratio of intensities of the coronal red (Fe X 637.4 nm) and green (Fe XIV 530.3 nm) forbidden lines.The Williams College 2013 total-eclipse expedition was supported in part by grant 9327-13 from the Committee for Research and Exploration of the National Geographic Society. Our continued work on the 2012 eclipse results is supported in part by grant AGS-1047726 from Solar Terrestrial Research/NSF AGS. Title: Book Review: A History of Telescopes Authors: Pasachoff, Jay M. Bibcode: 2014JHA....45..256P Altcode: No abstract at ADS Title: Venus' thermospheric temperature field using a refraction model at terminator : comparison with 2012 transit observations using SDO/HMI and NSO/DST/FIRS Authors: Widemann, Thomas; Tanga, Paolo; Père, Christophe; Jaeggli, Sarah; Reardon, Kevin; Pasachoff, Jay M. Bibcode: 2014EGUGA..1612916W Altcode: The transit of Venus in June 2012 provided a unique case study of an Earth-size planet's atmosphere transiting in front of its parent star at 0.7AU, while at the same time ESA's Venus Express orbiter observed the evening terminator at solar ingress and solar egress. We report on mesospheric temperature at Venus' morning terminator using SDO/HMI aureole photometry and comparison with Venus Express. Close to ingress and egress phases, we have shown that the aureole photometry reflects the local density scale height and the altitude of the refracting layer (Tanga et al. 2012). The lightcurve of each spatial resolution element of the aureole is compared to a two-parameter model to constrain the meridional temperature gradient along the terminator. Our measurements are in agreement with the VEx/SOIR temperatures obtained during orbit 2238 at evening terminator during solar ingress (46.75N - LST = 6.075PM) and solar egress (31.30N - LST = 6.047PM) captured from the Venus Express orbiter at the time Venus transited the Sun for Earth-based observers. We also performed spectroscopy and polarimetry during the transit of Venus focusing on extracting signatures of CO2 absorption. Observations were taken during the first half of the transit using the Facility InfraRed Spectropolarimeter on the Dunn Solar Telescope. Although the predicted CO2 transmission spectrum of Venus was not particularly strong at 1565 nm, this region of the H-band often used in magnetic field studies of the Sun's photosphere provides a particularly flat solar continuum with few atmospheric and molecular lines. Sun-subtracted Venus limb observations show intensity distribution of vibrational CO2 bands 221 2v + 2ν2 + ν3 at 1.571um and 141 ν1 + 4ν2 + ν3 at 1.606um. Data independently allow to constrain temperature as well as cross-terminator thermospheric winds. Title: Astronomy: Art of the eclipse Authors: Pasachoff, Jay M.; Olson, Roberta J. M. Bibcode: 2014Natur.508..314P Altcode: As the next solar eclipse approaches, Jay M. Pasachoff and Roberta J. M. Olson ponder how artists from the early Renaissance onwards have interpreted the phenomenon. Title: Nearest Star Authors: Golub, Leon; Pasachoff, Jay M. Bibcode: 2014nest.book.....G Altcode: Preface; Acknowledgments; 1. The Sun; 2. The once and future Sun; 3. What we see: the solar disk; 4. What we don't see; 5. Eclipses; 6. Space missions; 7. Between fire and ice; 8. Space weather; Bibliography; Glossary; Index. Title: Solar Activity and Motions in the Solar Chromosphere and Corona at the 2012 and 2013 Total and Annular Eclipses in the U.S., Australia, and Africa Authors: Pasachoff, Jay M.; Babcock, B. A.; Davis, A. B.; Demianski, M.; Lucas, R.; Lu, M.; Dantowitz, R.; Rusin, V.; Saniga, M.; Seaton, D. B.; Gaintatzis, P.; Voulgaris, A.; Seiradakis, J. H.; Gary, D. E.; Shaik, S. B. Bibcode: 2014AAS...22311801P Altcode: Our studies of the solar chromosphere and corona at the 2012 and 2013 eclipses shortly after cycle maximum 24 (2011/2012) of solar activity (see: http://www.swpc.noaa.gov/SolarCycle/) involved radio observations of the 2012 annular eclipse with the Jansky Very Large Array, optical observations of the 2012 total eclipse from Australia, optical observations of the 2013 annular eclipse from Tennant Creek, Australia, and the 3 November 2013 total solar eclipse from Gabon. Our observations are coordinated with those from solar spacecraft: Solar Dynamics Observatory AIA and HMI, Hinode XRT and SOT, SOHO LASCO and EIT, PROBA2 SWAP, and STEREO SECCHI. Our 2012 totality observations include a CME whose motion was observed with a 37-minute interval. We include first results from the expedition to Gabon for the 3 November 2013 eclipse, a summary of eclipse results from along the path of totality across Africa, and a summary of the concomitant spacecraft observations. The Williams College 2012 expeditions were supported in part by NSF grant AGS-1047726 from Solar Terrestrial Research/NSF AGS, and by the Rob Spring Fund and Science Center funds at Williams. The JVLA is supported by the NSF. The Williams College 2013 total-eclipse expedition was supported in part by grant 9327-13 from the Committee for Research and Exploration of the National Geographic Society. ML was also supported in part by a Grant-In-Aid of Research from the National Academy of Sciences, administered by Sigma Xi, The Scientific Research Society (Grant ID: G20120315159311). VR and MS acknowledge support for 2012 from projects VEGA 2/0003/13 and NGS-3139-12 of the National Geographic Society. We are grateful to K. Shiota (Japan) for kindly providing us with some of his 2012 eclipse coronal images. We thank Alec Engell (Montana State U) for assistance on site, and Terry Cuttle (Queensland Amateur Astronomers) for help with site arrangements. We thank Aram Friedman (Ansible Technologies), Michael Kentrianakis, and Nicholas Weber (Dexter Southfield School) for collaboration on imaging at the Australian total eclipse. Title: Pond, John Authors: Pasachoff, Naomi; Pasachoff, Jay M. Bibcode: 2014bea..book.1745P Altcode: No abstract at ADS Title: Observations of the Black-Drop Effect at the 2012 Transit of Venus Authors: Rogoszinski, Zeeve; Pasachoff, J. M.; Babcock, B. A.; Schneider, G.; Reardon, K. P. Bibcode: 2014AAS...22324716R Altcode: We observed the 2012 transit of Venus from several locations, including the Mees Solar Observatory of the University of Hawaii on Maui; the Dunn Solar Telescope at the Sacramento Peak Observatory of the National Solar Observatory in Sunspot, NM; and the Big Bear Solar Observatory of the New Jersey Institute of Technology in California. Our observations, mainly directed at the study of Venus's atmosphere, also included high-resolution views of the black-drop effect. Historically, the black-drop effect proved to be a daunting anomaly for measuring the path length of Venus across the Sun’s surface with sufficient time accuracy to allow satisfactory measurement of the astronomical unit. Therefore, this phenomenon set back the accurate calculations for centuries of the size and scale of the solar system. In this paper, we discuss data taken with the New Solar Telescope at the Big Bear Observatory and with the IBIS on the Dunn Solar Telescope. We show the evolution of isophotes as a function of time to demonstrate various limb effects during second and third contacts. Schneider, Pasachoff, and Golub (Icarus 168. 249-256, 2004) have shown that the black-drop effect as seen in a transit of Mercury resulted from both the point-spread function of the telescope and the extreme limb-darkening effect at the region of the solar limb where the black-drop effect is demonstrated, and the current paper extends the analysis to the recent transit of Venus. As they showed, and as is verified here, Venus's atmosphere plays no role in the black-drop effect. ZR (Vassar '14) was a Keck Northeast Astronomy Consortium Summer Fellow at Williams College, supported by an NSF/REU grant to the Keck Northeast Astronomy Consortium. This research used the following tools: IDL/IDP3, ImageJ, and DS9. For obtaining the data at the Big Bear Solar Observatory, we thank Vasyl Yurchyshyn. Special thanks goes to Dr. Steven Souza for his support. The 2012 observations were obtained with a grant from the Committee for Research and Exploration of the National Geographic Society. Title: Observation and Analysis of a Single-Chord Stellar Occultation by Kuiper Belt Object (50000) Quaoar Authors: Davis, Allen B.; Pasachoff, J. M.; Babcock, B. A.; Person, M. J.; Zuluaga, C. A.; Bosh, A. S.; Levine, S.; Naranjo, O. A.; Navas, G. R.; Gulbis, A.; Winters, J. G.; Bianco, F. Bibcode: 2014AAS...22324708D Altcode: The Williams-MIT collaboration (www.stellaroccultations.info) predicted and observed a stellar occultation of 2UCAC 26260847 (mag 14.35) by KBO 50000 Quaoar (mag 18.9) on 8/9 July 2013. Observations were attempted from a total of five sites in Chile, Venezuela, and Massachusetts. Only one site, Llano del Hato National Astronomical Observatory in Venezuela, had a positive detection of the occultation, giving us a single chord on Quaoar. All other sites were cloudy. The light curve from the 8/9 July 2013 event has been analyzed with the assumption that Quaoar is ellipsoidal or spherical, placing bounds on some of Quaoar’s properties: diameter (> 1138 ± 25 km), density (< 1.82 ± 0.28 g cm-3), and albedo (< 0.14 ± 0.10). An independent prediction of the occultation’s shadow path by Fraser, Gwyn, et al. (2013) suggests that the chord is near-equatorial, which means that our bounds on Quaoar’s properties are closer to estimates. We will compare our result with that of the 11 February 2011 single-chord occultation detected by Sallum et al. (2011) and Person et al. (2011). A subsequent attempt to observe a second Quaoar occultation, that of 12/13 July 2013 in South Africa, failed because of cloudy weather. This work was supported in part by NASA Planetary Astronomy grants NNX08AO50G and NNH11ZDA001N to Williams College, NNX10AB27G to MIT, and USRA grant #8500-98-003 to Lowell Observatory. We thank Steven P. Souza at Williams, and other collaborators in planning and carrying out the various observations: including Libardo Zerpa, Joresly Villarreal, Richard Rojas, and Jorge Moreno at Llano del Hato, and Patricio Rojo and Matias Jones at Cerro Calan/U. Chile. Title: Messier, Copernicus, Flamsteed: The SAF Rare-Book Collection in Paris Authors: Pasachoff, Jay M. Bibcode: 2014AAS...22310707P Altcode: The historic books belonging to the Société Astronomique de France, founded by Camille Flammarion in 1887, are located partly in Paris and partly at the Flammarion site in Juvisy, a Paris suburb. Their holdings include first editions of Copernicus's De Revolutionibus and of Flamsteed's star atlas, as well as Messier's own copy of his 1783 and 1784 papers with his handwritten comments and additions. I will describe the fruitless search for a Bevis atlas and the circumstances that led me to inspect these treasures. I thank David Valls-Gabaud and Philippe Morel of the Société Astronomique de France for their hospitality in Paris, Jean-Claude Pecker, and Owen Gingerich for his prior work on Messier's catalogue. Title: Morley, Edward Williams Authors: Pasachoff, Naomi; Pasachoff, Jay M. Bibcode: 2014bea..book.1524P Altcode: No abstract at ADS Title: Russell, Henry Norris Authors: Pasachoff, Naomi; Pasachoff, Jay M. Bibcode: 2014bea..book.1881P Altcode: No abstract at ADS Title: Hypatia Authors: Pasachoff, Naomi; Pasachoff, Jay M. Bibcode: 2014bea..book.1014P Altcode: No abstract at ADS Title: The 2011 June 23 Stellar Occultation by Pluto: Airborne and Ground Observations Authors: Person, M. J.; Dunham, E. W.; Bosh, A. S.; Levine, S. E.; Gulbis, A. A. S.; Zangari, A. M.; Zuluaga, C. A.; Pasachoff, J. M.; Babcock, B. A.; Pandey, S.; Amrhein, D.; Sallum, S.; Tholen, D. J.; Collins, P.; Bida, T.; Taylor, B.; Bright, L.; Wolf, J.; Meyer, A.; Pfueller, E.; Wiedemann, M.; Roeser, H. -P.; Lucas, R.; Kakkala, M.; Ciotti, J.; Plunkett, S.; Hiraoka, N.; Best, W.; Pilger, E. J.; Micheli, M.; Springmann, A.; Hicks, M.; Thackeray, B.; Emery, J. P.; Tilleman, T.; Harris, H.; Sheppard, S.; Rapoport, S.; Ritchie, I.; Pearson, M.; Mattingly, A.; Brimacombe, J.; Gault, D.; Jones, R.; Nolthenius, R.; Broughton, J.; Barry, T. Bibcode: 2013AJ....146...83P Altcode: On 2011 June 23, stellar occultations by both Pluto (this work) and Charon (future analysis) were observed from numerous ground stations as well as the Stratospheric Observatory for Infrared Astronomy (SOFIA). This first airborne occultation observation since 1995 with the Kuiper Airborne Observatory resulted in the best occultation chords recorded for the event, in three visible wavelength bands. The data obtained from SOFIA are combined with chords obtained from the ground at the IRTF, the U.S. Naval Observatory Flagstaff Station, and Leeward Community College to give the detailed state of the Pluto-Charon system at the time of the event with a focus on Pluto's atmosphere. The data show a return to the distinct upper and lower atmospheric regions with a knee or kink in the light curve separating them as was observed in 1988, rather than the smoothly transitioning bowl-shaped light curves of recent years. The upper atmosphere is analyzed by fitting a model to all of the light curves, resulting in a half-light radius of 1288 ± 1 km. The lower atmosphere is analyzed using two different methods to provide results under the differing assumptions of particulate haze and a strong thermal gradient as causes for the lower atmospheric diminution of flux. These results are compared with those from past occultations to provide a picture of Pluto's evolving atmosphere. Regardless of which lower atmospheric structure is assumed, results indicate that this part of the atmosphere evolves on short timescales with results changing the light curve structures between 1988 and 2006, and then reverting these changes in 2011 though at significantly higher pressures. Throughout these changes, the upper atmosphere remains remarkably stable in structure, again except for the overall pressure changes. No evidence of onset of atmospheric collapse predicted by frost migration models is seen, and the atmosphere appears to be remaining at a stable pressure level, suggesting it should persist at this full level through New Horizon's flyby in 2015. Title: Recent KBO (Pluto/Charon and beyond, including Quaoar) Occultation Observations by the Williams College Team as part of the Williams-MIT Collaboration Authors: Pasachoff, Jay M.; Babcock, B. A.; Davis, A. B.; Pandey, S.; Lu, M.; Rogosinski, Z.; Person, M. J.; Bosh, A. S.; Zangari, A. M.; Zuluaga, C. A.; Gulbis, A. S.; Naranjo, O.; Navas, G.; Zerpa, L.; Villarreal, J.; Rojo, P.; Förster, F.; Servajean, E. Bibcode: 2013DPS....4531001P Altcode: The Williams College-MIT collaboration has observed numerous occultations of stars by Pluto/Charon and other Kuiper-belt objects (www.stellaroccultations.info), since its establishment three decades ago with an attempted discovery of Neptune's rings in 1983. In this paper, we describe several recent occultation observations, both successful and (for reasons of path uncertainties and/or weather) unsuccessful. Light curves made or arranged by Williams College faculty and students were used together with light curves by MIT colleagues and others to study Pluto's atmosphere and Charon's size, to discover one of the highest-known solar-system albedos (KBO 55636), and to attempt to study 1000-km-diameter Quaoar. Observations discussed include light curves for KBO 55636 on 9 October 2009 from Hawaii; Pluto on 3/4 July 2010 from Chile, 22 May 2011 from Williamstown, Massachusetts, 23 June 2011 from Hawaii (in support of SOFIA observations of Pluto's atmosphere, discussed in an article in press in AJ and of the pair of Pluto/Charon occultations of the same star), and 4 May 2013 (Bosh et al., this conference) and 15 July 2013 from Williamstown; Charon on 15 June 2013 from Williamstown; Quaoar from a picket fence ranging from Chile through Venezuela (with a detection there) to Massachusetts on July 8/9 and in South Africa on 12 July 2013. This work was supported in part by NASA Planetary Astronomy grants NNX08AO50G and NNH11ZDA001N to Williams College, NNX10AB27G to MIT, and USRA grant #8500-98-003 to Lowell Observatory. We thank Steven P. Souza at Williams; Steven Levine at Lowell Obs.; Jennifer G. Winters (GSU) in Chile; Richard Rojas/Jorge Moreno in Venezuela; Scott Sheppard; Federica Bianco; David Osip; and others. ZR (Vassar '14) was a Keck Northeast Astronomy Consortium Summer Fellow at Williams College, supported by an NSF/REU grant to the Keck Northeast Astronomy Consortium. ES: partial support from Programa Nacional de Becas de Postgrado (CONICYT Grant 21110496). FF: support from FONDECYT through grant 3110042 and by the Millennium Center for Supernova Science, grant P10-064-F. funded by Programa Bicentenario de Ciencia y Tecnología de CONICYT and Programa Iniciativa Científíca Milenio de MIDEPLAN. Title: The Planetary and Eclipse Oil Paintings of Howard Russell Butler Authors: Pasachoff, Jay M.; Olson, R. M. Bibcode: 2013DPS....4510803P Altcode: The physics-trained artist Howard Russell Butler (1856-1934) has inspired many astronomy students through his planetary and eclipse paintings that were long displayed at the Hayden Planetarium in New York, the Fels Planetarium at the Franklin Institute in Philadelphia, and the Buffalo Museum of Science. We discuss not only the eclipse triptychs (1918, 1923, and 1925) at each of those institutions but also his paintings of Mars as seen from Phobos and from Deimos (with landscapes of those moons in the foreground depicted in additional oils hung at Princeton University) and the Earth from our Moon. We also describe his involvement with astronomy and his unique methodology that allowed him to surpass the effects then obtainable with photography, as well as his inclusion in a U.S. Naval Observatory eclipse expedition in 1918, as well as his auroral, solar-prominence, and 1932-eclipse paintings. Title: Characterization of a transiting exo-Venus : lessons from the 2012 Transit Authors: Widemann, Thomas; Jaeggli, S. A.; Reardon, K. P.; Tanga, P.; Pasachoff, J. M.; Schneider, G. Bibcode: 2013DPS....4511811W Altcode: The transit of Venus in June 2012 provided a unique chance to view a well studied planetary atmosphere as we might see that of a transiting exoplanet, through scattered and refracted illumination of its parent star. We report on mesospheric temperature at Venus' morning terminator using SDO/HMI aureole photometry and comparison with Venus Express. Close to ingress and egress phases, we have shown that the aureole photometry reflects the local density scale height and the altitude of the refracting layer (Tanga et al. 2012). The lightcurve of each spatial resolution element of the aureole is compared to a two-parameter model to constrain the meridional temperature gradient along the terminator. Our measurements are in agreement with the VEx/SOIR temperatures obtained during orbit 2238 at evening terminator during solar ingress (46.75N - LST = 6.075PM) and solar egress (31.30N - LST = 6.047PM) as seen from the orbiter. Imaging data using IBIS/ROSA on the Dunn Solar Telescope in the G-band (430 nm) are also presented. We also performed spectroscopy and polarimetry during the transit of Venus focusing on extracting signatures of CO2 absorption. Observations were taken during the first half of the transit using the Facility InfraRed Spectropolarimeter on the Dunn Solar Telescope. Although the predicted CO2 transmission spectrum of Venus was not particularly strong at 1565 nm, this region of the H-band often used in magnetic field studies of the Sun's photosphere provides a particularly flat solar continuum with few atmospheric and molecular lines. Sun-subtracted Venus limb observations show intensity distribution of vibro-rotational CO2 band 221 2ν + 2ν2 + ν3 at 1.571μm allowing for an additional constraint on Venus' thermospheric temperature. Title: The State of Pluto's Atmosphere in 2012-2013 Authors: Bosh, Amanda S.; Person, M. J.; Levine, S. E.; Zuluaga, C. A.; Zangari, A. M.; Ruprecht, J. D.; Bowens-Rubin, R.; Brothers, T. C.; Berry, K. L.; Babcock, B. A.; Pasachoff, J. M.; Rojo, P.; Servajean, E.; Förster, F.; Naranjo, O. A.; Taylor, B. W.; Dunham, E. W.; Oswalt, T.; Batcheldor, D.; Murison, M.; Tilleman, T.; Harris, H. C.; Bright, L. P.; Schaefer, G.; Sallum, S.; Midkiff, A. H.; Mailhot, E. A.; Miller, C.; Morris, D.; Wodaski, R.; Bell, D.; Bird, P.; Fey, D.; Geisert, E.; Hastings, D.; Mizusawa, T.; Solenski, P.; Watson, B. Bibcode: 2013DPS....4540401B Altcode: We observed two stellar occultations on UT 4 May 2013 and UT 9 September 2012, with the aim of measuring Pluto's atmospheric parameters. Both of these events were a world-wide collaboration of many observers, and both occurred within one month of Pluto's stationary point. For the May 2013 occultation of an R=14.0 star, observations were attempted from several sites in Chile, Venezuela, Arizona, and Massachusetts. Positive detections were made from the DuPont 2.5-m at Las Campanas, the SMARTS 1-m at Cerro Tololo, and the 0.45-m telescope at Cerro Calan, all in Chile. For the September 2012 occultation of an R=15.2 star, observations were attempted from many sites along the east coast of the U.S., and in Arizona, New Mexico, and Texas. Successful atmosphere occultation light curves were obtained from the MONET 1.2-m at the McDonald Observatory and the FIT Ortega 0.8-m in Melbourne, Florida. From these data, we find that Pluto's atmosphere has maintained the basic parameters of the 2011 measurement (Person, et al., in press) with some small but significant structural changes. The atmospheric temperature and pressure are similar to 2011 values, while the "knee" structure at half-light has continued to evolve and has been further modified since 2011. This light curve evolution maps to changes in the temperature structure and/or haze distribution in the lower atmosphere approximately 1-2 scale heights above the surface. We will present these recent data and discuss their implications for atmospheric change on Pluto as well as extrapolations toward the New Horizons encounter in 2015. This work was supported in part by NASA Planetary Astronomy grants to MIT (NNX10AB27G) and Williams College (NNX08AO50G, NNH11ZDA001N), as well as grants from USRA (#8500-98-003) and Ames Research (#NAS2-97-01) to Lowell Observatory. The observations made at FIT were partially supported by the James and Sara Ortega Endowment. Title: The Cosmos Authors: Pasachoff, Jay M.; Filippenko, Alex Bibcode: 2013cosm.book.....P Altcode: Preface; About the authors; 1. A grand tour of the heavens; 2. Light, matter and energy: powering the Universe; 3. Light and telescopes: extending our senses; 4. Observing the stars and planets: clockwork of the Universe; 5. Gravitation and motion: the early history of astronomy; 6. The terrestrial planets: Earth, Moon, and their relatives; 7. The Jovian planets: windswept giants; 8. Pluto, comets, and space debris; 9. Our Solar System and others; 10. Our star: the Sun; 11. Stars: distant suns; 12. How the stars shine: cosmic furnaces; 13. The death of stars: recycling; 14. Black holes: the end of space and time; 15. The Milky Way: our home in the Universe; 16. A Universe of galaxies; 17. Quasars and active galaxies; 18. Cosmology: the birth and life of the cosmos; 19. In the beginning; 20. Life in the Universe; Epilogue; Appendices; Selected readings; Glossary; Index. Title: Letters to the Editor Authors: Pasachoff, J. M. Bibcode: 2013JRASC.107..179P Altcode: No abstract at ADS Title: 1565 nm Observations of the transit of Venus, Proxy for a Transiting Exoplanet Authors: Jaeggli, Sarah A.; Reardon, K. P.; Pasachoff, J. M.; Schneider, G.; Widemann, T.; Tanga, P. Bibcode: 2013SPD....44..150J Altcode: The transit of Venus in June 2012 provided a unique chance to view its atmosphere as we might see that of a transiting Cytherean exoplanet, through scattered and refracted illumination from its parent star. We performed spectroscopy and polarimetry during the transit of Venus focusing on extracting signatures of CO2 absorption of Venus from the solar spectrum. Although the predicted CO2 transmission spectrum of Venus was not particularly strong at 1565 nm, this region of the H-band often used in magnetic-field studies of the Sun's photosphere provides a particularly flat solar continuum with few atmospheric and molecular lines. Observations of Venus were taken throughout first contact and on the solar disk using the Facility InfraRed Spectropolarimeter on the Dunn Solar Telescope at the National Solar Observatory. The transit also provided a unique opportunity to investigate instrumental effects. In this poster we discuss initial results from the transit, including estimates for an exoplanet detection of this kind, preliminary comparison with atmospheric models, and the stray light properties of the instrument. This work was performed in collaboration with the Williams College Venus transit expedition, which was sponsored by Natl Geog/Comm for Research and Exploration. Title: The 2012 Total Eclipse Expeditions in Queensland Authors: Pasachoff, Jay M.; Babcock, B. A.; Lu, M.; Dantowitz, R.; Lucas, R.; Seiradakis, J. H.; Voulgaris, A.; Gaintatzis, P.; Steele, A.; Sterling, A. C.; Rusin, V.; Saniga, M. Bibcode: 2013SPD....44...51P Altcode: A total eclipse swept across Queensland and other sites in northeastern Australia on the early morning of 14 November 2012, local time. We mounted equipment to observe coronal images and spectra during the approximately 2 minutes of totality, the former for comparison with spacecraft images and to fill in the doughnut of imaging not well covered with space coronagraphs. Matching weather statistics, viewing was spotty, and our best observations were from a last-minute inland site on the Tablelands, with some observations from a helicopter at 9000 feet altitude over our original viewing site at Miallo. Only glimpses of the corona were visible at our Port Douglas and Trinity Beach, Cairns, locations, with totality obscured from our sites at Newell and Miallo, though some holes in the clouds provided coronal views from Palm Cove and elsewhere along the coast. Preliminary analysis of the spectra again shows Fe XIV stronger than Fe X, as in 2010 but not earlier, a sign of solar maximum, as was the coronal shape. An intriguing CME is discernible in the SE. Acknowledgments: We thank Terry Cuttle, Aram Friedman, Michael Kentrianakis, and Nicholas Weber for assistance and collaboration in Australia and Wendy Carlos for image processing. Our expedition was supported in part by NSF grant AGS-1047726 from Solar Terrestrial Research of the Atmospheric and Geospace Sciences Division, and by the Rob Spring Fund and Science Center funds at Williams College. ML was also supported in part by a Grant-In-Aid of Research from the National Academy of Sciences, administered by Sigma Xi, The Scientific Research Society (Grant ID: G20120315159311). VR and MS acknowledge support from projects VEGA 2/0003/13 and NGS-3139-12 of the National Geographic Society. We are grateful to K. Shiota (Japan) for kindly providing us with some of his 2012 eclipse coronal images. Title: Observations and Modeling of Solar Coronal Structures Using High-Resolution Eclipse Images and Space-based Telescopes with Wide Field of View Authors: Lu, Muzhou; Pasachoff, J. M.; Su, Y.; Van Ballegooijen, A. A.; Seaton, D. B.; West, M. Bibcode: 2013SPD....44...25L Altcode: We present a comparison of the solar corona observed during the total solar eclipses on 2010 July 11 and on 2012 November 13. The white light images were taken at Easter Island in 2010 and at Northeast Queensland, Australia, in 2012; while the concurrent EUV images were take with SDO/AIA and PROBA2/SWAP. The 2010 eclipse was observed at the beginning of Sunspot Cycle 24 [1], which peaked near our 2012 observation. We compare a plethora of corona features in the white light images and reveal some interesting differences in the enhanced EUV images taken by SDO/AIA and PROBA2/SWAP. We construct potential field models using our newly refined Coronal Modeling System (CMS2) software with line-of-sight photospheric magnetograms from SDO/HMI. The source surface heights derived from detailed comparison between our models and observations are compared to the standard source-surface model. We also compare the dynamics of the two eclipse observations. Similar to the 2010 eclipse, a CME was observed using temporally spaced eclipse images. We address unresolved problems in the models and observations with the hope of correcting them for future eclipse observations, such as the 2017 total solar eclipse across the continental U.S. References [1] Pasachoff, J. M., Rusin, V., Druckmüllerová, H., Saniga, M., Lu, M., Malamut, C., Seaton, D. B., Golub, L., Engell, A. J., Hill, S. W., Lucas, R., 2011, ApJ, 734, 114 Title: Transit Observations of Venus's Atmosphere in 2012 from Terrestrial and Space Telescopes as Exoplanet Analogs Authors: Pasachoff, Jay M.; Schneider, G.; Babcock, B. A.; Lu, M.; Penn, M. J.; Jaeggli, S. A.; Galayda, E.; Reardon, K. P.; Widemann, T.; Tanga, P.; Ehrenreich, D.; Vidal-Madjar, A.; Nicholson, P. D.; Dantowitz, R. Bibcode: 2013AAS...22221701P Altcode: We extensively observed the 8 June 2012 transit of Venus from several sites on Earth; we provide this interim status report about this and about two subsequent ToVs observed from space. From Haleakala Obs., we observed the entire June transit over almost 7 h with a coronagraph of the Venus Twilight Experiment B filter) and with a RED Epic camera to compare with simultaneous data from ESA's Venus Express, to study the Cytherean mesosphere; from Kitt Peak, we have near-IR spectropolarimetry at 1.6 µm from the aureole and during the disk crossing that compare well with carbon dioxide spectral models; from Sac Peak/IBIS we have high-resolution imaging of the Cytherean aureole for 22 min, starting even before 1st contact; from Big Bear, we have high-resolution imaging of Venus's atmosphere and the black-drop effect through 2nd contact; and we had 8 other coronagraphs around the world. For the Sept 21 ToV as seen from Jupiter, we had 14 orbits of HST to use Jupiter's clouds as a reflecting surface to search for an 0.01% diminution in light and a differential drop that would result from Venus's atmosphere by observing in both IR/UV, for which we have 170 HST exposures. As of this writing, preliminary data reduction indicates that variations in Jovian clouds and the two periods of Jupiter's rotation will be too great to allow extraction of the transit signal. For the December 20 ToV as seen from Saturn, we had 22 hours of observing time with VIMS on Cassini, for which we are looking for a signal of the 10-hr transit in total solar irradiance and of Venus's atmosphere in IR as an exoplanet-transit analog. Our Maui & Sac Peak expedition was sponsored by National Geographic Society's Committee for Research and Exploration; HST data reduction by NASA: HST-GO-13067. Some of the funds for the carbon dioxide filter for Sac Peak provided by NASA through AAS's Small Research Grant Program. We thank Rob Ratkowski of Haleakala Amateur Astronomers; Rob Lucas, Aram Friedman, Eric Pilger, Stan Truitt, and Steve Bisque/Software Bisque for Haleakala support/operations; Vasyl Yurchyshyn and Joseph Gangestad '06 of The Aerospace Corp. at Big Bear Solar Obs; LMSAL and Hinode science/operations team. Title: Standardizing the astronomical unit Authors: Pasachoff, Jay M. Bibcode: 2013PhTea..51..260P Altcode: No abstract at ADS Title: Pen & Pixel NGC 1055 and M77 / Comet Hergenrother / Milky Way / IC 342 / November Eclipse / The Crab Nebula / Milky Way with Trees Authors: Hilborn, Lynn; Paquette, Andre; Brasch, Klaus; Pasachoff, Jay; Hilborn, Lynn; Wilson, Dalton; Wiwchar, Sheila Bibcode: 2013JRASC.107...25H Altcode: No abstract at ADS Title: Three 2012 Transits of Venus: From Earth, Jupiter, and Saturn Authors: Pasachoff, Jay M.; Schneider, G.; Babcock, B. A.; Lu, M.; Edelman, E.; Reardon, K.; Widemann, T.; Tanga, P.; Dantowitz, R.; Silverstone, M. D.; Ehrenreich, D.; Vidal-Madjar, A.; Nicholson, P. D.; Willson, R. C.; Kopp, G. A.; Yurchyshyn, V. B.; Sterling, A. C.; Scherrer, P. H.; Schou, J.; Golub, L.; McCauley, P.; Reeves, K. Bibcode: 2013AAS...22131506P Altcode: We observed the 2012 June 6/5 transit seen from Earth (E/ToV), simultaneously with Venus Express and several other spacecraft not only to study the Cytherean atmosphere but also to provide an exoplanet-transit analog. From Haleakala, the whole transit was visible in coronal skies; among our instruments was one of the world-wide Venus Twilight Experiment's nine coronagraphs. Venus's atmosphere became visible before first contact. SacPeak/IBIS provided high-resolution images at Hα/carbon-dioxide. Big Bear's NST also provided high-resolution observations of the Cytherean atmosphere and black-drop evolution. Our liaison with UH's Mees Solar Observatory scientists provided magneto-optical imaging at calcium and potassium. Solar Dynamics Observatory's AIA and HMI, and the Solar Optical Telescope (SOT) and X-ray Telescope (XRT) on Hinode, and total-solar-irradiance measurements with ACRIMSAT and SORCE/TIM, were used to observe the event as an exoplanet-transit analog. On September 20, we imaged Jupiter for 14 Hubble Space Telescope orbits, centered on a 10-hour ToV visible from Jupiter (J/ToV), as an exoplanet-transit analog in our own solar system, using Jupiter as an integrating sphere. Imaging was good, although much work remains to determine if we can detect the expected 0.01% solar irradiance decrease at Jupiter and the even slighter differential effect between our violet and near-infrared filters caused by Venus's atmosphere. We also give a first report on our currently planned December 21 Cassini UVIS observations of a transit of Venus from Saturn (S/ToV). Our E/ToV expedition was sponsored by the Committee for Research and Exploration/National Geographic Society; supplemented: NASA/AAS's Small Research Grant Program. We thank Rob Ratkowski, Stan Truitt, Rob Lucas, Aram Friedman, and Eric Pilger '82 at Haleakala, and Joseph Gangestad '06 at Big Bear for assistance, and Lockheed Martin Solar and Astrophysics Lab and Hinode science and operations teams for support for coordinated observations with NASA satellites. Our J/ToV observations were based on observations made with HST, operated by AURA, Inc., under NASA contract NAS 5-26555; these observations are associated with program #13067. Title: A Major Discovery in Doubt Authors: Pasachoff, Jay M.; Sheehan, William Bibcode: 2013S&T...125a..86P Altcode: No abstract at ADS Title: Innovation in Astronomy Education Authors: Pasachoff, Jay M.; Ros, Rosa M.; Pasachoff, Naomi Bibcode: 2013iae..book.....P Altcode: Preface; Part I. General Strategies for Effective Teaching: Introduction; 1. Main objectives of SpS2; 2. Learning astronomy by doing astronomy; 3. Hands-on Universe-Europe; 4. Life on Earth in the atmosphere of the Sun; 5. A model of teaching astronomy to pre-service teachers; 6. How to teach, learn about, and enjoy astronomy; 7. Clickers: a new teaching tool of exceptional promise; 8. Educational opportunities in pro-am collaboration; 9. Teaching history of astronomy to second-year engineering students; 10. Teaching the evolution of stellar and Milky Way concepts through the ages; 11. Educational efforts of the International Astronomical Union; 12. Astronomy in culture; 13. Light pollution: a tool for astronomy education; 14. Astronomy by distance learning; 15. Edible astronomy demonstrations; 16. Amateur astronomers as public outreach partners; 17. Does the Sun rotate around Earth or Earth rotate around the Sun?; 18. Using sounds and sonifications for astronomy outreach; 19. Teaching astronomy and the crisis in science education; 20. Astronomy for all as part of a general education; Poster abstracts; Part II. Connecting Astronomy with the Public: Introduction; 21. A status report from the Division XII working group; 22. Outreach using media; 23. Astronomy podcasting; 24. IAU's communication strategy, hands-on science communication, and the communication of the planet definition discussion; 25. Getting a word in edgeways: the survival of discourse in audiovisual astronomy; 26. Critical evaluation of the new Hall of Astronomy; 27. Revitalizing astronomy teaching through research on student understanding; Poster abstracts; Part III. Effective Use of Instruction and Information Technology: Introduction; 28. ESO's astronomy education program; 29. U.S. student astronomy research and remote observing projects; 30. Global network of autonomous observatories dedicated to student research; 31. Remote telescopes in education: report of an Australian study; 32. Visualizing large astronomical data holdings; Poster abstracts; Part IV. Practical Issues Connected with the Implementation of the 2003 IAU Resolution: Introduction; 33. Stellar evolution for students of Moscow University; 34. Astronomy for everybody: An approach from the CASAO/NAUH view; 35. Toward a new program in astronomy education in secondary schools in Turkey; 36. Universe awareness for young children; 37. Education in Egypt and Egyptian responses to eclipses; 38. Astronomy in the cultural heritage of African societies; 39. Education at the Pierre Auger Observatory: the cinema as a tool in science education; 40. Freshman seminars: interdisciplinary engagements in astronomy; 41. Astronomy for teachers; Poster abstracts; Conclusion. Title: Mingantu, 18th-Century Mongol Astronomer and Radioheliograph Namesake Authors: Pasachoff, Jay M. Bibcode: 2013AAS...22113003P Altcode: The 18th-century Mongol astronomer Mingantu (1692-1765) has been honored with a city named after him and a nearby solar telescope array. During the IAU/Beijing, my wife and I went to the new Chinese solar radioheliograph, the Mingantu Observing Station, in Inner Mongolia, ~400 km northwest of Beijing, a project of the National Astronomical Observatories, Chinese Academy of Sciences. It currently contains 40 dishes each 4.5 m across, with a correlator from Beijing. Within a year, 60 2-m dishes will be added. We passed by the 12-century ruins of Xanadu (about 20 km north of Zhangbei) about halfway. The radioheliograph is in a plane about 1 km across, forming a three-armed spiral for interferometric solar mapping, something colleagues and I had carried out with the Jansky Very Large Array, taking advantage of the lunar occultation before annularity at the 20 May 2012 solar eclipse. In the central square of Mingantu city, a statue ~10-m high of the Mongol astronomer Mingantu appears. Its base bears a plaque ~1-m high of IAU Minor Planet Circular MPC 45750 announcing the naming in 2002 of asteroid 28242 Mingantu, discovered at a Chinese observatory in 1999. Mingantu carried out orbital calculations, mapping, mathematical work on infinite series, and other scientific research. He is honored by a modern museum behind the statue. The museum's first 40% describes Mingantu and his work, and is followed by some artifacts of the region from thousands of years ago. The final, large room contains a two-meter-square scale model of the radioheliograph, flat-screen televisions running Solar Dynamics Observatory and other contemporary visualizations, orreries and other objects, and large transparencies of NASA and other astronomical imagery. See my post at http://www.skyandtelescope.com/community/skyblog/newsblog/ specfically Astro-Sightseeing_in_Inner_Mongolia-167712965.html. We thank Yihua Yan for arranging the visit and Wang Wei (both NAOC) for accompanying us. My solar research is supported by grant 1047726 from the Solar Research Program/Atmospheric and Geospace Sciences Division/NSF. I am also grateful for a NSF travel grant through AAS. Title: Syzygy x 3 Authors: Pasachoff, Jay M. Bibcode: 2013obha.book....9P Altcode: No abstract at ADS Title: The 2012 Transit of Venus: A Closer Look at the Cytherean Aureole Authors: Edelman, Eric; Pasachoff, J. M.; Schneider, G.; Babcock, B. A.; Lu, M.; Reardon, K.; Widemann, T.; Tanga, P.; Dantowitz, R. Bibcode: 2013AAS...22135304E Altcode: The 2012 Transit of Venus provided a new opportunity to study the events that occur during the ingress and egress of transit in greater detail. The Venus Twilight Experiment is a group that was formed to analyze the twilight phenomena of Venus through close and careful observation of planet’s 21st century transits. One particular object of interest to this group is the Cytherean aureole, or the arc of light caused by refraction of the Sun’s light through Venus’s upper atmosphere. A goal associated with the study of this aureole is to measure how the brightness of the atmosphere changes over time and as a function of latitude on Venus with the use of the multitude of images taken of the planet near the beginning and end of the transit. In order to further along this goal, I was tasked with sorting, processing, and aligning the images taken by the coronagraph used on the 2012 Williams College Transit of Venus Expedition at Haleakala, Hawaii. Our observations through a B filter will be compared with observations through VRI-filter observations from other coronagraphs in the set. This was research was performed with the support of the Keck Northeast Astronomy Consortium, sponsored by the NSF and the Keck foundation. The expedition to Haleakala and Sac Peak was sponsored by the Committee for Research and Exploration/National Geographic Society. Some funds for the IBIS carbon-dioxide filter came from NASA/AAS's Small Research Grant Program. We thank Rob Ratkowski, Stan Truitt, Rob Lucas, Aram Friedman, and Eric Pilger '82 for assistance with Haleakala observing. Title: Solar Eclipses Observed from Antarctica Authors: Pasachoff, Jay M. Bibcode: 2013IAUS..288..313P Altcode: Aspects of the solar corona are still best observed during totality of solar eclipses, and other high-resolution observations of coronal active regions can be observed with radio telescopes by differentiation of occultation observations, as we did with the Jansky Very Large Array for the annular solar eclipse of 2012 May 20 in the US. Totality crossing Antarctica included the eclipse of 2003 November 23, and will next occur on 2021 December 4; annularity crossing Antarctica included the eclipse of 2008 February 7, and will next occur on 2014 April 29. Partial phases as high as 87% coverage were visible and were imaged in Antarctica on 2011 November 25, and in addition to partial phases of the total and annular eclipses listed above, partial phases were visible in Antarctica on 2001 July 2011, 2002 December 4, 2004 April 19, 2006 September 22, 2007 September 11, and 2009 January 26, and will be visible on 2015 September 13, 2016 September 1, 2017 February 26, 2018 February 15, and 2020 December 14. On behalf of the Working Group on Solar Eclipses of the IAU, the poster showed the solar eclipses visible from Antarctica and this article shows a subset (see www.eclipses.info for the full set). A variety of investigations of the Sun and of the response of the terrestrial atmosphere and ionosphere to the abrupt solar cutoff can be carried out at the future eclipses, making the Antarctic observations scientifically useful. Title: The Comets of Caroline Herschel (1750-1848), Sleuth of the Skies at Slough Authors: Olson, Roberta J. M.; Pasachoff, Jay M. Bibcode: 2012arXiv1212.0809O Altcode: In this paper, we discuss the work on comets of Caroline Herschel, the first female comet-hunter. After leaving Bath for the environs of Windsor Castle and eventually Slough, she discovered at least eight comets, five of which were reported in the Philosophical Transactions of the Royal Society. We consider her public image, astronomers' perceptions of her contributions, and the style of her astronomical drawings that changed with the technological developments in astronomical illustration. Title: A Coral Sea Rehearsal for the Eclipse Megamovie Authors: Hudson, H. S.; Davey, A. R.; Ireland, J.; Jones, L.; Mcintosh, S. W.; Paglierani, R.; Pasachoff, J. M.; Peticolas, L. M.; Russell, R. M.; Suarez Sola, F. I.; Sutherland, L.; Thompson, M. J. Bibcode: 2012AGUFMSH11C..06H Altcode: The "Eclipse on the Coral Sea" - 13/14 November 2012 (GMT/Australia) - will have happened already. Our intention is to have used this opportunity as a trial run for the eclipse in 2017, which features 1.5 hours of totality across the whole width of the continental US. Conceived first and foremost as an education and public outreach activity, the plan is to engage the public in solar science and technology by providing a way for them to include images they have taken of the solar eclipse, into a movie representation of coronal evolution in time. This project will assimilate as much eclipse photography as possible from the public. The resulting movie(s) will cover all ranges of expertise, and at the basic smartphone or hand-held digital camera level, we expect to have obtained a huge number of images in the case of good weather conditions. The capability of modern digital technology to handle such a data flow is new. The basic purpose of this and the 2017 Megamovie observations is to explore this capability and its ability to engage people from many different communities in the solar science, astronomy, mathematics, and technology. The movie in 2017, especially, may also have important science impact because of the uniqueness of the corona as seen under eclipse conditions. In this presentation we will describe our smartphone application development (see the "Transit of Venus" app for a role model here). We will also summarize data acquisition via both the app and more traditional web interfaces. Although for the Coral Sea eclipse event we don't expect to have a movie product by the time of the AGU, for the 2017 event we do intend to assemble the heterogenous data into beautiful movies within a short space of time after the eclipse. These movies may have relatively low resolution but would extend to the base of the corona. We encourage participation in the 2012 observations, noting that no total eclipse, prior to 2017, will occur in a region with good infrastructure for extended observations. The National Center for Atmospheric Research is sponsored by the National Science Foundation. The Megamovie project is supported by NSF grant AGS-1247226, and JMP's eclipse work about the eclipses of 2012 is supported by NSF grant AGS-1047726. Title: Venus's Atmosphere: Discoverer Debatable I Authors: Pasachoff, Jay M.; Sheehan, William Bibcode: 2012S&T...124d...8P Altcode: No abstract at ADS Title: A Glorious Transit of Venus Authors: Pasachoff, Jay M. Bibcode: 2012S&T...124d..20P Altcode: No abstract at ADS Title: The Venus Twilight Experiment: Probing The Mesosphere In 2004 And 2012 Authors: Tanga, Paolo; Widemann, T.; Ambastha, A.; Babcock, B. A.; Berthier, J.; Bouley, S.; Braga-Ribas, F.; Brasch, K.; Burke, W.; Colas, F.; Fukuhara, T.; Fulham, L.; Imai, M.; Lu, M.; Machado, P.; Maquet, L.; Pasachoff, J. M.; Roberts, J.; Schneider, G.; Sheehan, W.; Sigismondi, C.; Thouvenin, N.; Vachier, F.; Veillet, C.; Wang, X. Bibcode: 2012DPS....4450807T Altcode: During the Venus transit in 2004 several observers collected data useful to the characterization of the mesosphere of the planet, by observing the solar light refracted at the corresponding altitude range. The "aureole" thus formed, is observable during the ingress and egress phases of the transit, when Venus is crossing the solar limb. For the 2012 opportunity we prepared a set of coronagraphs to obtain multi-wavelength, space- and time-resolved photometry of the aureole, in collaboration with other space- and ground-based campaigns. The coronagraphs were distributed in the visibility area around the Pacific, over eight sites where local logistic support and scientific expertise were present. Several sites obtained useful data at frame rates of several images/sec. We will give an account of the campaign presenting first results obtained at 450, 535, 607 and 760 nm (FWHM 10 nm). A comparison with data collected at the 2004 transit shows that variations in the aspects of the aureole are present. These can be linked to variations in the vertical distribution of the absorbers (aerosols and cloud-top level). A common feature in both the recent transits is the presence of a brightness peak at high latitude, which was imaged several minutes before and after first and last contact, respectively. The historical record of the aureole contains hints of varying features and a constant polar-spot presence, which can now be interpreted in the light of the measurements obtained in 2004 and 2012. Title: Pluto’s Atmosphere from the 23 June 2011 Stellar Occultation: Airborne and Ground Observations Authors: Person, Michael J.; Bosh, A. S.; Levine, S. E.; Gulbis, A. A. S.; Zangari, A. M.; Zuluaga, C. A.; Dunham, E. W.; Pasachoff, J. M.; Babcock, B. A.; Pandey, S.; Armhein, D.; Sallum, S.; Tholen, D. J.; Collins, P.; Bida, T.; Taylor, B.; Wolf, J.; Meyer, A.; Pfueller, E.; Wiedermann, M.; Roesser, H.; Lucas, R.; Kakkala, M.; Ciotti, J.; Plunkett, S.; Hiraoka, N.; Best, W.; Pilger, E. L.; Miceli, M.; Springmann, A.; Hicks, M.; Thackeray, B.; Emery, J.; Rapoport, S.; Ritchie, I. Bibcode: 2012DPS....4430402P Altcode: The double stellar occultation by Pluto and Charon of 2011 June 23 was observed from numerous ground stations as well as the Stratospheric Observatory for Infrared Astronomy (SOFIA). This first airborne occultation observation since 1995 resulted in the best occultation chords recorded for the event, in three optical wavelength bands. The data obtained from SOFIA were combined with chords obtained from the ground at the IRTF (including a full spectral light curve), the USNO--Flagstaff Station, and Leeward Community College to give a detailed profile of Pluto’s atmosphere. The data show a return to the distinct upper and lower atmospheric regions with a knee, or kink in the light curves separating them as was observed in 1988 (Millis et al. 1993), rather than the smoothly transitioning bowl-shaped light curves of recent years (Elliot et al. 2007). We analyze the upper atmosphere by fitting a model to all of the light curves obtained, resulting in a half-light radius of 1288 ± 1 km. We analyze the lower atmosphere with two different methods to provide results under the separate assumptions of particulate haze and a strong thermal gradient. Results indicate that the lower atmosphere evolves on short seasonal timescales, changing between 1988 and 2006, and then returning to approximately the 1988 state in 2011, though at significantly higher pressures. Throughout these changes, the upper atmosphere remains remarkably stable in structure, again excepting the overall pressure changes. No evidence of the onset of atmospheric collapse predicted by frost migration models is yet seen, and the atmosphere appears to be remaining at a stable pressure level. This work was supported in part by NASA Planetary Astronomy grants to MIT (NNX10AB27G) and Williams College (NNX08AO50G, NNH11ZDA001N), as well as grants from USRA (#8500-98-003) and Ames Research (#NAS2-97-01) to Lowell Observatory. Title: The 2012 Transit of Venus for Cytherean Atmospheric Studies and as an Exoplanet Analog Authors: Pasachoff, Jay M.; Schneider, G.; Babcock, B. A.; Lu, M.; Reardon, K. P.; Widemann, T.; Tanga, P.; Dantowitz, R.; Willson, R.; Kopp, G.; Yurchyshyn, V.; Sterling, A.; Scherrer, P.; Schou, J.; Golub, L.; Reeves, K. Bibcode: 2012DPS....4450806P Altcode: We worked to assemble as complete a dataset as possible for the Cytherean atmosphere in collaboration with Venus Express in situ and to provide an analog of spectral and total irradiance exoplanet measurements. From Haleakala, the whole transit was visible in coronal skies; our B images showed the evolution of the visibility of Venus's atmosphere and of the black-drop effect, as part of the Venus Twilight Experiment's 9 coronagraphs distributed worldwide with BVRI. We imaged the Cytherean atmosphere over two minutes before first contact, with subarcsecond resolution, with the coronagraph and a separate refractor. The IBIS imaging spectrometer at Sacramento Peak Observatory at H-alpha and carbon-dioxide also provided us high-resolution imaging. The NST of Big Bear Solar Observatory also provided high-resolution vacuum observations of the Cytherean atmosphere and black drop evolution. Our liaison with UH's Mees Solar Observatory scientists provided magneto-optical imaging at calcium and potassium. Spaceborne observations included the Solar Dynamics Observatory's AIA and HMI, and the Solar Optical Telescope (SOT) and X-ray Telescope (XRT) on Hinode, and total-solar-irradiance measurements with ACRIMSAT and SORCE/TIM, to characterize the event as an exoplanet-transit analog. Our expedition was sponsored by the Committee for Research and Exploration/National Geographic Society. Some of the funds for the carbon-dioxide filter for IBIS were provided by NASA through AAS's Small Research Grant Program. We thank Rob Lucas, Aram Friedman, and Eric Pilger '82 for assistance with Haleakala observing, Rob Ratkowski of Haleakala Amateur Astronomers for assistance with equipment and with the site, Stan Truitt for the loan of his Paramount ME, and Steve Bisque/Software Bisque for TheSky X controller. We thank Joseph Gangestad '06 of Aerospace Corp., a veteran of our 2004 expedition, for assistance at Big Bear. We thank the Lockheed Martin Solar and Astrophysics Laboratory and Hinode science and operations teams for planning and support. Title: Assymetry in the Polar Mesosphere Revealed by the 2012 Venus Transit Aureole Authors: Widemann, Thomas; Tanga, P.; Reardon, K. P.; Limaye, S.; Wilson, C.; Vandaele, A.; Wilquet, V.; Mahieux, A.; Robert, S.; Pasachoff, J. M.; Schneider, G. Bibcode: 2012DPS....4450808W Altcode: Close to ingress and egress phases, the fraction of Venus disk projected outside the solar photosphere appears outlined by an irregular thin arc of light called the "aureole." We have shown that the deviation due to refraction and the aureole intensity are related to the local density scale height and the altitude of the refraction layer (Tanga et al. 2012). Since the aureole brightness is the quantity that can be measured during the transit, an appropriate model allows us to determine both parameters. We now compare this model developed for the 2004 data to the first results of 2012 campaign. Ingress pictures of NASA's SDO/HMI observations, OP-OCA/VTE coronagraph observations at Haleakala and Lowell stations, and Dunn/IBIS observations at Sacramento Peak, NM, show latitudinal structure of the aureole during the ingress phase of the Venus transit. For the HMI data, the temporal cadence is 3.75 sec and the pixel scale is 0.5 arcsec/pixel. The polar region, significantly brighter in initial phases due to the larger scale height of the polar mesosphere, appears consistently offset toward morning terminator by about 15 deg. latitude, peaking at 75N at 6:00 local time. This result reflects local latitudinal structure in the polar mesosphere, either in temperature or aerosol altitude distribution. Relation with ESA / Venus Express / SOIR simultaneous measurements and dynamical interpretation will be discussed at the meeting. Tanga et al. 2012, Icarus 218, 207-219 Title: Print, Web, And Podcast Tov Public Outreach Authors: Pasachoff, Jay M. Bibcode: 2012DPS....4441110P Altcode: As part of alerting the general public to the subtly spectacular transit of Venus as an intellectual marvel not available to us from Earth until AD 2117/2125, in addition to our scientific plans (Pasachoff et al., this meeting), I provided: (1) an article in the children's magazine Odyssey (May/June 2011); (2) a discussion in National Geographic Society's BreakingOrbit blog (March 1, 2011); (3) and a year's advance notice as "June 5: Transit of Venus," 365daysofastronomy.org. (4) Nantes DPS: I participated in "Transits of Venus in Public Education and Contemporary Research" (http://transitofvenus.nl/wp/2011/10/16/four-giants-talk-about-transits). (5) 22-minute lecture on the Phi Beta Kappa website: http://www.pbk.org/home/playpodcast.aspx?id=772. (6) E/PO summary at Historical Astronomy Division News, #79, October. Closer to the event, I had a (7) Comment in Nature ("Transit of Venus: Last Chance to See," Nature 485, 303-304) and (8, 9) articles in Physics World, 25, 36-41; and Scientific American, http://www.scientificamerican.com/article.cfm?id=transit-venus-june-5). The day before the transit, (10) I had a radio/podcast Academic Minute (http://www.wamc.org/post/dr-jay-pasachoff-williams-college). (11) On transit day, I had an Op-Ed piece in The New York Times ("Learning from Celestial Beauty," http://www.nytimes.com/2012/06/05/opinion/learning-from-celestial-beauty.html) that was seen by largely a non-scientific audience. Subsequently, (12) I gave a Keck-Observatory-sponsored Waimea general-public lecture (http://keckobservatory.org/news/video_venus_transits_past_present_future), and (13) an invited public lecture at the AAS meeting in Anchorage (http://aas.org/meetings/aas220/video_session_127). I had a podcast on (14) 365daysofastronomy.org (June 29). (15) My article for Sky & Telescope appeared in its October issue. (16) My editorial "Syzygy x 3" will be in RASC Observer's Handbook 2013. (16) These efforts as well as links to history and science of transits of Mercury and Venus are at http://sites.williams.edu/transitofvenus2012/links/ as part of my website http://www.transitofvenus.info. Acknowledgments: My expeditions to the 2004 and 2012 transits of were supported by grants from the Committee for Research and Exploration of the National Geographic Society. Title: Probing Pluto’s Upper Atmosphere: a 2011 Occultation Graze in Visible Images and Infrared Spectra Authors: Gulbis, Amanda A. S.; Emery, J. P.; Person, M. J.; Bosh, A. S.; Zuluaga, C. A.; Pasachoff, J. M.; Babcock, B. A. Bibcode: 2012DPS....4430403G Altcode: On 2011 June 23, a 14.43 UCAC2 magnitude star was occulted by Pluto as observed from multiple sites. Observations made at NASA’s 3-m Infrared Telescope Facility (IRTF) on Mauna Kea, Hawaii, detected a full occultation of the star by Charon followed by an atmospheric graze by Pluto. Data were taken simultaneously with MORIS (the MIT Optical Rapid Imaging System; Gulbis et al. 2011, PASP, 123, 461) and SpeX (Rayner et al. 2003, PASP, 115, 362). MORIS recorded visible images of a 1 arcmin by 1 arcmin field of view, with an effective central wavelength of 0.74 microns, at a cadence of 0.3 seconds and negligible deadtime. Low-resolution spectral IR data of the occultation star and a comparison were taken with SpeX, using the 1.6 arcsec slit, over the range of 0.9-2.5 microns, at a cadence of 1.5 seconds including approximately 0.75 seconds deadtime. Pluto’s lower atmosphere has been evolving since the first definitive detection in 1988 (e.g., Elliot et al. 2007, AJ, 134,1; Young et al. 2008, AJ, 136, 1757). Possibilities for explaining the lower atmospheric structure include a steep thermal gradient and/or extinction, the latter of which can be characterized as a dependence between occultation flux and wavelength. This graze reached a minimum normalized flux level of roughly 0.35, serving primarily as a probe of Pluto’s upper atmosphere. However, there appears to be a slight dependence of flux with wavelength in the minimum portion of the graze. We will present the IRTF lightcurves and an analysis of the wavelength-resolved data. Funding for this work was provided in part by the South African National Research Foundation and NASA grants NNX08AO50G & NNH11ZDA001N (Williams), NNX10AB27G (MIT), and NNX10AB23G (UT). Title: Venus Twilight Experiment : Observation and analysis of the aureole during the 2012 transit Authors: Widemann, T.; Tanga, P.; Sicardy, B.; Machado, P.; Braga-Ribas, F.; Veillet, C.; Pasachoff, J.; Colas, F.; Vachier, F.; Bouley, S.; Maquet, L.; Berthier, J.; Fukuhara, T.; Luz, D. Bibcode: 2012epsc.conf..412W Altcode: 2012espc.conf..412W On 5-6 June 2012, Venus will be transiting the Sun for the last time in this century. This unique opportunity, besides offering the opportunity of investigating the mesosphere of the planet, also provides a significant nearby analog of exoplanet transits. Several studies using the transmission spectroscopy technique have provided significant insights into the atmospheric composition, structure, and dynamics of hot giant exoplanets. In this context, Venus is our closest model for a telluric exoplanet. Title: Expeditions to Death and Disaster: Chappe d'Auteroche and Charles Green at the 1769 Transit of Venus Authors: Pasachoff, Jay M. Bibcode: 2012icha.book...24P Altcode: Scientific expeditions usually bring back information or specimens that forward human knowledge. We also prefer them to bring back the humans in good shape, but that does not always occur. I discuss the expeditions to Siberia in 1761 and to Baja California in 1769 by the French abbé Jean Chappe d'Auteroche and to Tahiti in 1769 by the English astronomer Charles Green, accompanying Captain James Cook, to observe the transits of Venus. Neither Chappe d'Auteroche nor Green survived their expeditions. Chappe managed to hang on after the transit to see an eclipse of the Moon about two weeks later, and it is said that since ``the intent of his voyage was fulfilled, and the fruit of his observations secured,'' he ``died content,'' since ``he saw nothing more to wish for.'' Green died of dysentery caught in Batavia (now in Indonesia) on the continuation of his expedition with Capt. Cook on the ship Endeavour after the transit. Title: New Obituary Policy for the American Astronomical Society Authors: Pasachoff, Jay M. Bibcode: 2012opsa.book..319P Altcode: The American Astronomical Society has a permanent website with obituaries of nearly all its members who have died since 1990.The Vice Chair of the Historical Astronomy Division (HAD) is tasked with selecting authors and editing the obituaries, which are posted by the AAS headquarters staff on a site; an alphabetical index appears at the Historical Astronomy Division's site, which is linked from their top-level page. The HAD was asked to be in charge of obituaries by the AAS Council in 1990.Most obituaries are in the vicinity of 800 words, but longer essays are allowable for selected individuals. Title: Transit of Venus: Last chance to see Authors: Pasachoff, Jay M. Bibcode: 2012Natur.485..303P Altcode: The June 2012 transit of Venus across the Sun offers an opportunity to check our methods for spotting distant planets crossing far-away stars, says Jay M. Pasachoff. Title: The Black Drop Effect Authors: Pasachoff, Jay M. Bibcode: 2012S&T...123R...8P Altcode: No abstract at ADS Title: Spectroscopic Coronal Observations During the Total Solar Eclipse of 11 July 2010 Authors: Voulgaris, A. G.; Gaintatzis, P. S.; Seiradakis, J. H.; Pasachoff, J. M.; Economou, T. E. Bibcode: 2012SoPh..278..187V Altcode: 2012arXiv1202.1535V The flash spectra of the solar chromosphere and corona were measured with a slitless spectrograph before, after, and during the totality of the solar eclipse of 11 July 2010, at Easter Island, Chile. This eclipse took place at the beginning of Solar Cycle 24, after an extended minimum of solar activity. The spectra taken during the eclipse show a different intensity ratio of the red and green coronal lines compared with those taken during the total solar eclipse of 1 August 2008, which took place toward the end of Solar Cycle 23. The characteristic coronal emission line of forbidden Fe XIV (5303 Å) was observed on the east and west solar limbs in four areas relatively symmetrically located with respect to the solar rotation axis. Subtraction of the continuum flash-spectrum background led to the identification of several extremely weak emission lines, including forbidden Ca XV (5694 Å), which is normally detected only in regions of very high excitation, e.g., during flares or above large sunspots. The height of the chromosphere was measured spectrophotometrically, using spectral lines from light elements and compared with the equivalent height of the lower chromosphere measured using spectral lines from heavy elements. Title: Transits of Venus and Mercury: Exoplanet Analogs in Our Solar System Authors: Pasachoff, Jay M. Bibcode: 2012AAS...22012701P Altcode: Since Johannes Kepler's predictions of transits of Mercury and Venus in 1631, and observations by Jeremiah Horrocks and William Crabtree of the 1639 transit of Venus, only 5 other transits of Venus have been observed: in 1761 and 1769, 1874 and 1882, and 2004. Expeditions were sent all over the world for the 18th and 19th century transits to follow the methods of Halley and others to determine the Astronomical Unit, giving the size and scale of the solar system, arguably the most important problem in astronomy for centuries. I will discuss how the infamous black-drop effect bedeviled astronomers in that quest for an accurate A.U., and how Glenn Schneider and I explained the effect through satellite observations of transits of Mercury, showing that it was not simply caused by the Cytherean atmosphere. During the 2004 transit, we worked with Richard Willson of ACRIMsat to detect the 0.1% drop in the Total Solar Irradiance, showing the effect of solar limb darkening, positioning such observations of transits of Venus and of Mercury as analogs to exoplanet transits. Our observations of the atmosphere of Venus with NASA's Transition Region and Coronal Explorer in 2004 led us to plan extensive observations of Venus's atmosphere and other phenomena during the June 5, 2012, transit of Venus, the last to be visible from Earth until 2117. We will have used NASA's Solar Dynamics Observatory, Hinode, ACRIMsat, and other spacecraft, and ground-based solar telescopes at Sacramento Peak, Kitt Peak, Big Bear, and Haleakala to observe the transit; I hope to give preliminary reports on these observations during this talk. Further, I will discuss the plans of Ehrenreich and colleagues for Hubble observations of this transit and our hopes of detecting transits of Venus and Earth as seen from Jupiter and Saturn over the next few years. Title: Lomonosov, the discovery of Venus's atmosphere, and the eighteenth-century transits of Venus Authors: Pasachoff, Jay M.; Sheehan, William Bibcode: 2012JAHH...15....3P Altcode: The discovery of Venus's atmosphere has been widely attributed to the Russian academician M.V. Lomonosov from his observations of the 1761 transit of Venus from St. Petersburg. Other observers at the time also made observations that have been ascribed to the effects of the atmosphere of Venus. Though Venus does have an atmosphere one hundred times denser than the Earth's and refracts sunlight so as to produce an 'aureole' around the planet's disk when it is ingressing and egressing the solar limb, many eighteenth century observers also upheld the doctrine of cosmic pluralism: believing that the planets were inhabited, they had a preconceived bias for believing that the other planets must have atmospheres. A careful re-examination of several of the most important accounts of eighteenth century observers and comparisons with the observations of the nineteenth century and 2004 transits shows that Lomonosov inferred the existence of Venus's atmosphere from observations related to the 'black drop', which has nothing to do with the atmosphere of Venus. Several observers of the eighteenth-century transits, includ-ing Chappe d'Auteroche, Bergman, and Wargentin in 1761 and Wales, Dymond, and Rittenhouse in 1769, may have made bona fide observations of the aureole produced by the atmosphere of Venus. Therefore, it appears that several observers-but not Lomonosov-should receive credit for first detecting the aureole due to refraction of sunlight by the atmosphere of Venus during a transit. This crucial observation occurred almost three decades before Johann Schroeter independently demonstrated the existence of the atmosphere of Venus from his analysis of extensions of the semicircle of light of the planet near inferior conjunction, which are produced by back-scattering of light by aerosol-sized particles. Title: Sunlight refraction in the mesosphere of Venus during the transit on June 8th, 2004 Authors: Tanga, P.; Widemann, T.; Sicardy, B.; Pasachoff, J. M.; Arnaud, J.; Comolli, L.; Rondi, A.; Rondi, S.; Sütterlin, P. Bibcode: 2012Icar..218..207T Altcode: 2011arXiv1112.3136T Many observers in the past gave detailed descriptions of the telescopic aspect of Venus during its extremely rare transits across the Solar disk. In particular, at the ingress and egress, the portion of the planet’s disk outside the Solar photosphere has been repeatedly perceived as outlined by a thin, bright arc (“aureole”). Those historical visual observations allowed inferring the existence of Venus’ atmosphere, the bright arc being correctly ascribed to the refraction of light by the outer layers of a dense atmosphere. On June 8th, 2004, fast photometry based on electronic imaging devices allowed the first quantitative analysis of the phenomenon. Several observers used a variety of acquisition systems to image the event - ranging from amateur-sized to professional telescopes and cameras - thus collecting for the first time a large amount of quantitative information on this atmospheric phenomenon. In this paper, after reviewing some elements brought by the historical records, we give a detailed report of the ground based observations of the 2004 transit. Besides confirming the historical descriptions, we perform the first photometric analysis of the aureole using various acquisition systems. The spatially resolved data provide measurements of the aureole flux as a function of the planetocentric latitude along the limb. A new differential refraction model of solar disk through the upper atmosphere allows us to relate the variable photometry to the latitudinal dependency of scale-height with temperature in the South polar region, as well as the latitudinal variation of the cloud-top layer altitude. We compare our measurements to recent analysis of the Venus Express VIRTIS-M, VMC and SPICAV/SOIR thermal field and aerosol distribution. Our results can be used a starting point for new, more optimized experiments during the 2012 transit event. Title: Transits Of Venus: 1639, 1761, 1769, 1874, 1882, 2004, And 2012 Authors: Pasachoff, Jay M. Bibcode: 2012AAS...219.9001P Altcode: Transits of Venus are exceedingly rare predictable astronomical events, with only six having been observed since Jeremiah Horrox corrected Johannes Kepler's Rudolphine Tables and observed the transit of 1639. Edmond Halley's 1716 method of finding the size and scale of the Solar System and thus of the Universe led to hundreds of 18th-century and 19th-century transit-of-Venus expeditions for each event. I discuss the history and importance of the transit observations, and how spacecraft observations of the 1999 transit of Mercury, repeated at the 2003 and 2006 transits, led to the solution of the black-drop effect problem that had prevented Halley's method from reaching its desired accuracy and thus solution of the noble problem of astronomy to find the size and scale of the solar system. Other spacecraft observations of the 2004 transit of Venus have led to an analysis of how Venus's atmosphere becomes visible for about 25 minutes before second contact and after third contact, and links with prior historical claims, mostly invalid, to have discovered Venus's atmosphere at transits. Total-solar-irradiance spacecraft observations at the 2004 Venus transit link to exoplanet discoveries with NASA's aptly named Kepler Mission and ESA's CoRoT. I further link previous transit observations to planned observations for the June 5/6, 2012, Venus transit and the May 9, 2016, Mercury transit, together providing a historical basis for 22nd-century astronomers preparing to observe the December 10, 2117, Venus transit.

My observations at the 2004 and 2012 transits of Venus were and will be supported in large part by grants from the Committee for Research and Exploration of the National Geographic Society. My solar observations were supported in part by NASA grant NNG04GK44G for work with the TRACE spacecraft and NASA Marshall grant NNX10AK47A and planetary work supported in part by NNX08AO50G from NASA Planetary Astronomy. Title: Ten years of the high-resolution imaging process of the eclipse white-light corona Authors: Rusin, V.; Saniga, M.; Pasachoff, J.; Druckmuller, M.; Belik, M. Bibcode: 2011AGUFMSH33A2031R Altcode: The corona is the uppermost part of the Sun's atmosphere and, up to now, total solar eclipses provide the best conditions for observing it from Earth's surface. The white-light corona (WLC) is the scattered light of the photosphere off free electrons and it dominates in the regions up to 2-3 solar radii. As the motion of electrons is governed by magnetic fields of the corona, and these fields are sensitive to the phase of the solar cycle, the WLC exhibits many faces and a variety of fine structures throughout a cycle. When observing the WLC, one faces problems due to a steep gradient of its brightness and difficulties in discerning individual structures. Our contribution presents a set of unique eclipse pictures of the WLC that were processed by Druckmüller's method; they cover the period from 2001 to 2010 and thus give a fairly good idea about the changes in both the shape and the fine structure of the WLC over a whole solar cycle. Title: Structure and Dynamics of the 2009 July 22 Eclipse White-light Corona Authors: Pasachoff, J. M.; Rušin, V.; Saniga, M.; Druckmüllerová, H.; Babcock, B. A. Bibcode: 2011ApJ...742...29P Altcode: The white-light corona (WLC) during the total solar eclipse of 2009 July 22 was observed by several teams in the Moon's shadow stretching from India and China across the Pacific Ocean with its many isolated islands. We present a comparison of the WLC as observed by eclipse teams located in China (Shanghai region) and on the Enewetak Atoll in the Marshall Islands, with observations taken 112 minutes apart, combined with near-simultaneous space observations. The eclipse was observed at the beginning of solar cycle 24, during a deep solar minimum (officially estimated as 2008 December according to the smoothed sunspot number, but very extended). The solar corona shows several different types of features (coronal holes, polar rays, helmet streamers, faint loops, voids, etc.), though it was extremely sparse in streamers as shown from Large-Angle Spectroscopic Coronagraph data. No large-scale dynamical phenomena were seen when comparing the observations from the two sites, confirming that the corona was quiescent. We measure a Ludendorff flattening coefficient of 0.238, typical of solar minimum. Title: Transits of Venus in Public Education and Contemporary Research Authors: Pasachoff, J. M. Bibcode: 2011epsc.conf.1773P Altcode: 2011DPS....43.1773P Transits of Venus are among the rarest predictable astronomical event that humans can enjoy, and the 2012 transit will be visible by almost all the people on Earth. It is our job as educators to bring out the thrill of being able to see the tiny dot of Venus silhouetted against the solar disk even with just a simple eye-protection filter. My Website at http://www.transitofvenus.info brings together not only historical information about the five previous transits of Venus that were observed through the 20th century--1639, 1761, 1769, 1874, and 1882--but also the scientific work carried out at the 2004 transit and at recent transits of Mercury. Based on space observations of the 1999 transit of Mercury with NASA's Transition Region and Coronal Explorer (TRACE), Glenn Schneider and I provided proof of the contemporary explanation of the black-drop effect as an amalgam of instrumental point-spread and solar limb-darkening [1]. Based on observations of the changes in the total solar irradiance during the transit, we provided an analysis of this solar-system analogue to exoplanet transits [2]. High-resolution (0.5 arcsec pixels) observations of ingress and egress with TRACE during the 2004 transit provided information about the visibility of Venus's atmosphere through its refraction of sunlight, interpreted with Venus Express observations [3]. We anticipate observing the 2012 transit with groundbased facilities of the University of Hawaii at Haleakala, and of the National Solar Observatory at Sacramento Peak, and Kitt Peak, as well as with NASA and JAXA spacecraft, including Solar Dynamics Observatory, ACRIMsat, and Hinode. The Program Group on Public Education on the Occasions of Eclipses and Transits of Commission 46 on Education and Development of the International Astronomical Union, which I chair, looks forward to participating in Education and Public Outreach efforts related to the 2012 transit. Title: The Double-Double Pluto-Charon and Pluto-Hydra Predicted Stellar Occultations of June 2011 Authors: Pasachoff, J. M.; Babcock, B. A.; Pandey, S.; Amrhein, D.; Person, M. J.; Gulbis, A. A. S.; Bosh, A. S.; Zuluaga, C. A.; Sallum, S.; Tholen, D. J.; Lucas, R.; Kakkala, M.; Ciotti, J.; Plunkett, S.; Hiraoka, N.; Best, W.; Pilger, E. J.; Miceli, M.; Levine, S. Bibcode: 2011epsc.conf.1821P Altcode: 2011DPS....43.1821P MIT astrometry predicted an occultation of Pluto and Charon within 11 minutes of each other on 23 June 2011 and an occultation of Pluto on 27 June 2011 with an occultation of Hydra following in a narrow shadow-path 33 minutes later. Our Williams-MIT team organized a network of telescopes around the Pacific-Asia region, including use of two telescopes in Hawaii, on which we report here. On 23 June, we successfully observed a 49 s occultation of Charon at 2 Hz with our Portable Occultation, Eclipse, and Transit System, POETS, from Leeward Community College's 0.5-m telescope in Pearl City. Our site at Windward Community College in Kaneohe with its 0.4-m telescope and a POETS was cloudy for both events, as was the Leeward Community College site for the second event with a 0.3-m telescope, used because the event was only 16° above the horizon, too low for their larger telescope, and a POETS. We place our successful Charon occultation in the context of observations by others, including our collaborators on SOFIA and observing with IRTF, and we discuss the predictions, observations, and prospective scientific value of the predicted double events with Pluto (radius 1400 km) and Charon (radius 605 km) prospectively occulting the same star on 23 June 23 UT and Pluto and Hydra (possibly only 50 km in radius) prospectively occulting a different star on 27 June UT. Title: Measured Pluto-Charon Offset from the Stellar Occultations of 23 June 2011 Authors: Zuluaga, C. A.; Person, M. J.; Bosh, A. S.; Levine, S. E.; Gulbis, A. A. S.; Zangari, A. M.; Pasachoff, J. M.; Babcock, B. A.; Pandey, S.; Amrhein, D.; Sallum, S.; Dunham, E. W.; Tholen, D. J.; Collins, P.; Bida, T.; Taylor, B.; Lucas, R.; Kakkala, M.; Ciotti, J.; Plunkett, S.; Hiraoka, N.; Best, W.; Pilger, E. J.; Miceli, M.; Springmann, A.; Hicks, M.; Thackeray, B.; Emery, J.; Rapoport, S.; Ritchie, I.; Pearson, M.; Mattingly, A.; Brimacombe, J.; Gault, D.; Jones, R.; Nolthenius, R.; Broughton, J.; Barry, T. Bibcode: 2011epsc.conf.1866Z Altcode: 2011DPS....43.1866Z We report on our Charon results from the double occultation observed on 23 June 2011 [1,2,3]. Our group successfully observed the occultation of the same star, 2UCAC 24677089, by Pluto and Charon shown in Figure 1. Charon occulted the star first, and its shadow was offset from that of Pluto by about 1200 km to the north. Thus, observers on the big island of Hawaii and along most of Baja were in the double-occultation zone, where occultations by both Pluto and Charon could be observed. Observers were located around the globe for this event. In Table 1 we list the sites and instruments used. Using GPStriggered instrument MORIS [4] at the NASA Infrared Telescope Facility (IRTF), we were able to record both occultations within approximately 11 minutes of each other. We obtained Charon-only light curves at an additional three sites. Observations at Leeward Community College on Oahu were made using a GPS-triggered Portable Occultation, Eclipse, and Transit System (POETS [5]). Observers at Table Mountain Observatory (CA) used a GPS-triggered Portable Instrument for Capturing Occultations (PICO [6]). Data were acquired at the U. S. Naval Observatory - Flagstaff Station (AZ) with the USNO Array Camera, an array of six 2k by 4k chips by e2v. We will analyze these data to solve for the shape and size of Charon as well as to how its position relative to Pluto compares to the JPL PLU017 ephemeris. Title: The 22 May 2011 Pluto occultation - observed Authors: Pasachoff, J. M.; Souza, S. P.; Babcock, B. A.; Pandey, S.; Hosek, M. W.; Person, M. J.; Gulbis, A. A. S.; Bosh, A. S.; Zuluaga, C. A.; Ryan, E. V.; Ryan, W. H.; Briggs, J. W.; Winkler, P. F.; Hoette, V.; Haislip, J. Bibcode: 2011epsc.conf.1784P Altcode: 2011DPS....43.1784P Based on a prediction from MIT with astrometric observations from the USNO and Lowell Observatory, we observed the 22 May 2011 UT 06:22 occultation of a star by Pluto (www.stellaroccultations.info and occult.mit.edu), predicted time. The star occulted was UCAC2 magnitude 15.3, and the event's geocentric velocity was 18.2 km s-1. We used the 0.6-m telescope of Williams College's Hopkins Observatory in Williamstown, MA, and one of our Portable Occultation, Eclipse, and Transit System (POETS) CCD/GPS. The centerline of the predicted path was just above the north pole, with the southern limit passing through the U.S. mid-Atlantic, so telescopes in the northeast were potentially in the path, though at high air mass. An occultation of approximately 100 s was clearly detected after calibrating on a nearby comparison star (and barely visible on the CCD monitoring screen in real time), given the relatively cloudy and variable nature of the observing conditions. We used the observation to refine the prediction model that is crucial for the 23/27 June occultations of Pluto-Charon/Pluto-Hydra, respectively. Observations in clear conditions with the Magdalena Ridge Observatory's 2.4-m telescope in New Mexico and another of our POETS did not show an occultation to better than 1%. This nondetection provides a constraint for a Pluto atmospheric graze or the potential shift of the path of Charon sufficiently far north to that site from the predicted path in northernmost South America. Title: Is the Sunspot Cycle About to Stop? Authors: Pasachoff, Jay; MacRobert, Alan M. Bibcode: 2011S&T...122c..12P Altcode: No abstract at ADS Title: Astronomy: Supernova century Authors: Pasachoff, Jay M. Bibcode: 2011Natur.476..280P Altcode: Jay Pasachoff relishes a novel that brings to life the scientific stars of the 1600s. Title: The U.S. Eclipse Megamovie in 2017: a white paper on a unique outreach event Authors: Hudson, Hugh S.; McIntosh, Scott W.; Habbal, Shadia R.; Pasachoff, Jay M.; Peticolas, Laura Bibcode: 2011arXiv1108.3486H Altcode: Totality during the solar eclipse of 2017 traverses the entire breadth of the continental United States, from Oregon to South Carolina. It thus provides the opportunity to assemble a very large number of images, obtained by amateur observers all along the path, into a continuous record of coronal evolution in time; totality lasts for an hour and a half over the continental U.S. While we describe this event here as an opportunity for public education and outreach, such a movie -with very high time resolution and extending to the chromosphere - will also contain unprecedented information about the physics of the solar corona. Title: The Solar System in the Age of Space Exploration Authors: Pasachoff, Jay M. Bibcode: 2011mtpr.conf....3P Altcode: We are celebrating the 50th anniversary of the launch of Sputnik, which began the space age. Though the manned exploration of the solar system has been limited to the Moon, in NASA's Apollo Program that ended over 35 years ago, robotic exploration of the solar system continues to be very successful. This paper explores the latest space mission and other observations of each planet and of each type of solar-system object, including dwarf planets, asteroids, and comets, as well as the sun. Title: Structure and Dynamics of the 2010 July 11 Eclipse White-light Corona Authors: Pasachoff, J. M.; Rušin, V.; Druckmüllerová, H.; Saniga, M.; Lu, M.; Malamut, C.; Seaton, D. B.; Golub, L.; Engell, A. J.; Hill, S. W.; Lucas, R. Bibcode: 2011ApJ...734..114P Altcode: The white-light corona (WLC) during the total solar eclipse on 2010 July 11 was observed by several teams in the Moon's shadow stretching across the Pacific Ocean and a number of isolated islands. We present a comparison of the WLC as observed by eclipse teams located on the Tatakoto Atoll in French Polynesia and on Easter Island, 83 minutes later, combined with near-simultaneous space observations. The eclipse was observed at the beginning of the solar cycle, not long after solar minimum. Nevertheless, the solar corona shows a plethora of different features (coronal holes, helmet streamers, polar rays, very faint loops and radial-oriented thin streamers, a coronal mass ejection, and a puzzling "curtain-like" object above the north pole). Comparing the observations from the two sites enables us to detect some dynamic phenomena. The eclipse observations are further compared with a hairy-ball model of the magnetic field and near-simultaneous images from the Atmospheric Imaging Assembly on NASA's Solar Dynamics Observatory, the Extreme Ultraviolet Imager on NASA's Solar Terrestrial Relations Observatory, the Sun Watcher, using Active Pixel System Detector and Image Processing on ESA's PRoject for Onboard Autonomy, and the Naval Research Laboratory's Large Angle and Spectrometric Coronagraph on ESA's Solar and Heliospheric Observatory. The Ludendorff flattening coefficient is 0.156, matching the expected ellipticity of coronal isophotes at 2 R sun, for this rising phase of the solar-activity cycle. Title: Blinded by the Light: Solar Eclipses in Art-Science, Symbolism, and Spectacle Authors: Olson, R. J. M.; Pasachoff, J. M. Bibcode: 2011ASPC..441..205O Altcode: After a short discussion of the history of astronomical representations-beginning with Giotto's Scrovegni Chapel-this paper briefly surveys highlights of solar eclipses portrayed by western artists, considering the impact of astronomical discoveries on them. Title: Attempted Stellar-Occultation Observations for KBO (20000) Varuna on 10 February 2011 Authors: Pasachoff, Jay M.; Babcock, B. A.; Elliot, J. L.; Person, M. J.; Gulbis, A. A. S.; Zuluaga, C.; Zangari, A.; Rosing, W.; Bianco, F. B.; Ciotti, J. E.; Kessler, M. R.; Plunkett, S. W. L., Jr.; Hiraoka, N. D.; Mohanan, K.; Pilger, E.; George, T.; Breit, D.; Preston, S.; Lonergan, K.; Menaker, S.; Egger, J.; Lockhart, M.; Gutoski, M.; Rulon, P.; Hampton, D.; Jiang, X.; Bai, J.; Chen, W. P.; Lehner, M.; Wang, J. H.; Zhang, Z. W.; Tokimasa, N. Bibcode: 2011AAS...21822411P Altcode: 2011BAAS..43G22411P We attempted to observe the 10 February 2011 occultation of a star of UCAC2 magnitude 15.5 by the Kuiper-belt object (20000) Varuna (visual magnitude 20.2), to determine its size, albedo, and other basic properties. Our original predictions showed the path going between Hawaii and Alaska, but SMARTS astrometry a month before the event moved the prediction 1,646 km north, so we added sites in the northwestern continental US and Alaska. We had clear weather at several sites in the predicted path (Alaska, Pacific Northwest), another site in the 1-sigma path (California), and several sites near the 3-sigma path (Hawaii, China, Taiwan, Japan), though no occultation was detected. Clouds or other problems prevented observations at several other sites. The appulse observations will be used to improve the ephemeris for future Varuna observations. See http://occult.mit.edu/research/occultations/kbo/Varuna/Varuna.20110210/index.html and stellaroccultations.info.

This work was supported, in part, by grants NNX10AB27G to MIT and NNX08AO50G to Williams College from NASA's Planetary Astronomy Division. We thank Don Hampton of the Poker Flat Research Range, Alaska, for his assistance. Title: The Solar Corona and a CME at the 2010 Total Eclipse Authors: Pasachoff, Jay M.; Rusin, V.; Druckmüllerová, H.; Saniga, M.; Lu, M.; Malamut, C.; Seaton, D. B.; Golub, L.; Engell, A. J.; Hill, S. W.; Lucas, R. Bibcode: 2011SPD....42.1813P Altcode: 2011BAAS..43S.1813P The 11 July 2010 total solar eclipse was observed on the ground from French Polynesia and, 83 minutes later, from Easter Island, and near-simultaneous images were made with spacecraft instruments including AIA/SDO, HMI/SDO, EUVI/STEREO, SWAP/PROBA2, EIT/SOHO, and LASCO/SOHO. We report on changes in the corona detectable with high-resolution image processing of the ground-based eclipse coronal imaging, including two CME's that were seen to evolve. We compare with the spacecraft images to give a complete depiction of coronal structure at the time of the eclipse, which corresponded to a low but rising phase of the solar-activity cycle.

We acknowledge the support of NASA's MSFC NNX10AK47A, NSF REU AST-1005024 with DoD ASSURE, VEGA 2/0098/10 of the Slovak Acad. Sci, 205/09/1469 of the Czech Science Foundation, PRODEX C90345 of ESA/BELSPO, FP7/2007-2013/218816 SOTERIA, Lockheed Martin; for equipment: Nikon Professional Services, ASTELCO Systems GmbH (Germany), and National Geographic Society's Photographic Division; and colleagues Y.-M. Wang (NRL), S. Habbal (U. Hawaii), H. Lanteires (Tatakoto), and J. Kern (Carnegie Obs.). Title: Music for Dwarf Planets Authors: Pasachoff, Jay Bibcode: 2011S&T...121d..10P Altcode: No abstract at ADS Title: High-resolution Satellite Imaging of the 2004 Transit of Venus and Asymmetries in the Cytherean Atmosphere Authors: Pasachoff, Jay M.; Schneider, Glenn; Widemann, Thomas Bibcode: 2011AJ....141..112P Altcode: This paper presents the only space-borne optical-imaging observations of the 2004 June 8 transit of Venus, the first such transit visible from Earth since AD 1882. The high-resolution, high-cadence satellite images we arranged from NASA's Transition Region and Coronal Explorer (TRACE) reveal the onset of visibility of Venus's atmosphere and give further information about the black-drop effect, whose causes we previously demonstrated from TRACE observations of a transit of Mercury. The atmosphere is gradually revealed before second contact and after third contact, resulting from the changing depth of atmospheric layers refracting the photospheric surface into the observer's direction. We use Venus Express observations to relate the atmospheric arcs seen during the transit to the atmospheric structure of Venus. Finally, we relate the transit images to current and future exoplanet observations, providing a sort of ground truth showing an analog in our solar system to effects observable only with light curves in other solar systems with the Kepler and CoRoT missions and ground-based exoplanet-transit observations. Title: A Search for Satellites of Kuiper Belt Object 55636 from the 2009 October 9 Occultation Authors: Jensen-Clem, Rebecca; Elliot, J. L.; Person, M. J.; Zuluaga, C. A.; Bosh, A. S.; Adams, E. R.; Brothers, T. C.; Gulbis, A. A. S.; Levine, S. E.; Lockhart, M.; Zangari, A. M.; Babcock, B. A.; DuPre, K.; Pasachoff, J. M.; Souza, S. P.; Rosing, W.; Secrest, N.; Bright, L.; Dunham, E. W.; Kakkala, M.; Tilleman, T.; Rapoport, S.; Zambrano-Marin, L.; Wolf, J.; Morzinski, K. Bibcode: 2011AAS...21730605J Altcode: 2011BAAS...4330605J A world-wide observing campaign of 21 telescopes at 18 sites was organized by Elliot et al. (2010 Nature 465, 897) to observe the 2009 Oct. 9 stellar occultation of 2UCAC 41650964 (UCAC2 magnitude 13.1) by the Kuiper Belt object 55636 (visual magnitude 19.6). Integration times varied between 0.05 seconds at the Vatican Advanced Technology Telescope and 5 seconds at Mauna Kea mid-level. Data from the two sites that successfully observed the occultation (Haleakala and the Mauna Kea mid-level) were analyzed by Elliot et al. (2010) to determine the diameter and albedo of 55636. In this study, we use the entire data set to search for signatures of occultations by nearby satellites. One satellite previously discovered with occultation data is Neptune's moon Larissa, which was detected during Neptune's close approach to a star in 1982 (Reitsema et al. 1982). No satellites are found in this study, and upper limits will be reported on satellite radii within the volume probed (2 x 10-8 of the Hill Sphere). This work was supported, in part, by NASA Grants NNX10AB27G (MIT), NNX08AO50G (Williams College), and NNH08AI17I (USNO-FS) and NSF Grant AST-0406493 (MIT). Student participation was supported in part by NSF's REU program and NASA's Massachusetts Space Grant. Title: Simultaneous Observations of the Chromosphere with TRACE and SUMER Authors: Pasachoff, Jay M.; Tingle, Evan D.; Dammasch, Ingolf E.; Sterling, Alphonse C. Bibcode: 2011SoPh..268..151P Altcode: 2010SoPh..tmp..209P; 2010SoPh..tmp..233P; 2010arXiv1010.4814P Using mainly the 1600 Å continuum channel and also the 1216 Å Lyman-α channel (which includes some UV continuum and C IV emission) aboard the TRACE satellite, we observed the complete lifetime of a transient, bright chromospheric loop. Simultaneous observations with the SUMER instrument aboard the SOHO spacecraft revealed interesting material velocities through the Doppler effect existing above the chromospheric loop imaged with TRACE, possibly corresponding to extended nonvisible loops, or the base of an X-ray jet. Title: Report of Some Comets: The Discovery of Uranus and Comets by William, Caroline, and John Herschel Authors: Pasachoff, Jay M.; Olson, R. J. M. Bibcode: 2011AAS...21711101P Altcode: 2011BAAS...4311101P We report on the discovery and drawings of comets by William, Caroline, and John Herschel. The first discovery, by William Herschel, in 1781 from Bath, published in the Philosophical Transactions of the Royal Society with the title "Report of a Comet," turned out to be Uranus, the first planet ever discovered, Mercury through Saturn having been known since antiquity. William's sister Caroline was given duties of sweeping the skies and turned out to be a discoverer of 8 comets in her own right, in addition to keeping William's notes. Caroline's comets were discovered from Slough between 1786 and 1797. In the process, we also discuss original documents from the archives of the Royal Society and of the Royal Astronomical Society. We conclude by showing comet drawings that we have recently attributed to John Herschel, including Halley's Comet from 1836, recently located in the Ransom Center of the University of Texas at Austin.

Acknowledgments: Planetary astronomy at Williams College is supported in part by grant NNX08AO50G from NASA Planetary Astronomy. We thank Peter Hingley of the Royal Astronomical Society and Richard Oram of the Harry Ransom Center of The University of Texas at Austin for their assistance. Title: The Making of History's Greatest Star Map and A Grand and Bold Thing: An Extraordinary New Map of the Universe Ushering in a New Era of Discovery Authors: Perryman, Michael; Finkbeiner, Ann; Pasachoff, Jay M. Bibcode: 2011PhT....64e..45P Altcode: No abstract at ADS Title: Pluto's Atmosphere from the July 2010 Stellar Occultation Authors: Person, Michael J.; Elliot, J. L.; Bosh, A. S.; Gulbis, A. A. S.; Jensen-Clem, R.; Lockhart, M. F.; Zangari, A. M.; Zuluaga, C. A.; Levine, S. E.; Pasachoff, J. M.; Souza, S. P.; Lu, M.; Malamut, C.; Rojo, P.; Bailyn, C. D.; MacDonald, R. K. D.; Ivarsen, K. M.; Reichart, D. E.; LaCluyze, A. P.; Nysewander, M. C.; Haislip, J. B. Bibcode: 2010DPS....42.2003P Altcode: 2010BAAS...42R.983P We have observed the 4 July 2010 stellar occultation by Pluto as part of our program of monitoring Pluto's atmospheric changes over the last decade. Successful observations were obtained from three sites: Cerro Calan and Cerro Tololo, Chile, as well as the HESS-project site (High Energy Stereoscopic System) in southwestern Namibia. Successful telescope apertures ranged from 0.45 m to 1.0 m and resulted in seven occultation light curves for the event from among the three sites. Simultaneous analysis of the seven light curves indicates that Pluto's atmosphere continues to be stable, as the calculated atmospheric radii are consistent with those detected in 2006 (Elliot et al., AJ 134, 1, 2007) and 2007 (Person et al., AJ 136, 1510, 2008), continuing the stability that followed the large pressure increase detected between 1988 (Millis et al., Icarus 105, 282, 1993) and 2002 (Elliot et al., Nature 424, 165, 2003). We will present the overall astrometric solution as well as current profiles for Pluto's upper atmospheric temperature and pressure obtained from inversion of the light curves (Elliot, Person, and Qu, AJ 126, 1041, 2003).

This work was supported, in part, by grants NNX10AB27G to MIT, NNX08AO50G to Williams College, and NNH08AI17I to the USNO from NASA's Planetary Astronomy Division. The 0.75-m ATOM (Automatic Telescope for Optical Monitoring) light curve was obtained with the generous assistance of the HESS-project staff, arranged by Stefan Wagner and Marcus Hauser of the University of Heidelberg. The 0.45-m Goto telescope at Cerro Calán National Astronomical Observatory, Universidad de Chile, was donated by the Government of Japan. PROMPT (Panchromatic Robotic Optical Monitoring and Polarimetry Telescopes) observations at Cerro Tololo were made possible by the Robert Martin Ayers Science Fund. Student participation was supported in part by NSF's REU program and NASA's Massachusetts Space Grant. Title: The 3/4 July 2010 Pluto Stellar-Occultation Observations Authors: Pasachoff, Jay M.; Elliot, J. L.; Souza, S. P.; Person, M. J.; Zuluaga, C.; Bosh, A. S.; Zangari, A. M.; Jensen-Clem, R.; Lockhart, M.; Gulbis, A. A. S.; Rojo, P.; Lu, M.; Malamut, C.; Levine, S. E.; Ivarsen, K. M.; Reichart, D. E.; LaCluyze, A. P.; Nysewander, M. C.; Haislip, J. B.; MacDonald, R. K. D.; Bailyn, C. D.; Emilio, M.; Jehin, E.; Gillon, M.; Manfroid, J.; Chantry, V.; Magain, P.; Hutsemekers, D.; Queloz, D. Bibcode: 2010DPS....42.2002P Altcode: 2010BAAS...42Q.983P Continuing our monitoring of Pluto's atmospheric temperature and pressure, previously shown by us to be increasing (Elliot et al., Nature 424, 165, 2003; Pasachoff et al., AJ 129, 1718, 2005) and subsequently found by us to be leveling off (Elliot et al., AJ 134, 1, 2007), we report on a stellar occultation by Pluto of UCAC2 mag=15.3, observed from South America and Africa on 4 July 2010 UT. Success was achieved with a 0.45 m at Cerro Calan using one of our POETS (Portable Occultation, Eclipse, and Transit System; Souza et al. PASP 118, 1550, 2006), a 1.0 SMARTS (Small and Medium Aperture Research Telescope System) at Cerro Tololo, four 0.6 m telescopes of PROMPT (Panchromatic Robotic Optical Monitoring and Polarimetry Telescopes) on Cerro Tololo, and TRAPPIST's (TRansiting Planets and Planetesimals Small Telescope) 0.6-m telescope on La Silla in Chile; the 0.35 m telescope of U. Ponta Grossa, Brazil; and the 0.75-m ATOM (Automatic Telescope for Optical Monitoring), Namibia, using POETS. Winds prevented opening the 6.5 m Magellan/Clay telescope on Las Campanas, Chile, with its own frame-transfer camera, and clouds obscured the 1.9 m telescope at Sutherland, South Africa, which had POETS. With shadow velocity 23.6 km/s, it was a rapid event: maximum occultation <2 minutes.

The observations were supported in part by grants NNX08AO50G to Williams College and NNX10AB27G to MIT from NASA's Planetary Astronomy Division, and NNH08AI17I to USNO for astrometry. Student participation was supported in part by NASA's Massachusetts Space Grant and NSF's REU. Japan's government donated U. Chile's Cerro Calan Goto telescope. PROMPT observations were made possible by the Robert Martin Ayers Science Fund. TRAPPIST is a project driven by the University of Liège, in close collaboration with the Observatory of Geneva, supported by the Belgian Fund for Scientific Research and the Swiss National Science Foundation. Title: Size and Albedo of the Kuiper Belt Object 55636 Authors: Elliot, James L.; Person, M. J.; Zuluaga, C. A.; Bosh, A. S.; Adams, E. R.; Brothers, T. C.; Gulbis, A. A. S.; Levine, S. E.; Lockhart, M.; Zangari, A. M.; Babcock, B. A.; DuPré, K.; Pasachoff, J. M.; Souza, S. P.; Rosing, W.; Secrest, N. Bibcode: 2010DPS....42.2302E Altcode: 2010BAAS...42..991E Due to the small sizes and great distances of Kuiper belt objects (KBOs), it is difficult to determine their diameters. We report multi-chord observations of a KBO stellar occultation, which occurred on 2009 October 9 (Elliot, J. L., et al. 2010, Nature, 465, 897). We set up a network of 21 telescopes at 18 stations, spanning a distance of 5920 km perpendicular to the predicted shadow path for the 2009 October 9 stellar occultation by the KBO 55636. Of these stations, seven could not observe due to weather, nine reported non-detections, and two observed an occultation, both in Hawai'i: the 2.0-m Faulkes North telescope at Haleakala and a 0.36-m portable telescope at the Visitor Information Station at the Onizuka Center for International Astronomy on Mauna Kea (located at the Mauna Kea Mid Level). We find that 55636 (2002 TX300), which is a member of the water-ice rich Haumea KBO collisional family (Brown, M. E., et al. 2007, Nature, 446, 294), has a mean radius of 143 ± 5 km (for a circular solution). Allowing for possible elliptical shapes we find a geometric albedo of 0.88 +0.15/-0.06 in the V photometric band. This firmly establishes that 55636 is smaller than previously thought and like its parent body, Haumea, is among the most highly reflective objects in the Solar System. Dynamical calculations by two groups indicate that the collision that created 55636 occurred at least 1 Gyr ago (Ragozzine, D., & Brown, M. E. 2007, AJ, 134, 2160; Schlichting, H. E., & Sari, R. 2009, ApJ, 700, 1242), which implies either that 55636 has an active resurfacing mechanism, or that fresh water ice in the outer solar system can persist for Gyr timescales. This work was supported, in part by NASA Grants NNX10AB27G (MIT), NNX08AO50G (Williams College), and NNH08AI17I (USNO-FS). Title: Solar Eclipses for Science and for Public Education Authors: Pasachoff, Jay Bibcode: 2010AIPC.1283...40P Altcode: On the rare occurrences of total solar eclipses, about 350 years apart at a given terrestrial location and 18 months apart in the world, people in the zone of totality are dazzled and impressed by the spectacular phenomena that become visible in the midst of atmospheric darkening. I describe a selection of scientific results about the solar chromosphere corona that are obtained at eclipses, from the historic discovery of helium to present-day investigations of how the corona gets to be 2,000,000 K. I also describe how the attention to the eclipse, to astronomy, and to science in general that often accompanies eclipse day in not only the zone of totality but also to thousands of kilometers to either side, can lead to teaching opportunities not only for students participating in the scientific observing but also to all students and the general public. Title: Pluto and Beyond: Stellar-Occultation Web Pages for Education and Observation Planning Authors: Pasachoff, Jay M.; Brown, M. E.; Person, M. J.; Tam, Y. H. Ng Bibcode: 2010DPS....42.0701P Altcode: 2010BAAS...42..953P The method of stellar occultation is a powerful way to investigate objects in the outer solar system, including their sizes, their shapes, their atmospheres, and, when present, rings. Following series of observations of outer-solar-system objects, including the dwarf planets Pluto and Haumea, satellites Charon and Nix, additional Kuiper-belt object 55636, and Triton, we have prepared web pages at Williams College describing the results and linking published papers and meeting abstracts as well as light curves, images, and expedition photographs. Brown's pages at Caltech (www.gps.caltech.edu/ mbrown/2003EL61/) discuss the mutual occultation and transit events of Haumea and its moon Namaka, showing predictions over the last couple of years, though no observations of the mutual events (from the Hale 5-m telescope at the Palomar Observatory on down) have yet been successful. This paper will include Haumea/Namaka predictions for the coming observation season. The MIT Planetary Astronomy Lab's web pages (occult.mit.edu) are more technical in nature, providing information useful for planning observations, which are usually made simultaneously with multiple telescopes to provide a variety of chords across the objects. For overall access to our occultation information, go to http://www.stellaroccultations.info or http://www.williams.edu/Astronomy/research/occultations.

Observations have been supported in part by grants NNX08AO50G to Williams College, NNX10AB27G to MIT, and NNG05GI02G to Caltech from NASA's Planetary Astronomy Division. Student participation was supported in part by NASA's Massachusetts Space Grant. Title: Tales of Meteors I Authors: Olson, Roberta M. J.; Pasachoff, Jay M. Bibcode: 2010S&T...120c...8O Altcode: No abstract at ADS Title: Resource Letter SPh-1: Solar Physics Authors: Pasachoff, Jay M. Bibcode: 2010AmJPh..78..890P Altcode: This Resource Letter provides a guide to printed literature, listing selected books and articles and online resources about scientific and cultural references to the Sun and the related topics of solar spectroscopy and space weather. Topics include helioseismology, the chromosphere and corona at solar eclipses, sunspots and other solar activity, and total solar irradiance, as well as instrumental references including spectroheliographs, coelostats, and observatories on the ground and in space. References to general works on heliophysics and plasma physics are minimized. Title: The origin and diffusion of the H and K notation Authors: Pasachoff, Jay M.; Suer, Terry-Ann Bibcode: 2010JAHH...13..120P Altcode: Though many or most astronomers and astronomy students may think that H and K, as in the Ca II ‘H and K lines’, were named by Fraunhofer, actually only the H line was in Fraunhofer's original notation. He also used ‘I’ to indicate the end of the spectrum in his widely-reproduced 1814 drawing, of which an engraved version was published in 1817. We have searched references from nineteenth-century books and journals to find the first use of ‘K’ to indicate the ionized-calcium spectral line at 393.3 nm and located the probable first use and eventually the reuse of the notation. Title: A Comparison of the Red and Green Coronal Line Intensities at the 29 March 2006 and the 1 August 2008 Total Solar Eclipses: Considerations of the Temperature of the Solar Corona Authors: Voulgaris, A.; Athanasiadis, T.; Seiradakis, J. H.; Pasachoff, J. M. Bibcode: 2010SoPh..264...45V Altcode: 2010SoPh..tmp...98V; 2009arXiv0911.0325V During the total solar eclipse at Akademgorodok, Siberia, Russia, on 1 August 2008, we imaged the flash spectrum with a slitless spectrograph. We have spectroscopically determined the duration of totality, the epoch of the second and third contacts and the duration of the flash spectrum. Here we compare the 2008 flash spectra with those that we similarly obtained from the total solar eclipse of 29 March 2006, at Kastellorizo, Greece. Any changes of the intensity of the coronal emission lines, in particularly those of Fe X and Fe XIV, could give us valuable information about the temperature of the corona. The results show that the ionization state of the corona, as manifested especially by the Fe XIV emission line, was much weaker during the 2008 eclipse, indicating that following the long, inactive period during the solar minimum, there was a drop in the overall temperature of the solar corona. Title: Size and albedo of Kuiper belt object 55636 from a stellar occultation Authors: Elliot, J. L.; Person, M. J.; Zuluaga, C. A.; Bosh, A. S.; Adams, E. R.; Brothers, T. C.; Gulbis, A. A. S.; Levine, S. E.; Lockhart, M.; Zangari, A. M.; Babcock, B. A.; Dupré, K.; Pasachoff, J. M.; Souza, S. P.; Rosing, W.; Secrest, N.; Bright, L.; Dunham, E. W.; Sheppard, S. S.; Kakkala, M.; Tilleman, T.; Berger, B.; Briggs, J. W.; Jacobson, G.; Valleli, P.; Volz, B.; Rapoport, S.; Hart, R.; Brucker, M.; Michel, R.; Mattingly, A.; Zambrano-Marin, L.; Meyer, A. W.; Wolf, J.; Ryan, E. V.; Ryan, W. H.; Morzinski, K.; Grigsby, B.; Brimacombe, J.; Ragozzine, D.; Montano, H. G.; Gilmore, A. Bibcode: 2010Natur.465..897E Altcode: The Kuiper belt is a collection of small bodies (Kuiper belt objects, KBOs) that lie beyond the orbit of Neptune and which are believed to have formed contemporaneously with the planets. Their small size and great distance make them difficult to study. KBO 55636 (2002 TX300) is a member of the water-ice-rich Haumea KBO collisional family. The Haumea family are among the most highly reflective objects in the Solar System. Dynamical calculations indicate that the collision that created KBO 55636 occurred at least 1Gyr ago. Here we report observations of a multi-chord stellar occultation by KBO 55636, which occurred on 9 October 2009 UT. We find that it has a mean radius of 143+/-5km (assuming a circular solution). Allowing for possible elliptical shapes, we find a geometric albedo of 0.88-0.06+0.15 in the V photometric band, which establishes that KBO 55636 is smaller than previously thought and that, like its parent body, it is highly reflective. The dynamical age implies either that KBO 55636 has an active resurfacing mechanism, or that fresh water-ice in the outer Solar System can persist for gigayear timescales. Title: Commission 46: Astronomy Education and Development Authors: Stavinschi, Magda D.; Ros, Rosa M.; Pasachoff, Jay M.; Andersen, Johannes; Deustua, Susana; De Greve, Jean-Pierre; Guinan, Edward F.; Haubold, Hans J.; Earnshaw, John B.; Jones, Barrie W.; Kochhar, Rajesh K.; Leung, Kam-Ching; Marschall, Laurence A.; Percy, John R.; Torres-Peimbert, Silvia Bibcode: 2010IAUTB..27..270S Altcode: Commission 46 had held two sessions of business meetings during the General Assembly in Rio de Janeiro. Both of them were chaired by Magda Stavinschi. Title: Search for 1-Hz Coronal-Loop Oscillations at the 2008 and 2009 Total Eclipses Authors: Pasachoff, Jay M.; Babcock, B. A.; DuPré, K.; Kern, J.; Nesterenko, A.; Nesterenko, I. Bibcode: 2010AAS...21640716P Altcode: 2010BAAS...41..862P We report observations through narrow-band filters at total solar eclipses at high cadence to search for Fourier power 1 Hz, a prediction of certain classes of coronal heating through MHD waves, such as surface Alfvén waves. We previous reported such power at the 1999 eclipse (Pasachoff, Babcock, Russell, Seaton, Solar Phys. 207, 241-257, 2002). We observed at 10 Hz for 2 min 20 sec in Siberia in 2008 with the coronal red line at 637.4 nm and the coronal green line at 530.3 nm, and at 6 Hz for 5 min 50 sec at Tianhuangping, China, in 2009 with the coronal green line and a nearby continuum, using 20-cm telescopes. The sky was clear in 2008 while the eclipse was observed through moving clouds in 2009. The weakening corona gave few features on which to make a fine alignment, and much time has been spent on details of aligning the series of images. We report on the status of the alignment and the resulting transforms, and place the results in the context of the solar-activity cycle, which we show through a series of radial-filter images made as part of our expeditions in 1999, 2001, 2006, 2008, and 2009, spanning the most recent sunspot cycle.

Acknowledgments: We thank C. Alex Young, Daniel B. Seaton. Yihua Yan, Jin Zhu, Lin Lan and Chenying Lai. Williams collaborators were Jianjun Wang, Marek Demianski, Huajai Cao, Sara Dwyer, and Rachel Wagner-Kaiser in 2009 and Marcus Freeman, William G. Wagner, and Marek Demianski in 2008. Our expeditions were supported in part by grants from the Committee for Research and Exploration of the National Geographic Society. We thank the NSF Heliospheric Program for 2006 suppport and the Planetary Astronomy division of NASA for imaging-system support. Title: The Galactic deuterium gradient Authors: Lubowich, Donald; Pasachoff, Jay M. Bibcode: 2010IAUS..268..179L Altcode: The Galactic deuterium abundance gradient has been determined from observations of DCN in Galactic molecular clouds. This is the only way to observe D throughout the Galaxy because the molecular clouds are not limited to the 2 kpc region around the Sun observed with FUSE and from DI. We used an astrochemistry model and the DCN/HCN ratios to estimate the underlying D/H ratios in 16 molecular clouds including five in the Galactic Center. The resulting positive Galactic D gradient and reduced Galactic Center D/H ratio imply that there are no significant Galactic sources of D, there is continuous infall of low-metallicity gas into the Galaxy, and that deuterium is cosmological. Title: The Origin and Diffusion of the H and K Notation Authors: Pasachoff, Jay M.; Suer, T. A. Bibcode: 2010AAS...21530403P Altcode: 2010BAAS...42..301P Though many or most astronomers and astronomy students may think that H and K, as in the Ca II "H and K lines," were named by Fraunhofer, actually only the H line was in Fraunhofer's original notation. He also used "I" to indicate the end of the spectrum in his widely reproduced 1814 drawing, published in 1817. We have searched references from 19th-century books and journals to find the first use of "K" to indicate the ionized-calcium spectral line at 383.3 nm and located the probable first use and eventually the reuse of the notation. Title: Coronal Observations at the Siberian 2008 Total Solar Eclipse Authors: Pasachoff, Jay M.; Babcock, B. A.; Freeman, M. J.; DuPré, K. M.; Demianski, M.; Nesterenko, A.; Nesterenko, I.; Schneider, G. Bibcode: 2009AAS...21360003P Altcode: We successfully observed the 1 August 2008 total solar eclipse from the rooftop observatory of the State University of Novosibirsk in Akademgorodok, Siberia, latitude 55° N at 10:45 UT in clear skies and also from an airplane at 83° N latitude north of Svalbard at 9:43 UT. Our prime experiment in Akademgorodok was a set of high-cadence, 10 Hz, observations in the coronal green line at 530.3 nm from [Fe XIV] to verify and extend our previous findings of excess power in the 0.5 Hz to 1 Hz region as predicted by a subset of coronal-heating theories. We used twin 0.2-m telescopes with narrow-band interference filters and our POETS frame-transfer CCD's on the university's Paramount ME. Additional photography included graded-exposure sets of images meant for post-processing to compare with images taken earlier from the airplane and later from the ground in Mongolia and China to provide time differences of over 90 minutes. We also obtained HD video. Our comparison of the images from the airplane and from Siberia will be used to search for coronal motions. Title: Attempted Observations of the 2009 Occultation of a Star by Nix Authors: Pasachoff, Jay M.; Widemann, T.; Sicardy, B.; Lister, T.; Tholen, D. J.; Gulbis, A. A. S.; Adams, E. R. Bibcode: 2009AAS...21460601P Altcode: We attempted to observe the predicted 4 March 2009, 13:56 UT, approximately 6-second-long occultation of an 11th magnitude star by Pluto's small moon Nix, which is fainter than 23rd magnitude. In parallel starlight, the path was 88 km in width with a one-sigma range from 44 km to 110 km. The Tycho star is at 18 12 09.86 17 42 03.3 (J2000.0), and has R=11.8 and K=10.4. The occultation path was predicted to cross the Hawaiian islands, with a southern boundary cutting through Maui and missing the telescopes on Mauna Kea, but the uncertainty in the prediction (1 sigma) was about 500 km (though only 5 minutes in time). The path's speed was 15 km/s. In the event, we obtained data only from the 2-m Faulkes telescope on Maui, with uneven skies. Our trailed images did not show evidence of the occultation, which would have dropped the observed intensity at the merged star/Nix position by about 12 magnitudes or, more likely, if Nix and Pluto were merged by about 3 magnitudes. Weather prevented observations with MegaCam on the CFHT, with a MIT POETS on the IRTF, with PanSTARRS on Maui, as well as with an 0.4-m telescope at Windward Community College on Oahu. For administrative reasons, we did not succeed in obtaining data with the 3.7-m AEOS telescope on Maui. In any case, the event was at low altitude, only 21°, so pointing was at the limits for several of the telescopes.

Our collaboration between Williams College and MIT is with J. L. Elliot and M. J. Person at MIT and B. A. Babcock and S. P. Souza at Williams. We thank C. Veillet in Paris, J. Ciotti, M. Kessler, and G. T. Elliott on Oahu, and L. Young and M. Buie in Boulder for their collaboration. JMP's work on Pluto is supported in part by grant NNX08AO50G from NASA's Planetary Science Division and MIT's by NNX07AN63G. Title: To Boldly Go - Or Not - III Authors: Pasachoff, Jay M. Bibcode: 2009S&T...118f..10P Altcode: No abstract at ADS Title: Limb Spicules from the Ground and from Space Authors: Pasachoff, Jay M.; Jacobson, William A.; Sterling, Alphonse C. Bibcode: 2009SoPh..260...59P Altcode: 2009arXiv0909.0027P We amassed statistics for quiet-sun chromosphere spicules at the limb using ground-based observations from the Swedish 1-m Solar Telescope on La Palma and simultaneously from NASA's Transition Region and Coronal Explorer (TRACE) spacecraft. The observations were obtained in July 2006. With the 0.2 arcsecond resolution obtained after maximizing the ground-based resolution with the Multi-Object Multi-Frame Blind Deconvolution (MOMFBD) program, we obtained specific statistics for sizes and motions of over two dozen individual spicules, based on movies compiled at 50-second cadence for the series of five wavelengths observed in a very narrow band at Hα, on-band and at ± 0.035 nm and ± 0.070 nm (10 s at each wavelength) using the SOUP filter, and had simultaneous observations in the 160 nm EUV continuum from TRACE. The MOMFBD restoration also automatically aligned the images, facilitating the making of Dopplergrams at each off-band pair. We studied 40 Hα spicules, and 14 EUV spicules that overlapped Hα spicules; we found that their dynamical and morphological properties fit into the framework of several previous studies. From a preliminary comparison with spicule theories, our observations are consistent with a reconnection mechanism for spicule generation, and with UV spicules being a sheath region surrounding the Hα spicules. Title: The Solar Corona Authors: Golub, Leon; Pasachoff, Jay M. Bibcode: 2009soco.book.....G Altcode: 1. Introduction; 2. Brief history of coronal studies; 3. The coronal spectrum; 4. The solar cycle; 5. Ground-based observations; 6. Observations from space: I. The first 4 decades; 7. Activity of the inner corona; 8. Observations from space: II. Recent missions; 9. The solar wind; 10. Solar flares and coronal mass ejections; Notes; References; Index. Title: The MIT Program for Predicting Stellar Occultations by Kuiper Belt Objects Authors: Elliot, James L.; Zuluaga, C. A.; Person, M. J.; Adams, E. R.; Lockhart, M. F.; Zangari, A. M.; Bosh, A. S.; Gulbis, A. A. S.; Levine, S. E.; Sheppard, S. S.; Dunham, E. W.; Bright, L.; Souza, S. P.; Pasachoff, J. M.; Babcock, B. A.; Ryan, W. H.; Ryan, E. V. Bibcode: 2009DPS....41.6209E Altcode: With observations of a stellar occultation by a Kuiper belt object (KBO) from multiple stations, one could establish its radius with an accuracy of a few kilometers. Combining this radius with photometry would establish an accurate geometric albedo. For those KBOs with orbiting companions, these data will further provide highly accurate densities constraining material composition. Stellar occultation data also establish stringent upper limits on any atmospheres and probe for small, nearby companions. The difficulty in observing a KBO occultation has been in generating an accurate prediction so that observers can be deployed within the occultation shadow path. Current KBO ephemerides are at best accurate to a few tenths of an arcsecond, while angular radii of the largest bodies are less than 0.02 arcsec. To improve the ephemerides of the KBOs most promising for stellar occultations, we conduct astrometric observations of KBOs selected (i) for large angular radii, and (ii) in sky regions with large star densities. We have made bi-monthly observations with the Lowell 42-inch Hall telescope since Dec. 2004 and monthly to bi-monthly observations with the SMARTS 0.9 m at CTIO since May 2005. Approximately 1200 KBO astrometric measurements have been submitted to the Minor Planet Center. We use these data to establish ephemeris correction models with which we predict appulses by target KBOs. We observed three of these appulses to test our accuracy. The difference between the predicted and observed closeest approach agrees within the formal error for two of the three appulses, but the errors are somewhat larger than the body's radius. Hence our predictions are almost accurate enough to reliably place observers within the shadow path of a KBO occultation, and improving with each astrometric observation. This work is supported, in part, by USRA subcontract 8500-98-03 (Lowell Observatory) and NASA Grant NNX07AK73G (MIT). Title: The 2008 August 1 Eclipse Solar-Minimum Corona Unraveled Authors: Pasachoff, J. M.; Rušin, V.; Druckmüller, M.; Aniol, P.; Saniga, M.; Minarovjech, M. Bibcode: 2009ApJ...702.1297P Altcode: 2009arXiv0907.1643P We discuss the results stemming from observations of the white-light and [Fe XIV] emission corona during the total eclipse of the Sun of 2008 August 1, in Mongolia (Altaj region) and in Russia (Akademgorodok, Novosibirsk, Siberia). Corresponding to the current extreme solar minimum, the white-light corona, visible up to 20 solar radii, was of a transient type with well pronounced helmet streamers situated above a chain of prominences at position angles 48°, 130°, 241°, and 322°. A variety of coronal holes, filled with a number of thin polar plumes, were seen around the poles. Furthering an original method of image processing, stars up to 12 mag, a Kreutz-group comet (C/2008 O1) and a coronal mass ejection (CME) were also detected, with the smallest resolvable structures being of, and at some places even less than, 1 arcsec. Differences, presumably motions, in the corona and prominences are seen even with the 19 minutes time difference between our sites. In addition to the high-resolution coronal images, which show the continuum corona (K-corona) that results from electron scattering of photospheric light, images of the overlapping green-emission-line (530.3 nm, [Fe XIV]) corona were obtained with the help of two narrow-passband filters (centered on the line itself and for the continuum in the vicinity of 529.1 nm, respectively), each with an FWHM of 0.15 nm. Through solar observations, on whose scheduling and details we consulted, with the Solar and Heliospheric Observatory, Hinode's XRT and SOT, Transition Region and Coronal Explorer, and STEREO, as well as Wilcox Solar Observatory and Solar and Heliospheric Observatory/Michelson Doppler Imager magnetograms, we set our eclipse observations in the context of the current unusually low and prolonged solar minimum. Title: Teaching and Learning Astronomy Authors: Pasachoff, Jay; Percy, John Bibcode: 2009tla..book.....P Altcode: Preface; Part I. Astronomy in the Curriculum Around the World: Preface; 1. Why astronomy is useful and should be included in the school curriculum John R. Percy; 2. Astronomy and mathematics education Rosa M. Ros; 3. Astronomy in the curriculum around the world; 4. Engaging gifted science students through astronomy Robert Hollow; 5. Poster highlights: astronomy in the curriculum around the world; Part II. Astronomy Education Research: Preface; 6. Astronomy education research down under John M. Broadfoot and Ian S. Ginns; 7. A contemporary review of K-16 astronomy education research Janelle M. Bailey and Timothy F. Slater; 8. Implementing astronomy education research Leonarda Fucili; 9. The Astronomy Education Review: report on a new journal Sidney C. Wolff and Andrew Fraknoi; 10. Poster highlights: astronomy education research; Part III. Educating Students: Preface; 11. Textbooks for K-12 astronomy Jay M. Pasachoff; 12. Distance/internet astronomy education David H. McKinnon; 13. Educating students with robotic telescopes - open discussion; 14. Poster highlights - educating students; Part IV. Educating teachers: Preface; 15. Pre-service astronomy education of teachers Mary Kay Hemenway; 16. In-service education of teachers Michèle Gerbaldi; 17. Poster highlights: educating teachers; Part V. Astronomy and Pseudoscience: Preface; 18. Astronomy, pseudoscience and rational thinking Jayant V. Narlikar; 19. Astronomical pseudosciences in North America John R. Percy and Jay M. Pasachoff; Part VI. Astronomy and Culture: Preface; 20. Teaching astronomy in other cultures: archeoastronomy Julieta Fierro; 21. Poster highlights: astronomy and culture; Part VII. Astronomy in Developing Countries: Preface; 22. Astronomy Curriculum for developing countries Case Rijsdijk; 23. Science education resources for the developing countries James C. White II; Part VIII. Public Outreach in Astronomy: Preface; 24. What makes informal education programs successful? Nahide Craig and Isabel Hawkins; 25. The role of science centers and planetariums Nick Lomb; 26. Science education for the new century - a European perspective Claus Madsen; 27. Communicating astronomy to the public Charles Blue; 28. Poster highlights: public outreach in astronomy; Part IX. The Education Programs of the IAU: Preface; 29. A short overview of astronomical education carried out by the IAU Syuzo Isobe; Part X. Discussion; Index. Title: Scientific observations at total solar eclipses Authors: Pasachoff, Jay M. Bibcode: 2009RAA.....9..613P Altcode: The occasion of the longest totality of an eclipse in the 18 yr 11⅓ d saros cycle leads to taking stock of the scientific value of ground-based eclipse observations in this space age. Though a number of space satellites from the U.S., Europe, Japan, and Russia study the Sun, scientists at eclipses can observe the solar chromosphere and corona at higher spatial resolution, at higher temporal resolution, and at higher spectral resolution than are possible aloft. Furthermore, eclipse expeditions can transport a wide variety of state-of-the-art equipment to the path of totality. Thus, for at least some years to come, solar eclipse observations will remain both scientifically valuable and cost-effective ways to study the outer solar atmosphere. Title: Solar eclipses as an astrophysical laboratory Authors: Pasachoff, Jay M. Bibcode: 2009Natur.459..789P Altcode: Observations of the Sun during total eclipses have led to major discoveries, such as the existence of helium (from its spectrum), the high temperature of the corona (though the reason for the high temperature remains controversial), and the role of magnetic fields in injecting energy into-and trapping ionized gases within-stellar atmospheres. A new generation of ground-based eclipse observations reaches spatial, temporal and spectral-resolution domains that are inaccessible from space and therefore complement satellite studies. Title: Solar Eclipses and the International Year of Astronomy Authors: Pasachoff, Jay M. Bibcode: 2009AAS...21440101P Altcode: Solar eclipses capture the attention of millions of people in the countries from which they are visible and provide a major opportunity for public education, in addition to the scientific research and student training that they provide. The 2009 International Year of Astronomy began with an annular eclipse visible from Indonesia on 26 January, with partial phases visible also in other parts of southeast Asia. On 22 July, a major and unusually long total solar eclipse will begin at dawn in India and travel across China, with almost six minutes of totality visible near Shanghai and somewhat more visible from Japanese islands and from ships at sea in the Pacific. Partial phases will be visible from most of eastern Asia, from mid-Sumatra and Borneo northward to mid-Siberia. Eclipse activities include many scientific expeditions and much ecotourism to Shanghai, Hangzhou, and vicinity. My review article on "Eclipses as an Astrophysical Laboratory" will appear in Nature as part of their IYA coverage. Our planetarium presented teacher workshops and we made a film about solar research. Several new books about the corona or eclipses are appearing or have appeared. Many articles are appearing in astronomy magazines and other outlets. Eclipse interviews are appearing on the Planetary Society's podcast "365 Days of Astronomy" and on National Geographic Radio. Information about the eclipse and safe observation of the partial phases are available at http://www.eclipses.info, the Website of the International Astronomical Union's Working Group on Solar Eclipses and of its Program Group on Public Education at the Times of Eclipses of its Commission on Education and Development.

The Williams College Expedition to the 2009 Eclipse in the mountains near Hangzhou, China, is supported in part by a grant from the Committee for Research and Exploration of the National Geographic Society. E/PO workshops were supported by NASA. Title: The X-Ray Environment During the Epoch of Terrestrial Planet Formation: Chandra Observations of h Persei Authors: Currie, Thayne; Evans, Nancy Remage; Spitzbart, Brad D.; Irwin, Jonathan; Wolk, Scott J.; Hernandez, Jesus; Kenyon, Scott J.; Pasachoff, Jay M. Bibcode: 2009AJ....137.3210C Altcode: 2008arXiv0811.1753C We describe Chandra/ACIS-I observations of the massive ~ 13-14 Myr-old cluster, h Persei, part of the famous Double Cluster (h and χ Persei) in Perseus. Combining the list of Chandra-detected sources with new optical/IR photometry and optical spectroscopy reveals ~ 165 X-ray bright stars with V lsim 23. Roughly 142 have optical magnitudes and colors consistent with cluster membership. The observed distribution of Lx peaks at Lx ~ 1030.3 erg s-1 and likely traces the bright edge of a far larger population of ≈ 0.4-2 M sun X-ray active stars. From a short list of X-ray active stars with IRAC 8 μm excess from warm, terrestrial zone dust, we derive a maximum X-ray flux incident on forming terrestrial planets. Although there is no correlation between X-ray activity and IRAC excess, the fractional X-ray luminosity correlates with optical colors and spectral type. By comparing the distribution of Lx /L sstarf versus spectral type and V - I in h Per with results for other 1-100 Myr-old clusters, we show that stars slightly more massive than the Sun (gsim 1.5 M sun) fall out of X-ray saturation by ≈ 10-15 Myr. Changes in stellar structure for gsim 1.5 M sun stars likely play an important role in this decline of X-ray emission. Title: Pluto Stellar Occultation on 2008 Aug 25 Authors: Buie, Marc W.; Young, L. A.; Young, E. F.; Olkin, C. B.; Terrell, D.; Parker, J. W.; Durda, D.; Stansberry, J. A.; Reitsema, H.; French, R. G.; Shoemaker, K.; Brown, M. E.; Schaller, E. L.; Bauer, J. M.; Young, J. W.; Wasserman, L. H.; Pasachoff, J. M.; Lust, N.; Fernandez, Y. R.; Dellinger, J. A.; Garossino, P. G. A.; Grigsby, B.; Stone, R. P. S.; Dillon, W. G.; Mezzalira, F.; Ryan, E. V.; Ryan, W.; Souza, S. P.; Williams, R.; Sexton, C. Bibcode: 2009DPS....40.4805B Altcode: 2009BAAS...41..562B We report on a successful occultation of a star by Pluto that was observable over much of the south and western United States. The centerline was close to WIRO. We will present seven complete lightcurves from Crossley/Lick, WIRO, SBO/CU, Palomar, JPL/TMO, Sierra Stars Obs., and Magdalena Ridge Observatory. We have 2 partial lightcurves from Lowell Obs. and McDonald Obs. where data loss was caused by clouds. There were attempts at the Steward 90", George Observatory, and New Mexico Skies that were clouded out. The UCF station near Orlando was clearly an appulse. A number of other amateurs also succeeded in collecting data. Our presentation will provide a final geometric solution for the event as well as baseline fits to the atmospheric structure. This work was supported by NASA Planetary Astronomy grants NNX08AO626 and NNX08AO50G. Title: Division XII / Commission 46 / Program Group World-Wide Development of Astronomy Authors: Hearnshaw, John B.; Batten, Alan H.; Alsabti, A. Athem; Fierro, Julieta; Guinan, Edward F.; Kozai, Yoshihide; Levato, Hugo; Malasan, Hakim L.; Marschall, Laurence A.; Martinez, Peter; Narlikar, Jayant V.; Osório, J. Pereira; Pasachoff, Jay M.; Perkins, D. Kala; Zhu, Jin Bibcode: 2009IAUTA..27..429H Altcode: The Program Group for World-wide Development of Astronomy (PG-WWDA) is one of nine Commission 46 program groups engaged with various aspects of astronomical education or development of astronomy education and research in the developing world. In the case of PG-WWDA, its goals are to promote astronomy education and research in the developing world through a variety of activities, including visiting astronomers in developing countries and interacting with them by way of giving encouragement and support. Title: Commission 46: Astronomy Education and Development Authors: Stavinschi, Magdalena G.; Ros, Rosa M.; Pasachoff, Jay M.; Andersen, Johannes; Deustua, Susana E.; De Greve, Jean-Pierre; Guinan, Edward F.; Haubold, Hans J.; Hearnshaw, John B.; Jones, Barrie W.; Kochhar, Rajesh K.; Leung, Kam-Ching; Marschall, Laurence A.; Percy, John R.; Torres-Peimbert, Silvia Bibcode: 2009IAUTA..27..424S Altcode: Commission 46 continues its task in the triennium, which started in September 2006. It seeks to further contribute to the development and improvement of astronomical education at all levels all over the world through various projects initiated, maintained and to be developed by the Commission, and by disseminating information concerning astronomy education. Title: Comets, Charisma, and Celebrity: Reflections on Their Deep Impact Authors: Olson, R. J. M.; Pasachoff, J. M. Bibcode: 2009diwo.conf...41O Altcode: In celebration of the Deep Impact Mission, this essay explores the influence of comets on the arts and sciences since the beginning of recorded time. Through images, ranging from the sublime to the humorous, it probes the reasons why comets are among the most charismatic visual spectacles in the universe and why, even as scientific missions unmask their mysteries, they remain iconic symbols and harbingers of change. Title: Waves in Pluto's Upper Atmosphere Authors: Person, M. J.; Elliot, J. L.; Gulbis, A. A. S.; Zuluaga, C. A.; Babcock, B. A.; McKay, A. J.; Pasachoff, J. M.; Souza, S. P.; Hubbard, W. B.; Kulesa, C. A.; McCarthy, D. W.; Benecchi, S. D.; Levine, S. E.; Bosh, A. S.; Ryan, E. V.; Ryan, W. H.; Meyer, A.; Wolf, J.; Hill, J. Bibcode: 2008AJ....136.1510P Altcode: Observations of the 2007 March 18 occultation of the star P445.3 (2UCAC 25823784; R = 15.3) by Pluto were obtained at high time resolution at five sites across the western United States and reduced to produce light curves for each station using standard aperture photometry. Global models of Pluto's upper atmosphere are fitted simultaneously to all resulting light curves. The results of these model fits indicate that the structure of Pluto's upper atmosphere is essentially unchanged since the previous occultation observed in 2006, leading to a well-constrained measurement of the atmospheric half-light radius at 1291 ± 5 km. These results also confirm that the significant increase in atmospheric pressure detected between 1988 and 2002 has ceased. Inversion of the Multiple Mirror Telescope Observatory light curves with unprecedented signal-to-noise ratios reveals significant oscillations in the number density, pressure, and temperature profiles of Pluto's atmosphere. Detailed analysis of this highest resolution light curve indicates that these variations in Pluto's upper atmospheric structure exhibit a previously unseen oscillatory structure with strong correlations of features among locations separated by almost 1200 km in Pluto's atmosphere. Thus, we conclude that these variations are caused by some form of large-scale atmospheric waves. Interpreting these oscillations as Rossby (planetary) waves allows us to establish an upper limit of less than 3 m s-1 for horizontal wind speeds in the sampled region (radius 1340-1460 km) of Pluto's upper atmosphere. Title: Probing small bodies in the outer solar system with stellar occultations Authors: Person, M. J.; Elliot, J. L.; Pasachoff, J. M.; Gulbis, A. A. S. Bibcode: 2008epsc.conf..588P Altcode: We present a summary of results from the last decade of stellar occultation studies by members of the MITWilliams consortium. Research goals included investigations of the atmospheres and figures of small bodies in the outer solar system, focusing on Triton, Pluto, and Charon. We concentrated on the prediction, observation, and analysis of stellar occultations by these bodies. The method of observing stellar occultations provides higher spatial resolution than any other Earth-based observing method when examining bodies in the outer solar system. It also allows for direct measurements of atmospheric conditions, if any, as the observed starlight is refracted through the atmospheres of these planetary bodies during the occultation. This large spatial resolution (about 1 km in the atmosphere of Pluto) and direct interaction with any atmosphere allows for great sensitivity to the detailed pressure/temperature structure of a planetary atmosphere, and multiple observations over several years allow the monitoring of changes to that structure. Title: Total Solar Irradiance at the 2006 Transit of Mercury and Application to Transiting-Exoplanet Observations Authors: Pasachoff, Jay M.; Schneider, G.; Willson, R. C. Bibcode: 2008DPS....40.1119P Altcode: 2008BAAS...40..404P Following our earlier work on the Total Solar Irradiance (TSI) at the 2004 transit of Venus, in which an 0.4 percent drop in TSI was readily detectable with the ACRIM3 instrument on NASA's ACRIMsat, we report on ACRIM3 observations of the 29 November 2006 transit of Mercury. We also observed the transit from Haleakala and from Sacramento Peak. Mercury's cross-sectional angular area is only 1/30th that of Venus's, so the expected drop in TSI was only 0.01 percent. As expected, this tiny drop was not detected, though detailed statistical analysis continues. Our Venus and Mercury transit observations provide closeup views of phenomena increasingly observed for exoplanets and provide examples by which one can assess the limits at which exoplanet discoveries can be made with the transit method.

Acknowledgments: JMP's planetary occultation work and the POETS instrument (Portable Occultation, Eclipse, and Transit System) were funded in part by NASA Planetary Astronomy grants NNG04GE48G, NNG04GF25G, NNH04ZSS001N, and NNG05GG75G to M.I.T. and Williams College, and continues under NNX08AO50G. Our transit work was funded in part by the Committee for Research and Exploration of the National Geographic Society. ACRIMsat is supported by a grant from NASA to Columbia University. Title: Observations and Chemical Modelling of Edge Cloud 2 Authors: Ruffle, P. M. E.; Millar, T. J.; Roberts, H.; Lubowich, D. A.; Henkel, C.; Pasachoff, J. M.; Brammer, G. Bibcode: 2008ASPC..395..377R Altcode: Edge Cloud 2 (EC2) is a large molecular cloud with one of the largest galactocentric distances known in the Milky Way (Rgc∼24 kpc). We use observations of EC2 to determine its physical characteristics. A temperature of 20 K was estimated from our ammonia detections and a gas density of n({H}2) ∼ 104 cm-3 was determined by comparing LVG models of a number of species to their deconvolved line detections. Taking the clumpy structure of EC2 into account, we also calculated MEC2 ∼ 104 Msun, and from peak continuum emission we calculated a dust mass for EC2 and a dust-to-gas mass ratio ≥ 0.001. To establish the most likely chemical and physical properties of EC2, we made a pseudo-time-dependent chemical kinetic model. This uses our observationally derived temperatures and densities, and varies elemental initial abundances, photon flux, cosmic-ray ionisation rate and gas-to-dust ratio in an attempt to fit the observed results. We found that heavy elements may be depleted by a factor of ∼5 relative to local molecular clouds. The models also suggest a high UV photon field in EC2 (10-20× local values). Some of our models indicate that steady-state is reached very quickly after around 5,000 yr. Our observed high abundances of the radicals C2H and CN are typical of photon-dominated regions. This may be related to a large value of the UV flux to grain surface area compared to local clouds. Our best-fit models are consistent with reduced elemental abundances and a low dust-to-gas mass ratio. Such reduced abundances may be attributed to the low level of star formation in this region, and are probably also related to the continuing infall of low-metallicity halo gas since the Milky Way formed. Although EC2 does contain young stars, there is no evidence of the late-type stars which produce dust grains, thereby justifying the assumption of a high ratio of UV flux to grain surface area. We conclude that, despite the position of EC2 in the Galaxy, UV photons (rather than cosmic rays) play an important role in establishing its detailed chemical composition. Given that EC2 is in a region of extremely low gas pressure and very small spiral arm perturbation, questions remain as to the origin of its morphology and dynamics. A SNR associated with EC2, GSH 138-01-94, is the largest and oldest SNR known in the Milky Way. It consists of a H I shell with an expansion velocity of ∼12 km s-1 and an expansion age of 4.3 Myr, so EC2 could be as young as the ages derived from our time-dependent calculations. We conclude that the formation, structure, and subsequent chemistry of EC2 may be the direct result of shock fronts from GSH 138-01-94 propagating through the medium between 103 and 104 yr ago. Title: Innovation in Astronomy Education Authors: Pasachoff, Jay M.; Ros, Rosa M.; Pasachoff, Naomi Bibcode: 2008iae..book.....P Altcode: Preface; Part I. General Strategies for Effective Teaching: Introduction; 1. Main objectives of SpS2; 2. Learning astronomy by doing astronomy; 3. Hands-on Universe-Europe; 4. Life on Earth in the atmosphere of the Sun; 5. A model of teaching astronomy to pre-service teachers; 6. How to teach, learn about, and enjoy astronomy; 7. Clickers: a new teaching tool of exceptional promise; 8. Educational opportunities in pro-am collaboration; 9. Teaching history of astronomy to second-year engineering students; 10. Teaching the evolution of stellar and Milky Way concepts through the ages; 11. Educational efforts of the International Astronomical Union; 12. Astronomy in culture; 13. Light pollution: a tool for astronomy education; 14. Astronomy by distance learning; 15. Edible astronomy demonstrations; 16. Amateur astronomers as public outreach partners; 17. Does the Sun rotate around Earth or Earth rotate around the Sun?; 18. Using sounds and sonifications for astronomy outreach; 19. Teaching astronomy and the crisis in science education; 20. Astronomy for all as part of a general education; Poster abstracts; Part II. Connecting Astronomy with the Public: Introduction; 21. A status report from the Division XII working group; 22. Outreach using media; 23. Astronomy podcasting; 24. IAU's communication strategy, hands-on science communication, and the communication of the planet definition discussion; 25. Getting a word in edgeways: the survival of discourse in audiovisual astronomy; 26. Critical evaluation of the new Hall of Astronomy; 27. Revitalizing astronomy teaching through research on student understanding; Poster abstracts; Part III. Effective Use of Instruction and Information Technology: Introduction; 28. ESO's astronomy education program; 29. U.S. student astronomy research and remote observing projects; 30. Global network of autonomous observatories dedicated to student research; 31. Remote telescopes in education: report of an Australian study; 32. Visualizing large astronomical data holdings; Poster abstracts; Part IV. Practical Issues Connected with the Implementation of the 2003 IAU Resolution: Introduction; 33. Stellar evolution for students of Moscow University; 34. Astronomy for everybody: An approach from the CASAO/NAUH view; 35. Toward a new program in astronomy education in secondary schools in Turkey; 36. Universe awareness for young children; 37. Education in Egypt and Egyptian responses to eclipses; 38. Astronomy in the cultural heritage of African societies; 39. Education at the Pierre Auger Observatory: the cinema as a tool in science education; 40. Freshman seminars: interdisciplinary engagements in astronomy; 41. Astronomy for teachers; Poster abstracts; Conclusion. Title: Polar Plume Brightening During the 2006 March 29 Total Eclipse Authors: Pasachoff, J. M.; Rušin, V.; Druckmüller, M.; Druckmüllerová, H.; Bělík, M.; Saniga, M.; Minarovjech, M.; Marková, E.; Babcock, B. A.; Souza, S. P.; Levitt, J. S. Bibcode: 2008ApJ...682..638P Altcode: We discuss a remarkable brightening in a polar plume, as inferred from unique coordinated observations of the white-light corona during the total eclipse of the Sun of 2006 March 29. The polar plume (also known as a polar ray, with distinctions that we discuss) was observed at the positional angle of 9° the velocity at which the brightening propagated was about 65 km s-1, which is close to the values derived by modeling of mass/energy transfer in polar plumes/rays as well as to those acquired from images from the Extreme-ultraviolet Imaging Telescope on the European Space Agency/NASA Solar and Heliospheric Observatory (SOHO/EIT). Comparing our data with those from the SOHO/LASCO C2 coronagraph, we estimate the lifetime of the polar ray to be less than 24 hr. Title: Simultaneous SoHO and TRACE Observations of the Solar Atmosphere Authors: Tingle, E. D.; Pasachoff, J. M. Bibcode: 2008AGUSMSP31C..04T Altcode: From May 24-27, 2004, the Transition Region and Coronal Explorer (TRACE) and the Solar Ultraviolet Measurement of Emitted Radiation (SUMER) instrument aboard Solar and Heliospheric Observer (SoHO) simultaneously observed the northwest and southwest regions of the sun. Through SUMER's measurements, we made detailed velocity measurements from different layers of the solar atmosphere corresponding to different temperatures and emission lines. Original programs written in Interactive Data Language (IDL) revealed maximum and minimum velocities within the region populated by spicules from 2,000-10,000 km above the solar limb. These values were compared to TRACE observations taken in 1600 Å, which revealed a strong coronal loop feature with a strong blueshifted Si II (1533.4 Å) emission line and a simultaneously strong redshifted C IV (1548.2 Å) emission line suggesting differing flows of material at different temperatures within the loop feature. In this paper, we seek to further our knowledge of coronal loop evolution and dynamics, specifically the observed differing temperature flows. We thank Ingolf Dammasch for his expertise. Obtaining the data was supported in part by NASA grant NNG04GK44G and the current reduction work is supported in part by NASA grant NNM07AA01G from NASA's Marshall Space Flight Center. Title: Using SST and TRACE Observations to Test Spicule Models Authors: Jacobson, W. A.; Pasachoff, J. M. Bibcode: 2008AGUSMSP43B..02J Altcode: Spicules are jets of plasma that rise out of the solar photosphere at between 10 and 150 km/s to a maximum height of about 10,000 km. These jets, which typically live between five and fifteen minutes, make up the chromosphere and contribute to the heating of the lower solar atmosphere. Using Interactive Data Language (IDL) for image alignment and the processing program ImageJ, we were able to determine spicule statistics from observations taken at the solar limb with the Swedish 1-m Solar Telescope (SST) in July 2006. In addition, Dopplergram movies allowed for a more complete understanding of spicule formation, motions, and evolution. This understanding was further enhanced by comparing simultaneous SST and Transition Region and Coronal Explorer (TRACE) images, which allowed us to link corresponding spicule-related events in different layers of the solar atmospheric. We consider our results in terms of recent spicule models. We thank Mats Lofdahl of the Royal Swedish Academy of Sciences for his work on Multi-Object Multi-Frame Blind Deconvolution of the SST data. Obtaining the data was supported in part by NASA grant NNG04GK44G and the current reduction work is supported in part by NASA grant NNM07AA01G from NASA's Marshall Space Flight Center. Title: Chromosphere and Corona for Research and Education Authors: Pasachoff, Jay M. Bibcode: 2008mear.confE..29P Altcode: No abstract at ADS Title: Hinode's Solar Wonderland Authors: Pasachoff, Jay M. Bibcode: 2008S&T...115d..64P Altcode: No abstract at ADS Title: Recent Stellar Occultation Observations Using High-Speed, Portable Camera Systems Authors: Gulbis, A. A. S.; Elliot, J. L.; Person, M. J.; Babcock, B. A.; Pasachoff, J. M.; Souza, S. P.; Zuluaga, C. A. Bibcode: 2008AIPC..984...91G Altcode: We have recently constructed six observing systems identified as POETS (Portable Occultation Eclipse and Transit System[1]). These systems are optimized for (i) high-speed, high signal-to-noise observations at visible wavelengths and (ii) easy transport, to allow mounting on telescopes worldwide. The Andor iXon cameras have e2v CCD97 (frame transfer) sensors: a 512×512 array of 16-micron pixels, back illuminated, with peak quantum efficiency >90%. The maximum readout rate is 32 full frames per second, while binning and subframing can increase the cadence to a few hundred frames per second. Read noise in conventional modes goes below 6 electrons per pixel. Further, an electron-multiplying mode can effectively reduce the read noise to sub-electron levels, at the expense of dynamic range. The cameras are operated via a desktop computer that contains a 3 GHz Pentium 4 processor, 2 GB memory, and a 10,000 rpm hard disk. Images are triggered from a GPS receiver and have an approximately 50 nanosecond timing uncertainty. Each POETS can be transported as carry-on luggage. Here, we present instrument details, along with recent results from their use in stellar occultation observations by small bodies in the outer solar system. Occultations can produce data of the highest spatial resolution for any Earth-based observing method; therefore, they play a key role in determining diameters of distant solar-system bodies and probing the structure of atmospheres at the microbar level. We discuss POETS deployments in 2005-2007 to observe stellar occultations by Charon and Pluto (on 0.6- to 6.5-m telescopes) and future work on occultations by Kuiper Belt objects. Title: Executive Committee Working Group Young Astronomers Events Authors: Gerbaldi, Michèle; De Greve, Jean-Pierre; Dovčiak, Michal; Engvold, Oddbjørn; Guinan, Edward F.; Hearnshaw, John B.; Johnston-Hollitt, Melanie; Pasachoff, Jay M.; Percy, John R.; Ribas, Ignasi; White, James C.; Dovčiak, Michal; Goosmann, René; Pecháček, Tomáš; Stoklasová, Ivana Bibcode: 2007IAUTB..26..242G Altcode: At the IAU XXV General Assembly in Sydney, 2003, a questionnaire on the perception of participation of “young astronomers” at IAU meeting was distributed. Following the conclusions from the analysis of this questionnaire, the IAU EC recommended in 2004 that the “young astronomers” concept at the next GA in Prague should be worked out with specific activities. Title: Commission 46: Astronomy Education and Development Authors: Pasachoff, Jay M.; Jones, Barrie W.; Hearnshaw, John B.; Gerbaldi, Michèle; Christensen, Lars Lindberg; Tolbert, Charles R.; Percy, John R. Bibcode: 2007IAUTB..26..230P Altcode: The International Astronomical Union (IAU) was founded in 1922 to “promote and safeguard astronomy . . . and to develop it through international co-operation”. The IAU is funded through its National Members. Almost all of the funds supplied from the dues are used for the development of astronomy. Title: Galactic Edge Clouds. I. Molecular Line Observations and Chemical Modeling of Edge Cloud 2 Authors: Ruffle, P. M. E.; Millar, T. J.; Roberts, H.; Lubowich, D. A.; Henkel, C.; Pasachoff, J. M.; Brammer, G. Bibcode: 2007ApJ...671.1766R Altcode: 2007arXiv0708.2740R Edge Cloud 2 (EC2) is a molecular cloud, about 35 pc in size, with one of the largest galactocentric distances known to exist in the Milky Way. We present observations of a peak CO emission region in the cloud and use these to determine its physical characteristics. We calculate a gas temperature of 20 K and a density of n(H2)~104 cm-3. Based on our CO maps, we estimate the mass of EC2 at around 104 Msolar and continuum observations suggest a dust-to-gas mass ratio as low as 0.001. Chemical models have been developed to reproduce the abundances in EC2, and they indicate that heavy element abundances may be reduced by a factor of 5 relative to the solar neighborhood (similar to dwarf irregular galaxies and damped Lyα systems), very low extinction (AV<4 mag) due to a very low dust-to-gas mass ratio, an enhanced cosmic-ray ionization rate, and a higher UV field compared to local interstellar values. The reduced abundances may be attributed to the low level of star formation in this region and are probably also related to the continuing infall of primordial (or low-metallicity) halo gas since the Milky Way formed. Finally, we note that shocks from the old supernova remnant GSH 138-01-94 may have determined the morphology and dynamics of EC2. Title: Division Xii: Union-Wide Activities Authors: Trimble, Virginia L.; Andersen, Johannes; Aksnes, Kaare; Genova, Françoise; Gurshtein, Alexander A.; Johansson, Sveneric; Pasachoff, Jay M.; Smith, Malcolm G. Bibcode: 2007IAUTB..26..211T Altcode: Division XII consists of Commissions that formerly were organized under the Executive Committee, that concern astronomers across a wide range of scientific sub-disciplines and provide interactions with scientists in a wider community, including governmental organizations, outside the IAU. Title: Fifty Years Later: My New York City Moonwatch Observations Authors: Pasachoff, Jay M. Bibcode: 2007AAS...211.2301P Altcode: 2007BAAS...39..774P When Sputnik was launched on October 4, 1957, I was a member of the New York City Moonwatch team through the Amateur Astronomers Association. As 14-year-old sophomore at the Bronx High School of Science, I took the subway, the D train, from the Bronx to the RCA building in Rockefeller Center, where we observed from the roof. I remember our line or lines of elbow telescopes and our eventual success in detecting Sputnik overhead. My talk will include my recent reminiscences as a letter to the editor of The New York Times; the certificate that the Amateur Astronomers Association gave to the Pulkovo Observatory in what is now St. Petersburg, Russia; and a survey of Moonwatch history. I will also share reminiscences reported from some colleagues. Title: Book review: The Sun Kings: The Unexpected Tragedy of Richard Carrington and the Tale of How Modern Astronomy Began / Princeton University Press, Princeton and Oxford, xii + 211 pp., 2007, ISBN 978-0-691-12660-9. Authors: Pasachoff, Jay M.; Pasachoff, Naomi Bibcode: 2007JHA....38..524P Altcode: No abstract at ADS Title: Electron-Multiplying CCD Imaging: Effectiveness for Stellar Occultations by Faint Objects Authors: Gulbis, Amanda A.; Elliot, J. L.; Person, M. J.; Souza, S. P.; Babcock, B. A.; Pasachoff, J. M.; McKay, A. J.; Zuluaga, C. A. Bibcode: 2007DPS....39.3408G Altcode: 2007BAAS...39..480G Our Portable Occultation, Eclipse, and Transit Systems (POETS; Souza et al. 2006, PASP 118, 1550) have been successfully employed for multiple stellar occultation observations: (i) four systems obtained data in South America during the 11 July 2005 occultation of C313.2 (2UCAC 26257135) by Charon (Gulbis et al. 2006, Nature 439, 48; Person et al. 2006, AJ 132 1575); (ii) four systems obtained data in Australia during the 2006 June 12 occultation of P384.2 (2UCAC 26039859) by Pluto (Elliot et al. 2007, AJ 134, 1), and (iii) three systems were utilized in the Southwestern U.S. for the 2007 March 18 occultation of P445.2 (2UCAC 25823784) by Pluto (Person et al. 2007, this meeting).

Pluto and Charon have apparent V magnitudes of 14 and 16, and the stars for these events had UCAC magnitudes of 14.99 to 15.25. These events were bright enough to achieve fair to excellent signal-to-noise ratios (SNRs) at cadences between 2 and 10 Hz by using "conventional” camera modes. POETS also possess electron-multiplying (EM) readout modes, which we have not yet employed for occultation observations because conventional modes have been more than adequate. EM modes have higher read noise, generate an excess noise factor, and limit dynamic range; however, signal can be increased by a factor of up to 1000x, and read noise is effectively eliminated at high EM gain. Here, we explore the benefits and disadvantages of using EM capability for observations of stellar occultations by faint bodies. We focus on prospective occultations by Kuiper Belt objects, predictions of which are increasingly numerous as fainter stars are considered. We identify regimes in which EM modes are most effective by analyzing SNR as a function of exposure time and object/star magnitudes.

This work is supported by NASA Planetary Astronomy grants NNG04GF25G and NNG04GE48G. Title: High Altitude Structure in Pluto's Atmosphere from the 2007 March 18 Stellar Occultation Authors: Person, Michael J.; Elliot, J. L.; Gulbis, A. A.; Zuluaga, C. A.; Babcock, B. A.; Pasachoff, J. M.; McKay, A. J.; Souza, S. P.; Hubbard, W. B.; Kulesa, C. A.; McCarthy, D. W.; Kern, S. D.; Levine, S. E.; Bosh, A. S.; Ryan, E. V.; Ryan, W. H.; Meyer, A.; Wolf, J.; Hill, J. M. Bibcode: 2007DPS....39.5214P Altcode: 2007BAAS...39..519P Visible wavelength observations were made of the 2007 March 18 Pluto occultation of the star P445.3 (UCAC2 25823784; McDonald and Elliot, AJ 120, 1599) from five US sites by our consortium (Pasachoff, et al., 2007, this meeting). Simultaneous model fitting to all of our light curve data yielded 1207 ± 4 km as the half-light shadow radius of Pluto's atmosphere. This radius is consistent with the 1208 ± 9 km result measured in 2006 (Elliot, et al., AJ 134,1) and confirms that the large increase in atmospheric pressure measured between the 1988 and 2002 (Elliot, et al., Nature 424,165 Sicardy, et al., Nature 424, 168) observations has ceased. Inversion of the highest signal-to-noise visible light curve, obtained with the Portable Occultation Eclipse and Transit Systems (POETS; Souza, et al., PASP 118, 1550) at the 6.5-m MMT (MMTO, Fred Lawrence Whipple Observatory, Mt. Hopkins) resulted in number density, pressure, and temperature profiles for Pluto's atmosphere in the radius range of 1340 - 1460 km (assuming the dominant atmospheric component is N2). These inversions reveal oscillating deviations of the number density from a simple exponential profile in Pluto's upper atmosphere that are coherent across the 1000 km length of the grazing occultation and also in the 300 km line of sight. Here, we interpret this structure as vertically propagating waves in Pluto's upper atmosphere, and provide a feasible mechanism for the maintenance of this large-scale coherence in terms of Rossby planetary waves. This work was partially funded by NASA Planetary Astronomy grants NNG04GE48G, NNG04GF25G, NNH04ZSS001N, and NNG05GG75G. Partial funding for MMTO observations was also provided by Astronomy Camp. Some of the observations reported here were obtained at the MMT Observatory, a joint facility of the University of Arizona and the Smithsonian Institution. Title: Observational Results from the 2007 March 18 Pluto Stellar Occultation Authors: Pasachoff, Jay M.; Babcock, B. A.; Souza, S. P.; McKay, A. J.; Person, M. J.; Elliot, J. L.; Gulbis, A. A.; Zuluaga, C. A.; Hill, J. M.; Ryan, E. V.; Ryan, W. H. Bibcode: 2007DPS....39.6203P Altcode: 2007BAAS...39Q.541P Our consortium observed the 5-minute occultation by Pluto of the star we call P445.3 (2UCAC 25823784, UCAC magnitude 15.3; McDonald and Elliot, 2000, AJ 120, 1599) from sites in the American southwest on 2007 March 17/18 (18 March, UT). Shadow velocity was 6.8 km/s. The 2007 occultation grazed the atmosphere. We were able to use one of the 8.4-m mirrors of the Large Binocular Telescope Observatory, still in its engineering stage, though only with its facility guide camera and not with our Portable Occultation, Eclipse, and Transit System (POETS) CCD/GPS/computer instruments (Souza et al., 2006, PASP 118, 1550). Because of the accurate GPS timing, we were able to align the light curve obtained, which included only the second half of the occultation, with results from other telescopes, including the visible, beamsplit light curve obtained by our group with the 6.5-m MMT (Person et al., 2007, this meeting). We also used, with POETS, the 2.4-m Magdalena Ridge Observatory near Socorro, New Mexico; a partial light curve was obtained despite variable cloudiness throughout the 80 min observation. The location of this telescope was the farthest into the occultation path, and thus led to the deepest incursion into Pluto's atmosphere of the starlight of the major telescopes we used. Light curves were generated by frame-by-frame synthetic-aperture photometry. The large increase in atmospheric pressure we had earlier measured at the 2002 occultation compared with measurements at the first successful Pluto occultation, in 1988, has ceased, as shown by both the 2006 and the current, 2007 measurements.

Acknowledgments: We thank Richard Green for granting Director's Discretionary time for the LBT observations. This work was partially funded by NASA Planetary Astronomy grants NNG05GG75G, NNG04GE48G, NNG04GF25G, and NNH04ZSS001N to Williams College and to MIT. Title: Special Session 2 Innovation in teaching and learning astronomy Authors: Ros, Rosa M.; Pasachoff, Jay M. Bibcode: 2007HiA....14..541R Altcode: On August 17 and 18, 2006, Commission 46 on Astronomy Education and Development held a Special Session at the IAU XXVI General Assembly in Prague. The session, on Innovation in Teaching/Learning Astronomy, was organized around four themes: (i) general strategies for effective teaching, (ii) connecting astronomy with the public, (iii) effective use of instruction and information technology, and (iv) practical issues connected with the implementation of the 2003 IAU Resolution that recommended including astronomy in school curricula, assisting schoolteachers in their training and backup, and informing them about available resources. Approximately 40 papers were presented orally; in addition, 60 poster papers were displayed. Title: Fine Structures in the White-Light Solar Corona at the 2006 Eclipse Authors: Pasachoff, J. M.; Rušin, V.; Druckmüller, M.; Saniga, M. Bibcode: 2007ApJ...665..824P Altcode: Observations of the total solar eclipse of 2006 March 29, as it crossed Africa from southwest to northeast into a Greek island and beyond, allowed correlations with near-simultaneous coronal observations from several spacecraft, including SOHO and TRACE. New methods of compositing images allow the recovery of higher resolution (1"-2") on coronal features than had normally been available in the past, reaching substantially higher resolutions than are currently available from space. We discuss a variety of the new methods and observations, and use them to provide the most detailed portrait possible of the Sun, at least on 2006 March 29. Title: Changes in Pluto's Atmosphere: 1988-2006 Authors: Elliot, J. L.; Person, M. J.; Gulbis, A. A. S.; Souza, S. P.; Adams, E. R.; Babcock, B. A.; Gangestad, J. W.; Jaskot, A. E.; Kramer, E. A.; Pasachoff, J. M.; Pike, R. E.; Zuluaga, C. A.; Bosh, A. S.; Dieters, S. W.; Francis, P. J.; Giles, A. B.; Greenhill, J. G.; Lade, B.; Lucas, R.; Ramm, D. J. Bibcode: 2007AJ....134....1E Altcode: The 2006 June 12 occultation of the star P384.2 (2UCAC 26039859) by Pluto was observed from five sites in southeastern Australia with high-speed imaging photometers that produced time-series CCD images. Light curves were constructed from the image time series and fit by least-squares methods with model light curves. A new modeling procedure is presented that allows a simultaneous fit of the atmospheric parameters for Pluto and the astrometric parameters for the occultation to all of the light curves. Under the assumption of a clear atmosphere and using this modeling procedure to establish the upper atmosphere boundary condition, immersion and emersion temperature profiles were derived by inversion of the Siding Spring light curve, which had our best signal-to-noise ratio. Above ~1230 km radius, atmospheric temperatures are ~100 K and decrease slightly with altitude-the same as observed in 1988 and 2002. Below 1210 km, the temperature abruptly decreases with altitude (gradients ~2.2 K km-1), which would reach the expected N2 surface-ice temperature of ~40 K in the 1158-1184 km radius range. This structure is similar to that observed in 2002, but a much stronger thermal gradient (or stronger extinction) is implied by the 1988 light curve (which shows a ``kink'' or ``knee'' at 1210 km). The temperature profiles derived from inversion of the present data show good agreement with a physical model for Pluto's atmosphere selected from those presented by Strobel et al. (1996). Constraints derived from the temperature profiles (and considering the possibility of a deep troposphere) yield a value of 1152+/-32 km for Pluto's surface radius. This value is compared with surface-radius values derived from the series of mutual occultations and eclipses that occurred in 1985-1989, and the limitations of both types of measurements for determining Pluto's surface radius are discussed. The radius of Pluto's atmospheric shadow at the half-intensity point is 1207.9+/-8.5 km, the same as obtained in 2002 within measurement error. Values of the shadow radius cast by Pluto's atmosphere in 1988, 2002, and 2006 favor frost migration models in which Pluto's surface has low thermal inertia. Those models imply a substantial atmosphere when New Horizons flies by Pluto in 2015. Comparison of the shape of the stellar occultation light curves in 1988, 2002, and 2006 suggests that atmospheric extinction, which was strong in 1988 (15 months before perihelion), has been dissipating. Title: High-spectral-resolution Observations of the Solar Chromosphere and Corona Authors: Pasachoff, Jay M.; Bruck, M. A. Bibcode: 2007AAS...210.9507P Altcode: 2007BAAS...39..224P We continue to reduce high-spectral-resolution observations of the solar chromosphere from the Swedish 1-m Solar Telescope (SST) and TRACE; and, at the 29 March 2006 total solar eclipse, of the solar corona in the [Fe XIV] green line and the [Fe X] red line. (a) The SST observations in 2006 used the SOUP Lyot filter to observe H-alpha limb spicules in five positions with 128 milliangstrom resolution for velocity imaging with several cameras to allow restoration of even noisy images. One camera is near H-alpha, providing high S/N images for extracting wavefront information. The other is deliberately defocused for Phase Diversity information. We use Multi-Object Multi-Frame Blind Deconvolution (MOMFBD; momfbd.org), assisted by Michiel Van Noort and Mats Löfdahl (Royal Swedish Academy of Sciences) and the CfA Hinode center. Simultaneous TRACE observations show spicules in emission and, silhouetted against the EUV corona, in absorption. (b) Our Fabry-Perot 2006-eclipse coronal spectra were taken with David Rust's (JHUAPL) 0.16 angstrom Y-cut lithium-niobate filter. With Rust and Matthew Noble, the etalon was stepped across the red coronal line every 0.22 angstrom. We present the profile and Doppler shifts of the [Fe X] line. (c) We collected simultaneous 10 Hz observations in the red and green coronal lines at the 2006 eclipse, with the goal of detecting high-frequency intensity oscillations ( 1 Hz), which can be relevant to coronal heating, and to confirm previous results. We present FFT and wavelet analysis of the aligned data.

We thank Bryce Babcock and Steven Souza (Williams) for their eclipse collaboration. We acknowledge grants NNG04GK44G, NNG04GE48G, and NN05GG75G from NASA Planetary Astronomy. The eclipse observations were supported by NSF grant ATM-0552116 from the Solar Terrrestrial Program of the Atmospheres Sciences Division. Additional eclipse support was received from National Geographic's Committee on Research and Exploration and Williams's Rob Spring Fund. Title: (134340) Pluto Authors: Person, M. J.; Elliot, J. L.; Gulbis, A. A. S.; Zuluaga, C. A.; Babcock, B. A.; McKay, A. J.; Pasachoff, J. M.; Souza, S. P.; Hubbard, W. B.; Kulesa, C. A.; McCarthy, D. W.; Kern, S. D.; Levine, S. E.; Bosh, A. S.; Ryan, E. V.; Ryan, W. H.; Meyer, A.; Wolf, J. Bibcode: 2007IAUC.8825....1P Altcode: 2007IAUC.8825A...1P M. J. Person, J. L. Elliot, A. A. S. Gulbis, and C. A. Zuluaga, Massachusetts Institute of Technology; B. A. Babcock, A. J. McKay, J. M. Pasachoff, and S. P. Souza, Williams College; W. B. Hubbard, C. A. Kulesa, and D. W. McCarthy, University of Arizona; S. D. Kern, Space Telescope Science Institute; S. E. Levine, U.S. Naval Observatory; A. S. Bosh, Boston University; E. V. Ryan and W. H. Ryan, Magdalena Ridge Observatory; and A. Meyer and J. Wolf, SOFIA, report observations on Mar. 18 UT of an occultation by (134340) Pluto of the star/event called P445.3 by McDonald and Elliot (2000, A.J. 120, 1599; see also http://occult.mit.edu/research/occultations/Pluto/P445.3-preds/). The occultation was observed from five sites by their consortium (as well as by others). A preliminary astrometric solution based on the light curves from all of the stations places Pluto's shadow north of pre-event predictions. Based on this solution, the closest approach distance of the center of Pluto's shadow to their successful observation sites are as follows: Mount Hopkins, 1319 km; Magdalena Ridge, 1192 km; Fremont Peak, 1019 km; USNO Flagstaff Station, 1102 km; and Mt. Graham, 1258 km. All closest-approach distances are south of Pluto's center in the shadow plane, perpendicular to the direction to the star and shifted by the same amount within the uncertainties. The formal error on the astrometric solution is +/- 4 km, but error bars of +/- 15 km account for possible systematic effects. The half-light shadow radius from this solution is 1207 +/- 15 km, consistent with the shadow radius of 1208 +/- 10 km from 2006 (Elliot et al., A.J., in press). Title: Observing solar eclipses in the developing world Authors: Pasachoff, Jay M. Bibcode: 2007IAUSS...5..265P Altcode: No abstract at ADS Title: Education at the International Astronomical Union Meeting - Prague Czech Republic Authors: Ros, Rosa; Pasachoff, Jay Bibcode: 2007Spark...3...14R Altcode: No abstract at ADS Title: St. Benedict Sees the Light: Asam's Solar Eclipses as Metaphor Authors: Olson, Roberta J. M.; Pasachoff, Jay M. Bibcode: 2007ReArt..11..299O Altcode: During the Baroque period, artists worked in a style - encouraged by the Roman Catholic Church and the Council of Trent - that revealed the divine in natural forms and made religious experiences more accessible. Cosmas Damian Asam, painter and architect, and his brother Egid (Aegid) Quirin Asam, sculptor and stuccatore, were the principal exponents of eighteenth-century, southern-German religious decoration and architecture in the grand manner, the Gesamtkunstwerk. Cosmas Damian's visionary and ecstatic art utilized light, both physical and illusionistic, together with images of meteorological and astronomical phenomena, such as solar and lunar eclipses. This paper focuses on his representations of eclipses and demonstrates how Asam was galvanized by their visual, as well as metaphorical power and that he studied a number of them. He subsequently applied his observations in a series of paintings for the Benedictine order that become increasingly astronomically accurate and spiritually profound. From the evidence presented, especially in three depictions of St. Benedict's vision, the artist harnessed his observations to visualize the literary description of the miraculous event in the Dialogues of St. Gregory the Great, traditionally a difficult scene to illustrate, even for Albrecht Dürer. Asam painted the trio at Einsiedeln, Switzerland (1724-27); Kladruby, the Czech Republic (1725-27), where he captured the solar corona and the "diamond-ring effect"; and Weltenburg, Germany (1735), where he also depicted the diamond-ring effect at a total solar eclipse. We conclude that his visualizations were informed by his personal observations of the solar eclipses on 12 May 1706, 22 May 1724, and 13 May 1733. Asam may have also known the eclipse maps of Edmond Halley and William Whiston that were issued in advance. Astronomers did not start studying eclipses scientifically until the nineteenth century, making Asam's depictions all the more fascinating. So powerful was the image that Asam invented to visualize St. Benedict's vision that it found reflection in the subsequent Bavarian Benedictine visual tradition. Total solar eclipses are among the most spectacular sights in Nature. Therefore, in an age obsessed with revealing the divine through natural idioms and making religious experiences direct - not to mention that light had long functioned as a symbol of divinity in the Christian tradition - it seems fitting that solar eclipses would be interpreted as a metaphor of a divine presence or a miracle. Title: POETS: Portable Occultation, Eclipse, and Transit System Authors: Souza, Steven P.; Babcock, Bryce A.; Pasachoff, Jay M.; Gulbis, Amanda A. S.; Elliot, J. L.; Person, Michael J.; Gangestad, Joseph W. Bibcode: 2006PASP..118.1550S Altcode: Occultations of stars by small bodies in the outer solar system are opportunities to make high-resolution measurements of their geometries and orbital elements and to detect or probe their atmospheres. Such events are limited in space and time, so it is desirable to deploy highly capable camera systems on multiple fixed and/or portable telescopes anywhere in the world, potentially on short notice. Similar considerations apply to planetary transits and solar eclipses. We have designed a camera system called POETS (Portable Occultation, Eclipse, and Transit System), which is optimized for occultation and related observations, and have assembled five such systems. The core of this system is the Andor Technology DV-887 (now DU-897) frame-transfer camera, featuring a high frame rate, minimal dead time, high quantum efficiency, and low read noise. An electron-multiplying mode lowers effective read noise to below 1 e- pixel-1 and is capable of photon counting. Each POETS includes a compact GPS timing system with microsecond accuracy, and a high-performance computer system capable of sustained fast frame rates. Each POETS is designed to be transportable as carry-on luggage and is adaptable to a wide variety of sites. POETS were deployed for the first time for the 2005 July 11 Charon occultation event, and they performed extremely well on telescopes with apertures from 0.6 to 6.5 m. Three POETS were subsequently deployed for the 2006 March 29 total solar eclipse, and five for the 2006 June 12 Pluto occultation. Title: The April 8, 2005, Eclipse White-Light Corona Authors: Pasachoff, Jay M.; Kimmel, Shelby B.; Druckmüller, Miloslav; Rušin, Vojtech; Saniga, Metod Bibcode: 2006SoPh..238..261P Altcode: 2006SoPh..tmp...71P The hybrid solar eclipse of April 8, 2005, provided a good opportunity to observe the white-light solar corona, even though the eclipse lasted just 30 seconds and could be seen only from ships in the Pacific Ocean. During the eclipse, we detected a unique `cloud' of particles in the white-light corona above the west limb ≈260°-270°. We compare this feature with EUV images from SOHO. The feature's density and temperature seem comparable to a coronal condensation, and, like a coronal condensation, it is connected to the emergence of material from the solar surface without a flare. However, the morphology of the feature shows clear differences from a classical coronal condensation. Title: Charon's Radius and Density from the Combined Data Sets of the 2005 July 11 Occultation Authors: Person, M. J.; Elliot, J. L.; Gulbis, A. A. S.; Pasachoff, J. M.; Babcock, B. A.; Souza, S. P.; Gangestad, J. Bibcode: 2006AJ....132.1575P Altcode: 2006astro.ph..2082P The 2005 July 11 C313.2 stellar occultation by Charon was observed by three separate research groups, including our own, at observatories throughout South America. Here, the published timings from the three data sets have been combined to more accurately determine the mean radius of Charon: 606.0+/-1.5 km. Our analysis indicates that a slight oblateness in the body (0.006+/-0.003) best matches the data, with a confidence level of 86%. The oblateness has a pole position angle of 71.4d+/-10.4d and is consistent with Charon's pole position angle of 67°. Charon's mean radius corresponds to a bulk density of 1.63+/-0.07 g cm-3, which is significantly less than Pluto's (1.92+/-0.12 g cm-3). This density differential favors an impact formation scenario for the system in which at least one of the impactors was differentiated. Finally, unexplained differences between chord timings measured at Cerro Pachón and the rest of the data set could be indicative of a depression as deep as 7 km on Charon's limb. Title: Pluto's Atmospheric Structure: Results From The 2006 June 12 Stellar Occultation Authors: Gulbis, Amanda A.; Elliot, J. L.; Person, M. J.; Adams, E. R.; Kramer, E. A.; Zuluaga, C. A.; Pike, R. E.; Babcock, B. A.; Gangestad, J. W.; Jaskot, A. E.; Pasachoff, J. M.; Souza, S. P.; Francis, P. J.; Lucas, R.; Bosh, A. S.; Ramm, D. J.; Greenhill, J. G.; Giles, A. B.; Dieters, S. W. Bibcode: 2006DPS....38.3101G Altcode: 2006BAAS...38..541G Observations of the 2006 June 12 occultation by Pluto of P384.2 (McDonald & Elliot, AJ 120, 1599; UCAC2 26039859) were attempted by the MIT-Williams College collaboration from five sites in Australia and New Zealand. Four sites were successful: Black Springs, South Australia (0.8m); Mt. Canopus, Tasmania (1m); Mt. Stromlo, Australian Capital Territory (1.8m); and Siding Spring, New South Wales (2.3m). Data were recorded using Portable Occultation, Eclipse, and Transit Systems (POETS; Souza et al., in preparation).

Using these data, we characterize Pluto's atmosphere and compare our results to previous occultation observations. Above half-light level, the light curves exhibit the signature of an isothermal atmosphere. The scale height is consistent at 60 km, equivalent to a temperature of 110 K for an N2 atmosphere. Below half-light level, the light curves resemble those obtained in 2002 (Pasachoff et al., AJ 129, 1718) more than 1988 (Elliot et al., Icarus 77, 148). The data drop significantly below the isothermal curve at this level, due either to a thermal gradient or extinction (or some combination); however, the drop is not as abrupt as in 1988. Data from 2002 demonstrated that at least some extinction is at work, due to the wavelength dependence of the residual flux at the bottom of the light curves (Elliot et al., Nature 424, 165). Unfortunately, we do not have multi-wavelength observations for P384.2. Our highest signal-to-noise ratio data, from the 2.3m, exhibit spikes caused by density variations in Pluto's atmosphere and interesting structure in the bottom of the light curve, when the star is probing around the limb more than vertically. Data from this event are also discussed in Elliot et al., a derivation of Pluto's atmospheric size, and Pasachoff et al., a search for satellites, rings and debris.

Support partially provided by NASA grants NNG04GE48G, NNG04GF25G, and NNH04ZSS001N. Title: Astronomy through the years Authors: Pasachoff, Jay M. Bibcode: 2006Natur.443..274P Altcode: No abstract at ADS Title: A Search for Rings, Moons, or Debris in the Pluto System during the 2006 July 12 Occultation Authors: Pasachoff, Jay M.; Babcock, B. A.; Souza, S. P.; Gangestad, J. W.; Jaskot, A. E.; Elliot, J. L.; Gulbis, A. A.; Person, M. J.; Kramer, E. A.; Adams, E. R.; Zuluaga, C. A.; Pike, R. E.; Francis, P. J.; Lucas, R.; Bosh, A. S.; Ramm, D. J.; Greenhill, J. G.; Giles, A. B.; Dieters, S. W. Bibcode: 2006DPS....38.2502P Altcode: 2006BAAS...38..523P We examined our data runs from four sites for the 2006 July 12 occultation of the star P384.2 (McDonald & Elliot, AJ 120, 1599, 2000; UCAC2 26039859), to search for moons, rings, or other debris in the Pluto system. Our data runs extended 80 minutes, or 115,200 km. Motivated by the discovery of P1 (Hydra) and P2 (Nix), each approximately 50 km in diameter and thought to result from the same collision that formed Charon, S. A. Stern et al. (Nature 439, 946-948, 2006) suggested that such matter might be detectable. Though their first estimate was unobservably low at 5×10-6, it could change by a factor of 10,000 or more in either direction (Stern, private communication). Our cloudless data sets, in declining order of S/N, used our Portable Occultation, Eclipse, and Transit Systems (POETS; Souza et al., in preparation) and include those from the 2.3-m ANU telescope at Siding Spring, Australia; 0.8-m Black Springs telescope near Adelaide, and the 1.8-m EOS telescope at Mt. Stromlo; though the atmospheric observation time at the 1-m Mt. Canopus Telescope at Hobart could be recovered from the comparison stars, cloudy intervals prevent full recovery during the ring/debris possible interval. Our observing with the 1-m Mt. John University Observatory in New Zealand was rendered impossible by the lack of electricity resulting from a major snowstorm. For the ring/debris search, we also evaluated data from past Pluto (Pasachoff et al., AJ 129, 1718-1723, 2005) and Charon (Gulbis et al., Nature 439, 48-51, 2006) occultations. See also Elliot et al. and Gulbis et al. (this meeting).

We thank Ian Ritchie of Electro Optic Systems (Mt. Stromlo Observatory), Ian Bedford, Lyndon Hemer, and Fraser Farrell (Black Springs Observatory), and Blair Lade (Stockport Observatory). This work was partially supported by NASA Planetary Astronomy Grants NNH04ZSS001N, NNG04GE48G, and NNG04GF25G. Title: The Size of Pluto's Atmosphere As Revealed by the 2006 June 12 Occultation Authors: Elliot, James L.; Person, M. J.; Gulbis, A. A.; Adams, E. R.; Kramer, E. A.; Zuluaga, C. A.; Pike, R. E.; Pasachoff, J. M.; Souza, S. P.; Babcock, B. A.; Gangestad, J. W.; Jaskot, A. E.; Francis, P. J.; Lucas, R.; Bosh, A. S.; Giles, A. B.; Greenhill, J. G.; Dieters, S. W.; Ramm, D. J. Bibcode: 2006DPS....38.3102E Altcode: 2006BAAS...38..541E Observations of the 2006 June 12 occultation of P384.2 (McDonald & Elliot, AJ 120, 1599; aka UCAC2-26039859) were attempted at five sites by the MIT-Williams occultation group. Four were successful: the 0.8-m telescope at the Star Castle Observatory in Black Springs, the 1 m at the Mt. Canopus Observatory in Hobart, the 1.8 m at Mt. Stromlo, and the 2.3-m ANU telescope at Siding Spring. The data were recorded with our Portable Occultation, Eclipse, and Transit Systems (POETS; Souza et al., in preparation). These telescopes were located on both sides of the centerline and yielded light curves of good to excellent signal-to-noise ratio, in spite of Pluto being located 15º deg from a 15.7 day-old-moon. Above the 0.50 stellar flux level (and somewhat below it), Pluto's atmosphere is well described by an isothermal model, having the same scale height (within the errors) at all of our stations. Thus the 0.50 flux level provides a well-defined, consistent fiducial for measuring the radius of Pluto's atmosphere. All eight occultation timings (immersion and emersion at each station) were used in a least-squares fit for the radius. Results will be compared with Pluto's atmospheric size in 2002 (Person et al., Icarus, submitted), which had expanded significantly from that reported in 1988 (Elliot et al., Nature 424, 165). Pluto's atmospheric structure as derived from these data is discussed in the abstract by Gulbis et al. and the use of these data to probe for unknown satellites and debris in the Pluto-Charon system is discussed in the abstract by Pasachoff et al. This work was partially supported by NASA Planetary Astronomy Grants NNG04GE48G, NNG04GF25G, and NNH04ZSS001N. Title: Main Objectives for this I.A.U. Special Session on Innovation in Teaching/ Learning Astronomy Authors: Pasachoff, J. M.; Ros, R. M. Bibcode: 2006IAUSS...2E...1P Altcode: In the IAU resolution on the Value of Astronomy Education, passed by the IAU's General Assembly in 2003, it was recommended: to include astronomy in school curricula, to assist schoolteachers in their training and backup, and to inform teachers about available resources. The aim of this Special Session 2 on "Innovation in Teaching/Learning Astronomy" is to contribute to the implementation of these recommendations, introducing innovative points of view regarding methods of teaching and learning. Astronomers from all countries—developed or developing—will be equally interested. New methods of dissemination of information are making big changes in the opportunity of spreading astronomical knowledge. The World Wide Web continues to expand its reach, and the Astronomy Picture of the Day reaches the homepage of millions. The new phenomenon of podcasts is spreading rapidly. Astronomy attracts many young people to education in important fields in science and technology. But in many countries, astronomy is not part of the standard curriculum, and teachers do not receive adequate education and support. Still, many scientific and educational societies and government agencies have produced materials and educational resources in astronomy for all educational levels. Technology is used in astronomy both for obtaining observations and for teaching. In any case, it is useful to take their special opportunity to learn about the situation in different countries, to exchange opinions, and to collect information in order to continue, over at least the next triennium, the activities related to promoting astronomy throughout the world. In particular, we would like to invite all participants to explain their positive original experiences so they can be adapted for other regions. Everyone is invited to exchange their initiatives and to try to involve other countries in common projects. All of us are in the same boat. http://www.communicatingastronomy.org/innovation2006/ Title: Fabry-Perot Interferometric Study of the Green Coronal line during the Total Eclipse of 2001 from Zambia Authors: Chandrasekhar, T.; Ashok, N. M.; Rao, B. G. A.; Pasachoff, J. M.; Suer, Terry-Ann Bibcode: 2006IAUJD...3E...2C Altcode: We report an interesting ground based Fabry-Perot interferometric experiment on the green coronal line at 5303 Å carried out successfully during the total eclipse of 21 June 2001 from Lusaka.Unlike as in earlier experiments a cooled CCD was used to record as many as 17 Interferograms during the 194 sec of totality. The instrumental profile is well determined by a green He-Ne laser and has a FWHM of 0.2 Å. The Fabry-Perot was off centred with respect to the solar disk to permit wider fringe coverage of the corona. Radial scans from fringe centre of only one interferogram number over 500 and each scan has several fringes. The data base spread over 17 interferograms is huge and has been only partially analysed. Line width temperatures derived from fringes analysed so far range from 2.4 to 3.7 million degrees and many profiles are asymmetric. The data base permits a search of line width oscillations at many positions in the corona with a temporal resolution of a few seconds which has implications for wave heating of the corona. Details of the experiment and emerging results will be presented. Title: Cosmic Deuterium and Social Networking Software Authors: Pasachoff, J. M.; Suer, T. -A.; Lubowich, D. A.; Glaisyer, T. Bibcode: 2006IAUSS...2E..79P Altcode: For the education of newcomers to a scientific field and for the convenience of students and workers in the field, it is helpful to have all the basic scientific papers gathered. For the study of deuterium in the Universe, in 2004-5 we set up http://www.cosmicdeuterium.info with clickable links to all the historic and basic papers in the field and to many of the current papers. Cosmic deuterium is especially important because all deuterium in the Universe was formed in the epoch of nucleosynthesis in the first 1000 seconds after the Big Bang, so study of its relative abundance (D:H~1:100,000) gives us information about those first minutes of the Universe's life. Thus the understanding of cosmic deuterium is one of the pillars of modern cosmology, joining the cosmic expansion, the 3 degree cosmic background radiation, and the ripples in that background radiation. Studies of deuterium are also important for understanding Galactic chemical evolution, astrochemistry, interstellar processes, and planetary formation. Some papers had to be scanned while others are available at the Astrophysical Data System, adswww.harvard.edu, or to publishers' Websites. By 2006, social networking software (http:tinyurl.com/ zx5hk) had advanced with popular sites like facebook.com and MySpace.com; the Astrophysical Data System had even set up MyADS. Social tagging software sites like http://del.icio.us have made it easy to share sets of links to papers already available online. We have set up http://del.icio.us/deuterium to provide links to many of the papers on cosmicdeuterium.info, furthering previous del.icio.us work on /eclipses and /plutocharon. It is easy for the site owner to add links to a del.icio.us site; it takes merely clicking on a button on the browser screen once the site is opened and the desired link is viewed in a browser. Categorizing different topics by keywords allows subsets to be easily displayed. The opportunity to expose knowledge and build an ecosystem of web pages that use the functionality of a facebook-type application to capture knowledge collaboratively is considerable. Setting up such a system would marry one of the youngest isotopes with the latest software technologies. Title: Observing Solar Eclipses in the Developing World Authors: Pasachoff, J. M. Bibcode: 2006IAUSS...5E..29P Altcode: The paths of totality of total solar eclipses cross the world, with each spot receiving such a view about every 300 years. The areas of the world from which partial eclipses are visible are much wider. For the few days prior to a total eclipse, the attention of a given country is often drawn toward the eclipse, providing a teachable moment that we can use to bring astronomy to the public's attention. Also, it is important to describe how to observe the partial phases of the eclipse safely. Further, it is important to describe to those people in the zone of totality that it is not only safe but also interesting to view totality. Those who are misled by false warnings that overstate the hazards of viewing the eclipse, or that fail to distinguish between safe and unsafe times for naked-eye viewing, may well be skeptical when other health warnings--perhaps about AIDS or malaria prevention or polio inoculations--come from the authorities, meaning that the penalties for misunderstanding the astronomical event can be severe. Through the International Astronomical Union's Working Group on Solar Eclipses and through the I.A.U.'s Program Group on Public Education at the Times of Eclipses, part of the Commission on Education and Development, we make available information to national authorities, to colleagues in the relevant countries, and to others, through our Websites at http://www.eclipses.info and http://www.totalsolareclipse.net and through personal communication. Among our successes at the 29 March 2006 total solar eclipse was the distribution through a colleague in Nigeria of 400,000 eye-protection filters. Title: Education Efforts of the International Astronomical Union Authors: Pasachoff, J. M. Bibcode: 2006IAUSS...2E...6P Altcode: I describe the education activities of the International Astronomical Union, particularly the work of Commission 46 on Education and Development. We are most interested in education in schools and for general university education rather than for pre-professional training or graduate schools. We have over 75 National Liaisons, mostly from member countries of the I.A.U. but some from nonmembers or regional groupings. We operate through 10 program groups, which are described at our Website at http://www.astronomyeducation.org. We also organize Special Sessions at General Assemblies of the International Astronomical Union, such as this Special Session 2 on Innovation in Teaching/ Learning Astronomy Methods, organized by Rosa Ros and me, and Special Session 5 on Astronomy for the Developing World, organized by John Hearnshaw. A modified version of our Special Session from the 2003 Sydney General Assembly was published as Teaching and Learning Astronomy: Effective Strategies for Educators Worldwide (Jay M. Pasachoff and John R. Percy, eds., Cambridge University Press, 2005). Michele Gerbaldi and Ed Guinan run the International Schools for Young Astronomers. Jay White heads the Teaching Astronomy for Development Program Group. John Hearnshaw runs the Program Group for the Worldwide Development of Astronomy. Charles Tolbert and John Percy run an Exchange of Astronomers program with a limited number of grants for stays of over three months between astronomers in developing countries and established astronomical institutions. Barrie Jones, as vice-president, aided by Tracey Moore, runs the Newsletter and keeps track of the National Liaisons list. I run the Program group of Public Education at the Times of Solar Eclipses. Title: In Retrospect: Out of the darkness Authors: Pasachoff, Jay M. Bibcode: 2006Natur.442..986P Altcode: No abstract at ADS Title: Narrow-band Filter Observations of the Red-Line Corona at the 29 March 2006 Eclipse Authors: Rust, David M.; Noble, M. W.; Pasachoff, J. M.; Babcock, B. A.; Bruck, M. A.; Wittenmyer, R. A. Bibcode: 2006SPD....37.0110R Altcode: 2006BAAS...38..217R We report on observations of the corona above active region NOAA 10866, which was on the solar east limb at S 06 on 29 March 2006. Filtergrams were obtained at six 0.22 Å steps across the profile of the Fe X line at 6374.5 Å during the total solar eclipse, starting at about 1052 UT. The telescope was a 35-cm Schmidt-Cassegrain Meade RCX400 with the solar image relayed to a 512 x 512-pixel Andor Ixon DV887 CCD camera via telecentric optics and two narrow-bandpass filters: (1) a 2 Å thin-film Andover Corp. blocker and (2) a 0.16 Å tunable Fabry-Perot etalon, made by the CSIRO Australian Centre for Precision Optics. The F-P etalon is a Y-cut lithium niobate wafer of 0.200-mm thickness coated with reflective and conductive thin-film layers. Application of a voltage to the etalon produces a passband shift of 0.0011 Å/volt. Calibration at the eclipse site in Kastellorizo, Greece, was maintained by reference to a WSTech thermo-electrically stabilized diode laser tuned to 6375.16 Å. The profile and Doppler shifts of the Fe X line will be discussed.The expedition was supported by NSF (ATM-0552116), the Committee for Research and Exploration of the National Geographic Society, NASA's Planetary Astronomy Division for the CCD cameras (NNG04GE48G), Sigma Xi, and the Rob Spring Fund and the Ryan Patrick Gaishin Fund at Williams College. Title: High-Resolution Observations of Limb Spicules from the Transition Region and Coronal Explorer and the Swedish Solar Telescope Authors: Westbrook, Owen; Pasachoff, J. M.; Kozarev, K. A.; Yee, J. Bibcode: 2006SPD....37.0202W Altcode: 2006BAAS...38..221W We observed spicules at the solar limb with TRACE and the Swedish Solar Telescope on La Palma for four-day intervals in 2004 and 2005 as well as simultaneous SUMER/SOHO observations in 2004. We are evaluating the apparent motion of individual spicules to infer chromospheric heat flow and mass transfer and to improve the statistics of basic spicule parameters including height, velocity, and inclination. We use the highest available cadence to measure height vs. time curves, using parabolic and linear fits to extract average maximum heights and apparent velocities of rise and descent. Our semiautomatic measurements of several dozen individual Ca II H spicules find an average height of 7610 ± 20 km based on ballistic fits and 7990 ± 80 km based on linear fits, with average velocities 8.7 ± 0.2 km/s ascending and 5.6 ± 0.1 km/s descending. Our TRACE data include observations at 1600 Å, 171 Å, and Lyman-alpha; our SST observations using Lockheed Martin's SOUP include H-alpha (four wing wavelengths to measure velocities) and Ca II H. We are investigating the relationships between spicule height and intensity to search for evidence of sheathed vs. monolithic spicule models, and analyzing ionization fadeout vs. velocity reversals for limiting spicule heights. A third yearly session of simultaneous TRACE/SST observations is scheduled.We thank S. P. Souza, B. De Pontieu, L. Golub, and J. Cirtain; earlier collaboration by D. B. Seaton, J. P. Shoer, D. L. Butts, and J. W. Gangestad; as well as the Royal Swedish Academy of Sciences. Support was provided by a NASA/Solar-Terrestrial Guest Investigator Grant for TRACE (NNG04GK44G), from Sigma Xi, and from the NASA/Massachusetts Space Grant. Title: Deuterium in the Galactic Center: Evidence for a Cosmological Origin of D and the Infall of D Enriched Gas Authors: Lubowich, D. A.; Pasachoff, J. M.; Roberts, H. R.; Millar, T. J.; Henkel, C.; Brammer, G. Bibcode: 2006AAS...20721703L Altcode: If deuterium is produced via any stellar or Galactic nucleosynthesis process, then its abundance would be a maximum value in the Galactic Center (GC). Conversely, if there are no additional Galactic source of D, then astration would reduce the initial D abundance in the GC by 107 to D/H = (2-4)×10-12. We used the Arizona Radio Observatory and detected the J = 1-0 lines of DCN and H15CN in four GC molecular clouds located from 10-100 pc from the GC (Sgr A 50 km s-1; Sgr A 20 km s-1; Sgr B2; and G0.13-0.13 in the magnetic arc). We did not detect DCN or H15CN in the circumnuclear disk located 2 pc from the GC where any D is probably destroyed by a faster rate of astration. We used a 5300 chemical reaction model to analyze DCN (used to trace D) and D fractionation, which always enhances the abundance of D molecules. We estimate the underlying D/H ratio in the GC to be D/H = (2-5)×10-6 which is in agreement with the results of Lubowich et al. (2000, Nature, 405, 1025; D/H = 1.7×10-6) from DCN observations in one GC cloud. The GC D/H ratios are less than the local ISM D/H ratio but 106 times larger than D/H ratios predicted by chemical evolution models without an additional source of D. The most likely source of this additional D is the continuous infall of low-metallicty gas enhanced with D which would negate much of the effects of astration. Thus, there are no significant Galactic sources of deuterium, D is primarily cosmological, and the Galaxy has not had quasar or AGN activity in the past 1 Gyr.

DAL was supported by an AAS Small Research Grant Title: Coronal Observations at the 29 March 2006 Total Solar Eclipse Authors: Pasachoff, J. M.; Babcock, B. A.; Souza, S. P.; Bruck, M. A.; Hess, P. W.; Kimmel, S. B.; Levitt, J. S.; Steele, A. S.; Tsykalova, A. E.; Rust, D. M.; Noble, M. W.; Wittenmyer, R.; Kern, J.; Hawkins, R. L.; Seiradakis, J. H.; Voulgaris, A.; Pistikoudis, G.; Nestoras, J.; Demianski, M. Bibcode: 2006SPD....37.0107P Altcode: 2006BAAS...38Q.216P We report on our eclipse expedition to Kastellorizo, Greece, in the Dodecanese off the Turkish coast. We observed 3 min 00 sec of totality on 29 March 2006. All our observations worked very well. One of them was high-time-resolution (10 Hz) observations in the coronal green line looking at coronal loops; another was similar observations in the coronal red line; both are to determine among theories of coronal heating and continue earlier reports of excess Fourier power in the 1 Hz range. As we knew from SOHO observations from the day before the eclipse, an active region was stationed right on the east limb and it gave us very suitable loops to study, with pointing in agreement with TRACE. A third set of observations used a very narrow-band filter (Fabry-Perot), with 1/6 angstrom resolution, to make velocity (Doppler) images of the same coronal loops. A fourth set of observations used a telescope we had built to match the size of the now defunct innermost coronagraph on the NASA/ESA SOHO, and it indeed was used to merge with SOHO EIT disk coronal images and SOHO LASCO outer coronal coronagraph images. Further, radial-filter "Newkirk camera" images captured the role of magnetic fields in shaping coronal streamers, which we also display in mergers of images with sequential exposure times.

The expedition was supported by NSF (ATM-0552116), the Committee for Research and Exploration of the National Geographic Society, NASA's Planetary Astronomy Division for the CCD cameras (NNG04GE48G), Sigma Xi, and the Rob Spring Fund and the Ryan Patrick Gaishin Fund at Williams College. Title: The Effect of the Transit of Venus on ACRIM's Total Solar Irradiance Measurements: Implications for Transit Studies of Extrasolar Planets Authors: Schneider, G.; Pasachoff, J. M.; Willson, Richard C. Bibcode: 2006ApJ...641..565S Altcode: 2005astro.ph.12251S We have used the 2004 June 8 transit of Venus (ToV) as a surrogate to test observing methods, strategies, and techniques that are being contemplated for future space missions to detect and characterize extrasolar terrestrial planets (ETPs) as they transit their host stars, notably NASA's Kepler mission, planned for 2008. As an analog to ``Kepler-like'' photometric transit observations, we obtained (spatially unresolved) radiometric observations with the ACRIM 3 instrument on ACRIMSAT at a sampling cadence of 131 s to follow the effect of the ToV on the total solar irradiance (TSI). Contemporaneous high-resolution broadband imagery with NASA's TRACE spacecraft provided, directly, measures of the stellar (solar) astrophysical noise that can intrinsically limit such transit observations. During the Venus transit, which lasted ~5.5 hr, the planet's angular diameter was approximately 1/32 the solar diameter, thus covering ~0.1% of the stellar surface. With our ACRIM 3 data, we measure temporal changes in TSI with a 1 σ per sample (unbinned) uncertainty of approximately 100 mW m-2 (0.007%). A diminution in TSI of ~1.4 W m-2 (~0.1%, closely corresponding to the geometrically occulted area of the photosphere) was measured at mid-transit compared with a mean pre-/post-transit TSI of ~1365.9 W m-2. The radiometric light curve is complex because of the parallactic motion of Venus induced by ACRIMSAT's near-polar orbit, but exhibits the characteristic signature of photospheric limb darkening. These observations serve as a surrogate for future photometric observations of ETPs, such as Kepler will deliver. Detailed analysis of the ToV, a rare event within our own solar system, with time-resolved radiometry augmented with high-resolution imagery, provides a useful analog for investigating the detectability and characterization of ETPs from observations that are anticipated in the near future. Title: Film: Big trip to the red planet Authors: Pasachoff, Jay Bibcode: 2006Natur.440...28P Altcode: No abstract at ADS Title: Charon's radius and atmospheric constraints from observations of a stellar occultation Authors: Gulbis, A. A. S.; Elliot, J. L.; Person, M. J.; Adams, E. R.; Babcock, B. A.; Emilio, M.; Gangestad, J. W.; Kern, S. D.; Kramer, E. A.; Osip, D. J.; Pasachoff, J. M.; Souza, S. P.; Tuvikene, T. Bibcode: 2006Natur.439...48G Altcode: The physical characteristics of Pluto and its moon, Charon, provide insight into the evolution of the outer Solar System. Although previous measurements have constrained the masses of these bodies, their radii and densities have remained uncertain. The observation of a stellar occultation by Charon in 1980 established a lower limit on its radius of 600km (ref. 3) (later refined to 601.5km ref. 4) and suggested a possible atmosphere. Subsequent, mutual event modelling yielded a range of 600-650km (ref. 5), corresponding to a density of 1.56 +/- 0.22gcm-3 (refs 2, 5). Here we report multiple-station observations of a stellar occultation by Charon. From these data, we find a mean radius of 606 +/- 8km, a bulk density of 1.72 +/- 0.15gcm-3, and rock-mass fraction 0.63 +/- 0.05. We do not detect a significant atmosphere and place 3σ upper limits on atmospheric number densities for candidate gases. These results seem to be consistent with collisional formation for the Pluto-Charon system in which the precursor objects may have been differentiated, and they leave open the possibility of atmospheric retention by the largest objects in the outer Solar System. Title: Book Review - Theaters of Time and Space: American Planetaria, 1930-1970 Authors: Pasachoff, Jay M. Bibcode: 2006AEdRv...4b.106P Altcode: 2005AEdRv...4b.106. No abstract at ADS Title: Book Review: THEATERS OF TIME AND SPACE: AMERICAN PLANETARIA, 1930- 1970 / Rutgers University Press, 2005 Authors: Pasachoff, Jay M. Bibcode: 2006AEdRv...4b..12P Altcode: No abstract at ADS Title: Book Review: THE SUN / Abrams, 2006 Authors: Pasachoff, Jay M. Bibcode: 2006SB&F...42..257P Altcode: No abstract at ADS Title: Charon's Radius and Atmospheric Constraints from the 2005 July 11 Stellar Occultation Authors: Gulbis, A. A. S.; Elliot, J. L.; Person, M. J.; Adams, E. R.; Kern, S. D.; Kramer, E. A.; Babcock, B. A.; Gangestad, J. W.; Pasachoff, J. M.; Souza, S. P.; Osip, D. J.; Emililo, M.; Tuvikene, T. Bibcode: 2005DPS....37.5505G Altcode: 2005BAAS...37.1571G On 2005 July 11 (UT), Charon occulted the star ``C313.2" (originally identified as a Pluto occultation star [McDonald & Elliot, Astron. J. 120, 1599, 2000]; UCAC2 26257135; R = 14.8). We arranged to observe this event using five telescopes at four sites: the 0.6-m at Pico dos Dias Obs. (Brazil), the 0.84-m at Obs. Cerro Armazones, the 2.5-m du Pont and 6.5-m Clay at Las Campanas Obs., and the 8-m Gemini South at Cerro Pacha (Chile). The observations were successful at all stations excluding Pico dos Dias, which was clouded out.

The Acquisition Camera was employed at Gemini South, while the remaining sites used POETS (Portable Occultation, Eclipse, and Transit Systems). Each system utilized a high-speed camera, a control computer, and a GPS to establish accurate timing. The cameras contain back-illuminated CCDs, with > 90% quantum efficiency, ∼ 6 electrons read noise, and 1.74 ms deadtime during frame transfer. For this event, data rates were 2 - 10 Hz and signal-to-noise ratios were 28 - 273 (normalized to 1 s). The Clay telescope light curve had high enough time resolution and signal-to-noise to detect the first diffraction fringe.

This dataset marks significant improvement over the only previously viewed stellar occultation by Charon (Walker, MNRAS 192, 47, 1980; Elliot & Young, Icarus 89, 244, 1991). By fitting the light curves with models derived from French and Gierasch (Astron. J. 81, 445, 1976), we have calculated Charon's radius and placed strong constraints on an atmosphere. These results seem consistent with a collisional origin of the Pluto-Charon system in which either of the precursor bodies may have been differentiated (McKinnon, Astrophys. J. Lett. 344, L41, 1989).

Support provided, in part, by NASA Planetary Astronomy grants NNG04GE48G, NNG04GF25G, and NNH04ZSS001N, IAP P5/36 of the Belgian Federal Office, and BIL 01/3 of the Flemish Ministry. Title: Teaching and Learning Astronomy Authors: Pasachoff, Jay; Percy, John Bibcode: 2005tla..book.....P Altcode: Preface; Part I. Astronomy in the Curriculum Around the World: Preface; 1. Why astronomy is useful and should be included in the school curriculum John R. Percy; 2. Astronomy and mathematics education Rosa M. Ros; 3. Astronomy in the curriculum around the world; 4. Engaging gifted science students through astronomy Robert Hollow; 5. Poster highlights: astronomy in the curriculum around the world; Part II. Astronomy Education Research: Preface; 6. Astronomy education research down under John M. Broadfoot and Ian S. Ginns; 7. A contemporary review of K-16 astronomy education research Janelle M. Bailey and Timothy F. Slater; 8. Implementing astronomy education research Leonarda Fucili; 9. The Astronomy Education Review: report on a new journal Sidney C. Wolff and Andrew Fraknoi; 10. Poster highlights: astronomy education research; Part III. Educating Students: Preface; 11. Textbooks for K-12 astronomy Jay M. Pasachoff; 12. Distance/internet astronomy education David H. McKinnon; 13. Educating students with robotic telescopes - open discussion; 14. Poster highlights - educating students; Part IV. Educating teachers: Preface; 15. Pre-service astronomy education of teachers Mary Kay Hemenway; 16. In-service education of teachers Michèle Gerbaldi; 17. Poster highlights: educating teachers; Part V. Astronomy and Pseudoscience: Preface; 18. Astronomy, pseudoscience and rational thinking Jayant V. Narlikar; 19. Astronomical pseudosciences in North America John R. Percy and Jay M. Pasachoff; Part VI. Astronomy and Culture: Preface; 20. Teaching astronomy in other cultures: archeoastronomy Julieta Fierro; 21. Poster highlights: astronomy and culture; Part VII. Astronomy in Developing Countries: Preface; 22. Astronomy Curriculum for developing countries Case Rijsdijk; 23. Science education resources for the developing countries James C. White II; Part VIII. Public Outreach in Astronomy: Preface; 24. What makes informal education programs successful? Nahide Craig and Isabel Hawkins; 25. The role of science centers and planetariums Nick Lomb; 26. Science education for the new century - a European perspective Claus Madsen; 27. Communicating astronomy to the public Charles Blue; 28. Poster highlights: public outreach in astronomy; Part IX. The Education Programs of the IAU: Preface; 29. A short overview of astronomical education carried out by the IAU Syuzo Isobe; Part X. Discussion; Index. Title: Astronomy education research Authors: Pasachoff, Jay M. Bibcode: 2005AmJPh..73..997P Altcode: No abstract at ADS Title: Book Review—Theaters of Time and Space: American Planetaria, 1930-1970 by Jordan D. Marché Authors: Pasachoff, Jay M. Bibcode: 2005AEdRv...4..106P Altcode: No abstract at ADS Title: Chandra Observations of Open Cluster h Per Authors: Evans, N. R.; Wolk, S.; Bizunok, N.; Spitzbart, B.; Seward, F.; Kenyon, S.; Barnes, T.; Pasachoff, J. M. Bibcode: 2005JRASC..99R.136E Altcode: We have obtained a 40 ksec ACIS observation of the open star cluster h Per in December 2004, from which we have identified more than 200 X-ray sources and found optical counterparts for many of them. We are processing the h Per data with the ANCHORS pipeline, which is being used to process Chandra observations of star forming regions in a uniform manner. This will provide fits to the instrumental low-resolution spectra for cool pre-main sequence stars in h Per including fluxes, temperatures, and absorption. Title: Chandra observations of open cluster h Per. Authors: Evans, N. R.; Wolk, S.; Bizunok, N.; Spitzbart, B.; Seward, F.; Kenyon, S.; Barnes, T.; Pasachoff, J. M. Bibcode: 2005JRASC..99..136E Altcode: 2005JRASC..99V.136E We have obtained a 40 ksec ACIS observation of the open star cluster h Per in December, 2004, from which we have identified more than 200 X-ray sources and found optical counterparts for many of them. We are processing the h Per data with the ANCHORS pipeline which is being used to process Chandra observations of star forming regions in a uniform manner. This will provide fits to the instrumental low resolution spectra for cool pre-main sequence stars in h Per including fluxes, temperatures and absorption. Title: Portable, Photon-Counting Cameras for Observing Occultations, Eclipses, and Transits Authors: Gulbis, A. A. S.; Elliot, J. L.; Person, M. J.; Babcock, B. A.; Pasachoff, J. M.; Souza, S. P. Bibcode: 2005DPS....37.1810G Altcode: 2005BAAS...37T.651G Occultations, eclipses, and transits can produce data of the highest spatial resolution for any Earth-based observing method and are thus used to determine planetary diameters and probe atmospheric profiles. Observing these events requires precise geographic and temporal information. For occultations, the size of the shadow on the Earth is a function of the occulting body's size and distance. This shadow is significantly smaller than the Earth's angular diameter for objects in which we are particularly interested (Triton, Pluto, Charon, and Kuiper belt objects). Therefore, instruments capable of traveling to a predicted shadow path increase the opportunities for observing events. Having multiple systems is also beneficial, since multiple chords must be observed to derive a body's shape.

We have constructed four portable observing systems (POETS; Portable Occultation Eclipse and Transit Systems), which can be transported as carry-on luggage and attached to portable or fixed telescopes. The cameras have E2V CCD97 sensors: a 512 x 512 array of 16 micron pixels, back illuminated, with > 90% QE. The CCDs are thermoelectrically cooled to ∼80 degrees C in air. Readout modes are 1, 3, 5 and 10 MHz, with a maximum data rate of 32 full frames per second. Binning and subframes increase the rate to a few hundred frames per second. The lowest achievable read noise in conventional mode is approximately 6 electrons. One of the two amplifiers employs electron multiplying gain, which effectively reduces the read noise to sub-electron levels and allows the cameras to be used for counting photons. Event timing is done using a state-of-the-art GPS receiver to trigger images. We present details of the systems, an analysis of the use of photon counting in the field of small body occultations, and sample occultation data.

Funding for this work is provided by NASA Planetary Astronomy grants NNG04GE48G, NNG04GF25G, and NNH04ZSS001N. Title: Deuterium Nucleosynthesis in AGN: Is D Cosmological? Authors: Lubowich, D. A.; Kuno, N.; Roberts, H.; Millar, T. J.; Henkel, C.; Pasachoff, J.; Mauersberger, R. Bibcode: 2005NuPhA.758..795L Altcode: Although deuterium is predicted to be primarily cosmological, D can also be produced by cosmic-ray or γ-ray spallation reactions - possibly between high energy jets and the surrounding gas in AGN. We used the Nobeyama mm array with a 3" resolution (200 pc) in April 2003 to search for any enhanced D from the DCN J = 2 1 line in the 45"×45" (3 kpc) circumnuclear region of the Seyfert galaxy NGC 1068. NGC 1068 is an optimal target because it has jets, starburst activity, a circumuclear molecular ring and molecular disk, dense optically thick concentrations of HCN, and a low-energy X-ray flux of 1042 erg/s (the highest X-ray flux of any galaxy in which HCN has been detected and the flux required to produce high D abundances). Although DCN is detected in most Galactic or LMC molecular clouds with optically thick HCN, we did not detect DCN with Srms = 11 mJy/beam or Trms = 35.6 mK. Thus our 3σ upper limits are S⩽ 33 mJy/beam or Tmb ⩽ 106.7 mK and DCN/HCN⩽ 0.0044. Using our 5260 reaction chemical network we estimate the underlying D/H⩽ 1.5×10-5 less than or equal to but not greater than the local Galactic ISM D/H = 1.5 × 10-5. Thus there is no significant D production in the nuclear region of NGC 1068 and NGC 1068 has probably not had a recent period of activity with a γ-ray or cosmic-ray luminosity > 1042 erg/s. If jet-cloud nucleosynthesis produces significant amounts of D, then the D is either produced inside a very small nuclear region or transported outside the nuclear region whereby subsequent infall may continuously supply galactic nuclei with D. However, any enhanced D produced via spallation reactions would have been destroyed via astration due to the large AGN star formation rate. Our results are additional evidence that D is primarily cosmological and that AGN do not produce D. Title: h Persei: Young Star Cluster in X-rays Authors: Bizunok, Natalya; Wolk, S. J.; Evans, N. R.; Spitzbart, B.; Seward, F.; Kenyon, S.; Barnes, T.; Pasachoff, J. M. Bibcode: 2005sfet.confE..48B Altcode: We have obtained a 40 ksec ACIS observation of the open star cluster h Per in December, 2004, from which we have identified more than 200 X-ray sources and found optical counterparts for many of them. We are processing the h Per data with the ANCHORS pipeline, which is being used to process Chandra observations of star forming regions in a uniform manner. This will provide fits to the instrumental low-resolution spectra for cool pre-main sequence stars in h Per including fluxes, temperatures, and absorptions. Title: Spicules, mass transfer, oscillations, and the heating of the corona Authors: Pasachoff, J. M.; Kozarev, K. A.; Butts, D. L.; Gangestad, J. W.; Seaton, D. B.; de Pontieu, B.; Golub, L.; Deluca, E.; Wilhelm, K.; Dammasch, I. Bibcode: 2005AGUSMSH13C..02P Altcode: The mass moving in chromospheric spicules is enough to replace the corona in a brief time, so understanding the dynamics of spicules is important for understanding the support and heating of the solar corona. We have undertaken a program involving simultaneous high-resolution observations in various chromospheric visible lines (H-alpha, Ca II H, and G-band, as well as Dopplergrams) using the Swedish Solar Telescope on La Palma, ultraviolet chromospheric, transition-region, and coronal lines (Fe IX/X 171 A, Lyman-alpha 1216 A, and continuum/C I/C IV 1600 A) using NASA's TRACE, and ultraviolet chromospheric and transition-region lines (Si II 1533, C IV 1548, and Ne VIII 770) using SUMER on SOHO. Our first coordinated observing run, in May 2004, yielded a variety of images that are under study, especially for the morphological statistics and dynamics of spicules. The energy transfer through the chromosphere is relevant to the overlapping investigation of coronal heating through rapid (1Hz range) oscillations of coronal loops as observed at total eclipses by Williams College expeditions. This research is supported by NASA grant number NNG04GK44G to Williams College. TRACE analysis at SAO is supported by a contract from Lockheed Martin. SOHO is a project of international cooperation between ESA and NASA. Title: The Open Cluster h Per as Seen by Chandra Authors: Bizunok, N. S.; Evans, N. R.; Wolk, S. J.; Spitzbart, B.; Seward, F. D.; Kenyon, S. J.; Barnes, T. G.; Pasachoff, J. M. Bibcode: 2005AAS...206.3604B Altcode: 2005BAAS...37R.488B In December, 2004, we observed the open star cluster h Per with Chandra ACIS for 40 ksec. We have identified more than 200 X-ray sources on the image and found optical counterparts for many of them. The ANCHORS pipeline, which we used to process the data, provides homogeneous output products for this and many other star forming regions. Among the outputs are fits to the instrumental low resolution spectra for cool pre-main sequence stars in h Per that yield flux, temperature and absorption for these sources.

Funding for this investigation has been provided by Chandra contract NAS8-39073 and NASA Grant GO5-6007A Title: The black-drop effect explained Authors: Pasachoff, Jay M.; Schneider, Glenn; Golub, Leon Bibcode: 2005tvnv.conf..242P Altcode: 2005IAUCo.196..242P The black-drop effect bedeviled attempts to determine the Astronomical Unit from the time of the transit of Venus of 1761, until dynamical determinations of the AU obviated the need for transit measurements. By studying the 1999 transit of Mercury, using observations taken from space with NASA's Transition Region and Coronal Explorer (TRACE), we have fully explained Mercury's black-drop effect, with contributions from not only the telescope's point-spread function but also the solar limb darkening. Since Mercury has no atmosphere, we have thus verified the previous understanding, often overlooked, that the black-drop effect does not necessarily correspond to the detection of an atmosphere. We continued our studies with observations of the 2004 transit of Venus with the TRACE spacecraft in orbit and with ground-based imagery from Thessaloniki, Greece. We report on preliminary reduction of those data; see http://www.transitofvenus.info for updated results. Such studies are expected to contribute to the understanding of transits of exoplanets. Though the determination of the Astronomical Unit from studies of transit of Venus has been undertaken only rarely, it was for centuries expected to be the best method. The recent 8 June 2004 transit of Venus provided an exceptionally rare opportunity to study such a transit and to determine how modern studies can explain the limitations of the historical observations. Title: Repeated universes in the AJP statistics literature Authors: Pasachoff, Jay M. Bibcode: 2005AmJPh..73..199P Altcode: No abstract at ADS Title: The Structure of Pluto's Atmosphere from the 2002 August 21 Stellar Occultation Authors: Pasachoff, Jay M.; Souza, Steven P.; Babcock, Bryce A.; Ticehurst, David R.; Elliot, J. L.; Person, M. J.; Clancy, K. B.; Roberts, Lewis C., Jr.; Hall, D. T.; Tholen, David J. Bibcode: 2005AJ....129.1718P Altcode: We have observed the 2002 August 21 occultation by Pluto of the R=15.7 mag star P131.1, using 0.5 s cadence observations in integrated white light with the Williams College frame-transfer, rapid-readout CCD at the 2.24 m University of Hawaii telescope. We detected an occultation that lasted 5 minutes, 9.1+/-0.7 s between half-light points. The ``kinks'' in the ingress and egress parts of the curve that were apparent in 1988 had become much less pronounced by the time of the two 2002 occultations that were observed, indicating a major change in the structure of Pluto's atmosphere. Analysis of our light curves shows that the pressure in Pluto's atmosphere has increased at all the altitudes that we probed. Essentially, the entire pressure scale has moved up in altitude, increasing by a factor of 2 since 1988. Spikes in our light curve reveal vertical structure in Pluto's atmosphere at unprecedentedly high resolution. We have confirmation of our spikes at lower time resolution as part of observations of the emersion made at 1.4 s and 2.4 s cadence with the 3.67 m AEOS telescope on Maui. Title: The Astronomical Unit Authors: Pasachoff, Jay M. Bibcode: 2005PhTea..43...69P Altcode: No abstract at ADS Title: The 23 November 2003 Total Solar Eclipse in Antarctica Authors: Pasachoff, Jay M. Bibcode: 2005HiA....13..931P Altcode: No abstract at ADS Title: Textbooks for K-12 Astronomy Authors: Pasachoff, Jay M. Bibcode: 2005HiA....13.1048P Altcode: No abstract at ADS Title: Astronomy Textbooks Authors: Pasachoff, Jay M.; Pasachoff, Naomi Bibcode: 2005coas.conf...73P Altcode: No abstract at ADS Title: Space Studies of the Black-Drop Effect at a Mercury Transit Authors: Schneider, Glenn; Pasachoff, Jay M.; Golub, Leon Bibcode: 2005HiA....13...70S Altcode: The accuracy with which the Astronomical Unit was known has been historically limited by the ""black drop"" effect observed during Venus's rare transits. It is often mistakenly attributed to Venus's atmosphere. We report on observations taken outside the Earth's atmosphere of the 1999 and 2003 transits of Mercury with the NASA solar satellite known as the Transition Region and Coronal Explorer (TRACE). Though there was no contribution from the atmosphere of Mercury or the Earth nevertheless a faint black-drop effect was detected. We discuss and model the images showing the sources of the black-drop effect. The techniques we discuss are applicable to ground-based and space-based observations of the 8 June 2004 and 5-6 June 2012 transits of Venus. Title: The composition at the outer edge of the Galaxy Authors: Lubowich, D. A.; Brammer, G.; Roberts, H.; Millar, T. J.; Pasachoff, J. M.; Henkel, C.; Ruffle, P. Bibcode: 2005HiA....13..586L Altcode: We present observations of a 10-Gyr-old molecular cloud at the outer edge of the Galactic disk (28 kpc). We detected CO 13CO 18CO CS CN SO HCN HNC HCO+ CH3OH HCS+ H2CO C2H C3H2 and NH3 but we did not detect CO+ N2H+ DCN HC3N 34CS SiO SiS 17CO or SO2. The NH3 H2CO and CS abundances indicate that T = 20 K and n = 5x10(3) cm(-3). The N-containing molecules were weak and we did not detect the usually strong N2H+ or HC3N lines. Using our 5300 chemical reaction model we calculate that the N is depleted in this cloud by about 3x and this cloud has a lower metallicity (similar to dwarf irregular galaxies or damped Lyman alpha systems) and a lower cosmic-ray ionization rate possibly resulting from the infall of halo gas enriched in O C and S from a burst of massive star formation in the Galactic halo shortly after the Milky Way was formed. This activity would have produced both O and S which are produced by massive stars; C which is produced by massive and intermediate mass stars; but less N abundance because the secondary element N is produced primarily from low mass stars. Title: What to teach? What is learned? Astronomy as an amalgam of new and old Authors: Pasachoff, J. M. Bibcode: 2005EAS....16..137P Altcode: The tension between contemporary astronomy and traditional topics as subjects for general astronomy courses or fundamental science courses is healthy, but one must worry if either type crowds out the other. Too often only topics understood hundreds of thousands of years ago (such as gravity, tides, phases, and seasons) take up such a large fraction of the astronomy content that few or none of the fascinating and important discoveries of recent centuries not to mention recent years or months are included. I discuss aspects of this problem. Including topics of contemporary interest often motivates students to concentrate their attention and study time on the entire range of topics in the course. Practitioners of the new field of Astronomy Education Research seem often to attack their subject in perpendicular fashion to the methods of practitioners of communicating astronomy to the public. I also discuss some of the content of our International Astronomical Union's Commission on Education and Development's special session from 2003 on Effective Teaching and Learning of Astronomy, and of the forthcoming volume of the same title to be published by Cambridge University Press. I further discuss the role of inspiring events, such as George Ellery Hale's inspiration from the 1882 transit of Venus and the potential from the widespread observation of the 2004 transit of Venus and of solar eclipses. Title: Book Review: STELLAR ALCHEMY: THE CELESTIAL ORIGIN OF ATOMS / Cambridge University Press, 2003 Authors: Pasachoff, Jay M. Bibcode: 2004PhT....57l..69P Altcode: No abstract at ADS Title: Deuterium Nucleosynthesis in AGN: Is D Cosmological? Authors: Lubowich, D. A.; Kuno, N.; Roberts, H.; Millar, T. J.; Henkel, C.; Pasachoff, J. M.; Mauersberger, R. Bibcode: 2004AAS...20511807L Altcode: 2004BAAS...36Q1546L Although deuterium is predicted to be primarily cosmological, D can also be produced by cosmic-ray or γ -ray spallation reactions - possibly between high energy jets and the surrounding gas in AGN. We used the Nobeyama mm array with a 3" resolution (220 pc) in April 2003 to search for any enhanced D from the DCN J = 2-1 line in the Seyfert galaxy NGC 1068. NGC 1068 is an optimal target because it has jets, starburst activity, a circumuclear molecular ring and disk, dense optically thick concentrations of HCN, and a low-energy X-ray flux of 1042 erg/s (the highest X-ray flux of any galaxy in which HCN has been detected and the flux required to produce high D abundances). We did not detect DCN (which is detected in all other molecular clouds with optically thick HCN in the Galaxy or LMC) and we obtained an upper limit of S≤15 mJy/beam = 48.5 mK in the circumnuclear region and a DCN/HCN ratio of 0.0046. Using our 5300 reaction chemical network we estimate D/H leq1.5x10-5 as compared to the local Galactic ISM D/H = 1.4x10-5.

Thus there is no significant D production in the nuclear region of NGC 1068 and NGC 1068 has probably not had a recent period of activity with a γ -ray or cosmic-ray luminosity > 1042 erg/s. If jet-cloud nucleosynthesis produces significant amounts of D, then the D is produced outside of the nuclear region where the subsequent infall may be one way to continuously supply galactic nuclei with D. However, any enhanced D produced via spallation reactions would have been destroyed via astration due to the faster star formation rate. Our results are additional evidence that D is primarily cosmological and that AGN do not produce D. Title: The Effect of the Transit of Venus on ACRIM's Total Solar Irradiance Measurements: Implications for Transit Studies of Extrasolar Planets Authors: Pasachoff, J. M.; Schneider, G.; Willson, R. C. Bibcode: 2004AAS...20513511P Altcode: 2004BAAS...36.1566P We used 131-s-cadence observations made with ACRIM3 on ACRIMsat on 8 June 2004 to follow the effect of the transit of Venus, which lasted about 6 hours, on the total solar irradiance (TSI). Venus's angular diameter, in transit, is approximately 1/30 the solar diameter, so it covered approximately 0.1% of the sun's surface. With our ACRIM3 data, we measure temporal changes in TSI with a one-sigma per sample (unbinned) certainty of approximately 100 milliwatts per square meter (0.007%). We found a diminution in TSI of approximately 1.4 watts per square meter (approximately 0.1%, closely corresponding to the geometrically occulted area of the photosphere) at mid-transit compared with a mean pre/post transit TSI of 1365.9 watts per square meter. The measured light curve is complex because of the parallactic motion of Venus induced by the satellite's polar orbit, but exhibits the characteristic signature of photospheric limb-darkening when orbit-driven variations are accounted for. Analysis of the limb darkening can reveal temporal structure with height in the photosphere and asymmetries can, in principle, be attributable to planetary atmospheres. Similar observations will increasingly be detected from exoplanet transits, so detailed analysis of the transit within our solar system will provide a useful analogue for interpreting the many more such transits expected to be discovered within the next decade.

JMP's and GS's transit of Venus observations were supported by a grant from the Committee for Research and Exploration of the National Geographic Society. NASA provides support for RCW at Columbia University under contract NNG04HZ42C. Title: Stellar Alchemy: The Celestial Origin of Atoms Authors: Cassé, Michel; Lyle, Stephen; Pasachoff, Jay M. Bibcode: 2004PhT....57l..69C Altcode: No abstract at ADS Title: Satellite and Ground-Based Observations of the Transit of Venus Authors: Pasachoff, J. M.; Schneider, G.; Babcock, B. A.; Butts, D. L.; Gangestad, J. W.; Westbrook, O. W.; Cordova, A. R.; Gaydosh, K.; Seiradakis, J. H. Bibcode: 2004DPS....36.3901P Altcode: 2004BAAS...36.1161P We report on a coordinated program of CCD observations of the transit of Venus of 8 June 2004 made with NASA's Transition Region and Coronal Explorer (TRACE) spacecraft and with ground-based observations from Greece (including the first two contacts) and the U.S. (the last two contacts). We observed in white light, with special attention to imaging Venus's atmosphere at ingress and egress and to the presence and formation of the black-drop effect at second and third contacts. We analyze the data in terms of the telescope's point-spread function, the solar limb darkening (which we previously showed to have a role in the black-drop effect for a transit of Mercury), and seeing effects from the terrestrial atmosphere. Our TRACE data have a 7-s cadence at uncompressed data transmission and higher for compressed data, both over the 20-min ingress and egress phases.

Our expedition was supported by a grant from the Committee for Research and Exploration of the National Geographic Society. We thank Sigma Xi for additional student support. Title: Box: Transit Research in the 21st Century Authors: Pasachoff, Jay M. Bibcode: 2004S&T...108e..82P Altcode: No abstract at ADS Title: Fascinating Pluto Authors: Pasachoff, Jay M.; Elliot, James L. Bibcode: 2004PhT....57i..18P Altcode: No abstract at ADS Title: TRACE observations of the 15 November 1999 transit of Mercury and the Black Drop effect: considerations for the 2004 transit of Venus Authors: Schneider, Glenn; Pasachoff, Jay M.; Golub, Leon Bibcode: 2004Icar..168..249S Altcode: Historically, the visual manifestation of the "Black Drop effect," the appearance of a band linking the solar limb to the disk of a transiting planet near the point of internal tangency, had limited the accuracy of the determination of the Astronomical Unit and the scale of the Solar System in the 18th and 19th centuries. This problem was misunderstood in the case of Venus during its rare transits due to the presence of its atmosphere. We report on observations of the 15 November 1999 transit of Mercury obtained, without the degrading effects of the Earth's atmosphere, with the Transition Region and Coronal Explorer spacecraft. In spite of the telescope's location beyond the Earth's atmosphere, and the absence of a significant mercurian atmosphere, a faint Black Drop effect was detected. After calibration and removal of, or compensation for, both internal and external systematic effects, the only radially directed brightness anisotropies found resulted from the convolution of the instrumental point-spread function with the solar limb-darkened, back-lit, illumination function. We discuss these effects in light of earlier ground-based observations of transits of Mercury and of Venus (also including the effects of atmospheric "seeing") to explain the historical basis for the Black Drop effect. The methodologies we outline here for improving upon transit imagery are applicable to ground-based (adaptive optics augmented) and space-based observations of the 8 June 2004 and 5-6 June 2012 transits of Venus, providing a path to achieving high-precision measurements at and near the instants of internal limb tangencies. Title: The Chemical Composition of a Molecular Cloud at the Outer Edge of the Galaxy Authors: Lubowich, D. A.; Brammer, G.; Roberts, H.; Millar, T. J.; Henkel, C.; Pasachoff, J. M. Bibcode: 2004oee..sympE..37L Altcode: Centimeter and millimeter-wave observations of a molecular cloud at the extreme outer edge of the Galactic disk (kinematic ga lactocentric distance: ∼28 kpc) are presented. We detected CO, 13CO, 18CO, CS, CN, SO, HCN, HNC, C2H, HCO+, H13CO+, HCS+, NH3, H2CO, C3H2 and CH3OH, while 17CO, 34CS, SiO, SiS, N2H+, D CN, DNC, DCO+, SO2 and HC3N remained undetected. From the NH3 and H2CO data, a kinetic temperature of Tkin ∼20 K and a density of n(H2) ∼5×103 cm-3 are derived. Nitrogen bearing molecules show , when detected, only weak lines. Commonly strong line emitters such as N2H+ and HC3N were not seen. Using a numeri cal network including 5300 chemical reactions we determined that N is depleted by approximately 24 times, and the metallicit y is reduced by a factor of five (similar to dwarf irregular galaxies or damped Lyman alpha systems) relative to the solar ne ighborhood. These unusual abundances are probably the result of the infall of halo gas enriched in O, C, and S from a burst o f massive star formation in the Galactic halo shortly after the Milky Way was formed. This activity would have produced both O and S, which are produced by massive stars; C, which is produced by massive and intermediate mass stars; but less N abundan ce because the secondary element N is produced primarily from low mass stars. Thus the edge cloud probably results from infal ling halo gas from the early Galaxy that was not significantly processed during the last 10 Gyr and provides a new way to und erstand the origin of the Galactic disk. Our observations of the early Galactic disk abundances will constrain models of nu cleosynthesis, Galactic chemical evolution, and astrochemistry. Title: The Bohr Staircase Authors: Pasachoff, Jay M. Bibcode: 2004PhTea..42...38P Altcode: The attempt to bring students to critical thinking about topics in contemporary astronomy is a goal shared by many teachers. Since the rise of astrophysics in the early 20th century, spectroscopy has been the defining technique. Various techniques have been tried to give students a concrete understanding of emission lines and absorption lines in the hydrogen spectrum.1 Spectroscopy of hydrogen plays an important part of most textbooks in elementary astronomy.2 After years of jumping off lecture-room steps and trying (but never succeeding) in hovering between stair levels, I still find too many students drawing equally spaced hydrogen energy levels on exams. I thus arranged for carpenters to build a five-step staircase with the spacing matching that of the actual hydrogen energy levels. I can now use the staircase to demonstrate the Bohr atom3 in a memorable manner. ``Bohr staircase'' is therefore a suitable name for it. If a teacher wants to stress the visible spectrum rather than the energy levels, ``Balmer staircase'' is an alternate name. Title: Explanation of the Black-Drop Effect at Transits of Mercury and the Forthcoming Transit of Venus Authors: Pasachoff, J. M.; Schneider, G.; Golub, L. Bibcode: 2003AAS...203.0104P Altcode: 2003BAAS...35.1202P We used the observations of the transits of Mercury of 1999 and 2003 taken with NASA's Transition Region and Coronal Explorer (TRACE) solar spacecraft. For the 1999 Mercury transit, for which data were acquired with the highest digital fidelity available for TRACE, we detected a black-drop effect, in spite of the facts that we were observing from outside the Earth's atmosphere and that Mercury has no significant atmosphere. We were able to show that the Mercury black-drop effect comes from a convolution of the instrument's point-spread function and the solar limb darkening. By implication, we should be able to explain Venus's black-drop effect in a similar way. It has long been known that Venus's black-drop effect is too large to come from Venus's atmosphere. Title: Rowling Gets It Wrong Authors: Pasachoff, Jay M. Bibcode: 2003S&T...106f..12P Altcode: No abstract at ADS Title: The Value of the Great Observatories' Educational Programs Authors: Pasachoff, J. M. Bibcode: 2003AAS...20310701P Altcode: 2003BAAS...35.1376P What should non-major and school-level students learn about astronomy? The current trend in Physics Education Research, now being translated to Astronomy Education Research, is that "less is more." As a result, there may be little time for modern topics or there may be a judgment that these topics are too abstract to teach.

Yet NASA's Great Observatories and other missions have vital and interesting Education and Public Outreach programs. Through the Web, through distribution of CD-ROM's and other media, and through a variety of materials and activities these programs provide not only reports on current research but also substantial background information.

To explore the contemporary question of what we professional astronomers think we should be communicating to students at all levels, I have invited both scientists and public information officers of the Hubble Space Telescope, the Chandra X-ray Observatory, and the Space Infrared Telescope Facility to discuss the importance and the methodologies of their Education and Public Outreach programs. Title: Book review: The enigma of sunspots: a story of discovery and scientific revolution / Floris Books, Edinburgh, 192 pp., 2002, ISBN 0-86315-370-4. Authors: Pasachoff, Jay M. Bibcode: 2003JHA....34..458P Altcode: 2003JHA....34..458B No abstract at ADS Title: Feeling a Bit Green? Authors: Pasachoff, Jay M. Bibcode: 2003S&T...106d..16P Altcode: No abstract at ADS Title: Space Studies of the Black-Drop Effect at a Mercury Transit Authors: Schneider, G.; Pasachoff, J. M.; Golub, L. Bibcode: 2003astro.ph.10379S Altcode: Transits of Mercury and Venus across the face of the Sun are rare. The 20th century had 15 transits of Mercury and the 21st century will have 14, the two most recent occuring on 15 November 1999 and 7 May 2003. We report on our observations and analyses of a black-drop effect at the 1999 and 2003 transits of Mercury seen in high spatial resolution optical imaging with NASA's Transition Region and Coronal Explorer (TRACE) spacecraft. We have separated the primary contributors to this effect, solar limb darkening and broadening due to the instrumental point spread function, for the 1999 event. The observations are important for understanding historical observations of transits of Venus, which in the 18th and 19th centuries were basic for the determination of the scale of the solar system. Our observations are in preparation for the 8 June 2004 transit of Venus, the first to occur since 1882. Only five transits of Venus have ever been seen -- in 1639, 1761, 1769, 1874, and 1882. These events occur in pairs, whose members are separated by 8 years, with an interval between pairs of 105 or 122 years. Nobody alive has ever seen a transit of Venus. Title: The Complete Idiot's Guide to The Sun Authors: Pasachoff, Jay M. Bibcode: 2003cigs.book.....P Altcode: No abstract at ADS Title: The recent expansion of Pluto's atmosphere Authors: Elliot, J. L.; Ates, A.; Babcock, B. A.; Bosh, A. S.; Buie, M. W.; Clancy, K. B.; Dunham, E. W.; Eikenberry, S. S.; Hall, D. T.; Kern, S. D.; Leggett, S. K.; Levine, S. E.; Moon, D. -S.; Olkin, C. B.; Osip, D. J.; Pasachoff, J. M.; Penprase, B. E.; Person, M. J.; Qu, S.; Rayner, J. T.; Roberts, L. C.; Salyk, C. V.; Souza, S. P.; Stone, R. C.; Taylor, B. W.; Tholen, D. J.; Thomas-Osip, J. E.; Ticehurst, D. R.; Wasserman, L. H. Bibcode: 2003Natur.424..165E Altcode: Stellar occultations-the passing of a relatively nearby body in front of a background star-can be used to probe the atmosphere of the closer body with a spatial resolution of a few kilometres (ref. 1). Such observations can yield the scale height, temperature profile, and other information about the structure of the occulting atmosphere. Occultation data acquired for Pluto's atmosphere in 1988 revealed a nearly isothermal atmosphere above a radius of ~1,215km. Below this level, the data could be interpreted as indicating either an extinction layer or the onset of a large thermal gradient, calling into question the fundamental structure of this atmosphere. Another question is to what extent Pluto's atmosphere might be collapsing as it recedes from the Sun (passing perihelion in 1989 in its 248-year orbital period), owing to the extreme sensitivity of the equilibrium surface pressure to the surface temperature. Here we report observations at a variety of visible and infrared wavelengths of an occultation of a star by Pluto in August 2002. These data reveal evidence for extinction in Pluto's atmosphere and show that it has indeed changed, having expanded rather than collapsed, since 1988. Title: Pluto's Atmospheric Figure from the P131.1 Stellar Occultation Authors: Person, M. J.; Elliot, J. L.; Clancy, K. B.; Kern, S. D.; Salyk, C. V.; Tholen, D. J.; Pasachoff, J. M.; Babcock, B. A.; Souza, S. P.; Ticehurst, D. R.; Hall, D.; Roberts, L. C., Jr.; Bosh, A. S.; Buie, M. W.; Dunham, E. W.; Olkin, C. B.; Taylor, B.; Levine, S. E.; Eikenberry, S. S.; Moon, D. -S.; Osip, D. J. Bibcode: 2003DPS....35.2301P Altcode: 2003BAAS...35..957P The stellar occultation by Pluto of the 15th magnitude star designated P131.1 (McDonald and Elliot, AJ, 119, 1999) on 2002 August 21 (UT) provided the first significant chance to compare Pluto's atmospheric structure to that determined from the 1988 occultation of P8 (Millis, et al., Icarus, 105, 282). The P131.1 occultation was observed from several stations in Hawaii and the western United States (Elliot et al., Nature, in press, 2003). Numerous occultation chords were obtained enabling us to examine Pluto's atmospheric figure. The light curves from the observations were analyzed together in the occultation coordinate system of Elliot et al., (AJ, 106, 2544). The Mauna Kea and Lick datasets straddle the center of Pluto's figure, providing strong constraints on model fits to cross sections of the atmospheric shape.

In 1988, Millis (et al., Icarus, 105, 282) did not report any deviation from sphericity in Pluto's atmospheric figure. From the 2002 data, Pluto;s isobars at the radii probed by the occultation ( 1250 km) appear to be distorted from a circular cross-section. Least-squares fits to this cross-section by elliptical models reveal ellipticities in the range 0.05-0.08 although the shape may be more complex than ellipsoidal. The orientation of the distortion appears uncorrelated with Pluto;s rotational axis. Taken at face value, this ellipticity could imply wind speeds of up to twice the sonic speed ( 200 m/s), which would be difficult to explain. Similar distortions have been reported for Triton's atmosphere (Elliot, J. L., et al., Icarus 148, 347). This work has been supported in part by Research Corporation, the Air Force Research Laboratory, NSF, and NASA. Title: Book Review: Setting sail for the universe: astronomers and their discoveries / Rutgers University Press, Piscataway, NJ, 192 pp., 2002, ISBN 0-8135-3088-1. Authors: Pasachoff, Jay M. Bibcode: 2003JHA....34..238P Altcode: 2003JHA....34..238F No abstract at ADS Title: Working Group on Solar Eclipses (Groupe de Travail pour les Eclipses Solaires) Authors: Pasachoff, Jay M. Bibcode: 2003IAUTA..25...75P Altcode: 2003IAUTr..25A..75P No abstract at ADS Title: What Should Students Learn? Stellar Magnitudes? Authors: Pasachoff, Jay M. Bibcode: 2003AEdRv...2b.162P Altcode: 2003AEdRv...2..162P No abstract at ADS Title: Textbooks for K-12 Astronomy Authors: Pasachoff, Jay M. Bibcode: 2003IAUSS...4E..63P Altcode: Astronomy is a part of the science curriculum of the early years of K-12 education in the United States but after a grades 7-9 (ages 13-15 approximately) sequence that is usually Life Sciences/Earth Sciences/Physical Sciences no science is commonly required. Several national projects have addressed the astronomy content of K-12 education. I will discuss and show examples of the astronomy content in American school textbooks and various of the proposals that have been advanced for reform. Title: The 23 November 2003 Total Solar Eclipse in Antarctica Authors: Pasachoff, Jay M. Bibcode: 2003IAUSS...2E...9P Altcode: The total solar eclipse of 23 November 2003 will be visible only from Antarctica. The path of totality extends from Mirny at 93°E to the Maitri Novolazarevskaya 12°E. Totality lasts from 1 minute 54 seconds at Mirny with the Sun at an altitude of 14° to a maximum of 1 minute 57 seconds at greatest eclipse halfway in toward Vostok with the Sun at an altitude of 18° to 1 minute 20 s with the Sun 2° above the horizon where the path leaves the coast near Maitri. The rest of Antarctica will have only a partial eclipse with the Sun's diameter 77% covered at McMurdo and 65° covered at the tip near South America. An icebreaker passenger ship is planning a 28-day voyage and airplanes are being arranged for observation. Scientific observations will include electronic imaging of the corona to compare with simultaneous space observations of the Sun. Links to maps and other items of coordination can be found at www.eclipses.info and www.totalsolareclipse.net the sites of the IAU Program Group on Public Education at the Time of Eclipses and of the IAU Working Group on Eclipses respectively. The NASA site with maps and other information is at sunearth.gsfc.nasa.gov/eclipse/TSE2003/TSE2003.html Title: Space Studies of the Black Drop Effect at a Mercury Transit Authors: Pasachoff, Jay M.; Schneider, Glenn; Golub, Leon Bibcode: 2003IAUJD...2E...5P Altcode: The accuracy with which the Astronomical Unit was known has been historically limited by the ""black drop"" effect observed during Venus's rare transits. It is often mistakenly attributed to Venus's atmosphere. We report on observations taken outside the Earth's atmosphere of the 1999 and 2003 transits of Mercury with the NASA solar satellite known as the Transition Region and Coronal Explorer (TRACE). Though there was no contribution from the atmosphere of Mercury or the Earth nevertheless a faint black-drop effect was detected. We discuss and model the images showing the sources of the black-drop effect. The techniques we discuss are applicable to ground-based and space-based observations of the 8 June 2004 and 5-6 June 2012 transits of Venus. Title: The Composition at the Outer Edge of the Galaxy Authors: Lubowich, Donald; Brammer, Gabriel; Roberts, Helen; Millar, Tom; Henkel, Christian; Pasachoff, Jay; Ruffle, Paul Bibcode: 2003IAUJD..15E..51L Altcode: We present observations of a 10-Gyr-old molecular cloud at the outer edge of the Galactic disk (28 kpc). We detected CO 13CO 18CO CS CN SO HCN HNC HCO+ CH3OH HCS+ H2CO C2H C3H2 and NH3 but we did not detect CO+ N2H+ DCN HC3N 34CS SiO SiS 17CO or SO2. The NH3 H2CO and CS abundances indicate that T = 20 K and n = 5x10(3) cm(-3). The N-containing molecules were weak and we did not detect the usually strong N2H+ or HC3N lines. Using our 5300 chemical reaction model we calculate that the N is depleted in this cloud by about 3x and this cloud has a lower metallicity (similar to dwarf irregular galaxies or damped Lyman alpha systems) and a lower cosmic-ray ionization rate possibly resulting from the infall of halo gas enriched in O C and S from a burst of massive star formation in the Galactic halo shortly after the Milky Way was formed. This activity would have produced both O and S which are produced by massive stars; C which is produced by massive and intermediate mass stars; but less N abundance because the secondary element N is produced primarily from low mass stars. Title: The forgotten star atlas : John Bevis's Uranographia Britannica. Authors: Kilburn, K. J.; Pasachoff, J. M.; Gingerich, O. Bibcode: 2003JHA....34..125K Altcode: No abstract at ADS Title: Back to School Authors: Pasachoff, Jay M. Bibcode: 2003S&T...105a..12P Altcode: No abstract at ADS Title: Committee of Ten and Astronomy Authors: Pasachoff, Jay M. Bibcode: 2002PhTea..40..517P Altcode: No abstract at ADS Title: Pluto Occultation of P131.1 in 2002 August: Overview of Observations and Infrared Results Authors: Elliot, J. L.; Clancy, K. B.; Rayner, J. T.; Tholen, D. J.; Person, M. J.; Osip, D. J.; Pasachoff, J. M.; Babcock, B. A.; Ticehurst, D. R.; Hall, D.; Roberts, L. C., Jr.; Bosh, A. S.; Eikenberry, S. S.; Moon, D. -S.; Buie, M. W.; Dunham, E. W.; Olkin, C. B.; Taylor, B.; Kern, S. D.; Qu, S.; Salyk, C. V.; Leggett, S. K.; Levine, S. E.; Stone, R. C. Bibcode: 2002AAS...201.6101E Altcode: 2002BAAS...34.1211E Pluto's occultation of the star P131.1 (R = 15.7, K = 13.3; see McDonald & Elliot, 2002, AJ 120, 1599) on 2002 August 21 was successfully observed with nine telescopes: the IRTF, UH 2.2m, UH 0.6m, UKIRT, and CFHT on Mauna Kea; the AEOS telescope on Haleakala, the Shane telescope at Lick Observatory, the Perkins telescope at Lowell Observatory, and the Hale telescope at Palomar Observatory. Occultation light curves were recorded at a variety of time resolutions and wavelengths in order to facilitate several investigations of Pluto's atmosphere (see Pasachoff et al., Person et al., Clancy et al., this meeting). We confirm the main conclusion from the P126 occultation (Buie et al., BAAS 34, 877) that the structure of Pluto's atmosphere has changed substantially since it was last observed in 1988 (Elliot & Young et al., AJ 103, 991). The multi-wavelength nature of our P131.1 data set allows us to elucidate these changes. The IRTF data were recorded with SpeX (Rayner et al. 2003 PASP, in preparation) and span the 0.8 to 2.5 micron region of the spectrum. Although recorded at lower time resolution (about 4 spectra per minute) than the other data sets, comparison of the SpeX light curves at different wavelengths (and comparing them with the visible light curves) is being used to establish the role of extinction by possible hazes and clouds in Pluto's atmosphere throughout the occultation. These IR data and the UKIRT light curve with the H filter will be used to correct the visible-light curves for extinction effects (if present) prior to inverting the light curves to obtain temperature, pressure, and number-density profiles of Pluto's atmosphere. This work has been supported in part by Research Corporation, NASA, and NSF. Title: High-Time-Resolution White-Light Observations of Pluto's Occultation of P131.1 in 2002 August Authors: Pasachoff, J. M.; Elliot, J. L.; Babcock, B. A.; Ticehurst, D. R.; Tholen, D. J.; Person, M. J. Bibcode: 2002AAS...201.6102P Altcode: 2002BAAS...34Q1211P We observed a 304-s FWHM occultation of the 15th magnitude (R) star P131.1 by Pluto on 2002 August 21 (UT) with the University of Hawaii's 2.2-m telescope on Mauna Kea. We used a Princeton Instruments/Roper front-illuminated CCD in frame-transfer mode at a 0.5 s cadence, with no filter in order to maximize the signal-to-noise ratio. Seeing was 0.4 arcsec; Charon was distinctly visible throughout alongside Pluto. We obtained images with our 0.2 arcsec pixels for astrometric purposes at various times before and after the occultation on the night of the occultation and on the preceding night. In our occultation run of 20 min, we binned 5x5 and obtained 2400 images. A nearby double star allowed monitoring of the sky transparency. The light curve shows the occultation at a higher cadence than the visible and infrared light curves obtained at adjacent telescopes. We discuss the fully reduced and calibrated light curve, the implications for models of haze in Pluto's atmosphere from the lack of complete occultation even at full depth, and the interpretation of positive spikes in the light curve during the emersion as waves or turbulence in Pluto's atmosphere. We compare these white-light observations with the infrared results obtained simultaneously and discuss implications for Pluto's current atmospheric structure. This work was supported by Research Corporation, by NASA through its New Horizons project, and by Williams College. The CCD is part of NSF-supported solar-eclipse research. We thank A. Pickles for assistance with scientific arrangements at Mauna Kea and S. P. Souza for help with preliminary data reduction and other aspects of the expedition. Title: Examination of Pluto's Atmospheric Figure with the P131.1 Stellar Occultation Authors: Person, M. J.; Elliot, J. L.; Clancy, K. B.; Tholen, D. J.; Rayner, J. T.; Pasachoff, J. M.; Babcock, B. A.; Ticehurst, D. R.; Hall, D.; Roberts, L. C., Jr.; Bosh, A. S.; Eikenberry, S. S.; Moon, D. S.; Buie, M. W.; Dunham, E. W.; Olkin, C. B.; Taylor, B.; Kern, S. D.; Osip, D. J.; Qu, S.; Salyk, C. V.; Leggett, S. K.; Levine, S. E.; Stone, R. C. Bibcode: 2002AAS...201.6103P Altcode: 2002BAAS...34R1211P From the 1988 stellar occultation by Pluto, Millis (et al., Icarus, 105, 282) did not report any deviation from sphericity in Pluto's atmospheric figure. However, stellar occultation measurements of Triton throughout the late 1990's revealed a significant deviation from a spherical figure in Triton's atmospheric shape (Elliot et al., Icarus, 148, 347, and Person 2001, S.M. Thesis, Dept. of Earth Atmos. and Plan. Sci., Mass. Inst. Of Tech., Cambridge MA). This deviation is unexpected since Triton's rotation period is slow (5.88 days), but the resulting non-spherical shape could be due to high winds. The Triton results have prompted us to examine Pluto's atmospheric figure with more recent data. The stellar occultation by Pluto of the 15th magnitude star designated P131.1 (McDonald and Elliot, AJ, 119, 1999) on 2002 August 21 (UT) provided the first significant chance since the Triton results to measure such non-sphericity in Pluto's atmosphere. The occultation was observed from numerous stations in Hawaii and the western United States (see Elliot et al., Pasachoff et al., Clancy et al., this conference). We present the results of our analysis of these datasets in searching for non-spherical deviations in Pluto's atmospheric figure. The light curves from the observations were analyzed together in the occultation coordinate system of Elliot et al., (AJ, 106, 2544). The datasets from the various Mauna Kea telescopes are redundant with each other in figure space, but provide valuable cross checks among their timing systems. The Mauna Kea and Lick datasets straddle the center of Pluto's figure, providing strong constraints on model fits to cross sections of the atmospheric shape. As a second measure of possible non-sphericity, the individual light curves can be individually fit with atmospheric models in the manner of Elliot and Young (AJ, 103, 991), to search for asymmetry indicative of a non-circular atmospheric cross section around the limb of the planet. This work has been supported in part by Research Corporation, NASA, and NSF. Title: Comets, meteors, and eclipses: Art and science in early Renaissance Italy Authors: Olson, R. J. M.; Pasachoff, J. M. Bibcode: 2002M&PS...37.1563O Altcode: We discuss eight trecento (fourteenth century) paintings containing depictions of astronomical events to reveal the revolutionary advances made in both astronomy and naturalistic painting in early Renaissance Italy, noting that an artistic interest in naturalism predisposed these pioneering painters to make their scientific observations. In turn, the convincing representations of their observations of astronomical phenomena in works of art rendered their paintings more believable, convincing. Padua was already a renowned center for mathematics and nascent astronomy (which was separating from astrology) when Enrico Scrovegni commissioned the famous Florentine artist Giotto di Bondone to decorate his lavish family chapel (circa 1301-1303). Giotto painted a flaming comet in lieu of the traditional Star of Bethlehem in the Adoration of the Magi scene. Moreover, he painted a historical apparition that he recently had observed with a great accuracy even by modern standards. Halley's Comet of 1301 (Olson, 1979). While we do not know the identity of the artist's theological advisor, we discuss the possibility that Pietro d'Abano, the Paduan medical doctor and "astronomer" who wrote on comets, might have been influential. We also compare Giotto's blazing comet with two others painted by the artist's shop in San Francesco at Assisi (before 1316) and account for the differences. In addition, we discuss Giotto's pupil, Taddeo Gaddi, reputed to have been partially blinded by a solar eclipse, whose calamity may find expression in his frescoes in Santa Croce, Florence (1328-30; 1338?). Giotto also influenced the Sienese painter Pietro Lorenzetti, two of whose Passion cycle frescoes at Assisi (1316-20) contain dazzling meteor showers that reveal the artist's observed astronomical phenomena, such as the "radiant" effect of meteor showers, first recorded by Alexander von Humboldt in 1799 and only accepted in the nineteenth century. Lorenzetti also painted sporadic, independent meteors, which do not emanate from the radiant. It is also significant that these artists observed differences between comets and meteors, facts that were not absolutely established until the eighteenth century. In addition we demonstrate that artistic and scientific visual acuity were part of the burgeoning empiricism of the fourteenth century, which eventually yielded modern observational astronomy. Title: Haystack radio telescope Authors: Pasachoff, Jay M. Bibcode: 2002AmJPh..70..983P Altcode: No abstract at ADS Title: Changes in Pluto's Atmosphere Revealed by the P126A Occultation Authors: Buie, M. W.; Elliot, J. L.; Kidger, M. R.; Bosh, A. S.; Saá, O.; Van Malderen, R.; Uytterhoeven, K.; Davignon, G.; Dunham, E. W.; Olkin, C. B.; Taylor, B. W.; Wasserman, L. H.; Clancy, K.; Person, M. J.; Levine, S. E.; Stone, R. C.; Peréz-González, P. G.; Pasachoff, J. M.; Souza, S. P.; Ticehurst, D. R.; Fitzsimmons, A. Bibcode: 2002DPS....34.2102B Altcode: 2002BAAS...34..877B We will report the results from an occultation of P126A by Pluto on the night of 2002 July 20 UT. The event was successfully observed with a 0.4-m telescope at Mamiña, Chile under photometric conditions. Additional data were collected at CTIO on a 0.6-m telescope with heavy interference from clouds. The CTIO observations preclude an occultation at that location thus forcing the Mamiña chord to lie south of the centerline. Less-constraining negative results were obtained from the Canary Islands. The Mamiña lightcurve shows an occultation profile that clearly indicates the continued presence of a substantial atmosphere around Pluto. The profile does not show any trace of the ``kink'' seen in the 1988 occultation data at a similar distance from the centerline of the shadow. Depending on the specific model assumptions, the minimum distance of Mamiña from the center of Pluto's shadow lies in the range 1025-1130 km, which corresponds to a range of 1180-1260 km for the deepest radius probed in Pluto's atmosphere. These new occultation data cannot be well fitted with models derived from the 1988 data. Hence one or more changes have occurred in Pluto's atmosphere in the past 14 years. Either the haze/thermal gradient altitude has decreased (or disappeared altogether), or the temperature above this level has increased (accompanied by an increase in pressure), or some combination of the these two. These results challenge the current level of understanding of the nature of Pluto's atmosphere and its surface-atmosphere interaction. This work was supported, in part, by NASA Grants NAG5-10444, NAG5-9008, by NOAO and CTIO operated for NSF by AURA, NASA through the New Horizons project, and Research Corporation. Title: Short-Period Waves That Heat the Corona Detected at the 1999 Eclipse Authors: Pasachoff, Jay M.; Babcock, Bryce A.; Russell, Kevin D.; Seaton, Daniel B. Bibcode: 2002SoPh..207..241P Altcode: 2002astro.ph..2237P As a part of a study of the cause of solar coronal heating, we searched for high-frequency (∼ 1 Hz) intensity oscillations in coronal loops in the [Fe xiv] coronal green line. We summarize results from observations made at the 11 August 1999 total solar eclipse from Râmnicu-Vâlcea, Romania, through clear skies. We discuss the image reduction and analysis through two simultaneous series of coronal CCD images digitized at 10 Hz for a total time of about 140 s. One series of images was taken through a 3.6 Å filter isolating the 5303 Å[Fe xiv] coronal green line and the other through a 100 Å filter in the nearby K-corona continuum. Previous observations, described in Pasachoff et al. (2000), showed no evidence for oscillations in the [Fe xiv] green line at a level greater than 2% of coronal intensity. We describe several improvements made over the 1998 eclipse that led to increased image clarity and sensitivity. The corona was brighter in 1999 with the solar maximum, further improving the data. We use Fourier analysis to search in the [Fe xiv] channel for intensity oscillations in loops at the base of the corona. Such oscillations in the 1-Hz range are predicted as a result of density fluctuations from the resonant absorption of MHD waves. The dissipation of a significant amount of mechanical energy from the photosphere into the corona through this mechanism could provide sufficient energy to heat the corona. A Monte Carlo model of the data suggests the presence of enhanced power, particularly in the 0.75-1.0 Hz range, and we conclude that MHD waves remain a viable method for coronal heating. Title: Further Analysis of Short-Period Waves for Coronal Heating from the 1999 Eclipse Authors: Seaton, D. B.; Pasachoff, J. M.; Babcock, B. A.; Russell, K. D. Bibcode: 2002AAS...200.8804S Altcode: 2002BAAS...34..789S As a part of a study of the cause of solar coronal heating, we searched at several eclipses for high-frequency ( 1 Hz) intensity oscillations in coronal loops in the [Fe XIV] coronal green line. Such oscillations in the 1-Hz range are predicted as a result of density fluctuations from the resonant absorption of MHD waves. The dissipation of a significant amount of mechanical energy from the photosphere into the corona through this mechanism could provide sufficient energy to hear the corona. We summarize results from observations made at the 11 August 1999 total solar eclipse from Râmnicu-Vâlcea, Romania, through clear skies, where data were taken through two simultaneous series of coronal CCD images digitized at 10 Hz for a total time of about 140 s. Previous observations, described in Pasachoff, Babcock, Russell, McConnochie, and Diaz (2000), had a detection limit of 2% for intensity oscillations in the [Fe XIV] green line. We found stronger coronal intensity at the 1999 eclipse because of the peak in the sunspot cycle and we selected our region of observations in consultation with SOHO/EIT and TRACE scientists. One series of images was taken through a 3.6 Å filter isolating the 5303 Å [Fe XIV] coronal green line and the other through a 100 Å filter in the nearby K-corona continuum. We used Fourier analysis to search in the [Fe XIV] channel for intensity oscillations in loops at the base of the corona (Pasachoff, Babcock, Russell, & Seaton, 2002). A comparison with a Monte-Carlo model of the data suggested the presence of enhanced power, particularly in the 0.75-1.0 Hz range. We report on our ongoing wavelet analysis that may make a stronger case for the presence of oscillations in our data. We also discuss plans for observing the 4 December 2002 eclipse. Support for this research has been provided by the National Science Foundation, the National Geographic Society, and NASA; DBS is supported by the TRACE grant, contract NAS5-38099 from NASA to LMATC. Title: Menzel and eclipses Authors: Pasachoff, Jay M. Bibcode: 2002JHA....33..139P Altcode: No abstract at ADS Title: Book Review: Astronomy : from the earth to the universe.- 6th ed. / Thomson Learning, 2001 Authors: Pasachoff, J. M. Bibcode: 2002Obs...122..111P Altcode: No abstract at ADS Title: Eclipse Authors: Pasachoff, J. Bibcode: 2002eaa..bookE2017P Altcode: An eclipse of the Sun is an OCCULTATION at which the Moon comes between the Earth and the Sun, blocking some or all of the sunlight from reaching an observer. Eclipses result from the fortuitous circumstance that the angular sizes of the Sun and the Moon as seen from Earth are the same to within about 10%, although in absolute diameter they differ by a factor of 400.... Title: Pasachoff's Points Authors: Pasachoff, Jay M. Bibcode: 2002PhTea..40..196P Altcode: No abstract at ADS Title: A Universe from Nothing Authors: Filippenko, Alexei V.; Pasachoff, Jay M. Bibcode: 2002Mercu..31b..15F Altcode: Insights from modern physics suggest that our wondrous universe may be the ultimate free lunch. Title: Astronomical Sacred Sites - II Authors: Pasachoff, Jay M. Bibcode: 2002S&T...103b..16P Altcode: No abstract at ADS Title: Nearest star: The surprising science of our Sun Authors: Golub, Leon; Pasachoff, Jay M.; O'Connell, James Bibcode: 2002PhTea..40..127G Altcode: No abstract at ADS Title: What Should College Students Learn? Authors: Pasachoff, Jay M. Bibcode: 2002AEdRv...1a.124P Altcode: Editor's Note: One of the key goals of the Astronomy Education Review is to encourage open discussion about issues of interest to astronomy educators. We begin our series of opinion pieces with a contribution by veteran educator and author Jay Pasachoff on the subject of what we should be teaching in the introductory college astronomy course. We invite our readers to respond to his position and also to submit opinion pieces on other controversial topics. (Please see the "How to Submit" section of our site.) Title: Astronomy: From the Earth to the Universe Authors: Pasachoff, Jay Bibcode: 2002afeu.book.....P Altcode: Clear explanations, rare photographs, and authoritative commentary makes Pasachoff's book the definitive text in introductory astronomy. Title: The Chemical Composition at the Edge of the Galaxy Authors: Lubowich, D. A.; Pasachoff, J. M.; Millar, T. J.; Roberts, H.; Brammer, G. B.; Henkel, C. Bibcode: 2001AAS...199.5804L Altcode: 2001BAAS...33Q1390L We present initial observations to determine the chemical composition of a molecular cloud at the edge of the Galaxy (28 kpc from the Galactic Center). Our observations provide a unique opportunity to determine the chemical composition and physical conditions in 10-Gyr-old less evolved gas similar to the early Galactic disk to help understand the formation of the Galaxy. We used the Kitt Peak 12-m telescope in June 2001 and detected the 2-1 line of CS and the 1-0 lines of HCO+, HCN, and HNC with a peak TR* = 160 mK, 130 mK, 50 mK, and 40 mK respectively. For the 1-0 lines of DNC, DCO+, and N2H+ we obtained upper limits of TR* < 6 mK, 6 mK, and 10 mK respectively. The HCN/HNC ratio indicated that this is a cold cloud with Tkin = 10 K - 20 K. We present additional data from observations of SiO, SO, CH3OH, OCS, H2CO, H2CS, HC3N, CN, C2H, and H2S that will be conducted this fall with the Kitt Peak 12-m and Heinrich Hertz Submillimeter Telescope telescopes. We will test models of Galactic chemical evolution that predict that the abundances of C, N, O will be lower than in any other Galactic cloud and similar to dwarf irregular galaxies. We will test the possibility that we are observing gas from an early burst of massive star formation such as population III halo stars which would have produced some S and O but not a significant amount of the secondary element N that is also produced from low mass stars. We thank the Research Corporation for providing funding for general community access to Kitt Peak 12-meter telescope, presently operated by Steward Observatory and to the AAS for a small research grant. Title: The Role of Research in an Astronomy or Astrophysics Major Authors: Pasachoff, J. M. Bibcode: 2001AAS...19915404P Altcode: 2001BAAS...33S1534P Undergraduates have proven capable of substantial research success in the hundreds of projects undertaken at both Williams College and over the past decade at its associated institutions in the Keck Northeast Astronomy Consortium: Wellesley, Wesleyan, Middlebury, Colgate, Vassar, Haverford, and Swarthmore. We consider the undergraduate research to be central to our astronomy and astrophysics major programs. Research opportunities of underclass years, usually during summers, often help students decide to major in astronomy or astrophysics. The senior thesis research is often a highpoint of the undergraduate educational experience while nonthesis projects often also prove valuable for students assessing their interests and careers. Many of the projects have been on campus while others are at national observatories or in other non-local research programs. Our Keck consortium has included a student summer exchange in which 12-16 students, usually after their sophomore or junior years, undertake research projects at member institutions other than their own. The results are reported at a student research symposium each fall, with approximately 35 research papers delivered; the proceedings are available. See http://www.astro.wellesley.edu/keck/. Institutions such as those in the consortium, with typical enrollments of 1100-2800, have been shown to generate a higher rate of attainment of science professional degrees than universities. Of course, many students at universities also benefit from undergraduate research opportunities during their undergraduate careers. Whether at colleges at universities, the personal contact and opportunity to transfer one's abilities from book learning to independent investigation can be invaluable in preparing students for their post-undergraduate lives. Title: TRACE Observations of the 15 November 1999 Transit of Mercury Authors: Schneider, G.; Pasachoff, J. M.; Golub, L. Bibcode: 2001DPS....33.1002S Altcode: 2001BAAS...33.1037S We present time-resolved (38s) high-resolution (500mas) imagery of the ingress phase of the 15 November 1999 transit of Mercury observed with the Transition Region Coronal Explorer (TRACE) spacecraft in its "white light" (1600 - 6000 Angstrom) channel. As part of our photometric and astrometic analyses of this data set we examined the images in and around the point of internal tangency for evidence of the historical "black drop effect". After calibration (including careful removal of image/instrumental artifacts and flat-fielding) the only radially directed brightness anisotropes found were due to the interacting effects the back-light solar limb-darkening, diffraction of photospheric light around the Mercurian disk, and the instrument's Point Spread Function. We discuss, and model, these effects as they would have applied to earlier ground-based observations of Mercurian transits (also including the effects of atmospheric "seeing") to explain the historical basis for the black drop effect. Title: Nearest Star: The Surprising Science of Our Sun Authors: Golub, Leon; Pasachoff, Jay M.; Lopez, Ramon E. Bibcode: 2001PhT....54k..59G Altcode: No abstract at ADS Title: What Should College Students Learn? Authors: Pasachoff, Jay M. Bibcode: 2001AEdRv...1..124P Altcode: No abstract at ADS Title: What should students learn? Authors: Pasachoff, Jay M. Bibcode: 2001PhTea..39..381P Altcode: It is important for students to learn about the exciting things that are now going on in astronomy. But the application of physics research to astronomy seems bogged down in the phases of the Moon and the cause of the seasons. Title: Meteoritics as Visual Metaphors Authors: Olson, R. M. J.; Pasachoff, J. M. Bibcode: 2001M&PSA..36R.153O Altcode: No abstract at ADS Title: Eclipse/SOHO Joint Observations of Solar Eclipses Authors: Pasachoff, J. M.; Russell, K. D.; Seaton, D. B.; Babcock, B. A.; Martin, S. Bibcode: 2001AGUSM..SH41B25P Altcode: Eclipse observations extend upward from the lunar limb, and so include a region occulted by all coronagraphs, spaceborne and mountaintop. Prior to the 1998 total solar eclipse, we conceived a joint observation with LASCO on SOHO to observe the solar corona with the same field of view and same filter passband and central wavelength. We would not only fill in the occulted region from the SOHO C1 coronagraph but also measure the substantial scattered light on C1 as a function of position by comparing its observations with ours. We have used a purpose-built telescope matching SOHO's and IDL to obtain and calibrate those observations with a 0.3 nm passband at 530.0 nm, offband from the coronal green line. Further, with the demise of C1, we used an improvement in our apparatus to observe on-band at 530.3 nm during the total solar eclipse of 1999. For both eclipses, we have interposed the EIT disk observations with our eclipse observations of the lower corona and with LASCO C2 observations of higher coronal levels to provide a full-field continuous image of the corona, emphasizing streamers and other structure and tracing them from their feet on the solar disk upward through the corona. Title: Donald H. Menzel: Scientist, Educator Builder Authors: Pasachoff, J. M.; Gingerich, O.; Layzer, D.; Noyes, R. W.; Parkinson, W. H.; Welther, B. Bibcode: 2001AGUSM..SH41B26P Altcode: A centennial symposium in honor of Donald H. Menzel was held at the Harvard-Smithsonian Center for Astrophysics on May 11, 2001. Menzel was known especially for his studies of the solar chromosphere, for his theoretical work on gaseous nebulae, and for his role in founding the Sacramento Peak and High Altitude observatories and in bringing the Smithsonian Astrophysical Observatory to Cambridge. Menzel received his Ph.D. at Princeton, where he was fascinated and excited by the lectures of Henry Norris Russell about the new theoretical astrophysics. At Lick Observatory, Menzel investigated the solar chromosphere using solar eclipse spectra, and published the results in a major volume in 1931. The value for the mean molecular weight he deduced for the lower chromosphere helped persuade Russell and others that hydrogen was the major constituent of the solar atmosphere, as Cecilia Payne had intimated earlier. Menzel's studies of solar eclipse spectra also led him to propose, in a paper written with R. T. Birge, that hydrogen had an isotope of mass 2, a suggestion that motivated Harold Urey to isolate the isotope (deuterium) chemically. Menzel joined the Harvard faculty in 1932. His interest in investigating the sun led him to observe more than a dozen solar eclipses, to exploit the coronagraph, and to found two solar observatories: at Climax, Colorado, and at Sunspot, New Mexico. He served as Director of the Harvard College Observatory from 1952 to 1966. During this time he suggested bringing and arranged to bring the Smithsonian Astrophysical Observatory to Harvard. Speakers at the symposium on Menzel's life, times, and scientific legacy included Donald Osterbrock, David DeVorkin, David Layzer, Jay Pasachoff, Barbara Welther, Thomas Bogdan, Jack Zirker, and France Cordova. The organizing committee was Owen Gingerich, David Layzer, Robert Noyes, William Parkinson, Jay Pasachoff, and Barbara Welther. Title: Color Corrected Authors: Pasachoff, Jay M. Bibcode: 2001S&T...101e..18P Altcode: No abstract at ADS Title: On teaching introductory astronomy Authors: Pasachoff, Jay M. Bibcode: 2001PhTea..39..198P Altcode: No abstract at ADS Title: Pro-Am Solar-Eclipse Conference, A Authors: Pasachoff, Jay M. Bibcode: 2001S&T...101b..45P Altcode: No abstract at ADS Title: Early Eclipse Science Authors: Pasachoff, Jay M. Bibcode: 2001S&T...101b..46P Altcode: No abstract at ADS Title: Book Review: Shoemaker by Levy : the man who made an impact / Princeton University Press, Princeton, New Jersey, 303 pp., 2000, ISBN 0-691-00225-8. Authors: Pasachoff, Jay M. Bibcode: 2001Ast....29b.100P Altcode: No abstract at ADS Title: Solar-Eclipse Science: Still Going Strong Authors: Pasachoff, Jay M. Bibcode: 2001S&T...101b..40P Altcode: No abstract at ADS Title: Moon-Struck: Artists Rediscover Nature And Observe Authors: Pasachoff, Jay M.; Olson, Roberta J. M. Bibcode: 2001EM&P...85..303P Altcode: 1999EM&P...85..303P We discuss rare early depictions of the Moon by artists who actually observed Earth's nearest neighbor rather than relying on stylized formulas. The earliest, from the 14th and 15th centuries, reveal that revolutionary advances in both pre-telescopic astronomy and naturalistic painting could go hand-in-hand. This link suggests that when painters observed the world, their definition of world could also include the heavens and the Moon. Many of the artists we discuss - e.g., Pietro Lorenzetti, Giotto, and Jan Van Eyck - actually studied the Moon, incorporating their studies into several works. We also consider the star map on the dome over the altar in the Old Sacristy of San Lorenzo, Florence (c. 1442), whose likely advisor was Toscanelli. In addition, we examine representations by artists who painted for Popes Julius II and Leo X - Raphael and Sebastiano del Piombo, both of whom were influenced by individuals at the papal court, such as the astronomer, painter, and cartographer Johann (Giovanni) Ruysch and Leonardo da Vinci. We also discuss Leonardo's pre-telescopic notes and lunar drawings as they impacted on art and science in Florence, where Galileo would study perspective and chiaroscuro. Galileo's representations of the Moon (engraved in his Sidereus Nuncius, 1610) are noted, together with those by Harriot and Galileo's friend, the painter Cigoli. During the 17th century, the Moon's features were telescopically mapped by astronomers with repercussions in art, e.g., paintings by Donati Creti and Raimondo Manzini as well as Adam Elsheimer. Ending with a consideration of the 19th-century artists/astronomers John Russell and John Brett and early lunar photography, we demonstrate that artistic and scientific visual acuity belonged to the burgeoning empiricism of the 14th, 15th, and 16th centuries that eventually yielded modern observational astronomy. Title: The Cosmos: Astronomy in the New Millennium Authors: Pasachoff, Jay; Filippenko, Alex Bibcode: 2001canm.book.....P Altcode: Pasachoff/Filippenko represent a team that brings together experience in writing, research, and teaching. This book provides a brief, up-to-date, and beautifully illustrated overview of astronomy. Pasachoff/Filippenko are each very experienced in teaching elementary astronomy to their student and bring that experience to bear in this text. Visit www.harcourtcollege.com/astro/cosmos for further information. Title: A Proper Wave to Maxwell Authors: Pasachoff, Jay M. Bibcode: 2001S&T...101a..14P Altcode: No abstract at ADS Title: Nearest star : the surprising science of our sun Authors: Golub, Leon; Pasachoff, Jay M. Bibcode: 2001nsss.book.....G Altcode: No abstract at ADS Title: Public education in developing countries on the occasions of eclipses Authors: Pasachoff, Jay M. Bibcode: 2001IAUGA..24..101P Altcode: 2000IAUSS..24E..38P Total solar eclipses will cross southern Africa on June 21, 2001, and on December 4, 2002. Most of Africa will see partial phases. The total phase of the 2001 eclipse will be visible from parts of Angola, Zambia, Zimbabwe, Mozambique and Madagascar. The total phase of the 2002 eclipse will be visible from parts of Angola, Botswana, Zimbabwe, South Africa and Mozambique. Public education must be undertaken to tell the people how to look at the eclipse safely. We can take advantage of having the attention of the people and of news media to teach about not only eclipses but also the rest of astronomy. I am Chair of a "Public Education at Eclipses" subcommission of IAU Commission 46 on the Teaching of Astronomy, and we are able to advise educators and others about materials, procedures and information releases. Title: Deuterium Near and Far in the Galaxy Authors: Lubowich, D. A.; Pasachoff, Jay M.; Ostenson, Jason A. Bibcode: 2001coev.conf...63L Altcode: We report on our program to determine the deuterium abundance distribution in the Milky Way. We have reported D/H = 1.7×10-6 in a molecular cloud 10 pc from the Galactic Center, from which we infer recent continuous infall of pregalactic primordial gas. We have searched for the Balmer Da lines with high S/N = 300 - 1000 observations of a halo star (HD 140283), slowly rotating B stars (ι Her and γ Peg), H II regions (Orion Nebula and M17), and the planetary nebula NGC 7027. Title: The Prediction and Observation of the 1997 July 18 Stellar Occultation by Triton: More Evidence for Distortion and Increasing Pressure in Triton's Atmosphere Authors: Elliot, J. L.; Person, M. J.; McDonald, S. W.; Buie, M. W.; Dunham, E. W.; Millis, R. L.; Nye, R. A.; Olkin, C. B.; Wasserman, L. H.; Young, L. A.; Hubbard, W. B.; Hill, R.; Reitsema, H. J.; Pasachoff, J. M.; McConnochie, T. H.; Babcock, B. A.; Stone, R. C.; Francis, P. Bibcode: 2000Icar..148..347E Altcode: A variety of CCD astrometric data was used to predict the location of the path for the occultation of the star we have denoted "Tr176" by Triton, which occurred on 1997 July 18, and was visible from locations in northern Australia and southern North America. A network of fixed and portable telescopes equipped with high-speed photometric equipment was set up to observe the event, with the following observational goals: (i) mapping the central flash (to establish the global shape of Triton's atmosphere at about 20-km altitude by modeling the detailed shape of the central flash), (ii) obtaining one or more light curves of high signal-to-noise ratio from a large telescope (to accurately determine the thermal structure of Triton's atmosphere), and (iii) obtaining light curves distributed across Triton's disk (to probe the thermal structure of Triton's atmosphere above different areas and to establish the shape of the atmosphereat about 100-km altitude by modeling the half-light surface). Although the large, fixed telescopes proved to be outside of the occultation shadow and observations with some of the portable telescopes were foiled by clouds, light curves were successfully recorded from Brownsville, Texas, and Chillagoe, Queensland. These were combined with data from another group to determine the radius and shape of the half-light surface in Triton's atmosphere and the equivalent-isothermal temperatures at the sub-occultation latitudes on Triton. A circular solution for the half-light surface (projected into Triton's shadow) yielded a radius of 1439±10 km. However, the data are indicative of a global shape more complex than a sphere. Such a figure is most likely caused by strong winds. Light-curve models corresponding to the best fitting circular and elliptical atmospheres were fit to the data. The mean pressure at 1400-km radius (48-km altitude) derived from all of the data was 2.23±0.28 μbar for the circular model and 2.45±0.32 μbar for the elliptical model. These values suggest a global pressure increase at this level since a previous Triton occultation in 1995 August. The mean equivalent-isothermal temperature at 1400 km was 43.6±3.7 K for the circular model and 42.0±3.6 K for the elliptical model. Within their (sometimes large) uncertainties, the equivalent-isothermal temperatures agree for all Triton latitudes probed. Title: Further Evidence for Increasing Pressure and a Non-spherical Shape in Triton's Atmosphere Authors: Person, M. J.; Elliot, J. L.; McDonald, S. W.; Buie, M. W.; Dunham, E. W.; Millis, R. L.; Nye, R. A.; Olkin, C. B.; Wasserman, L. H.; Young, L. A.; Hubbard, W. B.; Hill, R.; Reitsema, H. J.; Pasachoff, J. M.; Babcock, B. A.; McConnochie, T. M.; Stone, R. C. Bibcode: 2000DPS....32.4502P Altcode: 2000BAAS...32.1082P An occultation by Triton of a star denoted as Tr176 by McDonald & Elliot (AJ 109, 1352), was observed on 1997 July 18 from various locations in Australia and North America. After an extensive prediction effort, two complete chords of the occultation were recorded by our PCCD portable data systems. These chords were combined with three others recorded by another group (Sicardy et al., BAAS 30, 1107) to provide an overall geometric solution for Triton's atmosphere at the occultation pressure. A simple circular fit to these five chords yielded a half-light radius of 1439 +/- 10 km, however least squares fitting revealed a significant deviation from the simple circular projection of a spherical atmosphere. The best fitting ellipse (a first order deviation from the circular solution) yielded a mean radius of 1440 +/- 6 km and an ellipticity of 0.040 +/- 0.003. To further characterize the non-spherical solutions to the geometric fits, methods were developed to analyze the data assuming both circular and elliptical profiles. Circular and elliptically focused light curve models corresponding to the best fitting circular and elliptical geometric solutions were fit to the data. Using these light curve fits, the mean pressure at the 1400 km radius (48 km altitude) derived from all the data was 2.23 +/- 0.28 microbar for the circular model and 2.45 +/- 0.32 microbar for the elliptical model. These pressures agree with those for the Tr180 occultation (which occurred a few months later), so these results are consistent with the conclusions of Elliot et al. (Icarus 143, 425) that Triton's surface pressure has increased from 14.0 microbar at the time of the Voyager encounter to 19.0 microbar in 1997. The mean equivalent-isothermal temperature at 1400 km was 43.6 +/- 3.7 K for the circular model and 42.0 +/- 3.6 K for the elliptical model. Within their calculated errors, the equivalent-isothermal temperatures were the same for all Triton latitudes probed. Title: A search at two eclipses for short-period waves that heat the corona Authors: Pasachoff, Jay M.; Babcock, Bryce A.; Russell, Kevin D.; McConnochie, Timothy H.; Diaz, J. Sebastian Bibcode: 2000SoPh..195..281P Altcode: As part of a study of the cause of solar coronal heating, we searched for high-frequency (∼1 Hz) intensity oscillations in coronal loops in the [Fe xiv] coronal green line. We summarize results from observations made at the 3 November 1994, total solar eclipse from the International Astronomical Union site in Putre, Chile, through partly cloudy skies, and at the 26 February 1998 total solar eclipse from Nord, Aruba, through clear skies. We discuss the image reduction and analysis of two simultaneous series of coronal CCD images digitized at 10 Hz for a total time of 160 s in Chile. One series of images was taken through a filter isolating the 5303 Å[Fe xiv] coronal green line and the other through a 100 Å filter in the nearby K-corona continuum. We then discuss the modifications made for the 1998 eclipse, and the image reduction and analysis for those image sequences. After standard calibrations and image alignment of both data sets, we use Fourier analysis to search in the [Fe xiv] channel for intensity oscillations in loops at the base of the corona. Such oscillations in the 1-Hz range are predicted as a result of density fluctuations from the resonant absorption of MHD waves. The dissipation of a significant amount of mechanical energy from the photosphere into the corona through this mechanism could provide sufficient energy to heat the corona. At neither eclipse do we find evidence for oscillations in the [Fe xiv] green line at a level greater than 2% of coronal intensity. Title: Deuterium in the Galactic Centre as a result of recent infall of low-metallicity gas Authors: Lubowich, D. A.; Pasachoff, Jay M.; Balonek, Thomas J.; Millar, T. J.; Tremonti, Christy; Roberts, Helen; Galloway, Robert P. Bibcode: 2000Natur.405.1025L Altcode: The Galactic Centre is the most active and heavily processed region of the Milky Way, so it can be used as a stringent test for the abundance of deuterium (a sensitive indicator of conditions in the first 1,000 seconds in the life of the Universe). As deuterium is destroyed in stellar interiors, chemical evolution models predict that its Galactic Centre abundance relative to hydrogen is D/H = 5 × 10-12, unless there is a continuous source of deuterium from relatively primordial (low-metallicity) gas. Here we report the detection of deuterium (in the molecule DCN) in a molecular cloud only 10 parsecs from the Galactic Centre. Our data, when combined with a model of molecular abundances, indicate that D/H = (1.7 +/- 0.3) × 10-6, five orders of magnitude larger than the predictions of evolutionary models with no continuous source of deuterium. The most probable explanation is recent infall of relatively unprocessed metal-poor gas into the Galactic Centre (at the rate inferred by Wakker). Our measured D/H is nine times less than the local interstellar value, and the lowest D/H observed in the Galaxy. We conclude that the observed Galactic Centre deuterium is cosmological, with an abundance reduced by stellar processing and mixing, and that there is no significant Galactic source of deuterium. Title: Eclipse Observations of Coronal Structure, Polarization, and Oscillations from 11 August 1999 Authors: Pasachoff, J. M.; Babcock, B. A.; Russell, K. D.; May, S. K. Bibcode: 2000AAS...196.4904P Altcode: 2000BAAS...32..750P We report on CCD observations of the corona from Ramnicu Valcea, Romania, during the total solar eclipse of 11 August 1999. One experiment searched for oscillations in the 530.3-nm coronal green line at about 1 Hz by digitizing at 10 Hz, as a determination of the coronal oscillation spectrum to test models of magnetohydrodynamic heating. The optical system was improved in several ways since the 1998 expedition, as was monitoring of the filter. The series of images was aligned and Fourier transforms were examined for individual pixels and groups of pixels. No oscillations were clearly detected above the 1% level, though statistical analysis continues at this writing. A second experiment took a series of 36 images through one filter wheel that contained three filters near 400 nm and a second filter wheel containing polarizers at three angles plus a parfocal clear filter. The results include a polarization map of a quadrant of the sun and an attempt to map the coronal temperature. The temperature map uses techniques suggested by Cram (1976) through a determination of the extent to which scattering off high-temperature electrons wash out the photospheric Fraunhofer lines. Low-pass filtering of our resultant images show detail in the form of coronal loops but do not show much non-radial structure in the temperature variations. We also compare composite photographic observations with EIT images from eclipse day. The expedition was supported by NSF grant ATM-9812408, National Geographic Society grant 6449-99, the Keck Northeast Astronomy Consortium, and NASA SOHO/EIT guest-investigator grant NRA-98-03-SEC-051. Title: SECIS: The Solar Eclipse Coronal Eclipse Imaging System Authors: Phillips, K. J. H.; Read, P. D.; Gallagher, P. T.; Keenan, F. P.; Rudawy, P.; Rompolt, B.; Berlicki, A.; Buczylko, A.; Diego, F.; Barnsley, R.; Smartt, R. N.; Pasachoff, J. M.; Babcock, B. A. Bibcode: 2000SoPh..193..259P Altcode: The Solar Eclipse Coronal Imaging System (SECIS) is an instrument designed to search for short-period modulations in the solar corona seen either during a total eclipse or with a coronagraph. The CCD cameras used in SECIS have the capability of imaging the corona at a rate of up to 70 frames a second, with the intensities in each pixel digitised in 12-bit levels. The data are captured and stored on a modified PC. With suitable optics it is thus possible to search for fast changes or short-period wave motions in the corona that will have important implications for the coronal heating mechanism. The equipment has been successfully tested using the Evans Solar Facility coronagraph at National Solar Observatory/Sacramento Peak and during the 11 August 1999 eclipse at a site in north-eastern Bulgaria. The instrument is described and preliminary results are outlined. Title: Wiliams College, Hopkins Observatory, Williamstown, Massachusetts 01267. Report for the period 1 Jul 1998 - 1 Sep 1999. Authors: Pasachoff, J. M.; Kwitter, K. B. Bibcode: 2000BAAS...32..619P Altcode: No abstract at ADS Title: The Deuterium Abundance In The Galactic Center 50 km/s Molecular Cloud: Evidence For A Cosmological Origin Of D Authors: Lubowich, D. A.; Pasachoff, J. M.; Galloway, R. P.; Balonek, T. J.; Tremonti, C.; Millar, T.; Roberts, H. Bibcode: 2000IAUS..198..167L Altcode: No abstract at ADS Title: Commission 46: Teaching of Astronomy: (Enseignement de L'astronomie) Authors: Fierro, Julieta; Isobe, Syuzo; Jones, B.; Batten, A.; Arellano, A.; Gervaldi, M.; Guinan, E.; Tush, W.; Hoff, D.; Martinez, P.; McNally, D.; Norton, A.; Narlikar, J.; Pasachoff, J.; Percy, J.; Wentzel, D. Bibcode: 2000IAUTA..24..423F Altcode: No abstract at ADS Title: The Williams College expedition to Râmnicu Vâlcea Authors: Pasachoff, Jay M. Bibcode: 2000ASIC..558...23P Altcode: 2000asre.conf...23P The Williams College expedition to Râmnicu Vâlcea, Romania, made observations of the solar corona (a) to compare with the Extreme ultraviolet Imaging Telescope (EIT) on the Solar and Heliospheric Observatory; (b) to search for the source of coronal heating through a study of the oscillatory power spectrum of coronal loops in an emission line typical of high temperature; (c) mapped the coronal temperature using ultraviolet continuum observations; (d) made videos and still photographs of coronal motions and details; and (e) collaborated with the scientists at the Astronomical Institute in Bucharest. Title: Fire in the Sky Authors: Olson, Roberta J. M.; Pasachoff, Jay M. Bibcode: 1999fisk.book.....O Altcode: Fire in the Sky collects many representations of comets and meteors in Britain during the eighteen and nineteenth century when a large number of works inspired by these celestial objects were produced. Over 100 photographs--and two sections of luscious color plates--beautifully portray the inspired output of some of the world's most talented artists, fully capturing the phenomenon that obsessed not only a nation but an era as well. Olson and Pasachoff reveal the many different ways that comets and meteors have appeared in paintings and literature and link these works to the achievements of British science in the wake of Newton and Halley. They also examine the different symbolism that writers and artists have attached to these spectacular objects. Throughout, Fire in the Sky conveys how the development of new technologies, and the burgeoning interest of the general public in science and art, dovetailed with an interest in nature and a strong literary tradition of comet and meteor symbolism. Beautifully illustrated and packed with engaging stories, this book will delight anyone with an interest in the art and astronomy of comets. Title: Comets, meteors, and eclipses: art and science in early renaissance Italy (Invited). Authors: Olson, R. J. M.; Pasachoff, J. M. Bibcode: 1999BAAS...31.1080O Altcode: No abstract at ADS Title: Comets, Meteors, and Eclipses: Art and Science in Early Renaissance Italy (Invited) Authors: Olson, R. J. M.; Pasachoff, J. M. Bibcode: 1999DPS....31.0701O Altcode: We discuss several topics relating artists and their works with actual astronomical events in early Renaissance Italy to reveal the revolutionary advances made in both astronomy and naturalistic painting. Padua, where Galileo would eventually hold a chair at the University, was already by the fourteenth century (trecento) a renowned center for mathematics and nascent astronomy (which was separating from astrology). It is no wonder that when Enrico Scrovegni commissioned the famous Florentine artist Giotto di Bondone to decorate his lavish family chapel (c. 1303) that in the scene of the Adoration of the Magi Giotto painted a flaming comet in lieu of the traditional Star of Bethlehem. Moreover, he painted an historical apparition he recently had observed with a great understanding of its scientific structure: Halley's Comet of 1301 (since Olson's first publication of this idea in Scientific American we have expanded the argument in several articles and talks). While we do not know the identity of the artist's theological advisor, we discuss the possibility that Pietro d'Abano, the Paduan medical doctor and ``astronomer" who wrote on comets, might have been influential. We also compare Giotto's blazing comet with two others painted by the artist's shop in San Francesco at Assisi (before 1316) and account for the differences. In addition, we tackle the question how Giotto's pupil, Taddeo Gaddi, who is documented as having been partially blinded by lengthy unprotected observation of the partial phase of an annular solar eclipse, reflects his observations in his frescoes in Santa Croce, Florence (1328-30). Giotto also influenced the Sienese painter Pietro Lorenzetti, two of whose Passion cycle frescoes at Assisi (1316-20), contain dazzling meteor showers that hold important symbolic meanings in the cyle's argument but more importantly reveal that the artist observed astronomical phenomena, such as the ``radiant" effect, which was first recorded by Alexander von Humboldt in 1799 and only accepted in the nineteenth century. Lorenzetti also painted sporadic, independent meteors, which do not emanate from the radiant, demonstrating that he observed this phenomenon as well. (It is significant that these artists knew the differences between comets and meteors, facts which were not absolutely established until the eighteenth century.) We demonstrate that artistic and scientific visual acuity were part of the burgeoning empiricism of the fourteenth century that eventually yielded modern observational astronomy. Our joint work has been supported in part by the National Endowment for the Humanities and the Getty Grant Program. Title: Halley and his maps of the Total Eclipses of 1715 and 1724 Authors: Pasachoff, Jay M. Bibcode: 1999JAHH....2...39P Altcode: Edmond Halley was perhaps the first, in 1715, to draw the path of an eclipse as seen from above, looking down at the Earth's surface. I compare four eclipse-path maps drawn for Halley: one before the 1715 eclipse, one with a corrected path after the eclipse and including the predicted path for the 1724 eclipse, a reissue of that map just before the latter eclipse, and a different map for that latter eclipse. These maps are in the collection of the Houghton Library of Harvard University. For comparison, I provide a current map of the 1999 total solar-eclipse path, which is similar to that of 1724. Title: Halley's Maps and Descriptions of the 1715 Total Solar Eclipse Authors: Pasachoff, J. M. Bibcode: 1999AAS...194.0108P Altcode: 1999BAAS...31..824P Edmond Halley was perhaps the first to present eclipse maps to the public in their common current form: looking down on the Earth's surface from above. For the 1715 total solar eclipse that crossed England, he prepared broadsheets showing the eclipse path and describing what would be expected. After the eclipse, he corrected the eclipse path, and added the path and description of the 1724 total solar eclipse. His separate path for the latter resembles the path of the August 11, 1999, eclipse as drawn by Fred Espenak in his NASA Reference Publication. All four of the Halley maps are in the Houghton Library, Harvard University. Halley described observations of the 1715 eclipse in the Philosophical Transactions of the Royal Society, including both his own observations and those of other observatories. The need for advising the public about forthcoming eclipses and how to observe them safely continues from Halley's time down to this day. Title: Halley and his maps of the total eclipses of 1715 and 1724 Authors: Pasachoff, Jay Bibcode: 1999A&G....40b..18P Altcode: No abstract at ADS Title: Halley et ses cartes des éclipses totales de 1715 et 1724. Authors: Pasachoff, J. M. Bibcode: 1999C&T...115...51P Altcode: No abstract at ADS Title: The Solar Corona Authors: Golub, Leon; Pasachoff, Jay M.; Smartt, Raymond N. Bibcode: 1999AmJPh..67..263G Altcode: No abstract at ADS Title: Williams College, Hopkins Observatory, Williamstown, Massachusetts 01267. Report for the period 1 Jul 1997 - 30 Jun 1998. Authors: Pasachoff, J. M.; Kwitter, K. B. Bibcode: 1999BAAS...31..650P Altcode: No abstract at ADS Title: Linking a Textbook with the World Wide Web Authors: Pasachoff, J. M. Bibcode: 1998AAS...193.7801P Altcode: 1998BAAS...30.1371P The pace of astronomy is such that a printed textbook is out of date by the time it appears, though a cooperative publisher can allow a book to be six months or so more current than others with the same copyright date. I have endeavored to allow faculty and students to bring their textbook up to date on the day of each lecture or each reading assignment by providing a Web site linked chapter-by-chapter to my text Astronomy: From the Earth to the Universe, 5th edition, 1998. The URL http://www.williams.edu/Astronomy/jay contains updates, new discussions, errata, and links to other sites. The site also allows feedback and links to both author and publisher. Title: Book Review: The solar corona / Cambridge U Press, 1997 Authors: Golub, L.; Pasachoff, J. M. Bibcode: 1998SoPh..183..227G Altcode: No abstract at ADS Title: Weighty planets Authors: Pasachoff, Jay M. Bibcode: 1998PhTea..36..324P Altcode: No abstract at ADS Title: The FAQs of astronomy Authors: Pasachoff, Jay M. Bibcode: 1998Natur.394..438P Altcode: No abstract at ADS Title: Global warming on Triton Authors: Elliot, J. L.; Hammel, H. B.; Wasserman, L. H.; Franz, O. G.; McDonald, S. W.; Person, M. J.; Olkin, C. B.; Dunham, E. W.; Spencer, J. R.; Stansberry, J. A.; Buie, M. W.; Pasachoff, J. M.; Babcock, B. A.; McConnochie, T. H. Bibcode: 1998Natur.393..765E Altcode: Triton, Neptune's largest moon, has been predicted to undergo significant seasonal changes that would reveal themselves as changes in its mean frost temperature. But whether this temperature should at the present time be increasing, decreasing or constant depends on a number of parameters (such as the thermal properties of the surface, and frost migration patterns) that are unknown. Here we report observations of a recent stellar occultation by Triton which, when combined with earlier results, show that Triton has undergone a period of global warming since 1989. Our most conservative estimates of the rate of temperature and surface-pressure increase during this period imply that the atmosphere is doubling in bulk every 10 years-significantly faster than predicted by any published frost model for Triton,. Our result suggests that permanent polar caps on Triton play a dominant role in regulating seasonal atmospheric changes. Similar processes should also be active on Pluto. Title: Williams College's Hopkins Observatory: the oldest extant observatory in the United States Authors: Pasachoff, Jay M. Bibcode: 1998JAHH....1...61P Altcode: The Hopkins Observatory, built at Williams College in 1836-1838, is the oldest astronomical observatory extant in the United States. Founded by Professor Albert Hopkins and built together with his students, it still contains the oldest known Alvan Clark telescope. Some of its historic instruments are mounted in its wings, known as the Mehlin Museum of Astronomy, and its central internal domed-ceiling room is the Milham Planetarium. Title: Fire in the Sky Authors: Olson, Roberta J. M.; Pasachoff, Jay M. Bibcode: 1998fisk.book.....O Altcode: Introduction; 1. Prelude: the beginning of telescopic astronomy and the background of British astronomy and artistic traditions; 2. The heavens on fire: the eighteenth century; 3. The comet-crazed century opens; 4. The triumph of realism; 5. Donati's comet, the watershed; 6. The origin of comet (and meteor) photography; 7. The triumph of the imagination; 8. Comets and the new century; Epilogue: comets and the new millennium; Appendices; List of illustrations; Bibliography; Index. Title: Fire in the Sky: Comets and Meteors, the Decisive Centuries, in British Art and Science Authors: Olson, R. J. M.; Pasachoff, J. M. Bibcode: 1998fscm.book.....O Altcode: Comets and meteors are spectacular and awe-inspiring natural phenomena, which are among nature's most compelling icons. Since the beginning of recorded time, they have mesmerized people, not least among them artists and astronomers. Britain during the eighteenth and nineteenth centuries produced a larger number and greater variety of representations of comets and meteors than any other country. The development of new technologies, and the burgeoning interest of the general public in science and art, dovetailed with the inherent British interest in nature and a strong literary tradition of comet and meteor symbolism. This beautifully illustrated book examines the link between these works and the achievements of British science in the wake of Newton and Halley. This book will be stimulating to anyone interested in the art or astronomy of comets. Title: Use of the World Wide Web in Astronomy Teaching Authors: Pasachoff, J. M. Bibcode: 1998ntat.coll...68P Altcode: 1998IAUCo.162...68P No abstract at ADS Title: Astronomy: From the Earth to the Universe Authors: Pasachoff, J. M. Bibcode: 1998afeu.book.....P Altcode: The latest edition of a wonderful general-astronomy book meant for the introductory survey course in American universities. Highly illustrated. Covers the wide range of astronomy. Title: A Field Guide to the Stars and Planets Authors: Pasachoff, J. M.; Menzel, D. H. Bibcode: 1998fgsp.book.....P Altcode: The standard field guide for amateur observing; also usable for reference at professional telescopes. Many useful tables. Title: Mars Pathfinder slide set Authors: Pasachoff, Jay M.; Britt, Daniel Bibcode: 1998mpss.book.....P Altcode: No abstract at ADS Title: Solar Eclipses and Public Education Authors: Pasachoff, J. M. Bibcode: 1998ntat.coll..202P Altcode: 1998IAUCo.162..202P No abstract at ADS Title: Total solar eclipse to sweep across Americas Authors: Pasachoff, Jay M. Bibcode: 1997PhTea..35Q.515P Altcode: No abstract at ADS Title: The Solar Corona Authors: Golub, Leon; Pasachoff, Jay M. Bibcode: 1997soco.book.....G Altcode: Observations from the ground and space have advanced our knowledge of the solar corona dramatically over the past three decades. This timely volume presents a lucid and synthesized review of the latest observations of the solar corona and discusses how these observations have advanced and shaped our understanding of coronal physics. In the process, the authors introduce a wide variety of exciting physics, including dynamo theory and radiative transfer. They also demonstrate how the transient effects of the solar cycle effect "space weather." This book provides a much-needed introduction to coronal physics for advanced students and researchers. Title: Hubble `worth the price' Authors: Pasachoff, Jay M. Bibcode: 1997Natur.387..754P Altcode: No abstract at ADS Title: Pitfalls in the Science Standards Authors: Pasachoff, Jay M. Bibcode: 1997APS..APR..M203P Altcode: The National Science Standards ask for "relevance" and use a very limited set of topics. The "less is more" approach leaves out many topics that practicing physicists and teachers believe are essential for equipping students to see the roles of science in the modern world. The Standards' request for "relevance" may also not match the inspirational topics of today's physics and astronomy. If these problems are not considered as the Standards become incorporated in curricula, a substantial fall in student interest in physics and astronomy could result. Title: Panel and Audience Discussion Authors: Quinn, Helen; Alberts, Bruce; Stith, James H.; Pasachoff, Jay M.; Orpwood, Graham Bibcode: 1997APS..APR..M205Q Altcode: Participating Panelists: Bruce Alberts, National Academy of Sciences James H. Stith, Department of Physics, Ohio State University Jay M. Pasachoff, Astronomy Department, Williams College Graham Orpwood, Faculty of Education, York University Title: Solar eclipses as a vehicle for international astronomy education. Authors: Pasachoff, J. M. Bibcode: 1997ASIC..494..249P Altcode: 1997topr.conf..249P The public's attention is drawn to astronomy whenever solar eclipse - partial, annular, or total - is visible, and we must take advantage of the opportunity to teach about the nature of science, the ability of astronomers to predict and analyze distant bodies and events, and the value of scientific research. We must also instruct people how to watch the partial and annular phases safely and that the total phase is not harmful. Title: Coronal heating experiments of the Williams College Group at Mukandgarh Fort, Rajasthan. Authors: Pasachoff, J. M.; Babcock, B. A.; Diaz, S.; Reardon, K. P.; Kutner, E. R. Bibcode: 1997KodOB..13...75P Altcode: The authors report on the Williams College expedition to Mukandgarh Fort, Rajasthan, for the total solar eclipse of 24 October 1995. The main experiments were a search for 1 Hz oscillations in coronal loops as an indication of magnetohydrodynamic theories of coronal heating and a mapping of the coronal temperature through comparison of images at specific ultraviolet wavelengths, measuring the difference between the photospheric and coronal continuum. The authors also obtained a variety of coronal images. Title: Eclipse observations relevant to the coronal heating problem. Authors: Pasachoff, J. M. Bibcode: 1997ASIC..494..181P Altcode: 1997topr.conf..181P The author is studying the coronal oscillation spectrum and its implications on the heating of the solar corona through the reduction of his data from observations of the total solar eclipse of 24 October 1995 and with further theoretical and observational investigations. The observations provide tests of proposed mechanisms to explain the heating of the solar corona via weakly compressive magnetohydrodynamic waves. The author is also mapping the electron temperature of the corona through study of the broadening by electron scattering of ultraviolet Fraunhofer lines. Title: Cosmic Questions: Galactic Halos, Cold Dark Matter, and the End of Time Authors: Morris, Richard; Kutner, Eric R.; Pasachoff, Jay M. Bibcode: 1996AmJPh..64.1437M Altcode: No abstract at ADS Title: The Earliest Comet Photographs: Usherwood, Bond, and Donati 1858 Authors: Pasachoff, Jay M.; Olson, Roberta J. M.; Hazen, Martha L. Bibcode: 1996JHA....27..129P Altcode: No abstract at ADS Title: The Universe Wide Web Authors: Pasachoff, Jay M. Bibcode: 1996PhTea..34..134P Altcode: No abstract at ADS Title: Textbooks and Electronic Media Authors: Pasachoff, Jay M. Bibcode: 1996ASPC...89...66P Altcode: 1996aecd.conf...66P No abstract at ADS Title: Study of the High-Frequency Coronal-Loop Oscillation Spectrum at the 1994 Total Solar Eclipse Authors: Pasachoff, J. M.; Babcock, B.; Diaz, J. S.; Reardon, K.; Nichols-Kiley, R. Bibcode: 1995AAS...18710106P Altcode: 1995BAAS...27.1427P We summarize results from observations made at the November 3, 1994, total solar eclipse from the International Astronomical Union site in Putre, Chile, through partly cloudy skies. We discuss the image reduction and analysis of two simultaneous series of coronal images with a cadence of 10 frames per second for a total time of 160 seconds. One series of images was taken through a filter isolating the 530.3 nm [Fe XIV] coronal green line and the other through a 10 nm filter in the nearby K-corona continuum. After standard calibrations and image alignment, we use Fourier analysis to search in the [Fe XIV] channel for high-frequency ( 1 Hz) intensity oscillations in loops at the base of the corona. Such oscillations are predicted as a result of density fluctuations from the resonant absorption of high-frequency Alfven waves. The dissipation of a significant amount of mechanical energy from the photosphere into the corona through this mechanism could provide sufficient energy to heat the corona. The observations were supported by NSF ATM-9005194 and Education Division DUE-9351279 grants; the National Geographic Society through their Committee on Research and Explorations (grant: 5190-94), and the Keck Northeastern Astronomy Consortium. Title: The Earliest Comet Photographs: Usherwood and Bond for Donati 1858 Authors: Pasachoff, J. M.; Olson, R. J. M. Bibcode: 1995AAS...187.3501P Altcode: 1995BAAS...27.1331P The first known photographs of a comet were taken in 1858. The earliest astronomical telescopic photographs, daguerreotypes from 1850-51, had been made only when the violet focus of telescopes was found. Tracking remained a problem preventing astronomical objects from being photographed. When the Harvard refractor's tracking was improved in 1858, it was used by the Bonds and colleagues to photograph Comet Donati on a collodion plate. The plate remains in the archives of the Harvard College Observatory, though the image shows only very faintly and no tail can be seen. Bond was scooped the previous night by the commercial English photographer W. Usherwood, who used a portrait camera at a much lower focal ratio to capture the comet's tail. The plate was seen and evaluated by W.C. Bond. No further comet photography took place until 1881, when P.J.C. Janssen and J.W. Draper took the first generally recognized photographs of a comet, followed by D. Gill's photographs of the Great September comet of 1882. This work was sponsored by two Senior Research Grants from the Getty Grant Program. Title: Showing Women in Astronomy Authors: Pasachoff, Jay M. Bibcode: 1995AmJPh..63..873P Altcode: No abstract at ADS Title: Book Review: The farthest things in the universe / Cambridge U Press, 1994 Authors: Pasachoff, J. M.; Spinrad, H.; Osmer, P.; Cheng, E.; Jones, T. Bibcode: 1995Obs...115..137P Altcode: No abstract at ADS Title: Book-Review - Astronomy - from the Earth to the Universe - ED.4 Authors: Pasachoff, J. M.; Mizon, B. Bibcode: 1995JBAA..105..185P Altcode: No abstract at ADS Title: Book-Review - the Farthest Things in the Universe Authors: Pasachoff, J. M.; Spinrad, H.; Osmer, P.; Cheng, E.; Glass, I. S. Bibcode: 1995MNSSA..54...46P Altcode: No abstract at ADS Title: Comets and meteors in 18th and 19th century British art and science. Authors: Pasachoff, J. M.; Olson, R. J. M. Bibcode: 1995PhyEd..30..156P Altcode: Comparing paintings, drawings and prints of comets and meteors in British works of art and scientific records of the 18th and 19th centuries brings us to a study of the relationship between science and art. Representations were sometimes naturalistic, sometimes symbolic and sometimes satirical. The British interest in images of comets and meteors, which were not clearly distinguished from each other during much of the period, coincided with the era that celebrated the progress in science exemplified by the discoveries of Newton and Halley. At the end of the period in question, the invention of photography, and its subsequent improvement to the point where faint objects like comets could be recorded, altered the dynamics. The changes in both intellectual climate and technology resulted in an increasing separation between the arts and the sciences. Title: Books-Received - Astronomy - from the Earth to the Universe - ED.4 Authors: Pasachoff, J. M. Bibcode: 1995Sci...268..136P Altcode: No abstract at ADS Title: Books-Received - the Farthest Things in the Universe Authors: Pasachoff, J. M. Bibcode: 1995Sci...268..315P Altcode: No abstract at ADS Title: Coronal Heating Studies at the 1994 Total Eclipse Authors: Pasachoff, J. M.; Babcock, B.; Reardon, K. Bibcode: 1995pist.conf...18P Altcode: No abstract at ADS Title: The Farthest Things in the Universe Authors: Pasachoff, Jay M.; Spinrad, Hyron; Osmer, Patrick; Cheng, Edward S. Bibcode: 1995ftu..book.....P Altcode: The quest for the farthest objects in the Universe remains one of the most challenging areas of modern astronomical research. Peering deeper and deeper into space reveals the most distant and powerful objects known and so unveils the embryonic epochs of the Universe not long after its birth in the Big Bang. Four world experts--chosen for their ability to communicate research astronomy at a popular level--each contributes a chapter to this lucid survey. They address the fundamental issues of scale in the Universe; the ghostly etchings seen on the cosmic background radiation; quasars and their evolution; and galaxy birth. This fascinating and accessible account offers an exceptional chance for the general audience to share in the excitement of today's forefront research of the early Universe. Title: Experiments at Putre for the November 3 Total Solar Eclipse Regimiento de Caballería Blindada No. 1 "Granaderos" Site of the International Astronomical Union Expeditions Authors: Pasachoff, J. M. Bibcode: 1995pist.conf....1P Altcode: No abstract at ADS Title: Proceedings of the international symposium on the total solar eclipse of November 3, 1994. Lake Titicaca, Bolivia, May 14-17, 1995 Authors: Raljevic, Mirko S.; Zaratti, Francesco; Pasachoff, Jay M. Bibcode: 1995pist.conf.....R Altcode: 1994QB544.94.E25... No abstract at ADS Title: Textbooks and Electronic Media Authors: Pasachoff, J. M. Bibcode: 1995HiA....10..170P Altcode: No abstract at ADS Title: Astronomy, from the Earth to the universe Authors: Pasachoff, Jay M. Bibcode: 1995aetu.book.....P Altcode: 1995QB45.P287...... No abstract at ADS Title: An Upper Limit for the Deuterium Abundance in the Halo Star HD 140283 Authors: Lubowich, D. A.; Pasachoff, Jay M.; Galloway, Robert P.; Kurucz, R. L.; Smith, Verne V. Bibcode: 1994AAS...185.9805L Altcode: 1994BAAS...26.1479L Because of the possible enhanced deuterium abundance of D/H = 2.5 10(-4) (the ISM D/H = 1.65x10(-5) ) recently reported in quasar absorption spectra, we searched for the D_alpha line at 6561 A in the metal-poor halo star HD 140283 (G2IV, [Fe/H] = -2.6; Teff= 5700K). We observed HD 140283 using the .9m KPNO coude feed and the 2.7m McDonald Observatory telescopes with echelle spectrographs having a resolution Delta lambda = .05 A/pixel with S/N= 200 and Delta lambda = .11 A/pixel with S/N = 600 respectively. We did not detect the D_alpha line and compared our results to model atmosphere calculations for this star. We estimate an upper limit of D/H < 1x10(-5) which is smaller than the primordial or and Early Galactic D/H = 8x10(-5) . Since D is destroyed via reactions with protons at T > 5x10(5) K, the atmospheric deuterium has probably been destroyed during the pre-main sequence convection phase. Because (7) Li, (9) Be, and (11) B have all been detected in this star (Li/H=1.5x10(-10) and B/H=2.9x10(-12) ) and Li is destroyed at T > 2.5x10(6) K, the temperature at the bottom of the pre-main sequence convection zone is 1x10(6) K < T < 2.5x10(6) .K Title: An answer to an earlier question Authors: Pasachoff, Jay M. Bibcode: 1994PhTea..32..453P Altcode: No abstract at ADS Title: Books-Received - the Cambridge Eclipse Photography Guide - how and where to Observe and Photograph Solar and Lunar Eclipses Authors: Pasachoff, J. M.; Covington, M. A. Bibcode: 1994Sci...264..297P Altcode: No abstract at ADS Title: The Farthest Things in the Universe Authors: Pasachoff, J. M.; Spinrad, H.; Osmer, P. S.; Cheng, E. S. Bibcode: 1994ftu..book.....P Altcode: 1994QB43.2.F37..... Report of a symposium held at the American Association for the Advancement of Science yearly meeting. Title: Coronal Morphology and Heating Mechanism Observations at Total Eclipses Through 1992 Authors: Pasachoff, J. M. Bibcode: 1994scs..conf..523P Altcode: 1994IAUCo.144..523P The author describes the change of overall coronal morphology over the sunspot cycle, using most recently the total eclipse of 30 June 1992. He describes a series of eclipse observations meant to test a model of coronal heating via surface Alfvén waves by searching for 1 Hz coronal oscillations in coronal loops in the green line. Title: Journey through the universe Authors: Pasachoff, Jay M. Bibcode: 1994jtu..book.....P Altcode: 1994QB45.P293...... No abstract at ADS Title: Total Solar Eclipses, 1994 - 1999 Authors: Pasachoff, J. M. Bibcode: 1994scs..conf..579P Altcode: 1994IAUCo.144..579P The author summarizes total solar eclipses that will occur during the 1990s. These eclipses will provide several favorable opportunities to provide coronal and other solar observations not only for intrinsic data reduction but also to compare with observations obtained from a variety of spacecraft. Title: DCN in the 50 km/s Galactic Center SGR A Molecular Cloud: Confirmation of the existence of deuterium in the Galactic Center Authors: Lubowich, D. A.; Pasachoff, Jay M.; Balonek, Thomas J.; Tremonti, Christy P.; Galloway, Robert P.; Mancuso, Ann Bibcode: 1993AAS...18311608L Altcode: 1993BAAS...25R1467L We confirm the presence of deuterium in the Galactic Center Sgr A cloud (tentative detection by Penzias (ApJ, 228, 430, 1979) with T_a(*) = 0.02 Kq 0.15 K) by observing the 1-0 and 2-1 lines of DCN in the "50 km/s" Galactic Center molecular cloud (M-0.02-.07) using the NRAO 12-m telescope. We used the 3-mm and 2-mm SIS receivers in position switching mode with 1 MHz filters, 256 MHz bandwidth, 4.1 km/s resolution at the DCN 1-0 transition, and a typical T sys = 400K. We observed a Gaussian line peak intensity T_r(*) and integrated Gaussian intensity of 0.061 Kq.007 K, 2.0 K-km/s; and 0.042 Kq.02 K, 0.91 K-km/s for the optically thin 1-0 and 2-1 DCN lines, respectively. The DCN was concentrated along the north-south ridge observed in other molecules in this cloud. We also observed H13CN, HC15N, HNC, DNC and HCO+ at the position of the DCN 1-0 peak. From the DCN/H13CN we estimate DCN/HCN = .005. The inferred D/H is estimated to be less than the local ISM value of 2 x 10(-5) , but is sensitive to the chemistry and physical conditions in the molecular cloud. These results imply that deuterated molecules D are not significantly enhanced in the GC molecular clouds and is consistant with the upper limits for atomic D obtained for the GC molecular clouds (Lubowich, Anantharamaiah, and Pasachoff, ApJ, 345, 770, 1989). The DCN/HCN we obtained is similar to that of the hot core of Orion so that D might be enhanced by fractionation and the sublimation of fossil D from grains. If there are no Galactic sources of D, then each generation of stars reduces the ISM D/H via astration and the observed D is the primordial abundance reduced by astration and mixing and possibly enhanced by the infall of primordial matter. If the rate of astration is faster in the GC as suggested by models of chemical evolution, then infall of primordial matter is a likely source of the GC deuterium. Title: Curriculum Projects and their Effects on Astronomy Education Authors: Pasachoff, Jay M. Bibcode: 1993AAS...183.6101P Altcode: 1993BAAS...25.1389P National curriculum projects can have a long-lasting and widespread effect on the teaching of astronomy in schools and thus on the supply of astronomers and on knowledge of astronomy among the general public. For example, the omission of astronomy as a requirement in 1893 by the Committee of Ten (J.L. Bishop in Pasachoff and Percy, The Teaching of Astronomy, Proc. IAU Colloq 105) and the fact that an astronomer was not included on the committee has had major and long-lasting consequences to the detriment of astronomy. Thus it is important for us to become familiar with a set of curriculum projects that are now being intensively worked on. They include the American Association for the Advancement of Sciences Project 2061: Science for All Americans, the National Science Teachers Association's Scope, Sequence, and Coordination of Secondary-School Science Education, and the National Committee on Science Education Standards and Assessment's National Science Education Standards, the last under the aegis of the National Research Council. We will discuss these projects and their impacts on astronomy with principal participants James Rutherford for the AAS, Russell Aiuto for the NSTA, and Ken Hoffmann for the NRC/NCSESA. Title: Coronal Images from the 1984 Solar Eclipse Authors: Pasachoff, Jay M.; Reardon, Kevin P.; MacKenty, John W. Bibcode: 1993SoPh..146..405P Altcode: We present digitized photographs of the white-light solar corona taken during the total solar eclipse of 22-23 November, 1984, on both calibrated black-and-white film and on color film. Conditions on site in Hula, Papua New Guinea, were exceptionally clear. The color image was used to produce an isophotal map of the inner corona, from which a flattening coefficient of 0.23 was measured. The black-and-white image was enhanced through a digital radial filter. Our images are the best processed images available from the 1984 eclipse and so provide important data for synoptic observations. Title: Books-Received - Mcgraw-Hill Encyclopedia of Astronomy - ED.2 Authors: Parker, S. P.; Pasachoff, J. M. Bibcode: 1993Sci...261.1189P Altcode: No abstract at ADS Title: Rediscovering the Color of the Crab Nebula Authors: Malin, David; Pasachoff, Jay M. Bibcode: 1993S&T....86...43M Altcode: 1993S&T....86a..43M No abstract at ADS Title: CCD Observations of SN1993J in M81 from the Keck Northeast Astronomy Consortium Authors: Benson, P. J.; Little-Marenin, I. R.; Herbst, W.; Salzer, J. J.; Vinton, G.; Elmegreen, D.; Chromey, F.; Balonek, T. J.; Strom, C.; Tremonti, C.; Hanson, G. J.; Ratcliff, S.; Winkler, P. F.; Gloria, K.; Kwitter, K.; Pasachoff, J. M.; Partan, J.; Crawford, F.; Elmegreen, B.; Wells, L.; Tweedy, R. Bibcode: 1993AAS...182.2916B Altcode: 1993BAAS...25..835B We present UBVRI photometry for SN 1993J, as well as data on its likely progenitor. The post-explosion data were obtained with CCDs attached to telescopes (0.4 to 0.6m) on the campuses of the Keck Northeast Astronomy Consortium (KNAC) and on the Burrell Schmidt telescope of the Warner and Swasey Observatory, Case Western Reserve University, at KPNO by the authors and their undergraduate students. We have obtained a fairly well-sampled light curve of the early stages in the outburst, including the rapid decay (0.30 magnitude per day at V) from the initial maximum and the subsequent slower rise to the secondary maximum. The position of the supernova, as measured on our images agrees to within 0.1 arc-sec with the position of a faint, apparently stellar image, taken with the 0.9m telescope at KPNO on 1992 October 2. The brightness of this object (Perelmuter, IAUC 5736; Filippenko, IAUC 5737; Humphreys et al., IAUC 5739) are consistent with its being a late-type supergiant. A series of images of M81 taken in 1992 November and 1993 February are analyzed to provide further constraints on the likely progenitor and its photometric behavior in the months before its explosion. We acknowledge the generous support of the W. M. Keck Foundation for providing the CCD cameras and workstations and for their support of astronomy at the KNAC institutions. Title: McGraw-Hill Encyclopedia of Astronomy Authors: Parker, S.; Pasachoff, J. M. Bibcode: 1993mhea.book.....P Altcode: 1993QB14.M3725..... A wide-ranging one-volume encyclopedia of astronomy; extracted from the McGraw-Hill Encyclopedia of Science and Technology Title: The Cambridge eclipse photography guide : how and where to observe and photograph solar and lunar eclipses Authors: Pasachoff, Jay M.; Covington, Michael A.; Espenak, Fred Bibcode: 1993cepg.book.....P Altcode: 1993QB121.C69...... Eclipses of the 1990s and how to observe them. Title: Books-Received - a Field Guide to the Stars and Planets Authors: Pasachoff, J. M. Bibcode: 1993Sci...260Q.706P Altcode: No abstract at ADS Title: Book Review - Exercises in Practical Astronomy Using Photographs Authors: Pasachoff, J. M. Bibcode: 1992JRASC..86..162P Altcode: 1992JRASC..86..162B No abstract at ADS Title: Book-Review - the Teaching of Astronomy Authors: Pasachoff, J. M.; Percy, J. R. Bibcode: 1992JBAA..102..175P Altcode: No abstract at ADS Title: The 1816 Solar Eclipse and the Comet 1811I in Linnell's Astronomical Album Authors: Olson, R. J. M.; Pasachoff, J. M. Bibcode: 1992JHA....23..121O Altcode: No abstract at ADS Title: The great eclipse. Authors: Pasachoff, J. M. Bibcode: 1992NaGe..181...30P Altcode: No abstract at ADS Title: Unified units Authors: Pasachoff, J. M. Bibcode: 1992Obs...112...15P Altcode: No abstract at ADS Title: Williams College, Hopkins Observatory, Williamstown, Massachusetts 01267. Report for the period Jul 1990 - Jul 1991. Authors: Pasachoff, J. M. Bibcode: 1992BAAS...24..653P Altcode: No abstract at ADS Title: Stars and planets Authors: Pasachoff, Jay M.; Menzel, Donald H. Bibcode: 1992stpl.book.....P Altcode: 1992QB64.P37....... No abstract at ADS Title: Journey through the universe Authors: Pasachoff, Jay M. Bibcode: 1992jtun.book.....P Altcode: No abstract at ADS Title: Book-Review - Journey Through the Universe Authors: Pasachoff, J. M. Bibcode: 1992Natur.355..407P Altcode: No abstract at ADS Title: Save the U.S.NAVAL-OBS. Eclipse Circulars Authors: Pasachoff, J. M. Bibcode: 1991S&T....82..342P Altcode: No abstract at ADS Title: The Williams College 1991 Total Solar Eclipse Expedition Authors: Pasachoff, J. M. Bibcode: 1991BAAS...23.1443P Altcode: No abstract at ADS Title: The CUREA 1992 Summer Program in Astrophysics at Mount Wilson Observatory Authors: Snider, J.; Bracher, K.; Briggs, J.; Mickelson, M.; Mitchell, W., Jr.; Pasachoff, J.; Snodgrass, H.; Yorka, S. Bibcode: 1991BAAS...23.1437S Altcode: No abstract at ADS Title: The Teaching of Astronomy: International Astronomical Union Colloquium 105 Authors: Pasachoff, Jay M.; Percy, John R.; French, Richard G. Bibcode: 1991AmJPh..59..667P Altcode: No abstract at ADS Title: The Sun - a Star Close UP Authors: Pasachoff, J. M. Bibcode: 1991Mercu..20...66P Altcode: No abstract at ADS Title: Access to Contemporary Research Results for Teachers of Astronomy Courses on the School and University Levels Authors: Pasachoff, J. M. Bibcode: 1991BAAS...23..930P Altcode: No abstract at ADS Title: Book-Review - Astronomy - from the Earth to the Universe Authors: Pasachoff, J. M. Bibcode: 1991S&T....81Q.279P Altcode: No abstract at ADS Title: Daylight savings. Authors: Pasachoff, J. M. Bibcode: 1991PhTea..29R..71P Altcode: No abstract at ADS Title: Fabry-Pérot line profiles in the λ5303 å and λ6374 å coronal lines obtained during the 1983 Indonesian eclipse Authors: Chandrasekhar, T.; Desai, J. N.; Ashok, N. M.; Pasachoff, Jay M. Bibcode: 1991SoPh..131...25C Altcode: During the total solar eclipse of 11 June, 1983, an imaging dual-channel Fabry-Pérot interferometer was used to obtain line profiles simultaneously in the green λ5303 Å [Fe XIV] and the red λ6374 Å [Fe X] coronal lines at various positions in the corona. Extensive microdensitometry followed by multi-Gaussian curve-fitting analysis has resulted in the determination of coronal temperatures and velocity separations between different pockets of coronal gas in the line of sight over a large extent of the corona. Fewer high temperature zones are to be found in the corona of 1983 compared with our similar green-line measurements of the solar maximum corona of 1980. The data are consistent with a temperature maximum occurring at 1.2 R⊙, as found at the 1980 eclipse, but our new data are insufficient to observe farther out than this radius and so determine the position of a maximum. The velocity field in the corona at the 1983 eclipse is less structured compared with that at the 1980 eclipse and is mainly confined to the zone 20-30km s−1. Title: Williams College, Hopkins Observatory, Williamstown, Massachusetts 01267. Report for the period Jul 1989 - Jun 1990. Authors: Pasachoff, J. M. Bibcode: 1991BAAS...23..791P Altcode: 1991BAAS...23..791. No abstract at ADS Title: Measurements of 1-Hz Coronal Oscillations at Total Eclipses and Their Implications for Coronal Heating Authors: Pasachoff, J. M. Bibcode: 1991mcch.conf...25P Altcode: No abstract at ADS Title: Undergraduate Symposium on Research in Astronomy Authors: Benson, Priscilla J.; Pasachoff, Jay M.; Wong, Alex K. Bibcode: 1991usra.conf.....B Altcode: No abstract at ADS Title: Astronomy, from the earth to the universe Authors: Pasachoff, Jay M. Bibcode: 1991aeu..book.....P Altcode: 1991QB45.P287...... No abstract at ADS Title: Historical Comets Over Bavaria: the Nuremberg Chronicle and Broadsides Authors: Olson, R. J. M.; Pasachoff, J. M. Bibcode: 1991ASSL..167.1309O Altcode: 1991cphe.conf.1309O; 1991IAUCo.116.1309O No abstract at ADS Title: The Solar Corona Over the Recent Saros Authors: Pasachoff, Jay M. Bibcode: 1991LNP...380..285P Altcode: 1991sacs.coll..285P; 1991IAUCo.130..285P We are now at both the maximum of the solar activity cycle and at the most populated part of the saros. I discuss the solar corona over the recent saros and its changes with the solar activity cycle. We consider the scientific value of eclipse studies and how they relate to other ongoing coronal studies on the sun and other stars. Title: Observing Solar Eclipses Authors: Pasachoff, J. Bibcode: 1991atq..conf...67P Altcode: No abstract at ADS Title: Coronal Structures and the Sunspot Cycle Authors: Pasachoff, Jay M. Bibcode: 1991LNP...387..283P Altcode: 1991fpsa.conf..283P Several solar eclipses must be observed to study the, corona at different phases of the solar-activity cycle. I describe a series of coronal observations at various eclipses over the most recent saros. The most recent experiment studies a mechanism of coronal heating by measuring high-frequency intensity oscillations in coronal loops in the green line. I also describe an application of the monthly variation in the daily sunspot numbers to the solar-neutrino problem. Title: Book Review: The restless sun. By Donat G. Wentzel. Smithsonian Institution Press, Washington DC, 1989. 279 pp., including indexes. ISBN 0-87474-982-4. $27.95 cloth Authors: Pasachoff, Jay M. Bibcode: 1990Icar...88..262P Altcode: No abstract at ADS Title: Book-Review - the Teaching of Astronomy Authors: Pasachoff, J. M. Bibcode: 1990S&T....80..381P Altcode: No abstract at ADS Title: Coronal Velocities from Fabry-Perot Line Profiles at the 1983 Eclipse Authors: Pasachoff, J. M.; Chandrasekhar, T.; Desai, J. N.; Ashok, N. M. Bibcode: 1990BAAS...22.1196P Altcode: No abstract at ADS Title: Book-Review - the Teaching of Astronomy Authors: Pasachoff, J. M.; Percy, J. R. Bibcode: 1990Sci...249..574P Altcode: No abstract at ADS Title: Book-Review - the Teaching of Astronomy Authors: Pasachoff, J. M.; Percy, J. R. Bibcode: 1990JBAA..100R.103P Altcode: No abstract at ADS Title: Urania Observed Authors: Fernandez, Rafael; Pasachoff, Jay M.; Volz, Robert Bibcode: 1990teas.conf..431F Altcode: 1990IAUCo.105..431F No abstract at ADS Title: Fabry-Perot Interferogram Profiles in Lambda 5303 IN Relation to Coronal Structures - 1980 and 1983 Eclipses Authors: Desai, J. N.; Raju, K. P.; Chandrasekhar, T.; Ashok, N. M.; Pasachoff, J. M. Bibcode: 1990IAUS..142..251D Altcode: No abstract at ADS Title: Astronomy in American Textbooks Authors: Pasachoff, Jay M. Bibcode: 1990teas.conf..201P Altcode: 1990IAUCo.105..201P No abstract at ADS Title: Book-Review - the Teaching of Astronomy Authors: Pasachoff, J. M.; Percy, J. R. Bibcode: 1990AstQ....7..254P Altcode: No abstract at ADS Title: Peterson first guide to the solar system Authors: Pasachoff, Jay M.; Peterson, Roger Tory; Tirion, Wil Bibcode: 1990pfgs.book.....P Altcode: No abstract at ADS Title: The teaching of astronomy Authors: Pasachoff, Jay M.; Percy, John R. Bibcode: 1990teas.conf.....P Altcode: 1990IAUCo.105.....P This book stems from the proceedings of the International Astronomical Union Colloquium 105. Every facet of the teaching of astronomy is explored by the contributors. Courses, training and teaching techniques form a large sector of the book. Practical information on computers, textbooks and astronomical equipment is given, linking in with chapters on student projects and teaching techniques. The philosophical aspects and the history of astronomy are described in a chapter entitled astronomy and culture. Popularisation of astronomy is discussed including the role of planetariums and the contribution of amateur astronomers. This comprehensive and well illustrated book offers a unique overview of international teaching technology and expertise that will serve as a lasting guide to astronomers involved in education. Title: Is Comet p/ Halley of 684-A.D. Recorded in the Nuremberg Chronicle Authors: Olson, R. J. M.; Pasachoff, J. M. Bibcode: 1989JHA....20..171O Altcode: No abstract at ADS Title: A Search for Localized Sources of Noncosmological Deuterium near the Galactic Center Authors: Lubowich, D. A.; Anantharamaiah, K. R.; Pasachoff, Jay M. Bibcode: 1989ApJ...345..770L Altcode: The VLA at the 92 cm D I hyperfine transition was used to search for a possible localized concentration of atomic deuterium near the Galactic center over a velocity range of + or - 180 km/s. The search yielded an upper limit for the D column density N(D) = 7.78 x 10 to the 16th T(s)/sq cm where T(s) is the spin temperature of the D I hyperfine lines. For the smaller velocity range of + or - 30 km/s, a more sensitive upper limit of N(D) = 3.12 x 10 to the 16th T(s)/sq cm is obtained. If D is associated with the H I clouds to the Galactic center, an upper limit for the D/H ratio of 0.0043 is obtained for the clouds at V = 20 km/s and 50 km/s. If a significant fraction of the D exists in atomic form in molecular clouds, the upper limits are 1.2 x 10 to the -7th for the V = 20 km/s molecular cloud near the Galactic center and 8.3 x 10 to the -7th for the V = 50 km/s molecular cloud near the Galactic center. These results are consistent with the D observed in the Galactic center and the ISM being primarily cosmological in origin. Title: CUREA: The Consortium for Undergraduate Research and Education in Astronomy Authors: Snider, J.; Bracher, K.; Meyers, K.; Mickelson, M.; Mitchell, W., Jr.; Naftilan, S.; Pasachoff, J.; Snodgrass, H.; Yorka, S.; Zook, A. Bibcode: 1989BAAS...21.1065S Altcode: No abstract at ADS Title: Astrophysics of the Sun Authors: Zirin, Harold; Pasachoff, Jay M. Bibcode: 1989AmJPh..57..669Z Altcode: No abstract at ADS Title: A Search for Remnant Planetary Nebulae around Hot sdO Stars Authors: Kwitter, Karen B.; Massey, Philip; Congdon, Charles W.; Pasachoff, Jay M. Bibcode: 1989AJ.....97.1423K Altcode: Spectroscopic and imaging searches for nebular emission associated with a sample of hot subdwarf O (sdO) stars have been carried out. Of 45 stars searched, no evidence of such nebulosity is found in 44. The single exception is RWT 152, around which a planetary nebula had been discovered previously. These negative results place constraints on the evolutionary history of these stars. Title: Hopkins Observatory, Williams College, Williamstown, Massachusetts 01267. Report for the 1987 - 1988 academic year. Authors: Pasachoff, J. M. Bibcode: 1989BAAS...21..680P Altcode: No abstract at ADS Title: The need to observe the distribution of interstellar deuterium. Authors: Pasachoff, J. M.; Vidal-Madjar, A. Bibcode: 1989ComAp..14...61P Altcode: The abundance of deuterium is linked with nucleosynthesis in the first 1000 seconds of the history of the universe. Though the interstellar deuterium abundance is known in the solar neighborhood from ultraviolet studies of Lyman lines, it is poorly known in other parts of the Galaxy. Determining the deuterium abundance gradient in the Galaxy, or extending observations to distant galaxies, should resolve the question of non-cosmological deuterium formation and should give cosmological insights. Title: Contemporary astronomy Authors: Pasachoff, Jay M. Bibcode: 1989coas.book.....P Altcode: 1989QB45.P29....... No abstract at ADS Title: Teaching about the planets at (large) scale Authors: Pasachoff, Jay M. Bibcode: 1989PhTea..27...38P Altcode: No abstract at ADS Title: Book-Review - Peterson First Guide to Astronomy Authors: Pasachoff, J. M.; Tirion, W.; Brickman, R.; Byrd, D. Bibcode: 1989S&T....77...38P Altcode: No abstract at ADS Title: Deuterium in the Universe (May, 1974) Authors: Pasachoff, Jay M.; Fowler, William A. Bibcode: 1989ppc..book..151P Altcode: No abstract at ADS Title: Book-Review - Peterson First Guides - Astronomy Authors: Pasachoff, J. M.; Hilditch, R. Bibcode: 1988Obs...108..250P Altcode: No abstract at ADS Title: Up-to-date astronomy revisited Authors: Pasachoff, Jay M. Bibcode: 1988PhTea..26..424P Altcode: No abstract at ADS Title: Historical Comets of the "Nuremberg Chronicle" Authors: Pasachoff, J. M.; Olson, R. J. M. Bibcode: 1988BAAS...20..991P Altcode: No abstract at ADS Title: A Search for Remnant Planetary Nebulae Around Hot Subdwarf O Stars Authors: Kwitter, K. B.; Massey, P.; Congdon, C. W.; Pasachoff, J. M. Bibcode: 1988BAAS...20.1052K Altcode: No abstract at ADS Title: Book-Review - a Field Guide to Stars and Planets Authors: Menzel, D. H.; Pasachoff, J. M.; Tirion, W.; Soltynski, M. Bibcode: 1988MNSSA..47..161M Altcode: No abstract at ADS Title: Peterson first guide to astronomy maps Authors: Pasachoff, Jay M.; Peterson, Roger Tory; Tirion, Wil; Brickman, Robin Bibcode: 1988pfga.book.....P Altcode: 1988QB46.P376...... No abstract at ADS Title: The Peterson first guide to astronomy. A simplified field guide to the stars, planets and the universe. Authors: Pasachoff, J. M. Bibcode: 1988pfgt.book.....P Altcode: No abstract at ADS Title: New telescopes view the sky. Authors: Pasachoff, J. M. Bibcode: 1988itod....2....6P Altcode: Concerning the 4.2-m William Herschel Telescope, Roque de los Muchachos Observatory, La Palma, Canary Islands. Title: New Information on Comet p/ Halley as Depicted by Giotto DI Bondone and Other Western Artists Authors: Olson, R. J. M.; Pasachoff, J. M. Bibcode: 1987A&A...187....1O Altcode: Artists' depictions of comets provide the only visual evidence of historical comets, most notably of Halley's Comet. In this paper we discuss the visual evidence of comet P/Halley at several passages through that of 1301 and compare it with descriptions and modern images. Since it was first recognized that Giotto di Bondone painted a comet in place of the Star of Bethlehem and suggested that this was a portrait of the 1301 apparition of comet Halley (Olson, 1979), a great deal of new information has come to light. We present a synopsis of the textual, visual, and astronomical evidence to support the theory that when Giotto painted his comet in the Scrovegni Chapel he was reflecting his viewing of Comet Halley in 1301. Title: A Search for Localized Sources of Deuterium Near the Galactic Center Authors: Lubowich, D. A.; Anantharamaiah, K. R.; Pasachoff, J. M. Bibcode: 1987BAAS...19Q1076L Altcode: No abstract at ADS Title: Addendum - High-Frequency Oscillations in the Corona Observed at the 1983 Eclipse Authors: Pasachoff, J. M.; Ladd, E. F. Bibcode: 1987SoPh..110..412P Altcode: No abstract at ADS Title: Sesquicentennial of Williams College's Hopkins Observatory Authors: Pasachoff, J. M.; Kwitter, K. B.; Friend, D. Bibcode: 1987BAAS...19R1065P Altcode: No abstract at ADS Title: High-Frequency Oscillations in the Corona Observed at the 1983 Eclipse Authors: Pasachoff, Jay M.; Ladd, Edwin F. Bibcode: 1987SoPh..109..365P Altcode: We detected excess oscillatory power at 0.25-2.0 Hz in a coronal loop in the 1983 Indonesian total solar eclipse. In this second-generation experiment enlarging upon the work of Pasachoff and Landman (1984), we observed in two frequency channels, one coronal and one continuum, to monitor atmospheric and instrumental effects. We briefly discuss the effects of an oscillation near 1 Hz on the coronal heating problem. Title: Book-Review - Astronomy - from the Earth to the Universe Authors: Pasachoff, J. M. Bibcode: 1987S&T....74..263P Altcode: No abstract at ADS Title: Timing of the 1984 Total Solar Eclipse and the Size of the Sun Authors: Pasachoff, Jay M.; Nelson, Brant O. Bibcode: 1987SoPh..108..191P Altcode: We report accurate timing of second and third contacts made from videotape of the total solar eclipse of 23 November, 1984, observed in Papua New Guinea. The magnitude of the discrepancies between predicted and observed times indicates that the secular change in the size of the Sun reported by some observers is within the uncertainty. Title: Fabry-Perot Line Profiles in 5303A and 6374A Coronal Lines Obtained during the 1983 Eclipse Authors: Sekhar, T. C.; Desai, J. N.; Ashok, N. M.; Pasachoff, J. M. Bibcode: 1987BASI...15R..18S Altcode: No abstract at ADS Title: Astronomy, from the earth to the universe Authors: Pasachoff, Jay M. Bibcode: 1987afet.book.....P Altcode: 1987QB45.P287...... No abstract at ADS Title: Interpreting Quasar Redshifts Authors: Maltby, Per; Pasachoff, Jay M.; Kierein, John Bibcode: 1987PhT....40c.110M Altcode: No abstract at ADS Title: New Information on Comet Halley as Depicted by Giotto DI Bondone and Other Western Artists Authors: Olson, Roberta J.; Pasachoff, Jay M. Bibcode: 1986ESASP.250c.201O Altcode: 1986ehc3.conf..201O Artists' depictions of comets provide the only visual evidence of historical comets, most notably of Halley's comet. The authors discuss the visual evidence of comet Halley at several passages (684, 1066, 1145, 1222, 1301, 1456, 1531, 1682, 1759 and 1835) and compare these with descriptions and modern images. They also include their own images made with the Canada-France-Hawaii Telescope. Since it was first recognized that Giotto di Bondone painted a comet in place of the Star of Bethlehem and suggested that this was a portrait of the 1301 apparition of comet Halley. Title: A scientist's view of cosmology Authors: Pasachoff, Jay M. Bibcode: 1986PhTea..24..569P Altcode: No abstract at ADS Title: Book-Review - a Brief View of Astronomy Authors: Pasachoff, J. M.; McNally, D. Bibcode: 1986SSRv...44..408P Altcode: No abstract at ADS Title: Book-Review - Contemporary Astronomy Authors: Pasachoff, J. M.; Hill, P. W. Bibcode: 1986Obs...106..121P Altcode: No abstract at ADS Title: Historical Studies of Halley's and Other Comets via Artists' Depictions Authors: Pasachoff, J. M.; Olson, R. J. M. Bibcode: 1986BAAS...18..792P Altcode: No abstract at ADS Title: Book-Review - Contemporary Astronomy 3RD-ED Authors: Pasachoff, J. Bibcode: 1986Mercu..15...94P Altcode: No abstract at ADS Title: The X-Ray Universe Authors: Tucker, Wallace; Giacconi, Riccardo; Pasachoff, Jay M. Bibcode: 1986PhT....39f..87T Altcode: No abstract at ADS Title: Gamma Ray Astronomy Authors: Hiller, Rodney; Pasachoff, Jay M. Bibcode: 1986PhT....39g..71H Altcode: No abstract at ADS Title: A brief view of astronomy Authors: Pasachoff, Jay M. Bibcode: 1986bva..book.....P Altcode: 1986QB43.2.P357.... No abstract at ADS Title: Periodic Comet Halley (1982i) Authors: Hua, T.; Grundseth, B.; Pasachoff, J. M.; Ladd, E.; Schroder, M. F.; Pastoriza, M.; Dottori, H.; Kepler, S. O.; Bergmann, T. S.; Ducati, J. R.; Livi, S. H. B.; Schmidt, A.; Bonatto, C.; Costa, R. D. D.; Kosai, H.; Bortle, J.; Merlin, J. -C.; Krisciunas, K.; Cavagna, M.; Keen, R.; Green, D. W. E. Bibcode: 1985IAUC.4126....2H Altcode: T. Hua and B. Grundseth, Canada-France-Hawaii Telescope; and J. M. Pasachoff and E. Ladd, Hopkins Observatory, report observations of P/Halley on Oct. 23.3 UT with the photon-counting camera at the f/8 Cassegrain focus of the 3.6-m CFHT on Mauna Kea. Images with the CN (387.1 nm) filter show diffuse emission with central area 30" in size. Continuum emission through a 0.8-nm filter at 500.7 nm and a 0.47-nm H-alpha filter fills the field and is more peaked as is CO+ emission through the 426-nm P/Halley standard filter. M. F. Schroder, M. Pastoriza, H. Dottori, S. O. Kepler, T. S. Bergmann, J. R. Ducati, S. H. B. Livi, A. Schmidt, C. Bonatto and R. D. D. Costa, Departamento de Astronomia, Universidade Federal do Rio Grande do Sul, Brazil, find B = 15.3 and V = 14.8 (both +/- 0.2, total magnitude) on Sept. 22.29 UT from plates taken at the 1.6-m telescope of the Observatorio Astrofisico Brasileiro. H. Kosai, Tokyo Astronomical Observatory, reports V = 14.0 with a 30" diaphragm on the 0.91-m Okayama telescope on Sept. 13.67 UT. Total visual magnitude estimates: Oct. 7.39 UT, 11.0 (J. Bortle, Stormville, NY, 0.32-m reflector); 10.94, 11.0 (J.-C. Merlin, Le Creusot, France, 0.40-m reflector); 14.52, 10.8 (K. Krisciunas, Hilo, HI, 0.15-m reflector); 17.95, 10.2 (M. Cavagna, Valcava, Italy, 20 x 80 binoculars); 20.40, 9.1 (R. Keen, Mt. Thorodin, CO, 8 x 40 binoculars); 24.38, 8.5 (D. W. E. Green, Oak Ridge Observatory, 20 x 80 binoculars). Title: The Comet Book Authors: Chapman, Robert D.; Pasachoff, Jay M. Bibcode: 1985PhTea..23..387C Altcode: No abstract at ADS Title: Contemporary astronomy Authors: Pasachoff, Jay M. Bibcode: 1985coas.book.....P Altcode: 1985QB45.P29....... No abstract at ADS Title: The Invisible Unviverse: Probing the Frontiers of Astrophysics Authors: Field, George B.; Chaisson, Eric J.; Pasachoff, Jay M. Bibcode: 1985PhT....38j.107F Altcode: No abstract at ADS Title: A brief view of astronomy. Authors: Pasachoff, J. M. Bibcode: 1985bva..book.....P Altcode: No abstract at ADS Title: The Planetary Nebula around the sdO Star RWT 152 Authors: Pasachoff, J. M.; Kwitter, K. B.; Massey, P. Bibcode: 1984BAAS...16..994P Altcode: No abstract at ADS Title: Book-Review - a Field Guide to the Stars and Planets Authors: Menzel, D. H.; Pasachoff, J. M. Bibcode: 1984S&T....68..227M Altcode: No abstract at ADS Title: Coelostat and heliostat: alignment and use for eclipse and other field purposes Authors: Pasachoff, Jay M.; Livingston, William C. Bibcode: 1984ApOpt..23.2803P Altcode: No abstract at ADS Title: Coelostat and heliostat: Theory of alignment Authors: Demianski, M.; Pasachoff, J. M. Bibcode: 1984SoPh...93..211D Altcode: For perfectly aligned heliostats and coelostats tracking at the solar rate and half the solar rate, respectively, the solar beam has no translational motion. But, particularly in the field at eclipses, it is not possible to align heliostats and coelostats with infinite precision. We derive the effect of small misalignments on the translational motion of the beam, and give tables to allow the calculation of the accuracy to which the instruments must be mounted and adjusted to attain a desired accuracy over a given duration. Further, we show how to derive the necessary adjustments to improve alignment, given measurements of the tracking error. Title: High Frequency Coronal Oscillations and Coronal Heating Authors: Pasachoff, J. M.; Landman, D. A. Bibcode: 1984SoPh...90..325P Altcode: At the 1980 total solar eclipse, we searched for high-frequency (0.1-2 Hz) oscillations in the intensity of the 5303-Å coronal green line, as a test of predictions of theories of coronal heating via magnetohydrodynamic waves. Portions of the image 2.5- or 5-arc sec across were fed to cooled photomultipliers using fiber-optic probes. We detected excess power in Fourier transforms of the data for the region between 0.5 and 2 Hz at the level of 1% or 2% of the incident power. Such oscillations could be associated with Alfvén waves that are trapped on loops a few thousand kilometers long or with fast waves that are trapped on loops a few thousand kilometers in diameter. Additional observations at the 1983 eclipse are planned to resolve atmospheric and instrumental contributions. Title: Fabry-Perot interferometric observations of the coronal red and greenlines during the 1983 Indonesian eclipse. Authors: Chandrasekhar, T.; Ashok, N. M.; Desai, J. N.; Pasachoff, J. M.; Sivaraman, K. R. Bibcode: 1984ApOpt..23..508C Altcode: A dual-channel Fabry-Perot interferometric system was used to study simultaneously the coronal emission lines at 5303 Å (Fe XIV) and at 6374 Å (Fe X). Initial results indicate an emission corona confined largely within 1.2 R_sun;. Doppler temperatures derived from the width of the 5303-Å line appear to be appreciably lower than similar temperatures determined during the solar-maximum eclipse of 1980. Title: Book-Review - Astronomy - from the Earth to the Universe Authors: Pasachoff, J. M.; Boyle, R. J. Bibcode: 1984S&T....68..423P Altcode: No abstract at ADS Title: Book-Review - Astronomy - from the Earth to the Universe Authors: Pasachoff, J. Bibcode: 1984Mercu..13...91P Altcode: No abstract at ADS Title: Book-Review - a Field Guide to the Stars and Planets - ED.2 Authors: Menzel, D. H.; Pasachoff, J. M. Bibcode: 1984Natur.309..477M Altcode: No abstract at ADS Title: Book-Review - a Field Guide to the Stars and Planets Authors: Menzel, D. H.; Pasachoff, J. M.; de Jager, C. Bibcode: 1984SSRv...38..185M Altcode: No abstract at ADS Title: Book-Review - Sun and Planetary System Authors: Fricke, W.; Teleki, G.; Pasachoff, J. M. Bibcode: 1984ApL....24..129F Altcode: No abstract at ADS Title: Book-Review - Teacher's Guide to Astronomy - from the Earth to the Universe Authors: Pasachoff, J. M.; van der Hucht, K. A. Bibcode: 1984SSRv...37..402P Altcode: No abstract at ADS Title: Book-Review - a Field Guide to the Stars and Planets - ED.2 Authors: Menzel, D.; Pasachoff, J. Bibcode: 1984Mercu..13S..86M Altcode: No abstract at ADS Title: Book-Review - Astronomy from the Earth to the Universe Authors: Pasachoff, J. M.; van der Hucht, K. A. Bibcode: 1983SSRv...36..420P Altcode: No abstract at ADS Title: On the Balmer: Paschen ratio in prominences Authors: Pasachoff, Jay M.; Pilger, Eric J.; Platt, Stephen R. Bibcode: 1983SoPh...89...31P Altcode: Vidicon data for the intensities of Balmer and Paschen lines for n = 11 to 18 indicate a line ratio within 1σ of the theoretical value of 3.27, calculated with the assumptions of an optically thin atmosphere and angular momentum substates populated according to their statistical weights. The observed value is not consistent with the value of 8 reported in some early work, or with the model that higher angular momentum states have low populations. Title: POST-USE REVIEW: Astronomy: From the Earth to the Universe Authors: Pasachoff, Jay M.; Marschall, Laurence A. Bibcode: 1983AmJPh..51.1054P Altcode: No abstract at ADS Title: Book-Review - Astronomy - from the Earth to the Universe Authors: Pasachoff, J. Bibcode: 1983Sci...220..402P Altcode: No abstract at ADS Title: Book-Review - Astronomy - from the Earth to the Universe ED.2 Authors: Pasachoff, J.; Hughes, D. W. Bibcode: 1983Natur.302..186P Altcode: No abstract at ADS Title: A field guide to the stars and planets Authors: Menzel, Donald Howard; Pasachoff, Jay M. Bibcode: 1983fgts.book.....M Altcode: No abstract at ADS Title: Space Astronomy on Videodisk Authors: Pasachoff, Jay M. Bibcode: 1983S&T....65...32P Altcode: No abstract at ADS Title: Book-Review - Astronomy - from the Earth to the Universe Authors: Pasachoff, J. M. Bibcode: 1983S&T....65Q.242P Altcode: No abstract at ADS Title: Astronomy, from the earth to the universe Authors: Pasachoff, Jay M. Bibcode: 1983afeu.book.....P Altcode: 1983QB45.P287...... No abstract at ADS Title: Teacher's guide to astronomy: from the earth to the universe. Authors: Pasachoff, J. M. Bibcode: 1983tgta.book.....P Altcode: No abstract at ADS Title: Book-Review - Astronomy - from the Earth to the Universe - ED.2 Authors: Pasachoff, J.; Fraknoi, A. Bibcode: 1983Mercu..12...88P Altcode: No abstract at ADS Title: Book-Review - the Cambridge Encyclopedia of Earth Sciences Authors: Smith, D. G.; Pasachoff, J. M. Bibcode: 1983S&T....65..234S Altcode: No abstract at ADS Title: Book-Review - Contemporary Astronomy - ED.2 Authors: Pasachoff, J. M. Bibcode: 1982Natur.298..310P Altcode: No abstract at ADS Title: Letters: Ikeya-Seki, Its Authors: Seargent, David A. J.; Pasachoff, Jay M. Bibcode: 1982CNSMP..33....2S Altcode: No abstract at ADS Title: Book Review: Invitation of Physics Authors: Pasachoff, J. M.; Kutner, M.; Mewe, R. Bibcode: 1982SSRv...31..457P Altcode: No abstract at ADS Title: Erratum - Book-Review - Our Cosmic Universe Authors: Kraus, J.; Pasachoff, J. Bibcode: 1982S&T....63Q...5K Altcode: No abstract at ADS Title: Book Review: Contemporary Astronomy Authors: Pasachoff, J. M.; Houziaux, L. Bibcode: 1982SSRv...31..459P Altcode: No abstract at ADS Title: Book-Review - Contemporary Astronomy Authors: Pasachoff, J. M.; Lestrade, J. P. Bibcode: 1982S&T....63..156P Altcode: No abstract at ADS Title: Hopkins Observatory, Williams College, Williamstown, Massachusetts 01267. Report for the 1980 - 1981 academic year. Authors: Pasachoff, J. M. Bibcode: 1982BAAS...14..206P Altcode: No abstract at ADS Title: Astronomical Data Bank - the Largest Optical Telescopes Authors: Pasachoff, J. Bibcode: 1982Mercu..11..142P Altcode: No abstract at ADS Title: Helium excitation in quiescent prominences. Authors: Landman, D. A.; Bernat, A. P.; Pasachoff, J. M. Bibcode: 1981BAAS...13R.552L Altcode: No abstract at ADS Title: Helium Excitation in Quiescent Prominences Authors: Landman, D. A.; Bernat, A. P.; Pasachoff, J. M. Bibcode: 1981BAAS...13..552L Altcode: No abstract at ADS Title: Hopkins Observatory, Williams College, Williamstown, Massachusetts 01267. Report for the 1979 - 1980 academic year. Authors: Pasachoff, J. M.; Kwitter, K. B. Bibcode: 1981BAAS...13..157P Altcode: No abstract at ADS Title: Book-Review - Invitation to Physics Authors: Pasachoff, J. M.; Kutner, M. L. Bibcode: 1981S&T....62R.156P Altcode: No abstract at ADS Title: Invitation to physics. Authors: Pasachoff, J. M.; Kutner, M. L. Bibcode: 1981itp..book.....P Altcode: No abstract at ADS Title: Book-Review - Contemporary Astronomy Authors: Pasachoff, J. M. Bibcode: 1981Sci...213.1002P Altcode: No abstract at ADS Title: Book-Review - Our Cosmic Universe Authors: Kraus, J.; Pasachoff, J. Bibcode: 1981S&T....62..469K Altcode: No abstract at ADS Title: Book-Review - Contemporary Astronomy Authors: Pasachoff, J. M. Bibcode: 1981S&T....62..361P Altcode: No abstract at ADS Title: Contemporary astronomy Authors: Pasachoff, Jay M. Bibcode: 1981coas.book.....P Altcode: 1981QB45.P29....... No abstract at ADS Title: Projects and Demonstrations in Astronomy Authors: Tattersfield, Donald; Pasachoff, Jay M. Bibcode: 1981AmJPh..49...93T Altcode: No abstract at ADS Title: Preliminary Report of 1980 Eclipse - Coronal Oscillations Experiment Authors: Pasachoff, J. M.; Landman, D. A. Bibcode: 1980BASI....8..137P Altcode: No abstract at ADS Title: An Eclipse Search for 1-10 Hz Temporal Variations in Coronal Loops Authors: Pasachoff, J. M.; Landman, D. A.; Schierer, J. P. Bibcode: 1980BAAS...12Q.793P Altcode: No abstract at ADS Title: Turbulence in the dust cloud L134 - High-resolution observations of 6 centimeter formaldehyde absorption Authors: Dickman, R. L.; Kutner, M. L.; Pasachoff, J. M.; Tucker, K. D. Bibcode: 1980ApJ...238..853D Altcode: Observations of 6 cm formaldehyde absorption were made at high spatial and velocity resolution toward the central regions of the dust cloud Lynds 134. A least-squares fit to the hyperfine manifold of each spectrum yielded precise υLSR values at each position; these show no evidence of positional variation. This suggests that if previously observed smooth shifts in υLSR (which occur over a much larger portion of the cloud than observed here) are in fact due to rotation, this rotation is not carried into the most heavily obscured parts of the cloud.

The fit procedure also yielded precise values for the line velocity dispersion at each position. These vary significantly over the cloud core. These results are used to discuss turbulent models of the cloud velocity field. In the absence of an energy source, the resulting picture of the cloud must be regarded as highly improbable. One or more embedded T Tauri stars undergoing mass loss could account for the turbulent dissipation expected for the cloud, and the presence of such stars is not observationally excluded. The dynamical consistency of such a model remains to be established, however. We also briefly discuss the observations in terms of a systematic velocity field for the cloud. Subject headings: interstellar: molecules nebulae: individual Title: Book-Review - Astronomy - from the Earth to the Universe Authors: Pasachoff, J. M.; Hughes, D. W. Bibcode: 1980Natur.283..913P Altcode: No abstract at ADS Title: Book-Review - Astronomy - from the Earth to the Universe Authors: Pasachoff, J. M.; Andrews, P. J. Bibcode: 1980Obs...100R..48P Altcode: No abstract at ADS Title: Book-Review - Astronomy now Authors: Pasachoff, J. M.; Warasila, R. L. Bibcode: 1980ApL....20..148P Altcode: No abstract at ADS Title: Hopkins-Observatory / Williams-College Authors: Pasachoff, J. M. Bibcode: 1980BAAS...12..129P Altcode: No abstract at ADS Title: Book-Review - Astronomy now Authors: Pasachoff, J. M.; Andrews, P. J. Bibcode: 1980Obs...100Q..48P Altcode: No abstract at ADS Title: Book-Review - Astronomy : from the Earth to the Universe Authors: Pasachoff, J. Bibcode: 1980Mercu...9S..20P Altcode: No abstract at ADS Title: Book-Review - University Astronomy Authors: Pasachoff, J. M.; Kutner, M. L.; Zimmermann, R. E. Bibcode: 1980S&T....60..229P Altcode: No abstract at ADS Title: Some tests of astrology. Authors: Pasachoff, J. Bibcode: 1980Mercu...9..137P Altcode: No abstract at ADS Title: Book-Review - Astronomy Authors: Pasachoff, J. M. Bibcode: 1980Sci...207..174P Altcode: No abstract at ADS Title: The Maximum Eclipse - 1980FEB16 Authors: Ohno, H.; Fujii, A.; Tomioka, H.; Sperling, N.; Marschall, L. A.; Allan, R. P.; Lipschutz, S.; Brooks, E.; Gerber, L.; van den Bergh, S.; van den Bergh, G.; Pasachoff, J. Bibcode: 1980S&T....59..383O Altcode: No abstract at ADS Title: Popular Open Universe Authors: Pasachoff, J. M. Bibcode: 1980SciN..117..227P Altcode: No abstract at ADS Title: Response to ''Astronomical meaning of a tropical year'' Authors: Pasachoff, Jay M. Bibcode: 1979AmJPh..47.1017P Altcode: No abstract at ADS Title: Neutrinos for Interstellar Communication Authors: Pasachoff, Jay M.; Kutner, Marc L. Bibcode: 1979CosSe...1....2P Altcode: A method of interstellar communication employing neutrinos is presented and a brief history of the discovery of the neutrino is given. Advantages and disadvantages of neutrino communication are discussed emphasizing both the high cost and the difficulty in generating neutrino beams by means of proton beams impinging on targets (steel or aluminum shields) in large accelerators. The deep underwater muon and neutrino detection system is examined as well as a block diagram describing the neutrino communication system. Title: IUE and the Search for a Lukewarm Corona Authors: Pasachoff, J. M.; Linsky, J. L.; Haisch, B. M.; Boggess, A. Bibcode: 1979S&T....57..438P Altcode: The use of the International Ultraviolet Explorer (IUE) to search for stars having neither a hot corona nor a cool outer atmosphere, but a lukewarm corona is outlined. An interactive computer system permits extensive analysis of the data immediately after transmission to earth, allowing the results of one exposure to influence the taking of subsequent exposures. The observation program is illustrated for the star HR 1099, noting that observations were taken while previous spectra were being analyzed. Observations of many stars of spectral types G and K lead to the construction of a border region on the Hertzsprung-Russell diagram between stars with hot coronas and those with cool outer atmospheres. Stars lying near this border region were then observed; however, none with lukewarm coronas was found. The interactive control facility in the satellite control room is considered an important factor in the efficient implementation of the search procedure. Title: The future of the universe Authors: Pasachoff, Jay M. Bibcode: 1979PhTea..17..291P Altcode: Olber's paradox is discussed in terms of Hubble's law, and the question of the closure of the universe is considered in light of recent experimental observations. (AIP) Title: Laboratory Exercises in Astronomy -- Cepheid Variables and the Cosmic Distance Scale Authors: Pasachoff, Jay M.; Goebel, Ronald W. Bibcode: 1979S&T....57..241P Altcode: No abstract at ADS Title: Book-Review - Van-Nostrand Scientific Encyclopedia ED.5 Authors: Pasachoff, J. Bibcode: 1979ApL....20..112P Altcode: No abstract at ADS Title: Teacher's guide to Astronomy, from the Earth to the universe Authors: Pasachoff, Jay M. Bibcode: 1979tasg.book.....P Altcode: No abstract at ADS Title: Repechage Authors: Pasachoff, Jay M. Bibcode: 1979afeu.book...67P Altcode: A method is discussed of enhancing student learning by providing an opportunity for students to provide corrected answers to questions gotten wrong on examinations, with up to half credit awarded back. However, if the course is graded on a curve, if all students got half credit back, their relative scores and thus their grades would remain the same. The method thus provides an incentive for students to participate in the repechage, a term from the sport of crew. Title: Piaget Authors: Pasachoff, Jay M. Bibcode: 1979afeu.book...65P Altcode: Teachers of astronomy often misinterpret the reliability of Piaget's conclusions about concrete and abstract reasoning for young students. This misinterpretation can result in interesting material being excluded from teaching. The discussion here gives some references and broader conclusions evaluating Piaget's work and providing alternatives. Title: Book-Review - University Astronomy Authors: Pasachoff, J.; Kutner, M. L.; Nicolson, I. Bibcode: 1979JBAA...90...87P Altcode: No abstract at ADS Title: Hopkins Observatory, Williams College, Williamstown, Massachusetts 01267. Report for the 1978 - 1979 academic year. Authors: Pasachoff, J. M. Bibcode: 1979BAAS...11..128P Altcode: No abstract at ADS Title: Astronomy, from the Earth to the universe Authors: Pasachoff, Jay M. Bibcode: 1979afeu.book.....P Altcode: 1979QB45.P287...... No abstract at ADS Title: Contemporary Astronomy Authors: Pasachoff, Jay M. Bibcode: 1978AmJPh..46.1084P Altcode: No abstract at ADS Title: Spatial structure in lines in the 3398 3526 å region at the extreme limb: Observation, identification and interpretation Authors: Canfield, R. C.; Pasachoff, J. M.; Stencel, R. E.; Beckers, J. M. Bibcode: 1978SoPh...58..263C Altcode: We have obtained spectrograms of high spatial and spectral resolution of the extreme solar limb, using the vacuum tower telescope of Sacramento Peak Observatory. We have identified emission lines in the range 3398-3526 Å, and classified them according to intensity, spatial structure (intensity variation), and profile. Some lines show spatial intensity variation; others do not. We show that this effect is related to the abundance of the element responsible for the line and the mean lower-level excitation potential of interlocked lines. We explain the effect in terms of radiative interlocking with other lines, as well as the characteristic size of the volume contributing to the mean intensity. Title: Review of Publications Student Guide to Contemporary Astronomy Authors: Pasachoff, Jay M.; Kutner, Marc L.; Pasachoff, Naomi Bibcode: 1978JRASC..72R.117P Altcode: No abstract at ADS Title: Review of Publications Contemporary Astronomy Authors: Pasachoff, Jay M. Bibcode: 1978JRASC..72Q.117P Altcode: No abstract at ADS Title: Infrared Observations of the 1977 Total Solar Eclipse. Authors: Pasachoff, J. M.; Sanford, M. T., II; Keller, C. F., Jr. Bibcode: 1978BAAS...10..431P Altcode: No abstract at ADS Title: Hopkins Observatory, Williams College, Williamstown, Massachusetts. Report for the 1976 - 1977 academic year. Authors: Pasachoff, J. M. Bibcode: 1978BAAS...10..126P Altcode: No abstract at ADS Title: Teacher's guide to university astronomy. Authors: Pasachoff, J. M.; Kutner, M. L. Bibcode: 1978tgtu.book.....P Altcode: No abstract at ADS Title: University astronomy Authors: Pasachoff, J. M.; Kutner, Marc L. Bibcode: 1978unas.book.....P Altcode: 1978QB43.2.P36..... No abstract at ADS Title: A High Resolution Study of 6-cm Formaldehyde Absorption in L 134 Authors: Pasachoff, J. M.; Dickman, R. L.; Kutner, M. L.; Tucker, K. D. Bibcode: 1977BAAS....9..591P Altcode: No abstract at ADS Title: Hopkins Observatory, Williamstown, Massachusetts. Observatory report. Authors: Pasachoff, J. M. Bibcode: 1977BAAS....9..118P Altcode: No abstract at ADS Title: Student guide to contemporary astronomy. Authors: Pasachoff, J. M.; Kutner, M. L.; Pasachoff, N. Bibcode: 1977sgtc.book.....P Altcode: No abstract at ADS Title: Contemporary astronomy Authors: Pasachoff, Jay M. Bibcode: 1977coas.book.....P Altcode: 1977QB45.P29....... No abstract at ADS Title: Silicon vidicon spectrometry and its infrared capabilities for solar research Authors: Pasachoff, J. M.; Muzyka, D. F.; Schierer, J. P., Jr. Bibcode: 1976ApOpt..15.2884P Altcode: A description is given of the use of a rapid-scanning silicon vidicon spectrometer at the total solar eclipse of June 30, 1973. The instrument had been employed to observe the two strong IR coronal emission lines, which are forbidden lines, of Fe XIII. The ratio of the intensity of the 1074.7-nm and 1079.8-nm lines is relatively insensitive to coronal temperature and depends sensitively on the coronal electron density. Title: Fine Structure Variations in High-Spatial-Resolution Solar Spectra. Authors: Pasachoff, J. M.; Canfield, R. C.; Stencel, R. E.; Beckers, J. M. Bibcode: 1976BAAS....8..501P Altcode: No abstract at ADS Title: Infrared coronal lines : (Observations of infrared [iron XIII] at the 1973 total solar eclipse) Authors: Pasachoff, J. M.; Muzyka, D. F. Bibcode: 1976VA.....19..341P Altcode: IT HAS only been recently that vidicon systems have gained sufficient sensitivity as to allow their use in ground-based infrared studies of the solar corona. This paper reports on the use of a silicon vidicon spectrometer for ground-based eclipse studies of infrared coronal lines. Two forbidden spectral emission lines in the ground state of Fe XIII in the near infrared at 10,747 Å ( 3P 1 → 3P 0) and 10,798 Å ( 3P 2 → 3P 1) are the strongest coronal lines in line-to-continuum ratio accessible to ground-based observers. It has been shown that the ratio of the intensity of these lines is insensitive to temperature and provides a good measure of the electron density in corona since one level is radiatively and the other collisionally populated. Simultaneous observations of the 10,747 Å and 10,798 Å lines therefore provide a sensitive probe of coronal electron density. Both coronagraphic and eclipse observations of these lines have been made but all observations have been severely handicapped by the fact that the lines lie beyond the effective limit of most photographic film and on the upper end of the wavelength limit of the S-1 photocathode of the most commonly employed image tube. At the total solar eclipse of June 30, 1973 in Kenya, we observed the spectral region that included the two lines with a Tektronix J20/7J20 rapid scanning silicon vidicon spectrometer. We scanned the corona in height from 1.1 to 2.0 R⊙. We report here on the observations and their reduction, as well as describe the instrumentation and the theory of the [Fe XIII] lines. Title: Hopkins Observatory, Williamstown, Massachusetts. Observatory report. Authors: Pasachoff, J. M. Bibcode: 1976BAAS....8..111P Altcode: No abstract at ADS Title: Book reviews Authors: Grant athay, R.; Pasachoff, Jay M. Bibcode: 1975SoPh...43..513G Altcode: 1975SoPh...43..513. No abstract at ADS Title: Abstracts of papers from other journals Authors: Pasachoff, Jay M. Bibcode: 1975SoPh...43..521P Altcode: No abstract at ADS Title: Infrared Observations of the Solar Corona with a Silicon Vidicon Spectrometer. Authors: Pasachoff, J. M.; Muzyka, D. F. Bibcode: 1975BAAS....7..409P Altcode: No abstract at ADS Title: Astrophysical Concepts by Martin Hewitt. Reviewed Authors: Pasachoff, Jay M. Bibcode: 1975AmJPh..43..197P Altcode: No abstract at ADS Title: Hopkins Observatory, Williams College, Williamstown, Massachusetts. Observatory report. Authors: Pasachoff, J. M. Bibcode: 1975BAAS....7...73P Altcode: No abstract at ADS Title: Abstracts of papers from other journals Authors: Pasachoff, Jay M. Bibcode: 1974SoPh...39..267P Altcode: No abstract at ADS Title: Further observations at the interstellar deuterium frequency. Authors: Pasachoff, J. M.; Cesarsky, D. A. Bibcode: 1974ApJ...193...65P Altcode: Two sets of Sgr A observations of neutral deuterium in the direction of the galactic center are reported. A wider bandwidth was used in the second set with no significant reduction of overall noise levels. The line-peak temperature of the merged data from both years yields an upper limit for the D/H ratio of 0.00035; if the absorption is the deuterium line, this ratio will be between the above value and 0.00002. These values continue to imply cosmic densities insufficient to close the universe. Title: Hopkins Observatory, Williams College, Williamstown, Massachusetts. Observatory report. Authors: Pasachoff, J. M. Bibcode: 1974BAAS....6...60P Altcode: No abstract at ADS Title: Spatial and Spectral Structure of Chromospheric Lines Authors: Pasachoff, J. M.; Harris, F. S.; Beckers, J. M. Bibcode: 1974IAUS...56...31P Altcode: No abstract at ADS Title: The Solar Corona Authors: Pasachoff, Jay M. Bibcode: 1973SciAm.229d..68P Altcode: 1973SciAm.229...68P No abstract at ADS Title: Abstracts of papers from other journals Authors: Pasachoff, Jay M.; Uchida, Y.; Vassilyeva, G.; Henoux, J. C. Bibcode: 1973SoPh...30..273P Altcode: No abstract at ADS Title: 327 MHz observations of the galactic center: Possible detection of a deuterium absorption line. Authors: Cesarsky, D. A.; Moffet, A. T.; Pasachoff, J. M. Bibcode: 1973BAAS....5S.284C Altcode: No abstract at ADS Title: 372-MHz Observations of the Galactic Center: Possible Detection of a Deuterium Absorption Line Authors: Cesarsky, Diego A.; Moffet, Alan T.; Pasachoff, Jay M. Bibcode: 1973ApJ...180L...1C Altcode: We have observed the spectrum of radiation from the galactic center in the vicinity of the deuterium ground-state hyperfine transition. With 100 hours of observing time the spectrum shows rms fluctuations 7 X i0- of the on-source power level. An absorption feature at 327.38837 4 0.00001 MHz (corrected to the local standard of rest) has a depth of 2 X i0- of the continuum level. This feature is probably the deuterium line at VLSR = -3.7 km -1 Subject headings: abundances - hyperfine structure - interstellar matter Title: Detailed Correlation of Type III Radio Bursts with Hα Activity. I: Active Region of 22 May 1970 Authors: Kuiper, T. B. H.; Pasachoff, Jay M. Bibcode: 1973SoPh...28..187K Altcode: We compare observations of type III impulsive radio bursts made at the Clark Lake Radio Observatory with high-spatial-resolution cinematographic observations taken at the Big Bear Solar Observatory. Use of the log-periodic radio interferometer allows us to localize the radio emission uniquely. This study concentrates on the particularly active region close to the limb on 22 May 1970. Sixteen of the 17 groups were associated with some Hα activity, 11 of them with the start of such activity. Title: Hopkins Observatory, Williams College, Williamstown, Massachusetts. Observatory report. Authors: Pasachoff, J. M. Bibcode: 1973BAAS....5..129P Altcode: No abstract at ADS Title: Abstracts of papers from other journals Authors: Pasachoff, Jay M. Bibcode: 1972SoPh...26..260P Altcode: No abstract at ADS Title: Abstracts of papers from other journals Authors: De Feiter, L. D.; Pasachoff, Jay M.; Vassilyeva, G.; Gussmann, E. A.; Vassilyeva, G. J.; Henoux, J. -C.; Uchida, Y.; Namba, O. Bibcode: 1972SoPh...23..501D Altcode: No abstract at ADS Title: Helium D3 in Stellar Chromospheres. Authors: Pasachoff, J. M.; Lepler, E. C. Bibcode: 1972BAAS....4Q.235P Altcode: No abstract at ADS Title: Abstracts of papers from other journals Authors: Pasachoff, Jay M. Bibcode: 1972SoPh...22..503P Altcode: No abstract at ADS Title: Abstracts of papers from other journals Authors: Henoux, J. -C.; De Feiter, L. D.; Ambroš, P.; Pasachoff, JAY M. Bibcode: 1972SoPh...22..252H Altcode: No abstract at ADS Title: R Coronae Borealis. Authors: Pasachoff, J. M. Bibcode: 1972IAUC.2403....1P Altcode: No abstract at ADS Title: Absolute Intensity Calibrations of Solar K-Line Profiles Authors: Pasachoff, Jay M. Bibcode: 1971SoPh...19..323P Altcode: Individual K-line profiles from elements of fine structure on the surface of the Sun are calibrated absolutely. The continuum calibrations of Labs and Neckel and of Houtgast and Namba are considered, and the average K-profile is scaled to that of White and Suemoto. Title: Abstracts of papers from other journals Authors: Pasachoff, Jay M.; Vassilyeva, G. J.; Henoux, J. -C.; De Fetter, L. D. Bibcode: 1971SoPh...19..494P Altcode: No abstract at ADS Title: On K-Line Central Reversals Authors: Pasachoff, Jay M.; Zirin, Harold Bibcode: 1971SoPh...18...27P Altcode: No abstract at ADS Title: Book review Authors: Pasachoff, Jay M. Bibcode: 1971SoPh...18..177P Altcode: 1971SoPh...18..177. No abstract at ADS Title: Book Review: Astronomy and astrophysics. Edited by S. R. POTTASCH AND J. L. STEINBERG. Springer-Verlag, Berlin, Price: Institutional subscribers—DM 100 per volume; personal subscribers—DM 16 per volume Authors: Pasachoff, Jay M. Bibcode: 1971Icar...14..288P Altcode: No abstract at ADS Title: Abstracts of papers from other journals Authors: Pasachoff, Jay M.; Henoux, J. -C.; de Feiter, L. D. Bibcode: 1971SoPh...17..277P Altcode: No abstract at ADS Title: Motion picture record of the 7 March 1970 total solar eclipse. Authors: Pasachoff, J. M.; Menzel, D. H. Bibcode: 1971BAAS....3R.263P Altcode: No abstract at ADS Title: The Calibration of the Wilson-Bappu Effect on the Sun Authors: Pasachoff, Jay M. Bibcode: 1971ApJ...164..385P Altcode: A quantitative assessment of the contribution of very asymmetric spectral profiles from small areas on the solar disk to the mean K4ine profile for the Sun is now available. Implications for the ilsonBappu effect are indicated. Title: Abstracts of papers from other journals Authors: Pasachoff, Jay M.; Stepanyan, N.; Namba, O. Bibcode: 1970SoPh...13..504P Altcode: No abstract at ADS Title: Fine structure in Ca ii on the solar disc Authors: Pasachoff, Jay M. Bibcode: 1970SoPh...12..202P Altcode: High-dispersion spectra of the core of the K line of Ca II as seen at the center of the solar disc have been reduced. Resolution on the spectra approach 1 arc sec. Line profiles of individual elements are very asymmetric and often are peaked on only one side of the line center. Variations of the line profiles and the emission peaks are discussed. The doubly reversed mean profile of the K line is explained as a spatial average of individual profiles, and it is suggested that single peaks may be caused by Doppler-shifted discrete elements in the chromosphere. Title: Search for New Microwave Spectral Lines from Interstellar Molecules and Atoms Authors: Pasachoff, Jay M.; Gottlieb, Carl A.; Snyder, Lewis E.; Buhl, David; Palmer, Patrick; Zuckerman, B.; Dickinson, Dale F. Bibcode: 1970BAAS....2Q.213P Altcode: No abstract at ADS Title: Abstracts of papers from other journals Authors: Henoux, J. C.; Pasachoff, Jay M.; Vassilyeva, G. Y. Bibcode: 1970SoPh...11..343H Altcode: No abstract at ADS Title: Abstracts of papers from other journals Authors: Uchida, Y.; Gussmann, E. A.; De Feiter, L. D.; Henoux, J. -C.; Stepanyan, N. N.; Pasachoff, Jay. M. Bibcode: 1970SoPh...11..173U Altcode: No abstract at ADS Title: Eclipse instrumentation for the solar corona. Authors: Menzel, D. H.; Pasachoff, J. M. Bibcode: 1970ApOpt...9.2626M Altcode: No abstract at ADS Title: The Structure of the Solar Transition Zone Authors: Pasachoff, J. M. Bibcode: 1969cctr.conf..281P Altcode: No abstract at ADS Title: Abstracts of papers from other journals Authors: Stepanyan, N.; Pasachoff, Jay M.; Ambrož, P.; Vassilyeva, G.; Henoux, J. -C.; Fokker, A. D.; De Feiter, L. D.; Gussmann, E. A.; Uchida, Y.; Namba, O. Bibcode: 1969SoPh....8..491S Altcode: No abstract at ADS Title: Abstracts of papers from other journals Authors: Pasachoff, Jay M.; AmbroŽ, P.; Namba, O. Bibcode: 1969SoPh....8..248P Altcode: No abstract at ADS Title: Coronal Polarization and Structure at the Total Solar Eclipse of 22 September 1968 Authors: Schatten, Kenneth H.; Menzel, Donald H.; Pasachoff, Jay M. Bibcode: 1969BAAS....1Q.261S Altcode: No abstract at ADS Title: Radio Spectra and Related Observations of a Solar Active Region in July 1968 Authors: Pasachoff, Jay M.; Castelli, John P. Bibcode: 1969BAAS....1S.289P Altcode: No abstract at ADS Title: K-Line Profiles of Solar Fine Structure Authors: Pasachoff, Jay M. Bibcode: 1969BAAS....1R.289P Altcode: No abstract at ADS Title: Fine Structure in the Solar Chromosphere. Authors: Pasachoff, Jay Myron Bibcode: 1969PhDT.........1P Altcode: No abstract at ADS Title: Abstracts of papers from other journals Authors: Pasachoff, Jay M.; Gussmann, E. A.; Stepanyan, N. N.; de Feiter, L. D.; Uchida, Yutaka; Švestka, Z.; Vassilyeva, G. J. Bibcode: 1969SoPh....6..155P Altcode: No abstract at ADS Title: Ninety Minutes of Totality! Authors: Mercer, Robert D.; Pasachoff, Jay M. Bibcode: 1969S&T....37...20M Altcode: No abstract at ADS Title: Abstracts of papers from other journals Authors: Pasachoff, Jay M.; Vassilyeva, G. Y.; Henoux, J. -C.; Stepanyan, N. Bibcode: 1968SoPh....5..588P Altcode: No abstract at ADS Title: Spectral Observations of Spicules at Two Heights in the Solar Chromosphere Authors: Pasachoff, Jay M.; Noyes, Robert W.; Beckers, Jacques M. Bibcode: 1968SoPh....5..131P Altcode: An observational program at the Sacramento Peak Observatory in 1965 provided high-dispersion spectra of the solar chromosphere in several spectral regions simultaneously. These regions included various combinations of the spectral lines Hα, Hβ and Hɛ, the D3-line of HeI, the infrared triplet of OI, and the H- and K-lines and the infrared triplet of CaII. With the use of an image slicer the observations were made simultaneously at two heights in the solar chromosphere separated by several thousand kilometers. From these data we draw the following conclusions: Emission of different lines arises in the same chromospheric features. The intensity ratio of lines of different elements varies significantly from spicule to spicule. For the H- and K-lines of ionized calcium, this ratio remains constant, independent of wavelength throughout the line, overall intensity, and height in the chromosphere. Two rare-earth lines in the wing of the H-line show no spicular structure at all. Title: The Interpretation of the Absorption-Line Red-Shifts in the Solar Spectrum Authors: Pasachoff, Jay M.; Silk, Joseph I. Bibcode: 1968SoPh....4..474P Altcode: No abstract at ADS Title: On the Obliteration of Strong Fraunhofer Lines by Electron Scattering in the Solar Corona Authors: Menzel, Donald H.; Pasachoff, Jay M. Bibcode: 1968PASP...80..458M Altcode: No abstract at ADS Title: New Observations of Solar Chromospheric Spicules. Authors: Beckers, Jaques M.; Noyes, Robert W.; Pasachoff, Jay M. Bibcode: 1966AJ.....71T.155B Altcode: We observed the spectra of spicules on the solar limb simultaneously at two heights in the quiescent ebromosphere with the 16-in. coronagraph and the 12-m Littrow spectrograph at the Sacramento Peak Observatory during the summer of 1965. Time sequences of simultaneous observations were obtained, using the following combinations of lines: K, H, HE, and D3 H, HE, D3, and the 0 1 infrared triplet; H, HE, D3, and the Ca II infrared triplet; and Hp and HCL. Time intervals between exposures ranged from 5 to 30 sec, and the height separation was 2000 km. Our preliminary conclusions follow. (a) A strong correlation exists between the intensities of the spectra of spicules in HE and D3, while spectra in H and HE show less correlation. The rare earth line between H and HE shows no brightness or velocity structure. This suggests that it is nonspicular in Origin. (b) We see the line-of-sight velocities of some spicules reverse in direction. This suggests tbat the apparent rising and subsequent falling seen in HCL on the limb may represent actual mass motions. Further, most of il~e spicules with large line-of-sight velocities seem to be moving faster at the higher than at the lower levels. (c) The profiles of the H and K lines are indeed very broad with respect to the HCL line, in agreement with Athay. It is unlikely that these large widths are caused by overlapping spicules. (d) Many spicular spectra are tilted with respect to the direction of the dispersion. We believe this to be a real effect, caused by differential motions across the spicule. (e) The H and K lines are strongly self-reversed at low levels. We believe the self-reversal to be nonspicular in origin because it does not share the Doppler shifts of spicules. Microphotometry and detailed reduction of the data are underway.