explanation blue bibcodes open ADS page with paths to full text
Author name code: jones
ADS astronomy entries on 2022-09-14
author:"Jones, Harrison P."
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Title: Results from the WINCS Ion Energy Analyzer on the NASA Green
Propellant Infusion Mission
Authors: Nicholas, A. C.; Herrero, F. A.; Finne, T. T.; Jones, H.;
Aalami, D.
2020AGUFMSA023..12N Altcode:
The instrument suite WINCS (Wind Ion/Neutral Composition Suite) is
operating on the NASA GPIM (Green Propellant Infusion Mission). The
miniaturized charged-particle spectrometers measurements are: neutral
wind, temperature and composition - and ion-drift, ion temperature and
ion composition; the WINCS size being 3x3x3 inches<SUP>3</SUP> having a
mass of 650g and consuming power of 1.7W. This presentation will focus
on the data from the ion energy analyzer during the latter phase of
the GPIM mission when the orbit was eccentric, ~300 km x 700km. The
data have been analyzed using the Levenberg-Marquart algorithm via
discrete inverse theory to simultaneously fit the observed peaks from
ionospheric constituents in energy spectra. This analysis will provide
ion temperature and composition over the course of the orbit.
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Title: Site Selection and Instrument Considerations for Micro-Rover
Exploration of Lunar Polar Ice: The MoonRanger Mission
Authors: Schweitzer, L.; Elphic, R. C.; Jones, H.; Wettergreen, D. S.;
Whittaker, W.
2020AGUFMP023.0012S Altcode:
Lunar ice holds the prospect of water for drinking, growing
food, generating oxygen, and producing propellants. Successful ice
utilization relies heavily on yet-undetermined knowledge of accessible
concentrations at useful scales. This can only be achieved by surface
missions. Some explorations will be undertaken by MER-scale rovers
(e.g. VIPER in 2023), but a capable new class of micro-rovers may
provide complementary coverage over multiple landing sites. Micro-rovers
present, however, unique considerations of siting, instrumentation,
and operations for high-return missions. <P />Small rovers can cost
less, weigh less, and fly more frequently; however, they also have
lower energy storage and more limited slope capability for probing
into darkness and reaching stable ice. They likely offer less range
from their landers and no direct-to-Earth communication to provide
human oversight. Additionally, the small landers that deliver small
rovers may provide less precision in landing site targeting and less
tolerance of landing slopes and hazards. They require full sunlight
and line of sight to Earth. We present a methodology and results for
search and site selection based on these considerations. Favorable
sites are found to be a minor subset of those acceptable for VIPER-scale
roving. Several most-favorable sites are profiled and compared.
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Title: SEE: The 2017 Solar Eclipse Excursion, Mt. San Antonio
College Edition
Authors: Boryta, M. D.; Jones, H. P.; Lawlor, E.; Webb, C.; Hood,
M.; Bray-Ali, J.; Draper, J.
2020AGUFMSY0140004B Altcode:
Mt. SAC is a large single-campus two-year college in the greater
Los Angeles area. Our Department of Earth Sciences and Astronomy
has a strong education and outreach program that includes a busy
planetarium and astronomical observatory. Four Mt SAC faculty
and staff led a group of 19 students to Krupp Scout Hollow (KSH;
Rigby, Idaho) to view the 2017 Solar Eclipse. <P />Our 7-day trip
was designed to be affordable and educational for students. With
college support for vehicles and gas we were able to keep costs down
to $160 per student, using department telescopes and camping gear. We
camped in low-cost areas including National Parks, and everyone took
part in cooking meals at the campsite. <P />We attracted students by
offering a program of geological adventure and cultural significance in
addition to the eclipse experience. Geology and Anthropology faculty
researched and planned excursions along the trek to and from the final
eclipse destination. Students who attended got training in telescope
operating to prepare for the eclipse and to facilitate viewing
by the public. Astronomers planned activities for the 800+ drop-in
guests during the event. KSH arranged for other groups to be present;
e.g., NASA meteorologists carefully measured the drop in temperature
(11°C!) as a function of eclipse. We were able to live-stream the
entire eclipse, including footage from our solar telescope, back to
our Planetarium, where another 4000+ students and community members
were able to participate. <P />We have already begun planning a
similar excursion for the 2024 eclipse. We suggest looking for and
securing a viable spot far ahead of time - one with the least chance
of rain/cloudy weather for that time of year. Check on electrical
and internet connections, parking, bathroom and cooking facilities
for your group. Allow participants to take part as much as possible
in planning meals, duties, travel, etc. Plan too for an exponential
surge in interest and applicants close to the event!
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Title: Lunar Pit Exploration via Autonomous Micro-Rover
Authors: Ford, J.; Jones, H.; Wong, U.; Sharif, K.; Whittaker, W.
2020AGUFMP084...01F Altcode:
Lunar pits are compelling destinations for surface mission
exploration. They could access lava tubes with prospects of haven
from the extreme temperatures, radiation exposures and micrometeorite
hazards of the surface. Their walls offer direct observation of
the only geologic columns not obscured by regolith, and they are
scientifically interesting in their own right. The required vantages
and proximities for these inquiries are not possible from orbit and
motivate robotic surface exploration. <P />This paper presents an
autonomous micro-rover a pproach to exploration and mapping of lunar
pits by in-situ modeling via imagery gathered from their rims. The
mission concept incorporates a commercial lander, rover forays around
the rim, autonomous acquisition of a vast image dataset, and incremental
photogrammetric construction of a pit model from the imagery. We develop
the requisite autonomy, modeling, computing, and mobility technologies
and present results from a case study performed at a terrestrial
analog pit. We demonstrate the coverage and accuracy achievable by
this method and conclude with progress toward a fully integrated
rover for this important new class of mission. The rover incorporates
telephoto lensing to achieve the requisite resolution for observing
detail across vast pit dimensions. For frequent, affordable, commercial
landing opportunities, the rover must be small and solar powered. To
complete a long range mission before the onset of lunar night, the rover
requires unprecedented autonomy, steep-slope mobility, high performance
computing and state-of-the-art photogrammetry algorithms. We present a
case study applying micro-rover imaging, computing, and photogrammetry
to a terrestrial pit. This acquires 10,000 high resolution, high dynamic
range images from 26 poses around the rim of the West Desert Sinkhole
which is a terrestrial pit with diameter, depth, and stratification
analogous to known lunar mare pits. Results are compared to ground
truth LIDAR with error below 10cm across 90% of the pit surface.
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Title: Erratum: The first planet detected in the WTS: an inflated
hot-Jupiter in a 3.35 day orbit around a late F-star
Authors: Cappetta, M.; Saglia, R. P.; Birkby, J. L.; Koppenhoefer, J.;
Pinfield, D. J.; Hodgkin, S. T.; Cruz, P.; Kovács, G.; Sipőcz, B.;
Barrado, D.; Nefs, B.; Pavlenko, Y. V.; Fossati, L.; del Burgo, C.;
Martín, E. L.; Snellen, I.; Barnes, J.; Campbell, D.; Catalan, S.;
Gálvez-Ortiz, M. C.; Goulding, N.; Haswell, C.; Ivanyuk, O.; Jones,
H.; Kuznetsov, M.; Lodieu, N.; Marocco, F.; Mislis, D.; Murgas, F.;
Napiwotzki, R.; Palle, E.; Pollacco, D.; Sarro Baro, L.; Solano, E.;
Steele, P.; Stoev, H.; Tata, R.; Zendejas, J.
2020MNRAS.497..916C Altcode:
No abstract at ADS
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Title: Preliminary Results from the WINCS sensor on the NASA Green
Propellant Infusion Mission
Authors: Nicholas, A. C.; Herrero, F. A.; Finne, T. T.; Aalami, D.;
Jones, H.
2019AGUFMSA33B3144N Altcode:
The instrument suite WINCS (Wind Ion/Neutral Composition Suite) is
operating on the NASA GPIM (Green Propellant Infusion Mission). The
miniaturized charged-particle spectrometers measurements are: neutral
wind, temperature and composition - and ion-drift, ion temperature and
ion composition; the WINCS size being 3x3x3 inches<SUP>3</SUP> having
a mass of 650g and consuming power of 1.7W. Since the neutrals entering
WINCS are not affected by spacecraft charging, the combined neutral and
ion measurements provide a method to measure the spacecraft potential
in the ionosphere. Preliminary results will be presented to illustrate
this method of monitoring spacecraft charging. In addition it will be
possible to detect distortions of ion trajectories by unwanted electric
fields in the vicinity of WINCS. Understanding these instrumental
effects would then clear the way to obtain the six basic parameters of
the ionosphere/ thermosphere fluid, consisting of bulk velocity vectors
(neutral wind and ion-drift), temperatures, and compositions of the
neutrals and ions in the ionosphere/thermosphere system. Preliminary
determinations of these parameters will be presented.
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Title: Extraordinary rocks from the peak ring of the Chicxulub
impact crater: P-wave velocity, density, and porosity measurements
from IODP/ICDP Expedition 364
Authors: Christeson, G. L.; Gulick, S. P. S.; Morgan, J. V.; Gebhardt,
C.; Kring, D. A.; Le Ber, E.; Lofi, J.; Nixon, C.; Poelchau, M.; Rae,
A. S. P.; Rebolledo-Vieyra, M.; Riller, U.; Schmitt, D. R.; Wittmann,
A.; Bralower, T. J.; Chenot, E.; Claeys, P.; Cockell, C. S.; Coolen,
M. J. L.; Ferrière, L.; Green, S.; Goto, K.; Jones, H.; Lowery,
C. M.; Mellett, C.; Ocampo-Torres, R.; Perez-Cruz, L.; Pickersgill,
A. E.; Rasmussen, C.; Sato, H.; Smit, J.; Tikoo, S. M.; Tomioka, N.;
Urrutia-Fucugauchi, J.; Whalen, M. T.; Xiao, L.; Yamaguchi, K. E.
2018E&PSL.495....1C Altcode:
Joint International Ocean Discovery Program and International
Continental Scientific Drilling Program Expedition 364 drilled into the
peak ring of the Chicxulub impact crater. We present P-wave velocity,
density, and porosity measurements from Hole M0077A that reveal
unusual physical properties of the peak-ring rocks. Across the boundary
between post-impact sedimentary rock and suevite (impact melt-bearing
breccia) we measure a sharp decrease in velocity and density, and an
increase in porosity. Velocity, density, and porosity values for the
suevite are 2900-3700 m/s, 2.06-2.37 g/cm<SUP>3</SUP>, and 20-35%,
respectively. The thin (25 m) impact melt rock unit below the suevite
has velocity measurements of 3650-4350 m/s, density measurements of
2.26-2.37 g/cm<SUP>3</SUP>, and porosity measurements of 19-22%. We
associate the low velocity, low density, and high porosity of suevite
and impact melt rock with rapid emplacement, hydrothermal alteration
products, and observations of pore space, vugs, and vesicles. The
uplifted granitic peak ring materials have values of 4000-4200 m/s,
2.39-2.44 g/cm<SUP>3</SUP>, and 8-13% for velocity, density, and
porosity, respectively; these values differ significantly from typical
unaltered granite which has higher velocity and density, and lower
porosity. The majority of Hole M0077A peak-ring velocity, density,
and porosity measurements indicate considerable rock damage, and are
consistent with numerical model predictions for peak-ring formation
where the lithologies present within the peak ring represent some of
the most shocked and damaged rocks in an impact basin. We integrate
our results with previous seismic datasets to map the suevite near
the borehole. We map suevite below the Paleogene sedimentary rock
in the annular trough, on the peak ring, and in the central basin,
implying that, post impact, suevite covered the entire floor of the
impact basin. Suevite thickness is 100-165 m on the top of the peak
ring but 200 m in the central basin, suggesting that suevite flowed
downslope from the collapsing central uplift during and after peak-ring
formation, accumulating preferentially within the central basin.
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Title: Long-Term Recovery of Life in the Chicxulub Crater
Authors: Lowery, C.; Jones, H.; Bralower, T. J.; Smit, J.;
Rodriguez-Tovar, F. J.; Whalen, M. T.; Owens, J. D.; Expedition 364
Science Party, I. I.
2017AGUFM.P23H..07L Altcode:
The Chicxulub Crater on the Yucatán Peninsula of Mexico was formed
by the impact of an asteroid 66 Ma that caused the extinction of 75%
of genera on Earth. Immediately following the impact, the decimated
ecosystem began the long process of recovery, both in terms of primary
productivity and species diversity. This well-documented process was
heterogeneous across the world ocean, but until the present time
it has been inaccessible at ground zero of the impact. IODP/ICDP
Exp. 364 recovered 9.5 m of pelagic limestone spanning the entire
Paleocene, including a continuous section spanning the first 5 myr
following the impact. The Chicxulub Crater is the largest known marine
impact crater on Earth, and the recovery of the ecosystem presented
here is the first such record of long-term primary succession in
the sterile zone of a large impact crater. Planktic and benthic
foraminifera, calcareous nannoplankton, calcispheres, bioturbation,
and geochemical proxies all indicate that export productivity in
the Chicxulub Crater recovered rapidly (within 30 kyr) following
the impact. Recovery in terms of diversity and species abundance
took much longer, and varied between groups. Planktic foraminifera
quickly diversified, with all common Paleocene tropical/subtropical
species appearing roughly when expected. Trace fossils appear rapidly
after the event, with a progressive recovery through the lowermost
Paleocene. Calcareous nannoplankton took much longer to recover, and
disaster taxa like Braarudosphaera dominated the assemblage well into
the late Paleocene. Paleoecology and geochemistry relate these trends
to oceanographic conditions within the Chicxulub Crater. Planktic
foraminifera from known depth habitats, including Morozovellids,
Acarininids, Chiloguembelinids, and Subbotinids, track changes
in the water column structure and paleoredox conditions within the
crater. Diverse and abundant macro- and microbenthic organisms indicate
food availability and good oxygen conditions on the seafloor. The
latest Paleocene, just prior to the onset of the PETM, is characterized
by a typical and diverse assemblage of foraminifera and calcareous
nannoplankton; a normal open-marine assemblage with no trace of
long-term negative effects from the impact.
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Title: Terrestrial Palynology of Paleocene and Eocene Sediments
Above the Chicxulub Impact Crater
Authors: Smith, V.; Warny, S.; Bralower, T. J.; Jones, H.; Lowery,
C. M.; Smit, J.; Vajda, V.; Vellekoop, J.; 364 Scientists, E.
2017AGUFM.P33D2906S Altcode:
International Ocean Discovery Program (IODP) Expedition 364, with
support from the International Continental Scientific Drilling
Program, cored through Paleocene and Eocene sediments and into the
impact structure of the Chicxulub impact crater. Three palynological
studies of the post-impact section are currently underway. The two
other studies are investigating the dinoflagellate palynology and
terrestrial palynology of the K/Pg boundary section, while this study
focuses on the early Eocene terrestrial palynology of the IODP 364 core,
which has yielded a diverse and well preserved pollen assemblage. A few
samples from the Early Paleocene have also been examined but organic
microfossil preservation is quite poor. Samples from this core are
the oldest palynological record from the Yucatan peninsula. Sample
preparation and detailed abundance counts of sixty samples throughout
the post-impact section are in progress, with a particular focus
on the Paleocene-Eocene Thermal Maximum (PETM) and the Early Eocene
Climatic Optimum (EECO). Terrestrial palynomorph assemblages will be
used to reconstruct paleoclimatological conditions throughout this time
period. Floral response to hyperthermal events in the IODP 364 core
will be compared with records from other Gulf of Mexico and Caribbean
sections. In addition to the biological and paleoclimatological
implications of this research, age control from foraminiferal and
nannofossil biostratigraphy, paleomagnetism, and radiometric dating
will provide a chronological framework for the terrestrial pollen
biostratigraphy, with applications to hydrocarbon exploration in the
Wilcox Formation and age equivalent sections in the Gulf of Mexico.
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Title: The Recovery of Life in the Chicxulub Crater Following the
End Cretaceous Mass Extinction
Authors: Lowery, C. M.; Jones, H.; Smit, J.; Bralower, T. J.; Owens,
J. D.; IODP-ICDP Expedition 364 Science Party
2017LPI....48.2156L Altcode:
We present the first record of the recovery of life in a large impact
crater. Zoo- and phytoplankton follow diveregent trends for millions
of years post-impact.
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Title: IODP/ICDP Expedition 364-Drilling the Cretaceous-Paleogene
Chicxulub impact crater: Insights into large craters formation and
their effect on life.
Authors: Gulick, S. P. S.; Morgan, J. V.; Fucugauchi, J. U.; Bralower,
T. J.; Chenot, É.; Christeson, G. L.; Claeys, P.; Cockell, C. S.;
Collins, G. S.; Coolen, M.; Gebhardt, C.; Goto, K.; Kring, D. A.;
Xiao, L.; Lowery, C.; Mellett, C.; Ocampo-Torres, R.; Osinski, G. R.;
Perez-Cruz, L. L.; Pickersgill, A.; Poelchau, M.; Rae, A.; Rasmussen,
C.; Rebolledo-Vieyra, M.; Riller, U. P.; Sato, H.; Schmitt, D. R.;
Smit, J.; Tikoo, S.; Tomioka, N.; Whalen, M. T.; Zylberman, W.; Jones,
H.; Gareth, C.; Wittmann, A.; Lofi, J.; Yamaguchi, K. E.; Ferrière, L.
2016AGUFM.P31E..05G Altcode:
An international project to drill the Chicxulub impact crater was
conducted in April and May, 2016 as Expedition 364 of the International
Ocean Discovery Program (IODP) and International Continental Scientific
Drilling Project (ICDP). Site M0077 is located offshore Yucatan in
the southern Gulf of Mexico. The target was to core the only pristine
terrestrial peak ring and to measure physical properties of the entire
borehole. Specific questions included: What rocks comprise a topographic
peak ring? How are peak rings formed? How are rocks weakened during
large impacts to allow them to collapse and form relatively wide,
flat craters? What insights arise from biologic recovery in the
Paleogene within a potentially "toxic" ocean basin? Are impact craters
(including peak rings) habitats for life? Coring occurred from 503 -
1334.7 mbsf with nearly 100% recovery. Wireline logs were collected
from ultra slimline tools to total depth including gamma ray, magnetic
susceptibility, sonic, borehole fluid temperature and conductivity,
resistivity data, borehole images, and a finely spaced vertical
seismic profile. Stratigraphy cored included 110 m of Eocene and
Paleocene carbonates, 130 m of allochthonous impactites, and 590
m of crustal basement with dikes. All cores were measured using a
shipboard core logger (density, gamma ray, magnetic susceptibility
and resistivity) and shorebased dual energy, 0.3 mm resolution CT
scanner. These data allow us to: 1) refine numerical models of the
formation of the Chicxulub impact structure; 2) place constraints
on environmental perturbations that led to the K-Pg mass extinction;
3) improve simulations of impact craters on other planetary bodies;
4) examine deformation mechanisms for insights into how rocks weaken
during impacts; 5) study impact generated hydrothermal systems and 6)
understand the effects of impacts on the deep biosphere including as
a habitat for microbial life with implications for evolution on Earth
and astrobiology. Key results are that the Chicxulub peak ring is formed
from fractured basement rocks that may host a subsurface biosphere. The
impactite layer overlying the peak ring in turn provides insight into
resurge and tsunami processes, while the Paleogene sediments contain
the record of the recovery of life after the mass extinction event.
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Title: Route Planning Software for Lunar Polar Missions
Authors: Cunningham, C.; Jones, H.; Amato, J.; Holst, I.; Otten, N.;
Kitchell, F.; Whittaker, W.; Horchler, A.
2016LPICo1960.5062C Altcode:
Rover mission planning on the lunar poles is challenging due to
the long, time-varying shadows. This abstract presents software for
efficiently planning traverses while balancing competing demands of
science goals, rover energy constraints, and risk.
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Title: Quantitative Evaluation of a Planetary Renderer for Terrain
Relative Navigation
Authors: Amoroso, E.; Jones, H.; Otten, N.; Wettergreen, D.;
Whittaker, W.
2016LPICo1960.5037A Altcode:
A ray-tracing computer renderer tool is presented based on LOLA and
LROC elevation models and is quantitatively compared to LRO WAC and
NAC images for photometric accuracy. We investigated using rendered
images for terrain relative navigation.
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Title: Results of Lunar Rover Drivetrain TRL-6 Environmental Testing
Authors: Visscher, P.; Edmundson, P.; Ghafoor, N.; Jones, H.;
Kleinhenz, J.; Picard, M.
2016LPICo1960.5027V Altcode:
Latest results of work performed by Ontario Drive and Gear Ltd.,
Canadensys Aerospace Corporation, and partners on Canadian lunar rover
development activities for the Canadian Space Agency, including "dirty"
thermal vacuum testing of drivetrain unit.
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Title: Ca II 854.2 nm Spectromagnetograms: A Powerful Chromospheric
Diagnostic
Authors: Harvey, J. W.; Bertello, Luca; Branston, D.; Britanik, J.;
Bulau, S.; Cole, L.; Gosain, Sanjay; Harker, Brian; Jones, Harrison P.;
Marble, A.; Martinez Pillet, V.; Pevtsov, A.; Schramm, K.; Streander,
Kim; Villegas, H.
2016SPD....4710106H Altcode:
The transition from physical dominance by plasma flows in the
photosphere to magnetic pressure in the solar chromosphere motivates
as many diagnostic observations as possible across this important
region. Among the few ground-accessible spectral lines formed within
the chromosphere, the Ca II 854.2 nm line has the desirable properties
of presence everywhere on the solar disk, Zeeman sensitivity, and
narrow line width. Mapped observations of circular polarization within
this line (spectromagnetograms) have been made at NSO infrequently
since 1974, with regular daily full-disk observations starting in
August 1996. Full-disk spectral observations of the complete Stokes
polarization vector are now being made regularly since November
2015. It is not easy to estimate chromospheric magnetic field
properties from the 854.2 nm line profile polarization. To provide
rough quick-look vector field maps we found that the weak-field
approximation provides a fair first estimate of the line-of-sight
component but appears to be too simple to interpret the transverse
magnetic field from frequently asymmetric, linearly-polarized line
profiles. More realistic estimates of the chromospheric vector field,
short of extremely lengthy, full 3D, non-local radiative transfer
inversions, are being investigated. We briefly introduce recent
instrumental modifications and observational characteristics, sample
observations, and results concerning the expansion of the chromospheric
field with increasing height, the presence of large areas of weak,
nearly horizontal fields, and field estimates in plages, sunspots,
flares, filaments, and filament channels. The Stokes spectra will be
freely available to the community.This work utilizes SOLIS data obtained
by the NSO Integrated Synoptic Program (NISP), managed by the National
Solar Observatory, which is operated by the Association of Universities
for Research in Astronomy (AURA), Inc. under a cooperative agreement
with the National Science Foundation.
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Title: The EChO science case
Authors: Tinetti, Giovanna; Drossart, Pierre; Eccleston, Paul; Hartogh,
Paul; Isaak, Kate; Linder, Martin; Lovis, Christophe; Micela, Giusi;
Ollivier, Marc; Puig, Ludovic; Ribas, Ignasi; Snellen, Ignas; Swinyard,
Bruce; Allard, France; Barstow, Joanna; Cho, James; Coustenis, Athena;
Cockell, Charles; Correia, Alexandre; Decin, Leen; de Kok, Remco;
Deroo, Pieter; Encrenaz, Therese; Forget, Francois; Glasse, Alistair;
Griffith, Caitlin; Guillot, Tristan; Koskinen, Tommi; Lammer, Helmut;
Leconte, Jeremy; Maxted, Pierre; Mueller-Wodarg, Ingo; Nelson, Richard;
North, Chris; Pallé, Enric; Pagano, Isabella; Piccioni, Guseppe;
Pinfield, David; Selsis, Franck; Sozzetti, Alessandro; Stixrude,
Lars; Tennyson, Jonathan; Turrini, Diego; Zapatero-Osorio, Mariarosa;
Beaulieu, Jean-Philippe; Grodent, Denis; Guedel, Manuel; Luz, David;
Nørgaard-Nielsen, Hans Ulrik; Ray, Tom; Rickman, Hans; Selig,
Avri; Swain, Mark; Banaszkiewicz, Marek; Barlow, Mike; Bowles, Neil;
Branduardi-Raymont, Graziella; du Foresto, Vincent Coudé; Gerard,
Jean-Claude; Gizon, Laurent; Hornstrup, Allan; Jarchow, Christopher;
Kerschbaum, Franz; Kovacs, Géza; Lagage, Pierre-Olivier; Lim, Tanya;
Lopez-Morales, Mercedes; Malaguti, Giuseppe; Pace, Emanuele; Pascale,
Enzo; Vandenbussche, Bart; Wright, Gillian; Ramos Zapata, Gonzalo;
Adriani, Alberto; Azzollini, Ruymán; Balado, Ana; Bryson, Ian;
Burston, Raymond; Colomé, Josep; Crook, Martin; Di Giorgio, Anna;
Griffin, Matt; Hoogeveen, Ruud; Ottensamer, Roland; Irshad, Ranah;
Middleton, Kevin; Morgante, Gianluca; Pinsard, Frederic; Rataj, Mirek;
Reess, Jean-Michel; Savini, Giorgio; Schrader, Jan-Rutger; Stamper,
Richard; Winter, Berend; Abe, L.; Abreu, M.; Achilleos, N.; Ade, P.;
Adybekian, V.; Affer, L.; Agnor, C.; Agundez, M.; Alard, C.; Alcala,
J.; Allende Prieto, C.; Alonso Floriano, F. J.; Altieri, F.; Alvarez
Iglesias, C. A.; Amado, P.; Andersen, A.; Aylward, A.; Baffa, C.;
Bakos, G.; Ballerini, P.; Banaszkiewicz, M.; Barber, R. J.; Barrado,
D.; Barton, E. J.; Batista, V.; Bellucci, G.; Belmonte Avilés,
J. A.; Berry, D.; Bézard, B.; Biondi, D.; Błęcka, M.; Boisse, I.;
Bonfond, B.; Bordé, P.; Börner, P.; Bouy, H.; Brown, L.; Buchhave,
L.; Budaj, J.; Bulgarelli, A.; Burleigh, M.; Cabral, A.; Capria,
M. T.; Cassan, A.; Cavarroc, C.; Cecchi-Pestellini, C.; Cerulli,
R.; Chadney, J.; Chamberlain, S.; Charnoz, S.; Christian Jessen,
N.; Ciaravella, A.; Claret, A.; Claudi, R.; Coates, A.; Cole, R.;
Collura, A.; Cordier, D.; Covino, E.; Danielski, C.; Damasso, M.;
Deeg, H. J.; Delgado-Mena, E.; Del Vecchio, C.; Demangeon, O.; De Sio,
A.; De Wit, J.; Dobrijévic, M.; Doel, P.; Dominic, C.; Dorfi, E.;
Eales, S.; Eiroa, C.; Espinoza Contreras, M.; Esposito, M.; Eymet,
V.; Fabrizio, N.; Fernández, M.; Femenía Castella, B.; Figueira,
P.; Filacchione, G.; Fletcher, L.; Focardi, M.; Fossey, S.; Fouqué,
P.; Frith, J.; Galand, M.; Gambicorti, L.; Gaulme, P.; García López,
R. J.; Garcia-Piquer, A.; Gear, W.; Gerard, J. -C.; Gesa, L.; Giani,
E.; Gianotti, F.; Gillon, M.; Giro, E.; Giuranna, M.; Gomez, H.;
Gomez-Leal, I.; Gonzalez Hernandez, J.; González Merino, B.; Graczyk,
R.; Grassi, D.; Guardia, J.; Guio, P.; Gustin, J.; Hargrave, P.; Haigh,
J.; Hébrard, E.; Heiter, U.; Heredero, R. L.; Herrero, E.; Hersant,
F.; Heyrovsky, D.; Hollis, M.; Hubert, B.; Hueso, R.; Israelian, G.;
Iro, N.; Irwin, P.; Jacquemoud, S.; Jones, G.; Jones, H.; Justtanont,
K.; Kehoe, T.; Kerschbaum, F.; Kerins, E.; Kervella, P.; Kipping, D.;
Koskinen, T.; Krupp, N.; Lahav, O.; Laken, B.; Lanza, N.; Lellouch,
E.; Leto, G.; Licandro Goldaracena, J.; Lithgow-Bertelloni, C.; Liu,
S. J.; Lo Cicero, U.; Lodieu, N.; Lognonné, P.; Lopez-Puertas,
M.; Lopez-Valverde, M. A.; Lundgaard Rasmussen, I.; Luntzer, A.;
Machado, P.; MacTavish, C.; Maggio, A.; Maillard, J. -P.; Magnes, W.;
Maldonado, J.; Mall, U.; Marquette, J. -B.; Mauskopf, P.; Massi, F.;
Maurin, A. -S.; Medvedev, A.; Michaut, C.; Miles-Paez, P.; Montalto,
M.; Montañés Rodríguez, P.; Monteiro, M.; Montes, D.; Morais, H.;
Morales, J. C.; Morales-Calderón, M.; Morello, G.; Moro Martín,
A.; Moses, J.; Moya Bedon, A.; Murgas Alcaino, F.; Oliva, E.; Orton,
G.; Palla, F.; Pancrazzi, M.; Pantin, E.; Parmentier, V.; Parviainen,
H.; Peña Ramírez, K. Y.; Peralta, J.; Perez-Hoyos, S.; Petrov, R.;
Pezzuto, S.; Pietrzak, R.; Pilat-Lohinger, E.; Piskunov, N.; Prinja,
R.; Prisinzano, L.; Polichtchouk, I.; Poretti, E.; Radioti, A.; Ramos,
A. A.; Rank-Lüftinger, T.; Read, P.; Readorn, K.; Rebolo López,
R.; Rebordão, J.; Rengel, M.; Rezac, L.; Rocchetto, M.; Rodler, F.;
Sánchez Béjar, V. J.; Sanchez Lavega, A.; Sanromá, E.; Santos,
N.; Sanz Forcada, J.; Scandariato, G.; Schmider, F. -X.; Scholz,
A.; Scuderi, S.; Sethenadh, J.; Shore, S.; Showman, A.; Sicardy, B.;
Sitek, P.; Smith, A.; Soret, L.; Sousa, S.; Stiepen, A.; Stolarski,
M.; Strazzulla, G.; Tabernero, H. M.; Tanga, P.; Tecsa, M.; Temple,
J.; Terenzi, L.; Tessenyi, M.; Testi, L.; Thompson, S.; Thrastarson,
H.; Tingley, B. W.; Trifoglio, M.; Martín Torres, J.; Tozzi, A.;
Turrini, D.; Varley, R.; Vakili, F.; de Val-Borro, M.; Valdivieso,
M. L.; Venot, O.; Villaver, E.; Vinatier, S.; Viti, S.; Waldmann,
I.; Waltham, D.; Ward-Thompson, D.; Waters, R.; Watkins, C.; Watson,
D.; Wawer, P.; Wawrzaszk, A.; White, G.; Widemann, T.; Winek, W.;
Wiśniowski, T.; Yelle, R.; Yung, Y.; Yurchenko, S. N.
2015ExA....40..329T Altcode: 2015ExA...tmp...67T; 2015arXiv150205747T
The discovery of almost two thousand exoplanets has revealed an
unexpectedly diverse planet population. We see gas giants in few-day
orbits, whole multi-planet systems within the orbit of Mercury,
and new populations of planets with masses between that of the Earth
and Neptune—all unknown in the Solar System. Observations to date
have shown that our Solar System is certainly not representative of
the general population of planets in our Milky Way. The key science
questions that urgently need addressing are therefore: What are
exoplanets made of? Why are planets as they are? How do planetary
systems work and what causes the exceptional diversity observed as
compared to the Solar System? The EChO (Exoplanet Characterisation
Observatory) space mission was conceived to take up the challenge to
explain this diversity in terms of formation, evolution, internal
structure and planet and atmospheric composition. This requires
in-depth spectroscopic knowledge of the atmospheres of a large and
well-defined planet sample for which precise physical, chemical and
dynamical information can be obtained. In order to fulfil this ambitious
scientific program, EChO was designed as a dedicated survey mission
for transit and eclipse spectroscopy capable of observing a large,
diverse and well-defined planet sample within its 4-year mission
lifetime. The transit and eclipse spectroscopy method, whereby the
signal from the star and planet are differentiated using knowledge of
the planetary ephemerides, allows us to measure atmospheric signals
from the planet at levels of at least 10<SUP>-4</SUP> relative to
the star. This can only be achieved in conjunction with a carefully
designed stable payload and satellite platform. It is also necessary
to provide broad instantaneous wavelength coverage to detect as many
molecular species as possible, to probe the thermal structure of the
planetary atmospheres and to correct for the contaminating effects of
the stellar photosphere. This requires wavelength coverage of at least
0.55 to 11 μm with a goal of covering from 0.4 to 16 μm. Only modest
spectral resolving power is needed, with R ~ 300 for wavelengths less
than 5 μm and R ~ 30 for wavelengths greater than this. The transit
spectroscopy technique means that no spatial resolution is required. A
telescope collecting area of about 1 m<SUP>2</SUP> is sufficiently
large to achieve the necessary spectro-photometric precision: for the
Phase A study a 1.13 m<SUP>2</SUP> telescope, diffraction limited at 3
μm has been adopted. Placing the satellite at L2 provides a cold and
stable thermal environment as well as a large field of regard to allow
efficient time-critical observation of targets randomly distributed over
the sky. EChO has been conceived to achieve a single goal: exoplanet
spectroscopy. The spectral coverage and signal-to-noise to be achieved
by EChO, thanks to its high stability and dedicated design, would be
a game changer by allowing atmospheric composition to be measured
with unparalleled exactness: at least a factor 10 more precise and
a factor 10 to 1000 more accurate than current observations. This
would enable the detection of molecular abundances three orders of
magnitude lower than currently possible and a fourfold increase from
the handful of molecules detected to date. Combining these data with
estimates of planetary bulk compositions from accurate measurements
of their radii and masses would allow degeneracies associated with
planetary interior modelling to be broken, giving unique insight
into the interior structure and elemental abundances of these alien
worlds. EChO would allow scientists to study exoplanets both as a
population and as individuals. The mission can target super-Earths,
Neptune-like, and Jupiter-like planets, in the very hot to temperate
zones (planet temperatures of 300-3000 K) of F to M-type host stars. The
EChO core science would be delivered by a three-tier survey. The EChO
Chemical Census: This is a broad survey of a few-hundred exoplanets,
which allows us to explore the spectroscopic and chemical diversity of
the exoplanet population as a whole. The EChO Origin: This is a deep
survey of a subsample of tens of exoplanets for which significantly
higher signal to noise and spectral resolution spectra can be obtained
to explain the origin of the exoplanet diversity (such as formation
mechanisms, chemical processes, atmospheric escape). The EChO Rosetta
Stones: This is an ultra-high accuracy survey targeting a subsample
of select exoplanets. These will be the bright "benchmark" cases
for which a large number of measurements would be taken to explore
temporal variations, and to obtain two and three dimensional spatial
information on the atmospheric conditions through eclipse-mapping
techniques. If EChO were launched today, the exoplanets currently
observed are sufficient to provide a large and diverse sample. The
Chemical Census survey would consist of > 160 exoplanets with a range
of planetary sizes, temperatures, orbital parameters and stellar host
properties. Additionally, over the next 10 years, several new ground-
and space-based transit photometric surveys and missions will come
on-line (e.g. NGTS, CHEOPS, TESS, PLATO), which will specifically focus
on finding bright, nearby systems. The current rapid rate of discovery
would allow the target list to be further optimised in the years prior
to EChO's launch and enable the atmospheric characterisation of hundreds
of planets.
---------------------------------------------------------
Title: Lunar Rover Drivetrain Development to TRL-6
Authors: Visscher, P.; Edmundson, P.; Ghafoor, N.; Jones, H.;
Kleinhenz, J.; Picard, M.
2015LPICo1863.2009V Altcode:
The LRPDP and SPRP rovers are designed to provide high mobility and
robustness in a lunar working environment and are compatible with
various lunar surface activities. TRL-6 testing is scheduled for late
2015 on the rover drivetrain components.
---------------------------------------------------------
Title: Rover Traverse Planning to Support a Lunar Polar Volatiles
Mission
Authors: Heldmann, J. L.; Colaprete, A. C.; Elphic, R. C.; Bussey,
B.; McGovern, A.; Beyer, R.; Lees, D.; Deans, M. C.; Otten, N.; Jones,
H.; Wettergreen, D.
2015LPICo1863.2007H Altcode:
We present notional traverse plans for NASA’s Resource Prospector
mission for a lunar polar rover and utilize this mission architecture
and associated constraints to evaluate whether a suitable landing site
exists to support an RP flight mission.
---------------------------------------------------------
Title: The SAMI Galaxy Survey: cubism and covariance, putting round
pegs into square holes
Authors: Sharp, R.; Allen, J. T.; Fogarty, L. M. R.; Croom, S. M.;
Cortese, L.; Green, A. W.; Nielsen, J.; Richards, S. N.; Scott,
N.; Taylor, E. N.; Barnes, L. A.; Bauer, A. E.; Birchall, M.;
Bland-Hawthorn, J.; Bloom, J. V.; Brough, S.; Bryant, J. J.; Cecil,
G. N.; Colless, M.; Couch, W. J.; Drinkwater, M. J.; Driver, S.;
Foster, C.; Goodwin, M.; Gunawardhana, M. L. P.; Ho, I. -T.; Hampton,
E. J.; Hopkins, A. M.; Jones, H.; Konstantopoulos, I. S.; Lawrence,
J. S.; Leslie, S. K.; Lewis, G. F.; Liske, J.; López-Sánchez, Á. R.;
Lorente, N. P. F.; McElroy, R.; Medling, A. M.; Mahajan, S.; Mould,
J.; Parker, Q.; Pracy, M. B.; Obreschkow, D.; Owers, M. S.; Schaefer,
A. L.; Sweet, S. M.; Thomas, A. D.; Tonini, C.; Walcher, C. J.
2015MNRAS.446.1551S Altcode: 2014arXiv1407.5237S
We present a methodology for the regularization and combination of
sparse sampled and irregularly gridded observations from fibre-optic
multiobject integral field spectroscopy. The approach minimizes
interpolation and retains image resolution on combining subpixel
dithered data. We discuss the methodology in the context of the
Sydney-AAO multiobject integral field spectrograph (SAMI) Galaxy Survey
underway at the Anglo-Australian Telescope. The SAMI instrument uses
13 fibre bundles to perform high-multiplex integral field spectroscopy
across a 1° diameter field of view. The SAMI Galaxy Survey is targeting
∼3000 galaxies drawn from the full range of galaxy environments. We
demonstrate the subcritical sampling of the seeing and incomplete fill
factor for the integral field bundles results in only a 10 per cent
degradation in the final image resolution recovered. We also implement
a new methodology for tracking covariance between elements of the
resulting data cubes which retains 90 per cent of the covariance
information while incurring only a modest increase in the survey
data volume.
---------------------------------------------------------
Title: Erratum: The first planet detected in the WTS: an inflated
hot-Jupiter in a 3.35 d orbit around a late F star
Authors: Cappetta, M.; Saglia, R. P.; Birkby, J. L.; Koppenhoefer, J.;
Pinfield, D. J.; Hodgkin, S. T.; Cruz, P.; Kovács, G.; Sipőcz, B.;
Barrado, D.; Nefs, B.; Pavlenko, Y. V.; Fossati, L.; del Burgo, C.;
Martín, E. L.; Snellen, I.; Barnes, J.; Campbell, D.; Catalan, S.;
Gálvez-Ortiz, M. C.; Goulding, N.; Haswell, C.; Ivanyuk, O.; Jones,
H.; Kuznetsov, M.; Lodieu, N.; Marocco, F.; Mislis, D.; Murgas, F.;
Napiwotzki, R.; Palle, E.; Pollacco, D.; Sarro Baro, L.; Solano, E.;
Steele, P.; Stoev, H.; Tata, R.; Zendejas, J.
2014MNRAS.444.3150C Altcode: 2014arXiv1410.3235C
We report the discovery of WTS-1b, the first extrasolar planet found
by the WFCAM Transit Survey, which began observations at the 3.8-m
United Kingdom Infrared Telescope (UKIRT) in August 2007. Light
curves comprising almost 1200 epochs with a photometric precision of
better than 1 per cent to J ~ 16 were constructed for ~60000 stars and
searched for periodic transit signals. For one of the most promising
transiting candidates, high-resolution spectra taken at the Hobby-Eberly
Telescope (HET) allowed us to estimate the spectroscopic parameters of
the host star, a late-F main sequence dwarf (V=16.13) with possibly
slightly subsolar metallicity, and to measure its radial velocity
variations. The combined analysis of the light curves and spectroscopic
data resulted in an orbital period of the substellar companion of 3.35
days, a planetary mass of 4.01 +- 0.35 Mj and a planetary radius of
1.49+0.16-0.18 Rj. WTS-1b has one of the largest radius anomalies among
the known hot Jupiters in the mass range 3-5 Mj. The high irradiation
from the host star ranks the planet in the pM class.
---------------------------------------------------------
Title: Radial Velocity Studies of M Dwarfs
Authors: Jones, H.
2014hwat.confE..23J Altcode:
Our current view of exoplanets is one derived primarily from Solar-like
stars with a strong focus on understanding our Solar System. Our
knowledge about the properties of exoplanets around the dominant
stellar population by number, the so called low-mass stars or M dwarfs
is much more cursory. Based on combining radial velocities of nearby M
dwarfs obtained with UVES and HARPS we find 8 new M dwarf planets and
2 previous known from a sample of 41 stars. By computing the estimated
detection probability function the occurrence rate of planets less than
10 Earth masses around nearby M dwarfs is found to be of the order of
one planet per star and that of habitable zone planets between 3 and
10 Earth masses around 20 percent. The mass of radial velocity M dwarf
planets is relatively much lower than the expected mass dependency
based on stellar mass and thus it is inferred that planet formation
efficiency around low mass stars is relatively impaired. Techniques to
overcome the practical issue of obtaining good quality radial velocity
data for M dwarfs are considered: (1) the wavelength sensitivity of
radial velocity signals, (2) the combination of radial velocity data
from different experiments for robust detection of small amplitude
signals and (3) optimum selection of targets.
---------------------------------------------------------
Title: Meeting the Challenge of Affordable Lunar Exploration -
Heritage Systems, Flexible Partnerships, New Flight Opportunities
Authors: Ghafoor, N.; Jones, H.; Jessen, S.; McCoubrey, R.; Fulford,
P.; McCarthy, T.; Chappell, L.; Lackner, D.; Tadros, A.
2013LPICo1748.7058G Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Realistic limitations of detecting planets around young
active stars
Authors: Jeffers, S. V.; Barnes, J. R.; Jones, H.; Pinfield, D.
2013EPJWC..4709002J Altcode:
Current planet hunting methods using the radial velocity method
are limited to observing middle-aged main-sequence stars where
the signatures of stellar activity are much less than on young
stars that have just arrived on the main-sequence. In this work we
apply our knowledge from the surface imaging of these young stars to
place realistic limitations on the possibility of detecting orbiting
planets. In general we find that the magnitude of the stellar jitter
is directly proportional to the stellar vsini. For G and K dwarfs,
we find that it is possible, for models with high stellar activity
and low stellar vsini, to be able to detect a 1 M<SUB>Jupiter</SUB>
mass planet within 50 epochs of observations and for the M dwarfs it
is possible to detect a habitable zone Earth-like planet in 10s of
observational epochs.
---------------------------------------------------------
Title: The 2MASS Tully-Fisher Survey: Mapping the mass in the Universe
Authors: Hong, T.; Staveley-Smith, L.; Masters, K.; Springob, C.;
Macri, L.; Koribalski, B.; Jones, H.; Jarrett, T.
2013IAUS..289..312H Altcode: 2012arXiv1212.2090H
The 2MASS Tully-Fisher Survey (2MTF) aims to measure Tully-Fisher (TF)
distances for all bright, inclined spirals in the 2MASS Redshift Survey
(2MRS) using high-quality HI widths and 2MASS photometry. Compared
with previous peculiar-velocity surveys, the 2MTF survey provides
more accurate width measurements and more uniform sky coverage,
combining observations with the Green Bank, Arecibo, and Parkes
telescopes. With this new redshift-independent distance database, we
will significantly improve our understanding of the mass distribution
in the local Universe.
---------------------------------------------------------
Title: VVV high proper motion survey .
Authors: Gromadzki, M.; Kurtev, R.; Folkes, S.; Beamín, J. C.; Peña
Ramírez, K.; Borissova, J.; Pinfield, D.; Jones, H.; Minniti, D.;
Ivanov, V. D.
2013MmSAI..84..980G Altcode: 2013arXiv1310.4072G
Here we present survey of proper motion stars towards the Galactic
Bulge and an adjacent plane region base on VISTA-VVV data. The
searching method is based on cross-matching photometric K_s-band CASU
catalogs. The most interesting discoveries are shown.
---------------------------------------------------------
Title: A new UKIDSS proper motion survey and key early results,
including new benchmark systems
Authors: Smith, L.; Lucas, P.; Burningham, B.; Jones, H.; Pinfield,
D.; Smart, R.; Andrei, A.
2013MmSAI..84..976S Altcode:
We present a proper motion catalogue for the 1500 deg<SUP>2</SUP> of 2
epoch J-band UKIDSS Large Area Survey (LAS) data, which includes 120,000
stellar sources with motions detected above the 5sigma level. Our
upper limit on proper motion detection is 3\farcs3 yr<SUP>-1</SUP>
and typical uncertainties are of order 10 mas yr<SUP>-1</SUP> for
bright sources from data with a modest 1.8-7.0 year epoch baseline. We
developed a bespoke proper motion pipeline which applies a source-unique
second order polynomial transformation to UKIDSS array coordinates to
counter potential local non-uniformity in the focal plane. Our catalogue
agrees well with the proper motion data supplied in the current WFCAM
Science Archive (WSA) tenth data release (DR10) catalogue where there
is overlap, and in various optical catalogues, but it benefits from some
improvements, such as a larger matching radius and relative to absolute
proper motion correction. We present proper motion results for 128 T
dwarfs in the UKIDSS LAS and key early results of projects utilising
our catalogue, in particular searches for brown dwarf benchmark systems
through cross matches with existing proper motion catalogues. We report
the discovery of two new T dwarf benchmark systems.
---------------------------------------------------------
Title: First T dwarfs in the VISTA Hemisphere Survey
Authors: Lodieu, N.; Burningham, B.; Day-Jones, A.; Scholz, R. -D.;
Marocco, F.; Koposov, S.; Barrado y Navascués, D.; Lucas, P. W.;
Cruz, P.; Lillo, J.; Jones, H.; Perez-Garrido, A.; Ruiz, M. T.;
Pinfield, D.; Rebolo, R.; Béjar, V. J. S.; Boudreault, S.; Emerson,
J. P.; Banerji, M.; González-Solares, E.; Hodgkin, S. T.; McMahon,
R.; Canty, J.; Contreras, C.
2012A&A...548A..53L Altcode: 2012arXiv1210.5148L
<BR /> Aims: The aim of the project is to improve our current knowledge
of the density of T dwarfs and the shape of the substellar initial
mass function by identifying a magnitude-limited sample of T dwarfs
in the full southern sky. <BR /> Methods: We present the results of
a photometric search aimed at discovering cool brown dwarfs in the
southern sky imaged at infrared wavelengths by the Visible and Infrared
Survey Telescope for Astronomy (VISTA) and the Wide Infrared Survey
Explorer (WISE) satellite mission. We combined the first data release
(DR1) of the VISTA Hemisphere Survey (VHS) and the WISE preliminary
data release to extract candidates with red mid-infrared colours
and near- to mid-infrared colours characteristics of cool brown
dwarfs. <BR /> Results: The VHS DR1 vs. WISE search returned tens of
T dwarf candidates, 13 of which are presented here, including two
previously published in the literature and five new ones confirmed
spectroscopically with spectral types between T4.5 and T8. We estimate
that the two T6 dwarfs lie within 16 pc and the T4.5 within 25 pc. The
remaining three are 30-50 pc distant. The only T7 dwarf in our sample
is the faintest of its spectral class with J = 19.28 mag. The other
six T dwarf candidates remain without spectroscopic follow-up. We also
improve our knowledge on the proper motion accuracy for three bright
T dwarfs by combining multi-epoch data from public databases (DENIS,
2MASS, VHS, WISE, Spitzer). <P />Based on observations made with the
Calar Alto 3.5-m telescope, the Magellan telescope at Las Campanas,
the ESO Very Large Telescope at the Paranal Observatory, and the IAC80
at Teide Observatory.Figures 1 and 2 are available in electronic form
at <A href="http://www.aanda.org">http://www.aanda.org</A>
---------------------------------------------------------
Title: Towards an Imaging Mid-Infrared Heterodyne Spectrometer
Authors: Hewagama, T.; Aslam, S.; Jones, H.; Kostiuk, T.; Villanueva,
G.; Roman, P.; Shaw, G. B.; Livengood, T.; Allen, J. E.
2012LPICo1683.1125H Altcode:
We will discuss efforts in developing a compact, low-mass, low-power,
mid-infrared imaging heterodyne spectrometer for planetary science
applications.
---------------------------------------------------------
Title: Physical parameters of the binary star CM draconis components
Authors: Kuznetsov, M. K.; Pavlenko, Ya. V.; Pinfield, D.; Jones, H.
2012KPCB...28..137K Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Mapping the Dark Matter with 6dFGS
Authors: Mould, Jeremy R.; Magoulas, C.; Springob, C.; Colless, M.;
Jones, H.; Lucey, J.; Erdogdu, P.; Campbell, L.
2012AAS...22032101M Altcode:
Fundamental plane distances from the 6dF Galaxy Redshift Survey are
fitted to a model of the density field within 200/h Mpc. Likelihood is
maximized for a single value of the local galaxy density, as expected
in linear theory for the relation between overdensity and peculiar
velocity. The dipole of the inferred southern hemisphere early type
galaxy peculiar velocities is calculated within 150/h Mpc, before
and after correction for the individual galaxy velocities predicted
by the model. The former agrees with that obtained by other peculiar
velocity studies (e.g. SFI++). The latter is only of order 150 km/sec
and consistent with the expectations of the standard cosmological model
and recent forecasts of the cosmic mach number, which show linearly
declining bulk flow with increasing scale.
---------------------------------------------------------
Title: The 6dF Galaxy Survey: Baryon Acoustic Oscillations and the
Local Hubble Constant
Authors: Beutler, Florian; Blake, C.; Colless, M.; Staveley-Smith,
L.; Jones, H.
2012AAS...21940201B Altcode:
The large-scale correlation function of the 6dF Galaxy Survey (6dFGS)
allows the detection of a Baryon Acoustic Oscillation (BAO) signal. The
low effective redshift of 6dFGS makes it a competitive and independent
alternative to Cepheids and low-z supernovae in constraining the Hubble
constant. It also depends on very different (and arguably smaller)
systematic uncertainties. We found a Hubble constant of H<SUB>0 </SUB>=
67 +/- 3.2 km/s/Mpc in agreement with the current standard cosmological
model LCDM.
---------------------------------------------------------
Title: A Search for Extreme Ultracool Objects in UKIDSS+VISTA
Authors: Zhang, Z.; Pinfield, D.; Day-Jones, A.; Burningham, B.;
Jones, H.; Lucas, P.; Gomes, J.; Ruiz, M. T.; Gallardo, J.; Jenkins, J.
2011ASPC..448.1411Z Altcode: 2011csss...16.1411Z
Brown dwarfs with thick water cloud atmospheres, ancient population
III brown dwarfs, and nearby free-floating planetary mass objects
are targets in our new discovery space. We have developed a candidate
selection process that identifies near infrared sources without optical
counterparts whose infrared/optical fluxes are not consistent with
stars, and whose infrared colors are not like those of known L and
T dwarf populations. We plan to carry out this programme over the
next 3-4 years, and effectively give UKIDSS and VISTA the capability
to measure proper motions of unusual objects in 14000 sq degs of
infrared sky. High proper motion discoveries will be fast-tracked for
spectroscopy through our ongoing 8m class telescopes initiatives.
---------------------------------------------------------
Title: Age patterns in a sample of spiral galaxies
Authors: Sánchez-Gil, M. C.; Jones, H.; Pérez, E.; Bland-Hawthorn,
J.; Alfaro, E. J.; O'Byrne, J.
2011hsa6.conf..345S Altcode: 2011arXiv1103.4147S
We present the burst ages for young stellar populations in a sample of
6 nearby spiral galaxies using a differential pixel-by-pixel analysis
of the ionized gas emission. We explore a new approach for connecting
large-scale dynamical mechanisms with star formation processes in
disk galaxies, based on burst ages derived from the Hα to far UV
(FUV) flux ratio. Images of each galaxy in Hα were taken with Taurus
Tunable Filter (TTF) and matched to FUV imaging from GALEX. The
resulting flux ratio provides a robust measure of relative age across
the disk which we discuss in terms of the large-scale dynamical
motions. Systematic effects, such as a variable initial mass function
(IMF), non-solar metallicities, variable star-formation history (SFHs),
and dust attenuation, have been considered insofar as the models have
permitted. The resulting age maps show age gradients along the spiral
arms, in addition to circumnuclear regions (M94) or in HII complexes
(IC 2574) in specific cases. Remarkably, in the case of M51 we find
evidence for a stellar age gradient along short spurs of dust lane
branching off the main spiral arms. We find that a comparison of the
Hα and FUV observations of nearby spiral galaxies is a relatively
direct way to probe burst age variations in spirals.
---------------------------------------------------------
Title: Do Disk Galaxies Have Different Central Velocity Dispersions
At A Given Rotation Velocity?
Authors: Danilovich, Taissa; Jones, H.; Mould, J.; Taylor, E.; Tonini,
C.; Webster, R.
2011AAS...21840802D Altcode: 2011BAAS..43G40802D
Hubble's classification of spiral galaxies was one
dimensional. Actually it was 1.5 dimensional, as he distinguished
barred spirals. Van den Bergh's was two dimensional: spirals
had luminosity classes too. Other schemes are summarized at
http://www.daviddarling.info/encyclopedia/G/galaxyclassification.html
<P />A more quantitative approach is to classify spiral galaxies by
rotation velocity. Their central velocity dispersion (bulge) tends to
be roughly one half of their rotation velocity (disk). There is a trend
from σ/W = 0.8 to σ/W = 0.2 as one goes from W = 100 to 500 km/s,
where W is twice the rotation velocity. But some fraction of spirals
have a velocity dispersion up to a factor of two larger than that. <P
/>In hierarchical galaxy formation models, the relative contributions
of σ and W depend on the mass accretion history of the galaxy, which
determines the mass distribution of the dynamical components such
as disk, bulge and dark matter halo. The wide variety of histories
that originate in the hierarchical mass assembly produce at any value
of W a wide range of σ/W, that reaches high values in more bulge-
dominated systems. <P />In a sense the two classifiers were both right:
spirals are mostly one dimensional, but σ/W (bulge to disk ratio)
is often larger than average. Is this a signature of merger history?
---------------------------------------------------------
Title: Reduction of SOLIS/VSM Intensity, Line Depth, and Equivalent
Width Images
Authors: Jones, Harrison P.
2011SPD....42.1515J Altcode: 2011BAAS..43S.1515J
Most user interest in the SOLIS Vector Spectromagnetograph (VSM)
centers on full-disk vector and longitudinal magnetograms which are
used for many purposes including flare prediction, field extrapolation,
and studies of the solar cycle. However, pseudo-continuum intensity,
line-depth, and equivalent-width images, which are perfectly registered
both in time and space with their corresponding magnetograms,
are carried with the standard SOLIS data analysis to Level 1
(flat-fielding and sorting of individual scan lines into "raw"
images). These quantities potentially provide important thermodynamic
information which improve feature identification and inform models of
photospheric and chromospheric structures, but the raw images contain
many defects which prevent their direct use. Least-squares spline and
polynomial algorithms are presented for compputing contrast images
which are free of both these defects and center-to-limb variation.
---------------------------------------------------------
Title: Spectral Investigations of CM Dra
Authors: Kuznetsov, M. K.; Pavlenko, Y. V.; Pinfield, D.; Jones, H.
2010OAP....23...74K Altcode:
We present an analysis of a high resolution (R=47000) echelle spectra
of the low-mass eclipsing binary CM Draconis, which were obtained on
the 4.2-m William Herschel Telescope. Spectra were obtained for various
phases of the orbit. There are some difficulties in echelle spectra
processing of cool stars, since it is hard to get energy distribution
in a large scale in such spectra. We proposed an efficient method
for making the continuum of spectrum of cool stars. We refined the
parameters (effective temperature, rotational velocity and metallicity)
of the components of the system CM Dra using the method of stellar
atmospheres. The data that we obtained are in good agreement with the
results obtained by other authors. It is indicate on efficiency of our
technique. The errors of temperature and metallicity determinations
is about 100 K and 0.3 dex respectively.
---------------------------------------------------------
Title: Scaling relations of early-type galaxies in the 6dF Galaxy
Survey
Authors: Magoulas, C.; Colless, M.; Jones, H.; Mould, J.; Springob, C.
2010HiA....15...84M Altcode:
Over 10,000 early-type galaxies from the 6dF Galaxy Survey (6dFGS)
(Jones, D. H. et al. (2009), Jones et al. (2004)) have been used
to determine the Fundamental Plane at optical and near-infrared
wavelengths. We find that a maximum likelihood fit to an explicit
three-dimensional Gaussian model for the distribution of galaxies
in size, surface brightness and velocity dispersion can precisely
account for selection effects, censoring and observational errors,
leading to precise and unbiased parameters for the Fundamental Plane
and its intrinsic scatter.
---------------------------------------------------------
Title: Other SOLIS Data: Intensity, Line Depth, and Equivalent Width
from the VSM
Authors: Jones, Harrison P.
2010shin.confE.149J Altcode:
Most user interest in the SOLIS Vector Spectromagnetograph (VSM)
has centered on full-disk vector and longitudinal magnetograms
which are used for many purposes including flare prediction, field
extrapolation, and studies of the solar cycle. However, additional
thermodynamic information, is available which can potentially extend
and improve the usefulness of VSM observations for tasks such as
feature identification and informing models of photospheric and
chromospheric structures. Pseudo-continuum intensity, line-depth, and
equivalent-width images, which are perfectly registered both in time
and space with their corresponding magnetograms, are carried with the
standard SOLIS data analysis to Level 1 (flat-fielding and sorting of
individual scan lines into
---------------------------------------------------------
Title: Statistical Feature Recognition for Multidimensional Solar
Imagery
Authors: Turmon, Michael; Jones, Harrison P.; Malanushenko, Olena V.;
Pap, Judit M.
2010SoPh..262..277T Altcode: 2010SoPh..tmp...52T
A maximum a posteriori (MAP) technique is developed to identify solar
features in cotemporal and cospatial images of line-of-sight magnetic
flux, continuum intensity, and equivalent width observed with the
NASA/National Solar Observatory (NSO) Spectromagnetograph (SPM). The
technique facilitates human understanding of patterns in large data
sets and enables systematic studies of feature characteristics for
comparison with models and observations of long-term solar activity
and variability. The method uses Bayes' rule to compute the posterior
probability of any feature segmentation of a trio of observed
images from per-pixel, class-conditional probabilities derived from
independently-segmented training images. Simulated annealing is used
to find the most likely segmentation. New algorithms for computing
class-conditional probabilities from three-dimensional Gaussian
mixture models and interpolated histogram densities are described and
compared. A new extension to the spatial smoothing in the Bayesian
prior model is introduced, which can incorporate a spatial dependence
such as center-to-limb variation. How the spatial scale of training
segmentations affects the results is discussed, and a new method for
statistical separation of quiet Sun and quiet network is presented.
---------------------------------------------------------
Title: Analysis of Ca II 8542 Å scanning spectroscopy for statistical
feature recognition.
Authors: Malanushenko, O.; Jones, H.; Turmon, M.; Pap, J.
2010MmSAI..81..801M Altcode:
Previously, we used Bayesian methods to recognize active regions (AR),
enhanced magnetic network (EN), and sunspots (SS) in National Solar
Observatory/Kitt Peak Vacuum Telescope synoptic observations. In this
paper we study imaging spectroscopy of the chromospheric Ca II 8542
Å and photospheric Fe I 8688 Å lines to improve separation of ARs
and EN. We find that correlation plots between Ca line-center and ±
0.45 Å line-wing intensities show two identifiable but overlapping
distributions. The first includes ARs (bright and faint) and the second
includes ENs, network, and moat (“quiet Sun”). Active and Quiet
distributions overlap in areas of EN and faint AR, so that feature
identification using thresholds is unreliable. The statistical
methodology of our previous work, however, is particularly well
suited for distinguishing features with such partially overlapping
distributions. Additionally, we find features in the Ca line which
are not visible in the Fe observations, including a dark moat around
an AR and narrow dark points associated with network and strong
line-of-sight flows.
---------------------------------------------------------
Title: Solar Irradiance Variations Related to Intensity and Magnetic
Flux of Solar Features
Authors: Pap, Judit M.; Jones, H.; Parker, D.; Chapman, G.; Floyd, L.
2010cosp...38.1783P Altcode: 2010cosp.meet.1783P
Solar total and spectral irradiance have been measured since late
1978. These measurements have demonstrated that solar irradiance changes
from minutes to the 11-year solar cycle. Con-sidering the astrophysical
and climate importance of irradiance variations, considerable efforts
have been put forward to develop irradiance models to explain the origin
of irradiance varia-tions and have information for those time intervals
when measurements don't exist. However, most of the current models are
simple empirical models, using the Photometric Sunspot Index to describe
the darkening effect of sunspots and either the CaK index or the Mg II
h k core-to wing ratio to describe the facular excess flux. While these
models can explain reasonably well the short-term variations, long-term
variations over years to the cycle are not well-accounted. Since the
SOHO era we have combined the MDI intensity images and magnetograms
to ac-count for the effect and the role of active region evolution
to irradiance variations. Similar studies have been done routinely
at the San Fernando Observatory, California State University. More
recently we have used the SPM data from NSO Kitt Peak to deduct various
activity components, and new efforts at UCLA are in progress to develop
a sophisticated method to identify various features. Using observations
by SDO/HMI we will have further insight into active region evolution,
especially during the rising portion of cycle 24, following the long
and deep minimum of cycle 23. In this paper we compare data derived
from various images and compare them to irradiance variations. One of
the main goals is to identify weak magnetic fields and estimate their
contribution to irradiance changes. We will study cycle 23 in detail,
and will discuss how the used methods and techniques can be applied
to HMI on SDO.
---------------------------------------------------------
Title: Comparison of Independent Feature Recognition Method for
Time Series Analysis of Irradiance Variations Based on Statistical
Feature Recognition
Authors: Pap, Judit M.; Bertello, L.; Chapman, G.; Floyd, L. E.;
Jones, H.; Malanushenko, E.; Preminger, D.; Turmon, M.
2009SPD....41.0934P Altcode:
Solar total and UV irradiances have been observed over three decades,
and recently spectral irradiance data are available from the Solar
Irradiance Monitor (SIM) on the SORCE Mission. Results of these
measurements show that irradiance varies on various time scales from
minutes to decades. To better understand the origin of irradiance
changes, we need to use spatially resolved data rather than full
disk indices. For this purpose various automated image processing
and analyses techniques have been developed. Using these image
processing techniques, we separated quiet-sun, network, faculae and
sunspots. On one hand, we compare the area data of these features
derived from various images to validate results and discuss future
efforts needed to coordinate efforts between various groups working
on image analysis. Another goal is to compare the variations of the
identified features with total solar and UV irradiances to establish
to what degree <P />the identified images explain short and long-term
irradiance variations.
---------------------------------------------------------
Title: Experimental and Theoretical Characterization of the ANDE
Wind and Temperature Spectrometer (WATS)
Authors: Fenn, D.; Syrstad, E. A.; Dyer, J. S.; Vancil, B.; Roman,
P.; Jones, H.; Herrero, F.; Finne, T. T.; Nicholas, A. C.
2009AGUFMSA23A1463F Altcode:
The Wind and Temperature Spectrometer (WATS), developed at NASA-GSFC
and NRL, is currently flying aboard the Atmospheric Neutral Density
Experiment (ANDE). The primary mission objective of ANDE is validation
and improvement of spacecraft drag and thermospheric models by
measurement of the total atmospheric density. Drag determination
also requires accurate measurements of neutral wind, temperature, and
composition (O/N2 ratio). WATS provides the unprecedented capability to
simultaneously measure all of these parameters in situ, by analyzing
the angular and energy distribution of the gas stream passing its
entrance aperture. WATS imposes very low power and size requirements
on the host spacecraft, and is suitable for integration with small
satellite platforms such as CubeSat. After passing through a pair
of mutually-perpendicular collimating slits, neutrals are ionized
by electron impact and energy analyzed by a crossed Small Deflection
Energy Analyzer (SDEA) pair. The angular distribution of ions exiting
the SDEA pair is measured by a microchannel plate (MCP) detector with
linear spatial readout. The peak of this distribution indicates the
neutral stream velocity vector in spectrometer coordinates, while the
energy distribution yields the magnitude of this vector. Specification
of the full neutral wind follows from knowledge of the satellite
pointing angle. The width and shape of the angular distribution allows
determination of the neutral temperature. Additionally, the high
satellite velocity allows mass separation of the major thermospheric
constituents by energy analysis. For example, at 7500 m/s, O and N2
have kinetic energies of 4.7 and 8.2 eV, respectively, and are readily
resolved by the SDEA. This paper describes theoretical and experimental
efforts aimed to characterize WATS performance, validate instrument and
component functionality, augment sensor calibration, and improve data
analysis. Much of this work has involved ion trajectory simulations
(SIMION 3D) to characterize the operational parameters and performance
of the crossed SDEA pair. Due to the intersecting SDEA volume and
resulting potential field perturbations, energy analysis of low-angle
ions traveling near the instrument axis requires greater voltages than
predicted for a single SDEA. Additionally, the SDEA configuration in
WATS includes an open drift region between the ion source aperture
and analyzer entrance, which promotes ion beam divergence and yields
less-than-ideal energy resolution. We present a promising deflection
lens design predicted to collimate incident ion beams and significantly
improve energy resolution. Also presented is experimental performance
data for a novel low-power thermionic cathode (BaO-coated tungsten wire)
that acts as the source of ionizing electrons in WATS. Additionally,
ongoing laboratory experiments aim to characterize angle-dependent
SDEA performance testing using a monoenergetic ion beam.
---------------------------------------------------------
Title: GAMA: towards a physical understanding of galaxy formation
Authors: Driver, Simon P.; Norberg, Peder; Baldry, Ivan K.; Bamford,
Steven P.; Hopkins, Andrew M.; Liske, Jochen; Loveday, Jon; Peacock,
John A.; Hill, D. T.; Kelvin, L. S.; Robotham, A. S. G.; Cross,
N. J. G.; Parkinson, H. R.; Prescott, M.; Conselice, C. J.; Dunne,
L.; Brough, S.; Jones, H.; Sharp, R. G.; van Kampen, E.; Oliver, S.;
Roseboom, I. G.; Bland-Hawthorn, J.; Croom, S. M.; Ellis, S.; Cameron,
E.; Cole, S.; Frenk, C. S.; Couch, W. J.; Graham, A. W.; Proctor, R.;
De Propris, R.; Doyle, I. F.; Edmondson, E. M.; Nichol, R. C.; Thomas,
D.; Eales, S. A.; Jarvis, M. J.; Kuijken, K.; Lahav, O.; Madore, B. F.;
Seibert, M.; Meyer, M. J.; Staveley-Smith, L.; Phillipps, S.; Popescu,
C. C.; Sansom, A. E.; Sutherland, W. J.; Tuffs, R. J.; Warren, S. J.
2009A&G....50e..12D Altcode: 2009arXiv0910.5123D
Simon P Driver, Peder Norberg, Ivan K Baldry, Steven P Bamford,
Andrew M Hopkins, Jochen Liske, Jon Loveday, John A Peacock and
the GAMA Survey Team (Galaxy and Mass Assembly) review progress on
the latest large galaxy redshift survey now underway on the 3.9 m
Anglo-Australian Telescope.
---------------------------------------------------------
Title: Training Sets for Statistical Feature Recognition in
Multidimensional Solar Imagery
Authors: Jones, Harrison P.; Turmon, M. J.; Malanushenko, O. V.; Pap,
J. M.
2009SPD....40.1518J Altcode:
We have previously reported the multi-dimensional extension of a
statistical maximum likelihood algorithm for segmenting images into
different feature classes developed by Turmon, Pap, and Mukhtar
(2002, ApJ 568, p. 396). The method works best for features which
have overlapping but nonetheless distinct distributions of observed
variables. Developing these empirical class-conditional distributions
from independently classified training sets depends sensitively on
the match of spatial scales between the training segmentations and
the desired feature classes. We discuss recent progress in extracting
well-posed class distributions even when the training segmentations
are mixtures of the classes which we wish to identify. For example,
in addition to large-scale labelings, Harvey and White (1999, ApJ
515, p. 812) provide finely grained information which we use to help
isolate areas of pure quiet Sun. Quiet Sun distributions of observed
quantities can then be separated from distributions derived from
areas labeled as network which also include quiet Sun. Similarly,
these distributions can then be isolated from those mixed with active
regions and/or sunspots. This research is funded by a NASA Supporting
Research and Technology grant.
---------------------------------------------------------
Title: Galaxy And Mass Assembly (GAMA)
Authors: Driver, Simon P.; GAMA Team; Baldry, I. K.; Bamford, S.;
Bland-Hawthorn, J.; Bridges, T.; Cameron, E.; Conselice, C.; Couch,
W. J.; Croom, S.; Cross, N. J. G.; Driver, S. P.; Dunne, L.; Eales, S.;
Edmondson, E.; Ellis, S. C.; Frenk, C. S.; Graham, A. W.; Jones, H.;
Hill, D.; Hopkins, A.; van Kampen, E.; Kuijken, K.; Lahav, O.; Liske,
J.; Loveday, J.; Nichol, B.; Norberg, P.; Oliver, S.; Parkinson,
H.; Peacock, J. A.; Phillipps, S.; Popescu, C. C.; Prescott, M.;
Proctor, R.; Sharp, R.; Staveley-Smith, L.; Sutherland, W.; Tuffs,
R. J.; Warren, S.
2009IAUS..254..469D Altcode: 2008arXiv0807.0376D
The GAMA survey aims to deliver 250,000 optical spectra (3-7
Å resolution) over 250 sq. degrees to spectroscopic limits of
r<SUB>AB</SUB> < 19.8 and K<SUB>AB</SUB> < 17.0 mag. Complementary
imaging will be provided by GALEX, VST, UKIRT, VISTA, HERSCHEL and
ASKAP to comparable flux levels leading to a definitive multi-wavelength
galaxy database. The data will be used to study all aspects of cosmic
structures on 1kpc to 1Mpc scales spanning all environments and out
to a redshift limit of z ≈ 0.4. Key science drivers include the
measurement of: the halo mass function via group velocity dispersions;
the stellar, HI, and baryonic mass functions; galaxy component mass-size
relations; the recent merger and star-formation rates by mass, types and
environment. Detailed modeling of the spectra, broad SEDs, and spatial
distributions should provide individual star formation histories,
ages, bulge-disc decompositions and stellar bulge, stellar disc, dust
disc, neutral HI gas and total dynamical masses for a significant
subset of the sample (~ 100k) spanning both the giant and dwarf
galaxy populations. The survey commenced March 2008 with 50k spectra
obtained in 21 clear nights using the Anglo Australian Observatory's
new multi-fibre-fed bench-mounted dual-beam spectroscopic system (AAΩ).
---------------------------------------------------------
Title: Darwin-A Mission to Detect and Search for Life on Extrasolar
Planets
Authors: Cockell, C. S.; Léger, A.; Fridlund, M.; Herbst, T. M.;
Kaltenegger, L.; Absil, O.; Beichman, C.; Benz, W.; Blanc, M.; Brack,
A.; Chelli, A.; Colangeli, L.; Cottin, H.; Coudé du Foresto, V.;
Danchi, W. C.; Defrère, D.; den Herder, J. -W.; Eiroa, C.; Greaves,
J.; Henning, T.; Johnston, K. J.; Jones, H.; Labadie, L.; Lammer,
H.; Launhardt, R.; Lawson, P.; Lay, O. P.; LeDuigou, J. -M.; Liseau,
R.; Malbet, F.; Martin, S. R.; Mawet, D.; Mourard, D.; Moutou, C.;
Mugnier, L. M.; Ollivier, M.; Paresce, F.; Quirrenbach, A.; Rabbia,
Y. D.; Raven, J. A.; Rottgering, H. J. A.; Rouan, D.; Santos, N. C.;
Selsis, F.; Serabyn, E.; Shibai, H.; Tamura, M.; Thiébaut, E.;
Westall, F.; White, G. J.
2009AsBio...9....1C Altcode: 2008arXiv0805.1873C
The discovery of extrasolar planets is one of the greatest achievements
of modern astronomy. The detection of planets that vary widely in mass
demonstrates that extrasolar planets of low mass exist. In this paper,
we describe a mission, called Darwin, whose primary goal is the search
for, and characterization of, terrestrial extrasolar planets and the
search for life. Accomplishing the mission objectives will require
collaborative science across disciplines, including astrophysics,
planetary sciences, chemistry, and microbiology. Darwin is designed
to detect rocky planets similar to Earth and perform spectroscopic
analysis at mid-infrared wavelengths (6-20 μm), where an advantageous
contrast ratio between star and planet occurs. The baseline mission is
projected to last 5 years and consists of approximately 200 individual
target stars. Among these, 25-50 planetary systems can be studied
spectroscopically, which will include the search for gases such as
CO<SUB>2</SUB>, H<SUB>2</SUB>O, CH<SUB>4</SUB>, and O<SUB>3</SUB>. Many
of the key technologies required for the construction of Darwin
have already been demonstrated, and the remainder are estimated to
be mature in the near future. Darwin is a mission that will ignite
intense interest in both the research community and the wider public.
---------------------------------------------------------
Title: The application of Gaussian Mixture and Histogram-based
Bayesian methods to NSO/Kitt Peak VT data.
Authors: Malanushenko, O.; Jones, H. P.; Turmon, M.; Pap, J.
2008AGUFMSH13A1519M Altcode:
We applied Gaussian Mixture and Histogram-based Bayesian methods to
recognize several solar features using Kitt Peak Vacuum Telescope
(VT) observations from 1992-2003. We used 5D observations in the
868.8 nm line including LoS magnetic field, continuum intensity,
radial velocity, line depth, and EqW. We applied the analysis for
recognition of active regions, magnetic network, and sunspots, for
the purpose of automatic recognition of solar activity, and linking
solar activity to irradiance changes. The success of such a feature
recognition process strongly depends on separation and sensitivity
of observable and derivative parameters for different features. For
some features it works very well for two kind of data, but in some
other cases the probability of correct recognition of a feature is low
without the adding complementary data. We discuss the advantages and
limitations of these statistical methods, review the importance and
possibility of using the complementary data, and compare our results
with other methods which derive feature areas. This methodological
review will help to create the strategy for new SDO/HMI analysis.
---------------------------------------------------------
Title: Spectral Irradiance Variations and Magnetic Field Changes
During Solar Cycle 23.
Authors: Pap, J. M.; Bertello, L.; Chapman, G.; Floyd, L. E.; Harder,
J.; Jones, H.; Malanuskenko, O.; Preminger, D.; Turmon, M.
2008AGUFMSH13A1504P Altcode:
Both total irradiance and the Mg core-to-wing ratio was high at the
maximum of weak solar cycle 23. However, photometric observations
from the San Fernando Observatory show that both the number and size
of active regions (spots and faculae) were low at the maximum of
solar cycle 23 which points to the importance of the role of weak
magnetic fields in irradiance variations. The purpose of this paper
is to use new SOLIS spectromagnetograph observations in conjunction
with a newly developed image analysis technique to compare irradiance
time series as function of wavelengths with various surface magnetic
features. One major goal is to compare features derived from the
SOLIS images using the new technique with well-established features
from SFO. Another important goal is to determine the contribution
of active regions/weak fields to irradiance variations at various
wavelengths, using the SOHO/VIRGO and SORCE/SIM data. A third goal
is to determine the extent of irradiance variations not explained by
magnetic structures. To do this, we use a new analysis technique to
evaluate SOLIS spectromagnetograph observations.
---------------------------------------------------------
Title: Using SPICA Space Telescope to characterize Exoplanets
Authors: Goicoechea, J. R.; Swinyard, B.; Tinetti, G.; Nakagawa, T.;
Enya, K.; Tamura, M.; Ferlet, M.; Isaak, K. G.; Wyatt, M.; Aylward,
A. D.; Barlow, M.; Beaulieu, J. P.; Boccaletti, A.; Cernicharo, J.;
Cho, J.; Claudi, R.; Jones, H.; Lammer, H.; Leger, A.; Martín-Pintado,
J.; Miller, S.; Najarro, F.; Pinfield, D.; Schneider, J.; Selsis,
F.; Stam, D. M.; Tennyson, J.; Viti, S.; White, G.
2008arXiv0809.0242G Altcode:
We present the 3.5m SPICA space telescope, a proposed Japanese-led
JAXA-ESA mission scheduled for launch around 2017. The actively cooled
(<5 K), single aperture telescope and monolithic mirror will
operate from ~3.5 to ~210 um and will provide superb sensitivity in
the mid- and far-IR spectral domain (better than JWST at lambda >
18 um). SPICA is one of the few space missions selected to go to the
next stage of ESA's Cosmic Vision 2015-2025 selection process. In this
White Paper we present the main specifications of the three instruments
currently baselined for SPICA: a mid-infrared (MIR) coronagraph
(~3.5 to ~27 um) with photometric and spectral capabilities (R~200),
a MIR wide-field camera and high resolution spectrometer (R~30,000),
and a far-infrared (FIR ~30 to ~210 um) imaging spectrometer - SAFARI
- led by a European consortium. We discuss their capabilities in the
context of MIR direct observations of exo-planets (EPs) and multiband
photometry/high resolution spectroscopy observations of transiting
exo-planets. We conclude that SPICA will be able to characterize the
atmospheres of transiting exo-planets down to the super-Earth size
previously detected by ground- or space-based observatories. It will
also directly detect and characterize Jupiter/Neptune-size planets
orbiting at larger separation from their parent star (>5-10 AU),
by performing quantitative atmospheric spectroscopy and studying
proto-planetary and debris disks. In addition, SPICA will be a
scientific and technological precursor for future, more ambitious, IR
space missions for exo-planet direct detection as it will, for example,
quantify the prevalence exo-zodiacal clouds in planetary systems and
test coronographic techniques, cryogenic systems and lightweight,
high quality telescopes. (abridged)
---------------------------------------------------------
Title: Feature Classification of NSO/Kitt Peak Magnetograms
Authors: Malanushenko, O.; Jones, H. P.; Pap, J. M.; Turmon, M.
2008AGUSMSP31B..04M Altcode:
We present new segmentations of daily NASA/NSO Spectromagnetograph
(SPM) multidimensional magnetograms obtained at the NSO/Kitt Peak
Vacuum Telescope from 1992-2003. Full-disk images are divided into
areas of quiet Sun, network, active regions, and sunspots using a
three-dimensional adaptation of a statistical image classification
method developed by Turmon, Pap, and Mukhtar (ApJ 568:396-407,
2002). Probability distributions for each feature class are derived
from a training set of images independently segmented using thresholds
in magnetic flux and continuum intensity. We summarize our analysis
procedures and compare segmentations derived from class-conditional
probabilities computed with Gaussian mixture models and histogram
interpolation. We also compare our segmentations with features
identified by other methods and with solar irradiance variation.
---------------------------------------------------------
Title: A Comparison of Feature Classification Methods for Modeling
Solar Irradiance Variation
Authors: Jones, H. P.; Chapman, G. A.; Harvey, K. L.; Pap, J. M.;
Preminger, D. G.; Turmon, M. J.; Walton, S. R.
2008SoPh..248..323J Altcode:
Physical understanding of total and spectral solar irradiance variation
depends upon establishing a connection between the temporal variability
of spatially resolved solar structures and spacecraft observations of
irradiance. One difficulty in comparing models derived from different
data sets is that the many ways for identifying solar features such as
faculae, sunspots, quiet Sun, and various types of "network" are not
necessarily consistent. To learn more about classification differences
and how they affect irradiance models, feature "masks" are compared as
derived from five current methods: multidimensional histogram analysis
of NASA/National Solar Observatory/Kitt Peak spectromagnetograph data,
statistical pattern recognition applied to SOHO/Michelson Doppler
Imager photograms and magnetograms, threshold masks allowing for
influence of spatial surroundings applied to NSO magnetograms, and
"one-trigger" and "three-trigger" algorithms applied to California
State University at Northridge Cartesian Full Disk Telescope intensity
observations. In general all of the methods point to the same areas of
the Sun for labeling sunspots and active-region faculae, and available
time series of area measurements from the methods correlate well with
each other and with solar irradiance. However, some methods include
larger label sets, and there are important differences in detail,
with measurements of sunspot area differing by as much as a factor
of two. The methods differ substantially regarding inclusion of fine
spatial scale in the feature definitions. The implications of these
differences for modeling solar irradiance variation are discussed.
---------------------------------------------------------
Title: The Southern 2MASS Red AGN Survey: Spectroscopic Observations
with 6dF
Authors: Masci, Franco; Cutri, R.; Francis, P.; Nelson, B.; Huchra,
J.; Jones, H.; Colless, M.; Saunders, W.
2008AAS...21115709M Altcode:
Following the success of The Two Micron All-Sky Survey (2MASS) in
revealing large numbers of new optically red AGN and QSOs, we report
on an extension of this search in the Southern equatorial sky using the
Six Degree Field (6dF) multifibre spectrograph. Near-IR selected samples
are more sensitive to objects whose optical emission may be reddened by
dust, or is intrinsically weak. Our sample of red AGN candidates was
selected using a single color cut of J-Ks > 2 mag and a galactic
latitude |b| > 30 deg. For comparison, most optical/UV-selected
QSOs and (quiescent) galaxies at redshifts z< 0.4 have colors
of J-Ks < 2 mag. A subsample of 6386 candidates with Bj < 19
and rF < 18 were selected as auxiliary targets for the 6dF Galaxy
Redshift Survey. Spectra were obtained for 1182 objects. Approximately
700 are of sufficient quality to enable a reliable identification. We
present the results of the classification of the 6dF spectra, making
use of Bj, R (SuperCOSMOS) and J, H, Ks (2MASS) images to assist in
the identification process. We quantify the AGN content, types, host
morphologies (i.e., whether point-like or extended), and compare their
properties to those of AGN discovered at other wavelengths.
---------------------------------------------------------
Title: Physical and orbital properties of the Trojan asteroids
Authors: Melita, M. D.; Licandro, J.; Jones; C., D.; Williams, I. P.
2008arXiv0801.2497M Altcode:
All the Trojan asteroids orbit about the Sun at roughly the same
heliocentric distance as Jupiter. Differences in the observed visible
reflection spectra range from neutral to red, with no ultra-red
objects found so far. Given that the Trojan asteroids are collisionally
evolved, a certain degree of variability is expected. Additionally,
cosmic radiation and sublimation are important factors in modifying
icy surfaces even at those large heliocentric distances. We search for
correlations between physical and dynamical properties, we explore
relationships between the following four quantities; the normalised
visible reflectivity indexes ($S'$), the absolute magnitudes, the
observed albedos and the orbital stability of the Trojans. We present
here visible spectroscopic spectra of 25 Trojans. This new data increase
by a factor of about 5 the size of the sample of visible spectra of
Jupiter Trojans on unstable orbits. The observations were carried
out at the ESO-NTT telescope (3.5m) at La Silla, Chile, the ING-WHT
(4.2m) and NOT (2.5m) at Roque de los Muchachos observatory, La Palma,
Spain. We have found a correlation between the size distribution and the
orbital stability. The absolute-magnitude distribution of the Trojans
in stable orbits is found to be bimodal, while the one of the unstable
orbits is unimodal, with a slope similar to that of the small stable
Trojans. This supports the hypothesis that the unstable objects are
mainly byproducts of physical collisions. The values of $S'$ of both
the stable and the unstable Trojans are uniformly distributed over a
wide range, from $0 %/1000Å$ to about $15 %/1000Å$. The values for
the stable Trojans tend to be slightly redder than the unstable ones,
but no significant statistical difference is found.
---------------------------------------------------------
Title: The PRVS Pathfinder
Authors: Ramsey, Lawrence W.; Redman, S.; Wolszczan, A.; Jones, H.;
Barnes, J.
2007AAS...211.1118R Altcode: 2007BAAS...39..747R
The Precision Radial Velocity Spectrometer (PRVS) is a fiber coupled
near infrared (NIR) spectrometer being designed for the Gemini
International Observatory specifically to search for planets around
M stars. These stars emit most of their flux at wavelengths between 1
and 2 microns. These low mass stars are the most likely place where PRV
techniques will allow detection of earth mass planets in the so called
"Habitable Zone". The pathfinder instrument has become a significant
tool in mitigating design, performance and cost risks for the PRVS. Last
year we demonstrated the ability to detect radial velocity variations
at the 10-15 meter/sec level. Since then, we have made significant
progress in our understanding of the limitations of the PRVS in the
NIR. In particular, we present the latest improvements we have made to
the calibration spectra, as well as the characterization and suppression
of the modal noise in the optical fibers.
---------------------------------------------------------
Title: Application of Statistical Image Segmentation to Recognition
of Solar Magnetic Network
Authors: Jones, H. P.; Malanushenko, O. V.; Pap, J. M.; Turmon, M. J.
2007AGUFMSH13A1096J Altcode:
We have developed a statistical method for feature identification in NSO
multidimensional imagery which requires a training set of independently
determined image segmentations. The large spatial scale of our initial
training set determined by the algorithm of Harvey and White (1999, ApJ
515, p. 812) mixes the details of magnetic network which are contained
in the observations with quiet Sun and other features. We have found
it difficult to reproduce this large scale in models of conditional
and prior probabilities and are in fact interested in marking smaller
scale structures for comparison with variation of total and spectral
solar irradiance. We describe in this paper the performance of our
technique with finer scale training sets determined by observations
from other instruments and independently for the NSO data.
---------------------------------------------------------
Title: 2MTF - The 2MASS Tully-Fisher Survey
Authors: Masters, Karen L.; Huchra, J. P.; Crook, A. C.; Macri, L. M.;
Jarrett, T.; Koribalski, B.; Staveley-Smith, L.; Jones, H.; Springob,
C. M.
2007AAS...210.8403M Altcode: 2007BAAS...39..193M
The 2MASS Tully-Fisher survey (2MTF) is making use of existing high
quality rotations widths, new HI widths and 2MASS photometry to measure
Tully-Fisher (TF) distances/peculiar velocities for all bright inclined
spirals in the 2MASS redshift survey (2MRS). 2MRS has already provided
the best nearby galaxy density field, so we know where the baryons
are. The local universe is the only place where peculiar velocity
measurements are sufficiently accurate to compare this with the
distribution of mass. In the linear regime peculiar velocities are
directly proportional to the underlying gravity. Previous peculiar
velocity surveys have struggled to meet their potential because of
large errors on individual measurements, poor statistics and uneven
sky coverage. A survey based on 2MRS will provide significantly
more uniform sky coverage than has previously been available,
providing a qualitatively better sample for velocity--density field
reconstructions. Better coverage in the ZoA will also aid in studies
of the "Great Attractor” region. We provide a progress report on the
2MTF survey including a first look at over 300 hours of HI observations
at GBT, a report on ongoing southern hemisphere observations with the
Parkes Radio Telescope and a preview of a universal 2MASS Tully-Fisher
relation. KLM is supported by NSF grant AST-0406906.
---------------------------------------------------------
Title: Statistical Feature Recognition for Multidimensional NSO
Imagery
Authors: Malanushenko, Elena; Jones, H. P.; Pap, J. M.; Turmon, M. J.
2007AAS...210.2406M Altcode: 2007BAAS...39..129M
Turmon, Pap, and Mukhtar (2002: Astrophysical Journal 568, 396)
present a statistical method for identifying sunspots, faculae, and
quiet Sun region classes in co-registered SOHO/MDI magnetograms and
intensity images. This paper describes progress toward an extension
of this method for finding a more complete region classification
using multidimensional images (magnetic flux, line-of-sight velocity,
intensity, equivalent width, and central line depth) obtained from
1992-2003 with the NASA/NSO Spectromagnetograph (SPM) and since 2003
with the NSO/SOLIS Vector Spectromagnetograph (VSM). We discuss the
selection of the feature set, training images, and the temporal and
spatial consistency of the NSO data. We determine class-conditional
probability densities using both Gaussian mixture models and direct
histogram interpolation, and compare feature labelings driven by
both methods.
---------------------------------------------------------
Title: Bayesian Feature Recognition for Multidimensional NSO Imagery
Authors: Jones, H. P.; Pap, J. M.; Turmon, M. J.
2006AGUFMSH23B0372J Altcode:
Turmon, Pap, and Mukhtar (2002: Astrophysical Journal 568, 396) present
a statistical method for identifying sunspots, faculae, and quiet Sun
in SOHO/MDI magnetograms and intensity images. This paper describes
progress toward an extension of this method for identifying more
complete feature sets using the multidimensional images (magnetic flux,
line-of-sight velocity, intensity, equivalent width, and central line
depth) obtained from 1992-2003 with the NASA/NSO Spectromagnetograph
(SPM) and since 2003 with the NSO/SOLIS Vector Spectromagnetograph
(VSM). We discuss the selection of the feature set and training images,
and the temporal and spatial consistency of the NSO data. We determine
the class-conditional (Bayesian prior) probability densities using
both Gaussian mixture models and direct histogram interpolation,
and show projections of the multidimensional probability densities
derived from SPM observations. Finally, we compare various feature
identification methods driven by these two types of prior.
---------------------------------------------------------
Title: High Spectral Resolution Study of the He 10830 Spectral Region
Authors: Malanushenko, O.; Livingston, W.; Jones, H.; Malanushenko,
V. P.
2005ASPC..346..389M Altcode:
The He 1083 nm line, formed in the upper chromosphere, is used for
observations of coronal holes (CHs) near their origins at the solar
surface. The weak He profiles in CHs show some peculiarities such
as asymmetry, broadening, and different ratios between spectral
components. These effects are small and the influence of disturbing
noise and approximations in reductions may be crucial for their
definition. In the present work we used low noise and high spectral
resolution observations carried out at the Kitt Peak McMath-Pierce
telescope to establish the key characteristics of He profile. The
shape of He profile is affected by telluric water line and we suggest
a method for its correction. Also there are solar lines that lie
between the main and second He components and overlap with both. If
the He line is weak and blue shifted, as in a CH and in cell centers,
the blends distort the visual shape of the main component and obscure
the second component. As an example we analyze two integral spectra
of CH and quiet Sun and confirm the broadening and minor blue shift of
the He line in a CH. This result must be considered to be preliminary
and the work is in progress.
---------------------------------------------------------
Title: Magnetic Fields and Flows in Open Magnetic Structures
Authors: Jones, H. P.
2005ASPC..346..229J Altcode:
Open magnetic structures connect the solar surface to the heliosphere
and are thus of great interest in solar-terrestrial physics. This
paper is a selective observational review of what is known about
magnetic fields and outward flows in such regions with special focus
on coronal holes and origins of the fast solar wind. First evidence
of the connection between these two features was seen in Skylab data
after the discovery of coronal holes whose solar roots are now known to
be in unipolar photospheric regions. Subsequently many observations of
have been made, ranging from oscillations in the underlying photosphere
and chromosphere, to possible beginnings of the solar wind as observed
by Doppler shifts in high chromospheric and transition-region lines,
to coronagraphic time-lapse studies of outward-moving material which
perhaps trace elements of solar-wind plasma. Some of the many unresolved
and controversial issues regarding details of these observations and
their association with the solar wind will be discussed.
---------------------------------------------------------
Title: New high eccentricity planets from the AAT
Authors: Jones, H.; Anglo-Australian Planet Search Team
2005DPS....37.2801J Altcode: 2005BAAS...37..671J
The Anglo-Australian Planet Search is a long-term programme being
carried out on the Anglo-Australian Telescope to search for giant
planets around nearby Solar type stars. We began observing in January
1998 observing 200 target stars over 20 nights per year, and have very
recently grown to more than 60 nights per year targetting an expanded
sample. Twenty planet candidates with M sin i values ranging from 0.2
to 10 Mjup have been found from the programme, four planet candidates
have been confirmed using our data and several found by other programmes
disputed. Our precision Doppler velocity measurements are made with the
an echelle spectrograph with an iodine absorption cell. The iodine cell
enables us to achieve measured long-term velocity stability of 2 m/s
(for suitably stable stars) down to our survey magnitude limit. This
stability will be discussed in the context of our latest results
which include the discovery of two highly elliptical planets. <P
/>We acknowledge support for this programme by the partners of the
Anglo-Australian Telescope agreement as well as from NSF and NASA.
---------------------------------------------------------
Title: The 6dF Galaxy Survey: First Data Release
Authors: Jones, H.; Saunders, W.; Colless, M.; Read, M.; Parker, Q.;
Watson, F.; Campbell, L.
2005ASPC..329...11J Altcode:
The 6dF Galaxy Survey (6dFGS) is currently measuring the redshifts
of around 170 000 galaxies and the peculiar velocities of a 15
000-member sub-sample. It will be the largest redshift survey of
the local universe and more than an order of magnitude larger than
any peculiar velocity survey to date. When complete, it will cover
essentially the entire southern sky around a mean redshift of z =
0.05. Central to the survey is the Six-Degree Field (6dF) multi-fibre
spectrograph, an instrument able to record 150 simultaneous spectra
over the 5.7°-field of the UK Schmidt Telescope. Targets have been
drawn from the 2MASS Extended Source Catalog (XSC) to include all
galaxies brighter than K<SUB>tot</SUB> = 12.75, supplemented by 2MASS
and SuperCOSMOS galaxies that complete the sample to limits of (H, J,
r<SUB>F</SUB>, b<SUB>J</SUB>) = (13.05, 13.75, 15.6, 16.75). Here we
describe the implementation of the survey and the procedures used to
select sources and determine redshifts. We also describe early results
utilising the First Data Release of ∼ 45 000 redshifts. There is
an online database of 6dFGS data accessible from the 6dFGS web site
(http://www.mso.anu.edu.au/6dFGS).
---------------------------------------------------------
Title: Reduction of SOLIS/Vector Spectromagnetograph He I 1083
nm Observations
Authors: Jones, H. P.; Malanushenko, O. V.; Harvey, J. W.; Henney,
C. J.; Keller, C. U.
2005AGUSMSP51A..02J Altcode:
The SOLIS/Vector Spectromagnetograph (VSM) now continues the
three-decade record of full-disk He I 1083 nm spectroheliograms from
NSO/Kitt Peak (see poster by Henney et al.). Although the sensitivity
of the VSM interim cameras at 1083 nm is far greater than that of
previous NSO/KP instruments, the observations are compromised by
strong interference fringes produced within the detectors. We discuss
in some detail the extent to which this difficulty is overcome
in the simple algorithm used to produce the synoptic observations
and explore methods for removing remaining fringe effects for true
imaging spectroscopy. These techniques include Fourier and Wavelet
filtering, the flat-fielding algorithm used for earlier NASA/NSO
Spectromagnetograph (SPM) observations, and physical modeling of the
detector fringe pattern.
---------------------------------------------------------
Title: The He I 1083 nm line in Coronal Holes, a study with high
spectral resolution.
Authors: Malanushenko, O.; Jones, H. P.; Livingston, W.; Malanushenko,
V. P.
2005AGUSMSP51B..08M Altcode:
The He 1083 nm line (He), formed in the upper chromosphere, is used
for observations of coronal holes (CH) near their origins at the solar
surface. Weak He 1083 nm profiles in CHs show some peculiarities
such as asymmetry, broadening, and a different ratio between the
spectral components. These effects are small so that the influence
of disturbing noise and approximations in reduction processes are
important for the results. In this research we have used low noise
and high spectral resolution observations carried out at the Kitt Peak
McMath-Pierce telescope to establish the key characteristics of the He
profile in CHs. For accurate reduction we corrected the He profile for
spectral blending from water vapor and weak solar lines. We confirm
our previous result, based on imaging-spectroscopy data from the Kitt
Peak Vacuum Telescope, regarding broadening of the He line in CHs and
explain previous instability of CH contrast in our procedure for CH
recognition as an influence of hidden photospheric lines.
---------------------------------------------------------
Title: Differentiating Coronal Holes from the Quiet Sun by He 1083
nm Imaging Spectroscopy
Authors: Malanushenko, O. V.; Jones, H. P.
2005SoPh..226....3M Altcode:
The locations of coronal holes are usually based on equivalent-width
images in the He I 1083 nm line. However, it is difficult to
differentiate coronal holes from the centers of quiet chromospheric
network without complementary data and the skill of an experienced
observer. Analysis of imaging spectroscopy shows that line half-width
and central intensity are correlated differently in coronal holes
and a quiet Sun. This fact can be used to form linear combinations
of these images in which coronal holes are better separated from the
quiet Sun. Coronal hole borders agree well with SOHO/EIT data but can
show significant differences from National Solar Observatory maps.
---------------------------------------------------------
Title: The 6dF Galaxy Survey: Mass and Motions in the Local Universe
Authors: Colless, M.; Jones, H.; Campbell, L.; Burkey, D.; Taylor,
A.; Saunders, W.
2005IAUS..216..180C Altcode: 2003IAUS..216E..28C
The 6dF Galaxy Survey will provide 167000 redshifts and about 15000
peculiar velocities for galaxies over most of the southern sky out to
about cz = 30000 km/s. The survey is currently almost half complete,
with the final observations due in mid-2005. An initial data release
was made public in December 2002; the first third of the dataset
will be released at the end of 2003, with the remaining thirds being
released at the end of 2004 and 2005. The status of the survey,
the survey database and other relevant information can be obtained
from the 6dFGS web site at http://www.mso.anu.edu.au/6dFGS. <P />In
terms of constraining cosmological parameters, combining the 6dFGS
redshift and peculiar velocity surveys will allow us to: (1) break
the degeneracy between the redshift-space distortion parameter beta =
Omega_m<SUP>0.6b</SUP>/b and the galaxy-mass correlation parameter
r<SUB>g</SUB>; (2) measure the four parameters A<SUB>g</SUB>, Gamma,
beta and r<SUB>g</SUB> with precisions of between 1% and 3%; (3)
measure the variation of r<SUB>g</SUB> and b with scale to within a
few percent over a wide range of scales.
---------------------------------------------------------
Title: Helicity and the SOLIS Vector-Spectromagnetograph
Authors: Keller, Christoph U.; Harvey, John W.; Henney, Carl. J.;
Jones, Harrison P.
2005HiA....13..126K Altcode:
SOLIS (Synoptic Optical Long-term Investigations of the Sun)
is a suite of three innovative instruments that greatly improve
ground-based synoptic solar observations. The main instrument the
Vector Spectro-Magnetograph (VSM) is a compact high-throughput
vector-polarimeter that measures the magnetic field strength and
direction over the full solar disk within 15 minutes. Helicity can
be directly calculated from the full-disk vector field data provided
by the Stokes inversion of the observed polarized line profiles. We
present an anlysis of the difficulties and problems that one faces
when interpreting the the helicity derived from VSM data.
---------------------------------------------------------
Title: Analysis of He I 1083 nm Imaging Spectroscopy Using a Spectral
Standard
Authors: Malanushenko, O. V.; Jones, H. P.
2004SoPh..222...43M Altcode:
We develop a technique for the analysis of He i 1083 nm spectra which
addresses several difficulties through determination of a continuum
background by comparison with a well-calibrated standard and through
removal of nearby solar and telluric blends by differential comparison
to an average spectrum. The method is compared with earlier analysis
of imaging spectroscopy obtained at the National Solar Observatory/Kitt
Peak Vacuum Telescope (NSO/KPVT) with the NASA/NSO Spectromagnetograph
(SPM). We examine distributions of Doppler velocity and line width as
a function of central intensity for an active region, filament, quiet
Sun, and coronal hole. For our example, we find that line widths and
central intensity are oppositely correlated in a coronal hole and quiet
Sun. Line widths are comparable to the quiet Sun in the active region,
are systematically lower in the filament, and extend to higher values
in the coronal hole. Outward velocities of ≈ 2-4 km s<SUP>−1</SUP>
are typically observed in the coronal hole. The sensitivity of these
results to analysis technique is discussed.
---------------------------------------------------------
Title: SOLIS-VSM Longitudinal Magnetogram Calibration
Authors: Henney, C. J.; Harvey, J. W.; Keller, C. U.; Jones, H. P.
2004AAS...204.3702H Altcode: 2004BAAS...36..709H
The VSM (Vector SpectroMagnetograph) instrument started recording
daily full-disk magnetograms during August, 2003 at a temporary
site in Tucson, Arizona. Along with the other instruments that
constitute the SOLIS (Synoptic Optical Long-term Investigations of
the Sun) project, the VSM will be relocated to Kitt Peak in April,
2004. The VSM instrument provides a unique record of solar full-disk
vector magnetograms along with the high sensitivity photospheric and
chromospheric longitudinal magnetograms. In addition, the VSM takes
daily full-disk He I 1083 nm equivalent width observations. These
parameter-grams are constructed from individual scans in declination
of the projected solar image on the entrance slit with a relatively
large field angle of over a half of a degree in the spectrograph. The
calibration of the VSM longitudinal magnetic observations is reviewed,
along with a comparison between the VSM mean field, sun-as-a-star,
measurements with those by the Wilcox Solar Observatory. In addition,
the making of synoptic maps derived from the VSM magnetograms is
discussed, including the filling of data gaps in polar regions and
the use of accompanying weight maps. VSM magnetograms and synoptic
maps are available via the Internet at: http://solis.nso.edu/. This
research was supported in part by the Office of Naval Research Grant
N00014-91-J-1040. The National Solar Observatory is operated by AURA,
Inc. under a cooperative agreement with the National Science Foundation.
---------------------------------------------------------
Title: Early Results from SOLIS
Authors: Harvey, J.; Giampapa, M.; Henney, C.; Keller, C.; Jones, H.
2004AAS...204.3701H Altcode: 2004BAAS...36..708H
SOLIS (Synoptic Optical Long-Term Investigations of the Sun)
is a project that is replacing antiquated synoptic observing
equipment at the National Solar Observatory. SOLIS consists of
a suite of three instruments on an equatorial mount that will be
installed on Kitt Peak in April 2004. The major SOLIS instrument
is a vector spectromagnetograph (VSM) that maps magnetic fields
across the full solar disk using a slit spectrograph and one arc
sec pixels. Limited daily observations started at a temporary site
in August, 2003 and include line-of-sight component magnetograms in
the photosphere and chromosphere and, for the first time, full-disk
vector magnetograms. At a medium scan speed ( ∼ 10 minutes for the
full disk) noise is less than 1 Mx/cm<SUP>2</SUP>. This low noise,
combined with negligible instrumental polarization and well resolved
spectral line profiles, yields moderate resolution magnetograms of
unprecedented quality. Observations show magnetic flux nearly everywhere
in the photosphere from the disk center to the solar limb. Weak,
intranetwork fields are now routinely observed and show a tendency to
be of opposite polarity to the stronger surrounding fields. Diffuse
fields surround decaying active regions and appear to be distinct from
canopy fields. Vector magnetograms easily show the radial orientation
of network fields, and the diffuse component surrounding decaying active
regions. Near the disk center, the transverse magnetic fields of network
elements change on a time scale of minutes. Detailed quantitative
calibration of the observations is in progress. Good results have been
obtained from the other SOLIS instruments: a full-disk filter imager at
several narrow wavelengths and a double-pass grating spectrograph that
provides high-accuracy line spectra of integrated sunlight. SOLIS data
are freely available via the Internet and users are invited to submit
observing time requests for special observations. The National Solar
Observatory is operated by AURA, Inc. under a cooperative agreement
with the National Science Foundation. Additional support for the
development of SOLIS from NASA and ONR is gratefully acknowledged.
---------------------------------------------------------
Title: Differentiating Coronal Holes from the Quiet Sun by He 1083
nm imaging spectroscopy.
Authors: Malanushenko, O. V.; Jones, H. P.
2004AAS...204.7105M Altcode: 2004BAAS...36R.797M
We applied our new analysis technique to several examples of He I 1083
nm imaging spectroscopy obtained with the NASA/NSO Spectromagnetograph
at the NSO/Kitt Peak Vacuum Telescope. We studied correlations of
intensity vs width and Doppler velocity in several coronal holes and
areas of chromospheric network in the quiet Sun. We confirm our previous
result, which was based on a single example, that the correlation of
line width and central intensity is opposite in coronal holes and quiet
Sun. Suitably normalized linear combinations of width and intensity
can be used to distinguish between quiet Sun and coronal holes.
---------------------------------------------------------
Title: Measurement Scale of the SOLIS Vector Spectromagnetograph
Authors: Jones, H. P.; Harvey, J. W.; Henney, C. J.; Keller, C. U.;
Malanushenko, O. M.
2004AAS...204.3703J Altcode: 2004BAAS...36Q.709J
Longitudinal magnetograms obtained with the SOLIS Vector
Spectromagnetograph (VSM) during a cross-calibration period are
compared with similar data from the NASA/NSO Spectromagnetograph (SPM)
at the NSO/Kitt Peak Vacuum Telescope as well as with SOHO/MDI and GONG
magnetograms. The VSM began observations at the University of Arizona
agricultural test site and collaborative observations were obtained
with both the VSM and SPM from 2003 Aug 05 through 2003 Sep 21 when
the SPM was officially retired. The VSM replaces the SPM and continues
the 30-year NSO/Kitt Peak synoptic magnetogram record. Magnetograms
are compared by equating histograms and, for selected examples, by
pixel-by-pixel comparison of coregistered images. The VSM was not
corrected for polarization crosstalk and was operated without fast
guiding. Solar activity was at best moderate during this period. Over
the range of observed fields, the VSM magnetograms show greatly
improved sensitivity but are otherwise virtually identical with "raw"
SPM magnetograms. GONG magnetograms are also closely comparable with
the SPM while MDI flux values tend to be stronger by a factor of 1.2 -
1.4. Dependence of the results on seeing will be discussed. Partial
funding for this work was provided through Solar and Heliospheric
Research Supporting Research and Technology grants from NASA's Office
of Space Sciences.
---------------------------------------------------------
Title: DASL--Data and Activities for Solar Learning
Authors: Hill, F.; Gearen, M.; Henney, C.; Jones, H.; Stagg, T.
2004AAS...204.7703H Altcode: 2004BAAS...36..808H
Data and Activities for Solar Learning (DASL) provides a classroom
learning environment based on a twenty-five year record of solar
magnetograms from the National Solar Observatory (NSO) at Kitt Peak,
AZ. The data, together with image processing software for Macs or PCs,
can be used to learn basic facts about the Sun and astronomy at the
middle school level. At the high school level, students can study
properties of the Sun's magenetic cycle with classroom excercises
emphasizing data and error analysis and can participate in a new
scientific study, Research in Active Solar Longitudes (RASL), in
collaboration with classrooms throughout the country and scientists
at NSO and NASA. We will have available a compact disc with the data
and software, and a web site for uploading the RASL results.
---------------------------------------------------------
Title: Imaging the Chromosphere using Photospheric Mn 539.4 nm
Authors: Malanushenko, Olena; Jones, H. P.; Livingston, W.
2004IAUS..223..645M Altcode: 2005IAUS..223..645M
Archival full disk observations of the central depth of Mn 539.467,
a photospheric line, have been found to correlate with chromospheric
Ca K intensity. In this paper we present spectroheliograms taken in
Mn I 539.467 and 542.32 nm lines and other nearby lines to see if the
other photospheric lines show chromospheric structures. We see both
Mn images and also Si I 542.118 mimic magnetograms the similar way,
while strong Fe and Ti lines only faintly reveal magnetic features,
and weak Fe lines of comparable strength to Mn show nothing.
---------------------------------------------------------
Title: Data Calibration and Analysis for He I 1083 nm Imaging
Spectroscopy
Authors: Jones, Harrison P.
2003SoPh..218....1J Altcode:
Imaging spectroscopy in the He i 1083 nm lines is a powerful tool for
probing the top of the chromosphere and bottom of the transition region,
but simple techniques for spectral calibration and analysis often fail
for this line. A method for spectral flat-fielding using a uniform solar
exposure with spectral lines in place is presented and illustrated
with 1083 nm data obtained at the National Solar Observatory (NSO)
Kitt Peak Vacuum Telescope with the NASA/NSO Spectromagnetograph. An
efficient method for analysis of the data producing images in continuum
intensity, line-of-sight velocity, equivalent width, central line depth,
Doppler width, and line asymmetry is also presented and illustrated.
---------------------------------------------------------
Title: First Results from SOLIS
Authors: Harvey, J.; Giampapa, M.; Henney, C.; Jones, H.; Keller, C.
2003AGUFMSH42B0545H Altcode:
SOLIS (Synoptic Optical Long-term Investigations of the Sun) is a
project to replace antiquated synoptic observing equipment at the
National Solar Observatory. SOLIS includes a suite of three instruments
on an equatorial mount originally installed at a site in Tucson and will
be moved to Kitt Peak before the end of 2003. The major SOLIS instrument
is a vector spectromagnetograph that maps magnetic fields across the
full solar disk using a slit spectrograph and one arc sec pixels. Daily
observations include several line-of-sight component magnetograms in the
photosphere and chromosphere and, for the first time, full-disk vector
magnetograms. At a medium scan speed ( ∼10 minutes for the full disk)
noise is less than 1 Mx/cm<SUP>2</SUP>. This low noise, combined with
negligible instrumental polarization and well resolved spectral line
profiles, yields moderate resolution magnetograms of unprecedented
quality. Sample observations show magnetic flux nearly everywhere
in the photosphere from the disk center to the solar limb. The flux
is organized in large scale patterns that heretofore had been visible
only in strong flux elements or after substantial spatial smearing. Good
results have been obtained from the other SOLIS instruments: a full-disk
filter imager at several narrow wavelengths and a grating spectrograph
that provides high-accuracy line spectra of integrated sunlight. SOLIS
data are freely available via the Internet and users may submit
observing time requests for special observations. The National Solar
Observatory is operated by AURA, Inc. under a cooperative agreement
with the National Science Foundation. Additional support for the
development of SOLIS from NASA and ONR is gratefully acknowledged.
---------------------------------------------------------
Title: DASL--Data and Activities for Solar Learning
Authors: Hill, F.; Gearen, M. V.; Henney, C. J.; Jones, H. P.;
Stagg, T.
2003AGUFMED41D1189H Altcode:
Data and Activities for Solar Learning (DASL) provides a classroom
learning environment based on a twenty-five year record of solar
magnetograms from the National Solar Observatory (NSO) at Kitt Peak,
AZ. The data, together with image processing software for Macs or PCs,
can be used to learn basic facts about the Sun and astronomy at the
middle school level. At the high school level, students can study
properties of the Sun's magnetic cycle with classroom excercises
emphasizing data and error analysis and can participate in a new
scientific study, Research in Active Solar Longitudes (RASL), in
collaboration with classrooms throughout the country and scientists
at NSO and NASA. We will demonstrate a compact disc with the data and
software, and a web site for uploading the RASL results.
---------------------------------------------------------
Title: Comparison of Total Solar Irradiance with NASA/National Solar
Observatory Spectromagnetograph Data in Solar Cycles 22 and 23
Authors: Jones, Harrison P.; Branston, Detrick D.; Jones, Patricia B.;
Popescu, Miruna D.
2003ApJ...589..658J Altcode:
NASA/National Solar Observatory Spectromagnetograph (SPM) data are
compared with spacecraft measurements of total solar irradiance
(TSI) variations for 8 yr beginning with the declining phase of
solar cycle 22 and extending into the maximum of cycle 23. Previously
reported conclusions based on a similar comparison for a shorter time
period appear to be robust: three factors (sunspots, strong unipolar
regions, and strong mixed-polarity regions) describe most of the
variation in the SPM record, but only the first two are associated
with TSI. Additionally, the residuals of a linear multiple regression
of TSI against SPM observations over the entire 8 yr period show an
unexplained, increasing, linear time variation with a rate of about 0.05
W m<SUP>-2</SUP> yr<SUP>-1</SUP>. Separate regressions for the periods
before and after 1996 January 1 show no unexplained trends but differ
substantially in regression parameters. This behavior may reflect
a solar source of TSI variations beyond sunspots or uncompensated
nonsolar effects in one or both of the TSI and SPM data sets.
---------------------------------------------------------
Title: Calibration and Data Analysis for the SOLIS-VSM
Authors: Henney, C. J.; Harvey, J. W.; Keller, C. U.; Jones, H. P.;
SOLIS Team
2003SPD....34.0303H Altcode: 2003BAAS...35..808H
The Vector Spectromagnetograph (VSM) instrument of the Synoptic
Optical Long-term Investigations of the Sun (SOLIS) project will
provide a unique 25-year record of synoptic solar observations with
daily full-disk photospheric vector and high sensitivity longitudinal
magnetograms. In addition, the VSM will produce daily full-disk
chromospheric longitudinal magnetograms along with various He I 1083
nm parameter images. The VSM is being prepared for installation at a
temporary site in Tucson for a comparison period with observations from
the Kitt Peak Vacuum Telescope (KPVT). After the cross-calibration
period, the VSM will replace the KPVT spectromagnetograph at Kitt
Peak. We outline the various VSM data products, with emphasis on the
calibration and data reduction efforts. <P />The data transmission
and storage resources are such that the reduction of VSM data will be
performed at the observing site on Kitt Peak. Reduced data products
will be transmitted via a DS3 link from Kitt Peak to the National Solar
Observatory's digital archive in Tucson. During a typical observing day,
three full-disk photospheric vector magnetograms will be available over
the Internet in two stages: first, as a “quick-look” product within
10 minutes of data acquisition, and then as a full Milne-Eddington
(ME) inversion product within 12 hours of each observation. The
quick-look parameters will include estimates of the magnetic field
strength, azimuth and inclination based on Auer, Heasley, House (1977,
Solar Physics 55, p. 47). The high-precision vector products will be
determined with the High Altitude Observatory ME inversion technique
implemented by Skumanich and Lites (1987, ApJ, 322, p.473). The
flexible design of the VSM data handling system can incorporate
future improvements under consideration (e.g., principal component
analysis). <P />This research was supported in part by the Office of
Naval Research Grant N00014-91-J-1040.
---------------------------------------------------------
Title: A New Way to Identify Coronal Holes.
Authors: Malanushenko, O.; Jones, H. P.
2003SPD....34.0419M Altcode: 2003BAAS...35R.813M
The location of a coronal hole (CH) in the upper chromosphere is usually
based on equivalent width (EqW) images in the He 1083 nm line. A CH
is seen on these images as bright areas, which represents low values
of EqW. But sometimes it is difficult to differentiate a CH from the
bright centers of chromospheric network, or filament channels, without
complementary data and the skill of an experienced of observer. <P />To
remove the above ambiguity we apply a new spectral analysis technique
for the He I 1083 nm line to imaging spectroscopy of several CHs
obtained with the NASA/NSO spectromagnetograph (Malanushenko and Jones,
2002, BAAS 33, 700). Reduction includes making dark and flat-field
corrections; normalization to a non-linear continuum on the basis of
a comparison to a spectral standard; a differential method for the
de-blending of spectra; and multi-profile fitting to define the He line
components. <P />We fit a Gaussian profile to the main component of the
He line and deduce the parameters of central intensity (I) and half
width at half maximum (HW). On the HW-images, CHs are distinguished
from the surrounding regions as bright areas; similarly, they are
also seen as bright on the I-images. Chromospheric network is seen on
W-images as opposite in contrast to the I-images, and this distinction
is the basis for our CH identification method. We normalize the I- and
HW-images by subtracting their respective quiet-sun means and dividing
by the corresponding standard deviations. The sum of the normalized I-
and HW-images shows increasing contrast of the CH and a depression of
contrast in the network and can be used as an independent CH diagnostic.
---------------------------------------------------------
Title: A New Fitting Procedure for the Blended He I 1083 nm Multiplet
Authors: Jones, H. P.; Malanushenko, O. V.
2003SPD....34.1712J Altcode: 2003BAAS...35..839J
The He I 1083 nm multiplet is a powerful tool for observing the outer
solar atmosphere but is difficult to analyze because the lines are
weak, highly variable, and spectrally blended, both internally and
with other neighboring solar and telluric lines. After separation from
nearby spectral features (see accompanying poster by Malanushenko and
Jones), two components of the He I multiplet are resolved. Fitting these
lines with two unconstrained Gaussian profiles always gives a ratio
of major to minor component of less than half the value which would
be expected for optically thin lines. One possibility for explaining
the discrepancy between the weakness of the lines and the ratio of
the spectral components is to assume that the line formation regions
are concentrated in laterally unresolved, optically thick structures
with small filling factor. However, we present here a least-squares
fitting technique using cubic splines with fixed breakpoints with
the constraint that the blend is the sum of three identically shaped
profiles shifted in wavelength according to the atomic structure of
the blend and weighted by the corresponding statistical weights, in
agreement with optically thin line formation. The basis functions
for the fitting procedure have no built-in spectral symmetry or
shape. The resulting underlying profiles tend to be asymmetric with
excess absorption to the blue, consistent with formation by "hot" and
"cool" spatial elements within the observed volume, with the hotter
regions having differential motion toward the observer. The results
agree well with NASA/NSO Spectromagnetograph observations in quiet
sun and coronal holes. Partial funding of this research was provided
through the NASA Sun-Earth Connection SR&T program.
---------------------------------------------------------
Title: Recent Discoveries from the Anglo-Australian Planet Search
Authors: McCarthy, C.; Tinney, C.; Jones, H.; Butler, P.; Carter,
B.; Marcy, G.; Penny, A.; Blundell, J.; Bond, J.
2003ASPC..294...35M Altcode:
We present the latest precision radial velocity results from the Anglo
Australian Planet Search. These include new planet mass companions to
HD216437, HD196050, HD30177, HD73526, and HD2039, as well as evidence
for a second companion to HD160691 residing in a long period orbit. The
results come from a sample of approx. 200 nearby inactive FGKM dwarfs
with V<7.5 and a subsample of 20 more distant metal rich stars. At
least 25 ± 11% of metal rich stars appear to have planets within 2.5
AU, somewhat more than the 8% of stars which appear to have planets
within 3.5 AU.
---------------------------------------------------------
Title: Helicity and the SOLIS Vector-Spectromagnetograph
Authors: Keller, Christoph U.; Harvey, John W.; Henney, Carl J.;
Jones, Harrison P.
2003IAUJD...3E..18K Altcode:
SOLIS (Synoptic Optical Long-term Investigations of the Sun)
is a suite of three innovative instruments that greatly improve
ground-based synoptic solar observations. The main instrument the
Vector Spectro-Magnetograph (VSM) is a compact high-throughput
vector-polarimeter that measures the magnetic field strength and
direction over the full solar disk within 15 minutes. Helicity can
be directly calculated from the full-disk vector field data provided
by the Stokes inversion of the observed polarized line profiles. We
present an anlysis of the difficulties and problems that one faces
when interpreting the the helicity derived from VSM data.
---------------------------------------------------------
Title: Stokes V Profiles in a Post-flare Ca II 854.2nm Downflow
Authors: Penn, M. J.; Jones, H. P.
2003ASPC..286..355P Altcode: 2003ctmf.conf..355P
No abstract at ADS
---------------------------------------------------------
Title: Long-Term Solar Irradiance Variations From Solar Cycle 21 to 23
Authors: Pap, J. M.; Arge, C.; Jones, H.; Floyd, L.
2002AGUFMSH21B..03P Altcode:
In this paper we show the recent results on total solar and UV
irradiance variations and their relation to solar magnetic activity
over solar cycles 21 to 23. Comparison of the multi-decade long
irradiance and magnetic field measurements indicates that the shape and
magnitude of irradiance variations are different from that of magnetic
indices. Specifically, while magnetic indices show that solar cycle
23 is weaker than the two previous cycles, the long-term variation of
total solar irradiance over solar cycles 21 to 23 is rather symmetrical,
showing that its maximum and minimum levels were about the same within
their measuring uncertainties. In this paper we address the questions:
(1) is there a strict linear relationship between solar variability and
irradiance variations; (2) what is the role of polar magnetic fields in
irradiance changes; (3) is there a significant non-magnetic component
in the observed irradiance variations? The results presented in this
paper underscore the need to further develop new analysis techniques
to determine whether there is a secular variation in solar irradiance
over years to decades - a necessary step to study and predict the
climate impact of solar variability.
---------------------------------------------------------
Title: Comparison of Three Solar Magnetographs
Authors: Thornton, C. E.; Jones, H. P.
2002AAS...201.8307T Altcode: 2002BAAS...34.1243T
The Sun's magnetic field controls the structure and activity of the
outer solar atmosphere. Although the surface magnetic flux is now
frequently observed over the entire visible hemisphere by several
instruments, accurate quantitative measurment is still difficult
as reflected by comparisons of different instruments which can
show relative differences of 50% or more. We extend a previous study
(Jones and Ceja, 2001, ASP Conference Series 236, 87)comparing data via
histogram equating from three widely used sources: the SOHO Michelson
Doppler Imager (MDI), the refurbished Global Oscillations Network
Group (GONG+) and the NASA/NSO Spectromagnetograph (SPM). Data from
GONG+ and SPM are quite comparable but underestimate flux values in
comparison with MDI by 20-40%. Our analysis shows that MDI and SPM
magnetograms agree better in later time periods when solar activity
is higher, suggesting that strong-field regions are better measured
than weak-field ones. This is probably due to the broader extents
and higher filling factors for strong-field areas which cause them
to be less sensitive to blurring and cancellation by atmospheric
seeing in ground-based instruments. That seeing affects instrumental
comparisons is reinforced by our examination of contrasts in cotemporal
and cospatial intensity images accompanying SPM magnetograms; overall
agreement between MDI and SPM data is generally better for higher rms
contrasts in the SPM intensities.
---------------------------------------------------------
Title: Data analysis for the SOLIS Vector Spectromagnetograph
Authors: Jones, Harrison P.; Harvey, John W.; Henney, Carl J.; Hill,
Frank; Keller, Christoph U.
2002ESASP.505...15J Altcode: 2002solm.conf...15J; 2002IAUCo.188...15J
The National Solar Observatory's SOLIS Vector Spectromagnetograph, which
will produce three or more full-disk maps of the Sun's photospheric
vector magnetic field every day for at least one solar magnetic cycle,
is in the final stages of assembly. Initial observations, including
cross-calibration with the current NASA/NSO spectromagnetograph (SPM),
will soon be carried out at a test site in Tucson. This paper discusses
data analysis techniques for reducing the raw data, calculation of
line-of-sight magnetograms, and both quick-look and high-precision
inference of vector fields from Stokes spectral profiles. Existing
SPM algorithms, suitably modified to accommodate the cameras, scanning
pattern, and polarization calibration optics for the VSM, will be used
to "clean" the raw data and to process line-of-sight magnetograms. A
recent version of the High Altitude Observatory Milne-Eddington (HAO-ME)
inversion code will be used for high-precision vector fields.
---------------------------------------------------------
Title: New Analysis of He I 1083 nm Imaging Spectroscopy
Authors: Malanushenko, O. V.; Jones, H. P.
2002AAS...200.3812M Altcode: 2002BAAS...34..700M
We apply our new analysis method (Jones, H.P., Malanushenko, E.V,
American Geophysical Union, Spring Meeting 2001, abstract #SH31A-01),
which uses a spectral standard to determine the continuum and
least-squares fitting of all relevant spectral features to removed
effects of nearby solar and telluric lines, to imaging spectroscopy
in the He I 1083 nm line of coronal holes and quiet sun obtained with
the NASA/NSO spectromagnetograph. We find that in coronal holes the
central line depth is slightly lower compared to cell centers in nearby
quiet network, that the full-width-half maxima (FWHM)of coronal hole
profiles is significantly (approximately 35%) higher than in quiet cell
centers, and that the coronal hole line-of-sight velocities show a blue
shift of 3-4 km/s. Preferential asymmetry with excess blue absorption
is clearly evident in the processed profiles. We note that the blue
shift of line center is not seen using earlier analysis techniques and
explore the reasons for this difference. We suggest that FWHM may be
a better coronal hole diagnostic than the lower contrast equivalent
width which is currently used. Partial support of this research was
provided by NASA Supporting Research and Technology grants under the
Sun-Earth Connection program.
---------------------------------------------------------
Title: Stokes Inversion Techniques for the SOLIS-VSM
Authors: Henney, C. J.; Keller, C. U.; Jones, H. P.; SOLIS Team
2002AAS...200.5514H Altcode: 2002BAAS...34Q.734H
The Vector Spectromagnetograph (VSM) instrument of the Synoptic Optical
Long-term Investigations of the Sun (SOLIS) project will begin operation
in 2002 and provide a 25 year record of synoptic solar observations. The
50-cm aperture VSM will provide daily full-disk photospheric vector
and high sensitivity longitudinal magnetograms. In addition, the VSM
will produce daily full-disk chormospheric longitudinal magnetograms,
along with 1083 nm equivalent width images. Current data transmission
and storage resources are such that the reduction of VSM data will be
performed at the observing site on Kitt Peak. Reduced data products
will be transmitted via a DS3 link from Kitt Peak to the National
Solar Observatory's digital archive in Tucson. During a typical
observing day, three full-disk photospheric vector magnetograms will
be available over the web in two stages: first, as a “quick-look”
product within 10 minutes of data acquisition, and then as a full
Milne-Eddington (ME) inversion product within 24 hours of each
observation. The quick-look parameters will include estimates of
the magnetic field strength, azimuth and inclination based on Auer,
Heasley, House (1977, Solar Physics 55, p. 47). The high-precision
vector products will be determined with the High Altitude Observatory
ME inversion technique implemented by Skumanich and Lites (1987, ApJ,
322, p.473). The flexible design of the VSM data handling system can
incorporate future improvements under consideration (e.g., principal
component analysis). However, since the original Stokes profiles
observed will not be archived, a retrospective reduction of VSM data
will not be possible. Quick-look and full ME inversion results are
compared using simulated VSM Stokes profile data based on Kitt Peak
Vacuum Telescope magnetograms. This research was supported in part by
the Office of Naval Research Grant N00014-91-J-1040.
---------------------------------------------------------
Title: Solar Irradiance Variations over Solar Cycles 21 to 23
Authors: Pap, J. M.; Kuhn, J.; Jones, H.; Turmon, M.; Arge, N.;
Schmutz, W.; Floyd, L.
2002AAS...200.2803P Altcode: 2002BAAS...34..679P
In this paper we describe the science requirements and a new measurement
strategy to better understand solar variability and its potential effect
on climate. We study the relation between the variations in solar total
and UV irradiances and solar magnetic fields as observed within the last
three decades. The results of our analysis raise important questions:
(1) is there a significant non-magnetic component in the observed
irradiance variations?; (2) may polar magnetic fields play a role
in irradiance changes?; (3) is there a strict linear relationship
between solar variability and irradiance variations as the current
irradiance models used in climate studies assume? The results presented
in this paper underscore the need to further develop new measurement
and analysis techniques to study and predict the climate impact of
solar variability.
---------------------------------------------------------
Title: The Diagnostic Potential of the CaII 8542 spectral line for
Stokes I, V Spectropolarimetry
Authors: Balasubramaniam, K. S.; Uitenbroek, H.; Havey, J. W.;
Jones, H.
2002AAS...200.3807B Altcode: 2002BAAS...34R.699B
The number of available spectral lines to probe magnetic fields in the
solar chromosphere from the ground is practically limited to resonance
lines of hydrogen, calcium, sodium and magnesium and the multiplets of
helium. The range of heights over which each these spectral lines form
extends over several hundred kilometers and temperatures over several
hundreds of degrees, in a significantly non-local thermodynamic
equilibrium atmosphere. In this paper we explore the diagnostic
potential of the CaII 8542 A spectral line and the inference of active
region magnetic and velocity fields. We will provide a NLTE analysis of
the radiative transfer of this spectral line in the presence of magnetic
fields and compare theoretical and measured spectral line profiles
(observed using the NSO/KP Vacuum Telescope), to infer magnetic field
strengths using the center-of-gravity separation of the Stokes (I+V),
(I-V) components, and using the weak field approximation.
---------------------------------------------------------
Title: A comparison of feature classification methods for modeling
solar irradiancevariation
Authors: Jones, H.; Harvey, K.; Pap, J.; Preminger, D.; Turmon, M.;
Walton, S.
2002cosp...34E.641J Altcode: 2002cosp.meetE.641J
A physical understanding of both total (bolometric) and spectral solar
irradiance variations depends upon establishing a connection between
the temporal variability of spatially resolved solar structures and
spacecraft observations of irradiance. One difficulty in comparing
models derived from different data sets is that the many ways for
identifying solar features such as faculae, sunspots, quiet sun, and
various flavors of "network" are not necessarily consistent. To learn
more about classification differences and how they affect irradiance
models, we compare feature "masks" on selected days together with
the temporal variation of feature areas derived from four current
methods: multidimensional histogram analysis of NASA/NSO Kitt Peak
spectromagnetograph data (Jones et al., 2000, ApJ 529, 1070);
statistical pattern recognition applied to SOHO/MDI photograms
and magnetograms (Turmon et al., 2002, ApJ 568, 396); threshhold
masks allowing for influence of spatial surroundings applied to
NSO magnetograms (Harvey and White, 1999, ApJ 515, 541); and the
"three-trigger" algorithm applied to CSUN CFDT images (Preminger et al.,
2001, Sol. Phys. 202, 53.). Developing a more uniform classification
system of features contributing to irradiance variations will help
to improve irradiance models used for climate studies. A practical
benefit of understanding the relationships between various methods is
the possibility of constructing a more continuous and extensive time
series from several incomplete sources.
---------------------------------------------------------
Title: Long-term solar irradiance variations: results and perspectives
Authors: Pap, J.; Fleck, B.; Frohlich, C.; Jones, H.; Kuhn, J.;
Schmutz, W.
2002cosp...34E.553P Altcode: 2002cosp.meetE.553P
In this paper we show the recent result on irradiance variations and
their relation to solar magnetic activity over solar cycles 21 to
23. Comparison of the multi-decade long irradiance and magnetic field
measurements indicates that the shape and magnitude of irradiance
variations are different from that of magnetic indices. Specifically,
while magnetic indices show that solar cycle 23 is weaker than the two
previous cycles, the long-term variation of total solar irradiance
over solar cycles 21 to 23 is rather symmetrical, showing that its
maximum and minimum levels were about the same within their measuring
uncertainties. These results raise questions like: (1) is there a
strict linear relationship between solar variability and irradiance
variations as the current irradiance models used in climate studies
assume?; (2) what is the role of polar magnetic fields in irradiance
changes?; (3) is there a significant non-magnetic component in the
observed irradiance variations? The results presented in this paper
underscore the need to further develop new measurement and analysis
techniques to study and predict the climate impact of solar variability.
---------------------------------------------------------
Title: Solar irradiance variations over solar cycles 21 to 23
Authors: Pap, J.; Arge, N.; Floyd, L.; Helizon, R.; Jones, H.
2002cosp...34E1521P Altcode: 2002cosp.meetE1521P
The Sun's radiative output has been monitored at various UV wavelengths
and integrated over the entire solar spectrum - hence total irradiance -
for almost three consecutive solar cycles. These multi-decade long
measurements of total solar and spectral irradiance established
conclusively that the Sun's radiative output varies on time scales
from minutes to the 11-year solar cycle. To study long-term irradiance
variations and their possible effects on climate, solar irradiance
has been modeled empirically using the Photometric Sunspot Index and
proxy indicators for facular brightening. These empirical models assume
that solar irradiance varies in phase with the 11-year solar cycle,
being higher during high solar activity cycles and lower during weaker
cycles. However, direct photometric measurements of sunspots and faculae
have shown that both the number and size of active regions were smaller
during cycle 23 than during cycle 22. In addition, both the sunspot
number and the full disk magnetic flux show that cycle 23 was weaker
than the previous two solar cycles, while solar irradiance reached about
the same maximum level during cycle 23 as during the last cycles. In
this paper we compare the long-term variations of the composite total
and UV irradiances with solar magnetic indices, such as the Photometric
Sunspot Index, the equivalenth width of the He-line at 1083 nm, full
disk magnetic flux, polar magnetic fields and facular proxies. The
controversy between measured irradiance variations and their magnetic
surrogates over solar cycles 21 to 23 is discussed in the paper.
---------------------------------------------------------
Title: Ground-Based Correlates of Solar Irradiance Variation
Authors: Jones, H. P.
2001AAS...199.3603J Altcode: 2001BAAS...33.1360J
Ground-based instruments cannot directly measure solar irradiance
variablity at the 0.1% level at which it occurs because of the earth's
atmosphere. However, many forms of ground-based solar observations
correlate well with solar irradiance variations, and this fact has been
used to construct facular-sunspot models which can explain about 90%
of the variance of total solar irradiance as observed by spacecraft
radiometers. It is not yet clear whether remaining discrepancies are
observational or require additional sources in the model. This paper is
a selective review of the current status of the use of ground-based data
to understand spaceraft observations of solar irradiance and to apply
this understanding to periods before space-based measurements were
available. New results from the extension of the histogram analysis
of NASA/NSO spectromagnetograph observations (Jones et al., 2000, ApJ
529, 1070) to the period from Nov. 1992 to Sep. 2000 are reported which
confirm that strong mixed polarity magnetic regions (quiet network) are
not significantly correlated with total solar irradiance and which show
an unexplained linear trend in the residuals of a multiple regression.
---------------------------------------------------------
Title: Helioseismic Holography and a Study of the Process of Magnetic
Flux Disappearance in Canceling Bipoles
Authors: Lindsey, Charles; Harvey, Karen L.; Braun, D.; Jones, H. P.;
Penn, M.; Hassler, D.
2001STIN...0156300L Altcode:
Project 1: We have developed and applied a technique of helioseismic
holography along the lines of originally set out in our proposal. The
result of the application of this diagnostic technique to solar activity
and the quiet Sun has produced a number of important discoveries:
(1) acoustic moats surrounding sunspots; (2) acoustic glories
surround large active regions; (3) acoustic condensations beneath
active regions; and (4) temporally-resolve acoustic images of a solar
flare. These results have been published in a series of papers in the
Astrophysical Journal. We think that helioseismic holography is now
established as the most powerful and discriminating diagnostic in local
helioseismology. Project 2: We conducted a collaborative observational
program to define the physical character and magnetic geometry of
canceling magnetic bipoles aimed at determining if the cancellation
process is the result of submergence of magnetic fields. This assessment
is based on ground-based observations combining photospheric and
chromospheric magnetograms from NSO/KP, BBSO, and SOHO-MDI, and EUV
and X-ray images from SOHO EIT/CDS, Yohkoh/SXT, and TRACE. Our study
involves the analysis of data taken during three observing campaigns to
define the height structure of canceling bipoles inferred from magnetic
field and intensity images, and how this varies with time. We find
that some canceling bipoles can be explained by the submerge of their
magnetic flux. A paper on the results of this analysis will be presented
at an upcoming scientific meeting and be written up for publication.
---------------------------------------------------------
Title: 2p2 Team News
Authors: Jones, H.; Pompei, E.
2001Msngr.104....7J Altcode:
Team member Patrick Fran
---------------------------------------------------------
Title: Achieving 1% photometric accuracy with the ESO Wide Field
Imager
Authors: Manfroid, J.; Selman, F.; Jones, H.
2001Msngr.104...16M Altcode:
The highly successful Wide Field Imager on the ESO/MPG 2.2-m telescope
offers the possibility of undertaking photometry over a half-degree
field. The authors discuss findings concerning the photometric
performance of the camera. They describe strategies for dealing with
the flat-field calibration error, which is often underestimated by
observers.
---------------------------------------------------------
Title: Two-Component Fitting of Coronal-Hole and Quiet-Sun He I 1083
nm Spectra
Authors: Jones, H. P.; Malanushenko, E. V.
2001AGUSM..SH31A01J Altcode:
We present reduction techniques and first results for detailed
fitting of solar spectra obtained with the NASA/National Solar
Observatory Spectromagnetograph (NASA/NSO SPM) over a 2 nm bandpass
centered on the He I 1083 nm line. The observation for this analysis
was a spectra-spectroheliogram obtained at the NSO/Kitt Peak Vacuum
Telescope (KPVT) on 00 Apr 17 at 21:46 UT spanning an area of 512 x 900
arc-seconds; the field of view included a coronal hole near disk center
as well as surrounding quiet sun. Since the He I line is very weak and
blended with nearby solar and telluric lines, accurate determination
of the continuum intensity as a function of wavelength is crucial. We
have modified the technique of Malanushenko et al. (1992; AA 259, 567)
to tie regions of continuua and the wings of spectral lines which show
little variation over the image to standard reference spectra such
as the NSO Fourier Transform Spectrometer atlas (Wallace et al. 1993;
NSO Tech Report #93-001). We performed detailed least-squares fits of
spectra from selected areas, accounting for all the known telluric and
solar absorbers in the spectral bandpass. The best physically consistent
fits to the Helium lines were obtained with Gaussian profiles from two
components (one “cool”, characteristic of the upper chromosphere; one
“hot”, representing the cool transition region at 2-3 x 10<SUP>4</SUP>
K). In the coronal hole, the transition-region component, shifted by
6-7 km/s to the blue, is mildly dominant, consistent with mass outflow
as suggested by Dupree et al., (1996; Ap. J.~467, 121). In quiet-sun
spectra there is less evidence of outward flow, and the chromospheric
component is more important. All our fitted spectra show a very weak
unidentified absorption feature at 1082.880 nm in the red wing of the
nearby Si I line.
---------------------------------------------------------
Title: 2p2 Team News
Authors: Jones, H.
2001Msngr.103....9J Altcode:
In December we welcomed Emanuel Galliano to our team. Emanuel
is a French student at ESO Chile who is already familiar with La
Silla, through his previous work with the DENIS group. He will be
working primarily on operations at the 2.2-m. In February, however,
we bade farewell to Emanuela Pompei after nearly two years with the
team. Although Emanuela is leaving La Silla, she will remain with ESO
in Chile, commencing work as a Staff Astronomer on Paranal in March. We
wish her all the best in her move north.
---------------------------------------------------------
Title: Discovery of a bow-shock nebula around the pulsar B0740-28
Authors: Jones, H.; Stappers, B.; Gaensler, B.
2001Msngr.103...27J Altcode:
Bow-shock nebulae around highvelocity pulsars provide our primary
insight into the interaction between a pulsar and its surrounding
environment. Specifically, optical observations of such nebulae
allow us to derive full three-dimensional pulsar velocities which are
extremely important for the birth rates and evolution of pulsars. They
can also provide important information on the density, temperature
and composition of the surrounding ambient medium. Unfortunately,
only a few bow-shock nebulae have been discovered, despite there
being nearly a thousand pulsars known from radio surveys. We have
therefore commenced a search for pulsar bow-shocks, using the results
to characterise the properties of the associated pulsars, pulsar winds
and ambient environments.
---------------------------------------------------------
Title: Tunable filters and large telescopes
Authors: Jones, H.; Renzini, A.; Rosati, P.; Seifert, W.
2001Msngr.103...10J Altcode:
Traditionally, astronomy has relied upon filters with a fixed bandpass
to select the wavelengths of the light allowed to reach the detector,
thus allowing the astronomer to derive some colour information about
the objects under study. In the optical, these filters are most
often classical broadband UBVRI, or narrow passbands centred at the
wavelengths of the common emission-line features, either at rest-frame
or redshifted wavelengths. Examples of the latter are becoming numerous,
especially on the 8-10-mclass telescopes that make it possible to
detect very faint, distant emissionline objects, even through narrow
passbands. In this vein, Kurk et al. (2000) used FORS1 at the VLT with a
65-Åwide filter at 3814 Å to image a z = 2.2 radio galaxy, searching
for nearby Lyalpha detections at the same redshift. They detected
around 50 such objects, collectively suggestive of strong clustering
around the dominant radio galaxy. Moreover, they also found extended
Ly-alpha emission (~ 100 kpc in extent) centred on the galaxy, adding
further evidence to the possible scenario of protocluster formation.
---------------------------------------------------------
Title: Preliminary Comparison of Magnetograms from KPVT/SPM, SOHO/MDI
and GONG<SUP>+</SUP>
Authors: Jones, H. P.; Ceja, J. A.
2001ASPC..236...87J Altcode: 2001aspt.conf...87J
No abstract at ADS
---------------------------------------------------------
Title: Real Research In The Classroom - Solar Active Longitudes
Authors: Stagg, T.; Gearen, M.; Jacoby, S. H.; Jones, H. P.; Henney,
C. J.; Hill, F.
2000AAS...197.8709S Altcode: 2000BAAS...32.1556S
We present a high-school level educational/research module for a
project that improves computer and analytical skills and contributes
new scientific results to the field of solar astronomy and physics. The
module has been developed within the RET (Research Experience for
Teachers) program as a new application of a cooperative project
between the RBSE (Research-Based Science Education) initiative of
the NSF and the NASA Education/Public Outreach program. The research
goal is to improve our knowledge of the characteristics of solar
active longitudes, where sunspots tend to cluster. In particular,
the rotation rate of these regions is poorly known. It is suspected
that the active longitude rotation rate (ALRR) is different from the
rotation rate of the solar surface. If this is true, the ALRR can be
compared with the internal rotation rate deduced by helioseismology
providing an estimate of the active region depth. A good determination
of the ALRR requires the measurement of the position of thousands of
individual active regions, a step best done by interactive examination
of images, selection of regions, and determination of heliographic
position. These tasks are well-suited for high school students,
who are thus provided with a motivation to improve their computer
and scientific thinking skills. ScionImage (PC)/NIH Image (Macs)
macros for this purpose have been developed which access a CD-ROM of
25 years of NSO/Kitt Peak magnetogram data and laboratory exercises
developed previously for classroom use. In the future, a web site
will be created for collecting the data from classrooms across the US,
and for status reports on the results.
---------------------------------------------------------
Title: 2p2 Team News
Authors: Jones, H.
2000Msngr.102...12J Altcode:
In September we welcomed new team member Lisa Germany from
Australia. Lisa is a new ESO Fellow and has interests in supernovae
and their use in cosmological distance determinations. S e p t e m b
e r, however, was also a month for departures when we said goodbye
to long-time team member James Brewer. James was a pivotal member
of the 2p2 Team since his arrival at ESO in 1996. He has returned to
Canada to take up a position at the University of British Columbia,
in Vancouver, Canada. We wish him all the best under northern skies.
---------------------------------------------------------
Title: Water vapour in cool dwarf stars
Authors: Jones, H.; Viti, S.
2000ESASP.456..195J Altcode: 2000ibp..conf..195J
M dwarf spectra beyond 1.35 μm are dominated by water vapour yet
terrestrial water vapour makes it notoriously difficult to make accurate
measurement of the water vapour bands from ground-based observations. We
have used the short wavelength spectrometer on the Infrared Space
Observatory (ISO) at four wavelength settings to cover the 2.5 -
3.0 μm region for a range of M dwarfs. The observations show a good
match with previous ground-based observations and a reasonable match
with the best available synthetic spectra. In particular the synthetic
spectra and particularly the ab initio calculations for water vapour
on which they hinge now accurately predict the positions of water
vapour transitions. However, further work extending the calculation
of water vapour to higher energy levels is probably necessary before
a detailed match in intensity will be possible.
---------------------------------------------------------
Title: 2p2 Team News
Authors: Jones, H.
2000Msngr.100...29J Altcode:
The 2p2 Team continued towards the implementation at the 2.2-m of the
same BOB (Broker for Observation Blocks) observing interface as seen at
other ESO telescopes. This requires an interface to be written between
the existing BOB software and the non-VLT compatible control software
for the Wide-Field Imager (WFI) and 2.2-m. Cristian Urrutia, Tatiana
Paz and Eduardo Robledo are heading its development. With this software
in place, observers can use the VLT Phase 2 Proposal Preparation System
(P2PP) for definition of their exposures, whether they are for Visitor
or Service Mode.
---------------------------------------------------------
Title: Helium 1083 nm Imaging Spectroscopy: November 1999
Authors: Jones, H. P.
2000SPD....31.0231J Altcode: 2000BAAS...32..816J
An observing program using the NASA/NSO Spectromagnetograph (SPM) at
the NSO/Kitt Peak Vacuum Telescope and SOHO/SUMER to look for Doppler
shifts and line asymmetries in coronal holes was completed in early
November, 1999 in collaboration with D. Hassler. This paper presents
first results from the SPM only; analysis of and comparison with the
SUMER observations is in progress and will be reported at a later
date. SPM spectra-spectroheliograms were obtained on 99 Nov. 3-10 (no
data for Nov. 7) for two coronal holes, surrounding active regions,
and the decay phase of a small flare. Images and sample spectra are
displayed. The first target of opportunity for this program was a small
coronal hole approaching disk center whose identification was based on
EIT images but which was not identified as a hole in the NSO synoptic
1083 nm images (K. Harvey, private communication, 1999). The area did
not show 1083 nm line asymmetries as are often seen in polar holes near
the limb (Dupree et al, 1996). However, a larger and more prominent
coronal hole was observed in the latter portion of the observing run
over a wide range of heliocentric angle, including near disk center,
which showed strong 1083 nm asymmetry consistent with the observations
of Dupree et al (1996), Jones et al (1997), and Jones and Bender
(2000). Preliminary analysis of the SUMER observations in Si II, C IV,
and Ne VIII show blue shifts in the high temperature line (Hassler,
private communication, 2000), and future work will involve the removal
of systematics from both data sets and their careful registration
and comparison with each other and with magnetograms. This work was
supported by NASA tasks 682-344-12-19-01 and 682-370-16-22-0. NSO/Kitt
Peak data used here are produced cooperatively by NSF/NOAO, NASA/GSFC,
and NOAA/SEL.
---------------------------------------------------------
Title: Analysis of NASA/NSO Spectromagnetograph Observations for
Comparison with Solar Irradiance Variations
Authors: Jones, Harrison P.; Branston, Detrick D.; Jones, Patricia B.;
Wills-Davey, Meredith J.
2000ApJ...529.1070J Altcode:
The NASA/NSO Spectromagnetograph (SPM) at the National Solar
Observatory/Kitt Peak Vacuum Telescope (NSO/KPVT) has produced daily
full-disk solar images of line-of-sight (LOS) magnetic flux, LOS
velocity, continuum intensity, equivalent width, and central line depth
in either Fe I 550.7 nm or Fe I 868.8 nm since 1992 April. Internally,
these five images are strictly cospatial and cotemporal. This
paper describes reduction techniques for removing spurious effects
(principally from clouds and optical vignetting) from the images and
presents summary statistics from the first 2 years of operation. Pairs
of bivariate histograms as well as five-dimensional histograms are
formed from the “cleaned” images. Factor analysis of various summary
statistics from the histograms shows that mixed-polarity magnetic
elements of weak to moderate strength; unipolar magnetic features,
including active regions and strong enhanced network; and sunspots
are the most important sources of variance in the SPM data. Multiple
regressions of spacecraft measurements of bolometric solar irradiance
on the dominant factors, however, yield strong correlations with only
unipolar regions and sunspots; the weak and mixed-polarity features
that account for most of the SPM variance are only weakly correlated
with the spacecraft measurements.
---------------------------------------------------------
Title: The Tunable Filter Approach to Measuring Cosmic Star Formation
History
Authors: Jones, H.
2000ASPC..221..207J Altcode: 2000sgdg.conf..207J
No abstract at ADS
---------------------------------------------------------
Title: The Solar Magnetic Cycle: An Educational Display: Year 2
Authors: Jacoby, Suzanne H.; Jones, H. P.; Gearen, M. V.
2000ASPC..220..371J Altcode: 2000appa.conf..371J
No abstract at ADS
---------------------------------------------------------
Title: Does Magnetic Flux Submerge at Flux Cancelation Sites?
Authors: Harvey, Karen L.; Jones, Harrison P.; Schrijver, Carolus J.;
Penn, Matthew J.
1999SoPh..190...35H Altcode:
Simultaneous measurements of the magnetic fields in the photosphere and
chromosphere were used to investigate if magnetic flux is submerging
at sites between adjacent opposite polarity magnetic network elements
in which the flux is observed to decrease or `cancel'. These data
were compared with chromospheric and coronal intensity images to
establish the timing of the emission structures associated with these
magnetic structures as a function of height. We found that most of
the cancelation sites show either that the bipole is observed longer
in the photosphere than in the chromosphere and corona (44%) or that
the timing difference of the disappearance of the bipole between these
levels of the atmosphere is unresolved. The magnetic axis lengths of the
structures associated with the cancelation sites are on average slightly
smaller in the chromosphere than the photosphere. These observations
suggest that magnetic flux is retracting below the surface for most,
if not all, of the cancelation sites studied.
---------------------------------------------------------
Title: Low Transition-Region Outflow: Solar He I 1083 nm Asymmetry
in a Disk-Center Coronal Hole
Authors: Jones, H. P.; Bender, C. F.
1999AAS...19510703J Altcode: 1999BAAS...31.1531J
We analyze imaging spectroscopy in the He I 1083 nm line of a solar
coronal hole observed near disk center on 26 Feb 1999 with the NASA/NSO
Spectromagnetograph at the NSO/Kitt Peak Vacuum Telescope. For this
study we examine the equivalent width of the He I absorption feature
along with its wing asymmetry as determined by the difference in
the wavelength position of the line bisector at 30% of central line
depth from line center. Dupree, Penn, and Jones (1996, ApJ 467,
L121) previously used a similar measure to show that excess blue
absorption, indicative of line-of-sight motion towards the observer,
is found preferentially in some polar coronal holes where the line
is weakest. They suggested on the basis of the variation of this
asymmetry with heliocentric angle over the limited domain spanned by
their observations that these motions are vertical and are candidates
for source regions of high-speed solar wind. Our data confirm that this
phenomenon can be observed in coronal holes at disk center with about
the magnitude (7-9 km/s) suggested from extrapolating the results of
Dupree et al. Motions parallel to the solar surface cannot explain our
observations, and these areas may indeed point to low-lying origins
of the solar wind. We compare our results to observations on other
days of quiet Sun outside of coronal holes near disk center as well
as to other polar coronal holes. CFB participated in this research as
an NSO Student Research Assistant supported by NASA task 344-12-19-01
(NRA 96-OSS-09). NSO/Kitt Peak data used here are produced cooperatively
by NSF/NOAO, NASA/GSFC, and NOAA/SEL.
---------------------------------------------------------
Title: Large-Scale Chromospheric Magnetic Fields
Authors: Harvey, J.; Bippert-Plymate, T.; Branston, D.; Plymate, C.;
Recely, F.; Jones, H.
1999AAS...194.9406H Altcode: 1999BAAS...31R.991H
Since mid-1996, NSO and its partners have made regular full-disk,
line-of-sight component magnetograms using the 854.2 nm line of
Ca II. These observations are primarily sensitive to the magnetic
field about 800 km above the photosphere. Several new features of
the solar magnetic field have emerged in these observations. At a
sensitivity of about 3 Gauss and using one arc sec pixels, we observe
diffuse, large-scale magnetic fields in the chromosphere that have
no significant counterparts in the photosphere. The most obvious of
these fields are found surrounding the borders of active regions and
seem to correspond to the "circumfacule" phenomenon first described in
1910 by Deslandres. In other words, these fields seem to be the nearly
horizontal field component associated with long chromospheric fibrils
found around some active regions. The next most obvious example of
large-scale chromospheric fields is a surprise. These fields are found
closely associated with filament channels but, unlike the ubiquitous
polarity reversal always seen in the photospheric magnetic field
under filament channels, the chromospheric field has only one apparent
polarity across the filament channel. However, the apparent sign of the
chromospheric field reverses near the central meridian as the feature
traverses the solar disk. This behavior indicates that the field is
predominantly horizontal with a strong east-west component. These fields
are typically seen on the poleward side of mature active regions and may
last several solar rotations. They should be an important diagnostic of
magnetic field patterns surrounding solar filaments. It is not clear
why some filament channels show these fields while others do not. A
final type of large-scale chromospheric magnetic field is at our present
limit of detection and is simply a predominance of one magnetic polarity
or the other over large areas of the solar disk. Such patterns can
be seen in the photosphere after a large amount of spatial averaging,
but require no such averaging in the chromosphere. The NSO is one of
the National Optical Astronomy Observatories which are sponsored by
the National Science Foundation. The NSO data used here are produced
cooperatively by NSF/NOAO, NASA/GSFC, and NOAA/SEC.
---------------------------------------------------------
Title: Flat-Fielding Solar Spectroscopic Images
Authors: Jones, H. P.
1999AAS...194.7612J Altcode: 1999BAAS...31Q.958J
A key problem for the analysis of the spectral-spatial datacubes
produced by the many operational and planned solar spectroscopic imagers
(e.g., SUMER and CDS on SOHO; the SOLIS Vector Spectromagnetograph
(VSM)) is how to obtain a suitable "flat-field" image for
fixed-pattern correction of each slice (long-slit spectrum) of the
data. We describe here some algorithms developed for flat-fielding
NASA/NSO Spectromagnetograph (SPM) and NSO Near-Infrared Magnograph
(NIM 1) data both for analysis of He I 1083 nm data and as prototype
procedures for the future VSM. The 1083 nm line is a severe test since
the line is very weak, and similarly stringent requirements need to
be met for precision spectral polarimetry from the VSM. The procedures
remove spectrum lines from “raw” flat-fields derived by integrating
spectra as the solar image is scanned to give an equivalent exposure
to each spatial element along the spectrograph slit with the exact
instrument configuration that is used in the observations. We find
this preferable to other techniques such as moving the grating to
nearby continuum or image defocussing, both of which change fringe
patterns and/or the way optical impurities such as dust are imaged. An
iterative fitting procedure is described which works well on the SPM
data but is less satisfactory for NIM 1 because, in the latter case,
the detector readout introduces a columnar pattern parallel to the
spectrum lines which is removed by the SPM algorithm. The orientation
of read-out and spectrum will be the same as NIM-1 for the VSM. We
describe initial attempts to use a new least-squares spline technique
(Thijsse, Hollanders, and Hendrikse, 1998, Computers in Physics 12,
393) to address this difficulty.
---------------------------------------------------------
Title: An Educational Display of the Solar Magnetic Cycle: Year 2
Authors: Jones, H. P.; Gearen, M. V.; Jacoby, S. H.
1999AAS...194.7012J Altcode: 1999BAAS...31..939J
We are developing an educational module to improve student and public
understanding of the Sun's magnetic cycle. The instructional package
features a CDROM compatible with most personal computers available in
the home or classroom with a day-by-day record of an entire magnetic
cycle as recorded in magnetograms from the National Solar Observatory
Kitt Peak Vacuum Telescope (NSO/KPVT) near Tucson, AZ. These data have
in fact been crucial to developing our present understanding of the
solar cycle and its terrestrial effects. In the second year of the
project, we have loaded the data to compact disks both as individual
"gif" files for inspection and analysis and as QuickTime movies, have
prepared the first version of the accompanying textual material, and
are developing macros to aid extraction of information from the data
for various laboratory exercises. We will display samples of these
images and movies, and will furnish copies of the compact disks and
accompanying textual material for testing and comment.
---------------------------------------------------------
Title: Optical observations of GRB990907.
Authors: Palazzi, E.; Pian, E.; Masetti, N.; Frontera, F.;
Vreeswijk, P. M.; Rol, E.; Pedersen, H.; Hjorth, J.; van Paradijs,
J.; Kouveliotou, C.; Leisy, P.; Pizzella, A.; Pompei, E.; Mennickent,
R.; Tinney, C. G.; Freeman, F.; Lee, S.; Bland-Hawthorn, J.; McMahon,
R.; Maddox, S.; Singleton, C.; Jones, H.
1999GCN...413....1P Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Optical observations of GRB990217.
Authors: Palazzi, E.; Masetti, N.; Pian, E.; Frontera, F.;
Vreeswijk, P. M.; Rol, E.; Galama, T. J.; Dubus, G.; van Paradijs,
J.; Kouveliotou, C.; Hainaut, O.; Tinney, C.; Axelrod, T.; Schmidt,
B.; Jones, H.
1999GCN...262....1P Altcode:
No abstract at ADS
---------------------------------------------------------
Title: GRB980326 optical observations
Authors: Groot, P. J.; Vreeswijk, P. M.; Galama, T. J.; Pian, E.;
Frontera, F.; Palazzi, E.; Feroci, M.; Kouveliotou, C.; Robinson,
C.; van Paradijs, J.; Tinney, C.; Phillips; Driver; Smith; Jones;
Windridge; Keane, M.; Hall, P.; Smith, M.; Gonzalez, J. F.; Lidman,
C.; CTIO GRB Collaboration
1998GCN....32....1G Altcode:
Comparison of optical R-band observations of the error box of
GRB980326 (IAUC 6851) taken at the AAT at Mar 27.42 UT (480s),
the CTIO 4m-telescope at Mar 28.04 UT (600s) and the ESO 3.5m NTT
at Mar 28.01 UT (ESO1, 600s) and Mar 28.17 UT (ESO2, 600s) shows a
clearly variable object located at RA 08:36:34.28, Decl -18:51:23.9
(J2000). Differential photometry with respect to three local stars
shows a decrease between the AAT and ESO1 of 1.2(1) mag, AAT and CTIO
of 1.6(1) mag and AAT and ESO2 of 1.7(1) mag. The three local standards
have coordinate end-figures: 1) 36:35.41, 51:41.6; 2) 36:31.00, 51:17.3;
3) 36:34.03, 50:53.2. Their R-band magnitudes are: 1) 18.4(1); 2)
21.7(1); 3) 20.3(1), as determined with respect to Landolt SA 98,
no. 626, 624, 634, 590. At the time of the AAT observation (Mar. 27.42
UT) the R-band magnitude of the variable was R=21.7, equal to that
of comparison star 2. A finding chart of the variable can be found
at: http://www.astro.uva.nl/paulgr/grb/grb980326.html. This message
is citeable.
---------------------------------------------------------
Title: Histograms of Synoptic Spectromagnetograph Observations
Authors: Jones, Harrison P.
1998ASPC..140..145J Altcode: 1998ssp..conf..145J
No abstract at ADS
---------------------------------------------------------
Title: The Helium Spectrum in the Quiet Sun: The January 16/17 and
May 7-13 1997 Coordinated SOHO/Ground-Based Observational Campaigns
Authors: Andretta, Vincenzo; Jordan, Stuart D.; Muglach, Karin;
Garcia, Adriana; Jones, Harrison P.; Penn, Matthew J.; Soltau, Dirk
1998ASPC..155..336A Altcode: 1998sasp.conf..336A
No abstract at ADS
---------------------------------------------------------
Title: Investigating the Formation of the Helium Spectrum in the
Solar Atmosphere
Authors: Andretta, Vincenzo; Jordan, Stuart D.; Muglach, Karin;
Garcia, Adriana; Jones, Harrison P.; Soltau, Dirk
1998ASPC..154..559A Altcode: 1998csss...10..559A
We present the first results of coordinated observations with SOHO
(Solar Heliospheric Observatory) and ground-based observatories aimed
at investigating the mechanisms responsible for the formation of helium
lines in the quiescent solar atmosphere. The observations described
here were taken on 7-13 May 1997; the SOHO instruments involved were
CDS, SUMER and EIT, while ground-based support was provided by the
German Vacuum Tower Telescope on Tenerife (He 1 lambda10830 and Ca 2
lambda8498 spectra-spectroheliograms), Coimbra Solar Observatory (Hα
spectroheliograms), and NASA/NSO Vacuum Tower Telescope on Kitt Peak
(Ca 2 lambda8542 spectra-spectroheliograms and polarimetry).
---------------------------------------------------------
Title: The USAF Improved Solar Observing Optical Network (ISOON)
and its Impact on Solar Synoptic Data Bases
Authors: Neidig, D.; Wiborg, P.; Confer, M.; Haas, B.; Dunn, R.;
Balasubramaniam, K. S.; Gullixson, C.; Craig, D.; Kaufman, M.; Hull,
W.; McGraw, R.; Henry, T.; Rentschler, R.; Keller, C.; Jones, H.;
Coulter, R.; Gregory, S.; Schimming, R.; Smaga, B.
1998ASPC..140..519N Altcode: 1998ssp..conf..519N
No abstract at ADS
---------------------------------------------------------
Title: Comparison of NSO/KPVT 1083 NM and SOHO/CDS/SUMER Observations
of a Coronal Hole.
Authors: Jones, H. P.; Andretta, V.; Jordan, S. D.; Penn, M. J.
1997AAS...191.7304J Altcode: 1997BAAS...29.1321J
As part of SOHO Joint Observing Program 16 to study the solar formation
of Helium, coordinated observations of a coronal hole were obtained
on 17 Jan 97. In this paper, we compare the NSO/KPVT full-disk 1083 nm
spectroheliogram and a time sequence of spectra-spectroheliograms of the
coronal hole near the south solar pole with approximately cospatial and
cotemporal SOHO spatial-spectral data taken in He I (58.4 nm, CDS and
SUMER) and He II 30.4 nm (CDS) together with several transition-region
and coronal lines of CIII, OIII, OIV, MgIX, MgX, SiIX, and SiXII. We
have previously reported on correlations of line intensities. Here
we concentrate as well on Doppler shifts and, in particular, line
asymmetry in the He I 1083 nm line which shows augmented absorption
in the blue wing of the line within the coronal hole in the same sense
as reported by Dupree, Penn, and Jones (1996, ApJ 467, L121).
---------------------------------------------------------
Title: On the Role of the Solar Corona and Transition Region in the
Excitation of the Spectrum of Neutral Helium
Authors: Andretta, Vincenzo; Jones, Harrison P.
1997ApJ...489..375A Altcode:
We investigate the formation of the spectrum of neutral helium in the
solar atmosphere by solving the corresponding non-LTE problem in an
extended grid of model atmospheres. From the results we infer several
general properties and scaling laws that can be used to discriminate
the different proposed formation mechanisms. Some of the scaling laws
have also been tested in a comparison with previous calculations made
with different assumptions. <P />In our models, the excitation of
the spectrum by direct photoionization by EUV radiation shortward
of 504 Å followed by recombinations (PR mechanism), seems to be
capable of influencing significantly the resonance continuum and
the subordinate lines, even in the presence of other (collisional)
excitation mechanisms. While this influence is almost unavoidable in
most atmospheric features, it is hardly justifiable as the only possible
contribution. Moreover, the resonance lines seem inclined to respond
much more effectively to the conditions of the lower transition region,
even in the presence of a significant coronal EUV illumination. With the
help of the detailed non-LTE calculations and of the derived scaling
laws, we explore the interplay of the possible formation mechanisms
and their effect on the individual spectral features.
---------------------------------------------------------
Title: A model of the far-infrared emission from the Galaxy
Authors: Davies, J. I.; Trewhella, M.; Jones, H.; Lisk, C.; Madden,
A.; Moss, J.
1997MNRAS.288..679D Altcode:
The warm dust (<25K) that lies in the plane of the Galaxy
(scaleheight of about 0.13 kpc) was detected by IRAS and is
preferentially associated with star formation regions. In this paper
we describe a model of the diffuse far-infared emission from cool
dust within the Galaxy. We identify a more diffuse, cool (18-22K)
dust component (scaleheight of about 0.5 kpc) that has been detected
by the DIRBE (at 140 and 240 μm) on the COBE satellite. This dust may
be supported above the Galactic plane by radiation pressure. We show
that the excess emission cannot be accounted for by the far-infrared
background (upper limits of 1.0 and 0.5 MJ sr^-1 at 140 and 240mum
respectively) or by the zodiacal light. The total luminosity of this
cool component is ~7x10^9Lsolar, and it has a mass of ~3x10^7Msolar. We
calculate extinction values for the cool component of A_v~27 mag
towards the Galactic Centre, and A_v~0.3 mag at the poles.
---------------------------------------------------------
Title: Quiet Sun He I 1083 NM Chromospheric Events
Authors: Penn, M. J.; Jones, H. P.
1997SPD....28.1303P Altcode: 1997BAAS...29..917P
Several types of flows are observed in the quiet solar chromosphere
using the He I 1083 nm absorption line with data from the
NSO/KPVT. Downflow events, termed “He Rain” are described by about
4 km/sec Doppler red-shift of the line, an increased line width,
and enhanced line absorption. The “He Rain” events begin with a
small, compact morphology then evolve during 500 seconds to become
extended and diffuse. The birth-rate of these “He Rain” events
suggests an association with either coronal loop interactions or
macrospicules. Loop-flow events observed with the He I 1083 nm line
show blue-shifts followed by a red-shift, an increased line width and
enhanced line absorption. The events follow curving trajectories with
sizes about 30 arcsec. These events occur much less frequently than
spicules, but may be associated with a type of spicule or some flow
along the local magnetic field. Recent observations of these quiet
Sun events and discussion of the associated coronal events will be
presented.
---------------------------------------------------------
Title: Reduction and Analysis of He I 1083 NM
Spectra-Spectroheliograms
Authors: Jones, H. P.; Winters, W. F.; Penn, M. J.; Schwitters, J. D.
1997SPD....28.0225J Altcode: 1997BAAS...29..897J
Over two decades of synoptic 1083 nm data from the National Solar
Observatory/Kitt Peak Vacuum Telescope (NSO/KPVT) attest to the fact
that satisfactory equivalent width images may be obtained from simple
sums over “line”and “continuum” bandpasses. However, much more care
is needed to extract Doppler velocity, line depth, and asymmetry since
the 1083 nm line typically has line depths of only a few percent and
is blended with both telluric water vapor and the red wing of a nearby
Si I line at 1082.8 nm. We present a new algorithm for analysis of He
I 1083 nm data obtained with the NASA/NSO Spectromagnetograph (SPM) at
the KPVT. A linear fit to intensity averages over bands near 1082.4 nm
and 1083.6 nm specifies the continuum intensity across the wavelength
domain of interest. The spectral algorithm currently used for 868.8 nm
SPM magnetograms computes line-center wavelengths and depths for the
strong adjacent telluric and Si lines. Quick fits of the damping wings
of these features together with a scaled profile of the weak water
vapor feature which is coincident in wavelength with the 1083 nm line
(Breckenridge and Hall, 1973: Solar Phys. 28, 15) are removed from the
spectral region containing the 1083 nm line. The spectral algorithm then
computes the central wavelength and line depth of the 1083 nm line. An
extension of this algorithm locates the bisector at the 0.35 central
line-depth position on the profile to compute a line asymmetry parameter
(Dupree, Penn, and Jones, 1976: ApJ 467, L121). We show sample results
of the algorithm applied both off-line to spectra-spectroheliograms
and on-line to spatial-spectral data as they are acquired.
---------------------------------------------------------
Title: Investigating the Formation of the Helium Spectrum with
Coordinated SOHO/Kitt Peak/Sacramento Peak Observations
Authors: Andretta, V.; Jordan, Stuart D.; Jones, Harrison P.; Penn,
Matthew J.
1997ESASP.404..163A Altcode: 1997cswn.conf..163A
No abstract at ADS
---------------------------------------------------------
Title: The distribution of galactic inclinations - a clue to opacity?
Authors: Jones, H.; Davies, J. I.; Trewhella, M.
1996MNRAS.283..316J Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Online analysis and compression of spectra-spectroheliograms
Authors: Jones, Harrison P.
1996SPIE.2804..110J Altcode:
The on-line algorithm used by the NASA/National Solar Observatory
Spectromagnetograph for analysis of long-slit spectrum-line profiles is
presented with a view towards future application to processing large
volumes of data from spacecraft and other remote instruments. At
every spatial position, the procedure finds continuum intensity,
equivalent width, and wavelength position and intensity of the central
extremum of absorption or emission. The wavelength position of line
center is found from the zero- crossing of the convolution of the
line profile with a fixed anti-symmetric kernel. As currently used
with the spectromagnetograph, images based on the line parameters
computed at every spatial position are saved, but the original data are
discarded. This paper explores the possibility of preserving the data in
compressed form by saving, in addition to the derived line parameters,
the differences between the data and model profiles synthesized from
the on-line analysis.
---------------------------------------------------------
Title: Limb Observations of HE I 1083 NM
Authors: Penn, M. J.; Jones, H. P.
1996SoPh..168...19P Altcode:
Imaging spectroscopic data of the He I 1083 nm limb emission were
taken on several dates in October and November 1995 with the NASA/NSO
spectromagnetograph at the NSO/Kitt Peak vacuum telescope and on 9
December, 1993 with the Michigan infrared camera at the NSO/Sacramento
Peak vacuum tower telescope. Emission line profiles were observed in
quiet-Sun and coronal hole locations on the northern and southern solar
poles and on the east solar limb. The height of the He I 1083 nm shell
above the continuum limb at 1083 nm was measured to be 2.11 ± 0.12
Mm with the Kitt Peak data, and 1.74 ± 0.05 Mm with the Sacramento
Peak data. The Kitt Peak data show (1) within the measurement error
there is no significant difference in the height or thickness of
the emission shell in coronal holes compared with the quiet Sun,
(2) the 1083 nm emission intensity drops by 50% in coronal holes,
(3) the line width decreases by about 2 km s<SUP>-1</SUP> in coronal
holes (suggesting less inclined spicules), (4) the line width of the
He I 1083 nm line jumps significantly as the line of sight crosses the
solar limb (consistent with a higher temperature upper shell), (5) a
quiescent prominence shows a smaller spectral line width (consistent
with a cooler temperature or less velocity broadening), and (6) the
entire emission shell and the prominence show a He I spectral component
ratio of about 8 (suggesting optically thin emission).
---------------------------------------------------------
Title: He i 10830 Angstrom Wing Asymmetry in Polar Coronal Holes:
Evidence for Radial Outflows
Authors: Dupree, A. K.; Penn, M. J.; Jones, H. P.
1996ApJ...467L.121D Altcode:
Imaging spectroscopy of the Sun, carried out across the the solar
poles, yielded several thousand profiles of the He I 10830 A
chromospheric absorption line with effective spatial pixels of 1.1
x 2 arcsec2. Profiles of He I 10830 A show the relative blue-wing
absorption is stronger in the coronal holes than in the quiet Sun,
creating an asymmetric profile indicative of mass outflow. Within the
coronal holes, blueshifted line wings are found where He I absorption
is weak, corresponding to the center of supergranular cells. However,
in the quiet Sun, there is no line wing shift in supergranular
centers. Spatially compact regions of strong red-wing absorption also
occur across the disk. Within the polar coronal holes, the amplitude
of the wing shift shows a linear dependence with cos theta (where the
angle theta is measured with respect to an outward normal to the Sun's
surface), suggesting that a radial outflow occurs with a characteristic
speed of ~8 km s-1. These observations represent the first detection of
systematic outflows near the chromosphere transition region interface
that appear to mark the origin of the high-speed wind acceleration
from the solar surface.
---------------------------------------------------------
Title: GONG Observations of Solar Surface Flows
Authors: Hathaway, D. H.; Gilman, P. A.; Harvey, J. W.; Hill, F.;
Howard, R. F.; Jones, H. P.; Kasher, J. C.; Leibacher, J. W.; Pintar,
J. A.; Simon, G. W.
1996Sci...272.1306H Altcode:
Doppler velocity observations obtained by the Global Oscillation Network
Group (GONG) instruments directly measure the nearly steady flows in
the solar photosphere. The sun's differential rotation is accurately
determined from single observations. The rotation profile with respect
to latitude agrees well with previous measures, but it also shows a
slight north-south asymmetry. Rotation profiles averaged over 27-day
rotations of the sun reveal the torsional oscillation signal-weak,
jetlike features, with amplitudes of 5 meters per second, that are
associated with the sunspot latitude activity belts. A meridional
circulation with a poleward flow of about 20 meters per second is
also evident. Several characteristics of the surface flows suggest
the presence of large convection cells.
---------------------------------------------------------
Title: Limb Observations of He I 1083nm
Authors: Penn, M.; Jones, H.
1996AAS...188.7906P Altcode: 1996BAAS...28..956P
Imaging spectroscopic data of the He I 1083 nm limb emission
were taken on several dates in Oct and Nov 1995 with the NASA/NSO
Spectromagnetograph at the NSO/Kitt Peak Vacuum Telescope and on 09 Dec
1993 with the Michigan Infrared Camera at the NSO/Sac Peak Vacuum Tower
Telescope. Emission line profiles were observed in quiet Sun and coronal
hole locations on the northern and southern solar poles and on the east
solar limb. The height of the He I 1083 nm shell above the continuum
limb at 1083 nm was measured to be 2.11+/-0.12 Mm with the Kitt Peak
data, and 1.74+/-0.05 Mm with the Sac Peak data. The Kitt Peak data show
(1) within the measurement error there is no significant difference in
the height or thickness of the emission shell in coronal holes compared
with the quiet Sun, (2) the 1083 nm emission intensity drops by 50%
in coronal holes, (3) the line width decreases by about 2 km s(-1) in
coronal holes (suggesting less inclined spicules), (4) the line width
of the He I 1083 nm line jumps significantly as the line-of-sight
crosses the solar limb (consistent with a higher temperature upper
shell), (5) a quiescent prominence shows a smaller spectral line width
(consistent with a cooler temperature or less velocity broadening), and
(6) the entire emission shell and the prominence show a He I spectral
component ratio of about 8 (suggesting optically thin emission).
---------------------------------------------------------
Title: GONG Observations of Solar Surface Flows
Authors: Hathaway, D. H.; Gilman, P. A.; Jones, H. P.; Kasher, J.;
Simon, G. W.; GONG Nearly Steady Flows Team; GONG Magnetic Fields Team
1996AAS...188.5304H Altcode: 1996BAAS...28..903H
Doppler velocity observations obtained by the GONG instruments directly
measure the nearly steady flows in the solar photosphere. The Sun's
differential rotation profile is accurately determined from single
observations. This profile is well represented by a fourth order
polynomial which includes a rapidly rotating equator and a slight
north-south asymmetry. Rotation profiles averaged over 27 day rotations
of the Sun are sufficient to reveal the torsional oscillation signal -
weak, 5 m/s, jet-like features associated with the sunspot latitude
activity belts. A meridional circulation with poleward flow of about 20
m/s is also found from single observations and its spatial structure
is well determined. Several of the observed characteristics of the
surface flows suggest the presence of large convection cells. The
convection spectrum is measured and found to have peak power for cells
with wavelengths of about 50,000 km but the spectrum extends to much
larger wavelengths. Day-to-day variations in the observed structure of
the differential rotation and meridional circulation profiles indicate
the presence of large-scale, nonaxisymmetric velocity signals which may
be of solar origin. Studies correlating the convective flow patterns on
consecutive days also indicate the presence of large cellular patterns
that rotate at the Sun's rotation rate.
---------------------------------------------------------
Title: Solar-Cycle Variation of Polarity Inversion
Authors: Jones, H. P.
1996AAS...188.3505J Altcode: 1996BAAS...28..871J
Multi-scale polarity inversion maps are constructed from National
Solar Observatory/Kitt Peak magnetograms for periods coinciding with
those used by Harvey (1993, PhD Thesis, Utrecht University). The
motivation for this analysis stems from earlier work on a small
sample which suggested that neutral-line "length" varies as a power
of the scale used to determine the polarity inversion loci and that
only the amplitude, not the exponent, varies between maximum and
minimum phases of the solar cycle. Harvey observed similar behavior
in the areal distribution of new bipolar regions, and a plausible
hypothesis is that neutral line length vs. scale is a mapping of this
areal distribution, i.e., an efficient way to count bipoles. Broadly
speaking, the behavior of neutral line length vs. scale is confirmed
from this more extensive sample; the curves from many days at either
minimum or maximum are tightly clustered and are nearly parallel on
log-log plots. Empirically, if one represents the areal distribution
of new bipolar regions as a function of time and area as n(t,A)
\sim f(t)g(A), then neutral-line length, l, varies with scale, s,
as \ell(s) \sim const*[g(s<SUP>2</SUP>)/f(t)]<SUP>r</SUP> where r
=~ 0.2. To explore whether this relation has more than emperical
significance, future work is planned to compute neutral line maps
from synthesized magnetograms based on the superposition of known,
prespecified distributions of dipoles.
---------------------------------------------------------
Title: The Solar Acoustic Spectrum and Eigenmode Parameters
Authors: Hill, F.; Stark, P. B.; Stebbins, R. T.; Anderson, E. R.;
Antia, H. M.; Brown, T. M.; Duvall, T. L., Jr.; Haber, D. A.;
Harvey, J. W.; Hathaway, D. H.; Howe, R.; Hubbard, R. P.; Jones,
H. P.; Kennedy, J. R.; Korzennik, S. G.; Kosovichev, A. G.; Leibacher,
J. W.; Libbrecht, K. G.; Pintar, J. A.; Rhodes, E. J., Jr.; Schou, J.;
Thompson, M. J.; Tomczyk, S.; Toner, C. G.; Toussaint, R.; Williams,
W. E.
1996Sci...272.1292H Altcode:
The Global Oscillation Network Group (GONG) project estimates
the frequencies, amplitudes, and linewidths of more than 250,000
acoustic resonances of the sun from data sets lasting 36 days. The
frequency resolution of a single data set is 0.321 microhertz. For
frequencies averaged over the azimuthal order m, the median formal
error is 0.044 microhertz, and the associated median fractional error
is 1.6 x 10<SUP>-5</SUP>. For a 3-year data set, the fractional error
is expected to be 3 x 10<SUP>-6</SUP>. The GONG m-averaged frequency
measurements differ from other helioseismic data sets by 0.03 to 0.08
microhertz. The differences arise from a combination of systematic
errors, random errors, and possible changes in solar structure.
---------------------------------------------------------
Title: Infrared and optical studies of cool low-mass dwarfs
Authors: Jones, H.
1996Obs...116...62J Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Comparison and Relation of HeI 1083 NM Two-Ribbon Flares and
Large-Scale Coronal Arcades Observed by YOHKOH
Authors: Harvey, Karen L.; McAllister, Alan; Hudson, Hugh; Alexander,
David; Lemen, James R.; Jones, Harrison P.
1996ASPC...95..100H Altcode: 1996sdit.conf..100H
No abstract at ADS
---------------------------------------------------------
Title: The distribution of cold dust within the Galaxy
Authors: Davies, J. I.; Trewhella, M.; Jones, H.
1996ASSL..209..525D Altcode: 1996nepn.conf..525D
No abstract at ADS
---------------------------------------------------------
Title: Observations of a Quiescent Prominence Straddling the Solar
Limb during the Total Eclipse of 11 July 1991
Authors: Gaizauskas, V.; Deluca, E.; Golub, L.; Jones, H. P.;
November, L.
1996mpsa.conf..491G Altcode: 1996IAUCo.153..491G
No abstract at ADS
---------------------------------------------------------
Title: Helium in the Spectrum of the Sun and of Solar-Type Stars
Authors: Andretta, V.; Giampapa, M. S.; Jones, H. P.
1995IrAJ...22..177A Altcode:
We present results from detailed non-LTE radiative transfer calculations
of the He I spectrum in the Sun. Using an extended grid of model
chromospheres, we explore the relative importance of, respectively,
the coronal XUV illumination and the thermal structure of the lower
transition region. With reference to the He I lambda 587.6 and lambda
1083.0 triplet lines, we point out some implications for the study of
activity in solar-type stars.
---------------------------------------------------------
Title: Tracking Magnetogram Proper Motions by Multiscale
Regularization
Authors: Jones, H. P.
1995ESASP.376b.227J Altcode: 1995help.confP.227J; 1995soho....2..227J
No abstract at ADS
---------------------------------------------------------
Title: The dependence of disc galaxy properties on viewing angle:
simulating the observations
Authors: Davies, J. I.; Jones, H.; Trewhella, M.
1995MNRAS.273..699D Altcode:
Recent inclination-dependent tests have indicated that galaxies may
have high optical opacities at large distances from their centres. These
results are difficult to reconcile with other measures of opacity that
indicate very much lower values. In this paper we specifically consider
work by Burstein, Haynes & Faber, to see if their result with
regard to high opacities at large galactic distances is the correct
interpretation of the data used. We start by constructing simulated
samples of both optically thick and optically thin galaxies and show
that they are in excellent correspondence with the observational data
used by Burstein et al. The Burstein et al. method does appear to
have overcome many of the selection effects inherent in other surface
brightness inclination tests. The problem is that they now appear to
have introduced yet another selection effect by requiring that all of
the galaxies in their sample need a distance estimate. The redshift
cut-off of their data renders their distance-based test totally
inconclusive with regard to the opacity of galactic discs.
---------------------------------------------------------
Title: A Multiple Scale View of Magnetic Polarity Inversion
Authors: Jones, Harrison P.
1995SPD....26.1010J Altcode: 1995BAAS...27..979J
No abstract at ADS
---------------------------------------------------------
Title: Working Group 7 - Surface Flows and Feature Tracking
Authors: Hathaway, D.; Hurlburt, N.; Jones, H.; Simon, G.
1995ESASP.376a.205H Altcode: 1995heli.conf..205H
No abstract at ADS
---------------------------------------------------------
Title: The distribution of galactic inclinations.
Authors: Jones, H.; Davies, J.; Trewhella, M.
1995ASIC..469..115J Altcode: 1995osd..conf..115J
No abstract at ADS
---------------------------------------------------------
Title: The NSO/NASA He I 1083.0 nm Video Filtergraph/Magnetograph
Authors: Jones, H. P.; Harvey, J. W.
1995itsa.conf...97J Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Why a distance selection effect invalidates the Burstein,
Haynes and Faber opacity test.
Authors: Davies, J.; Jones, H.; Trewhella, M.
1995ASIC..469...85D Altcode: 1995osd..conf...85D
No abstract at ADS
---------------------------------------------------------
Title: Opacity from luminosity functions.
Authors: Trewhella, M.; Davies, J.; Disney, M.; Jones, H.
1995ASIC..469..293T Altcode: 1995osd..conf..293T
No abstract at ADS
---------------------------------------------------------
Title: Preliminary Comparison of NASA/NSO Spectromagnetograph
Observations with Solar Irradiance
Authors: Jones, H. P.; Wills, M. J.
1994AAS...185.4409J Altcode: 1994BAAS...26.1378J
The NASA/NSO Spectromagnetograph (SPM) at the National Solar
Observatory/Kitt Peak Vacuum Telescope has obtained diachronic,
full-disk images of the Sun in photospheric magnetic flux, line-of-sight
velocity, continuum intensity, equivalent width, and central line
depth from 21 Apr 92 to 19 Nov 92 in Fe I 550.7 nm and from 21 Nov
92 to date in Fe I 868.8 nm. The five daily images are formed from
on-line analysis of spatially and spectrally resolved line profiles
obtained by scanning the solar image across a long-slit spectrograph
and are thus strictly simultaneous and cospatial. We discuss a set
of curve-fitting procedures for measuring and removing center-to-limb
variations, systematic instrumental effects, and terrestrial atmospheric
variations with which we have reduced six months of data from 12 Aug 92
to 3 Feb 93. One major purpose of this analysis is to explore how the
spatial structures in the SPM diachronic data relate to variations
in total solar irradiance. To reduce the data volume (each day's
observation is 32 Mbytes) while retaining flexibility to explore a
wide variety of possible criteria for classification of features, we
have prepared pairs of 2-D histograms comparing each of the four other
variables to magnetic flux as well as coarse but strategically binned
5-D histograms. We compare summary statistics based on preliminary
feature classification with solar irradiance data obtained over the
same period.
---------------------------------------------------------
Title: Bright Rims Adjacent to a Quiescent Hα Filament
Authors: Gaizauskas, V.; de Luca, E.; Golub, L.; Jones, H. P.
1994AAS...18512304G Altcode: 1994BAAS...26.1522G
Recent models of filament-formation invoke reconnection between
small-scale magnetic elements adjacent to the polarity inversion line
separating large areas of unipolar magnetic fields. In an attempt to
confirm this process, we examine joint observations of a quiescent
filament straddling the SW limb of the Sun during the total solar
eclipse of 1991 July 11. We test a hypothesis that a signature of the
reconnection process might be carried by the prominent bright rims
beside or enclosed between curved feet, or 'barbs', which connect
the body of the Hα filament to structures near the base of the
atmosphere. We spatially register digitized Hα (ORSO) images of the
filament with coronal (NIXT) images and with photospheric magnetograms
(NSO/KP) to a precision of +/- 2". Our findings relate to five rims,
elongated bright patches in Hα with a maximum length of 20". We find
a better spatial association of the rims with bipolar magnetic elements
(4/5) than with small patches of weakly enhanced soft X-rays (2/4). We
point out that projection effects at these extreme limb positions could
alter these associations. We conclude from these limited 'snapshot'
observations that we are not yet able to decide whether or not bright
rims on quiescent prominences are locations of magnetic reconnection
on a small scale. Because reconnection is highly dynamic, compelling
evidence for or against this process will have to await prolonged
observations at multiple wavelengths in X-rays of a single filament
at high spatial and temporal resolution, such as those envisaged for
the Transition Region and Coronal Explorer (TRACE).
---------------------------------------------------------
Title: Joint observations of the chromosphere, transition region,
and corona from SOHO and NSO/Kitt Peak
Authors: Jones, H. P.; Harvey, John W.; Andretta, Vincenzo
1994ESASP.373..345J Altcode: 1994soho....3..345J
No abstract at ADS
---------------------------------------------------------
Title: The Global Oscillation Network Group Site Survey - Part Two
Authors: Hill, Frank; Fischer, George; Forgach, Suzanne; Grier,
Jennifer; Leibacher, John W.; Jones, Harrison P.; Jones, Patricia
B.; Kupke, Renate; Stebbins, Robin T.; Clay, Donald W.; Ingram,
Robert E. L.; Libbrecht, Kenneth G.; Zirin, Harold; Ulrichi, Roger
K.; Websteri, Lawrence; Hieda, Lester S.; Labonte, Barry J.; Lu,
Wayne M. T.; Sousa, Edwin M.; Garcia, Charles J.; Yasukawa, Eric
A.; Kennewell, John A.; Cole, David G.; Zhen, Huang; Su-Min, Xiao;
Bhatnagar, Arvind; Ambastha, Aashok; Al-Khashlan, Abdulrahman Sa'ad;
Abdul-Samad, Muhammad-Saleh; Benkhaldoun, Zouhair; Kadiri, Samir;
Sánchez, Francisco; Pallé, Pere L.; Duhalde, Oscar; Solis, Hernan;
Saá, Oscar; González, Ricardo
1994SoPh..152..351H Altcode:
The Global Oscillation Network Group (GONG) Project will place a
network of instruments around the world to observe solar oscillations as
continuously as possible for three years. The Project has now chosen the
six network sites based on analysis of survey data from fifteen sites
around the world. The chosen sites are: Big Bear Solar Observatory,
California; Mauna Loa Solar Observatory, Hawaii; Learmonth Solar
Observatory, Australia; Udaipur Solar Observatory, India; Observatorio
del Teide, Tenerife; and Cerro Tololo Interamerican Observatory, Chile.
---------------------------------------------------------
Title: Flow Patterns in Active Regions
Authors: Jones, Harrison P.
1994ASPC...68..286J Altcode: 1994sare.conf..286J
No abstract at ADS
---------------------------------------------------------
Title: Interpreting Recent Observations of He 110830 Angstrom
Authors: Jones, H. P.
1994IAUS..154...49J Altcode: 1994IAUS..154..498J
No abstract at ADS
---------------------------------------------------------
Title: Zodiacal Light and Ancient Symbolism
Authors: Jones, H.
1993JBAA..103..283J Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Contrast of faculae near the disk center and solar variability
Authors: Lawrence, J. K.; Topka, K. P.; Jones, H. P.
1993JGR....9818911L Altcode:
We analyze simultaneous, or near-simultaneous, coregistered, digital,
photometric images of solar photospheric intensity and line-of-sight
magnetic field. Images were made with the Lockheed tunable filter
instrument at the Swedish Solar Observatory, La Palma, with the video
spectra-spectroheliograph system at the San Fernando Observatory and
with the new NASA spectromagnetograph at the National Solar Observatory
at Kitt Peak. We study the disk center contrasts of small magnetic
elements. While active region faculae are dark at disk center quiet
Sun network features are bright. The populations of magnetic field
elements that make up these two kinds of are quite different. Different
contrast center-limb functions must be used when estimating their
irradiance or luminosity contributions. The disk center contrasts of
active region faculae are color dependent and indicate a depth effect
related to the H<SUP>-</SUP> opacity of the facular atmosphere. This
result is important for calibration of monochromatic observations
of faculae to bolometric irradiance fluctuations. We emphasize the
value of cooperative observations among installations whose differing
strengths are complementary.
---------------------------------------------------------
Title: Correlation of He II lyman alpha with He I 10830 Å, and with
chromospheric and EUV coronal emission
Authors: Thompson, W. T.; Neupert, W. M.; Jordan, S. D.; Jones, H.;
Thomas, R. J.; Schmieder, B.
1993SoPh..147...29T Altcode:
This paper describes the results of comparing SERTS-3 images obtained
in the transition region line of HeII 304 å with chromospheric HeI
10830 å absorption, with strong coronal lines of MgIX 368 å, FeXV
284 å and 417 å, and FeXVI 335 å and 31 å, with Hα, with CaII
8542 å, and with magnetograms in FeI 8688Hα. All of the images are
illustrated, and the image reconstruction techniques used are described
and evaluated. The high correlation of the HeII 304 å and HeI 10830
å images, originally found by Harvey and Sheeley (1977), is confirmed
and is put on a quantitative basis. We find that the supergranulation
network has greater contrast, and that filaments appear darker, in
10830 å than in 304 å. In active regions, the 304 å line follows more
closely the behavior of Hα and CaII 8542 å than the 10830 å line.
---------------------------------------------------------
Title: Simultaneous Observations of Solar Plage with the Solar
Extreme Ultraviolet Rocket Telescope and Spectrograph (SERTS),
the VLA, and the Kitt Peak Magnetograph
Authors: Brosius, Jeffrey W.; Davila, Joseph M.; Thompson, William T.;
Thomas, Roger J.; Holman, Gordon D.; Gopalswamy, N.; White, Stephen
M.; Kundu, Mukul R.; Jones, Harrison P.
1993ApJ...411..410B Altcode:
We obtained simultaneous images of solar plage on 1991, May 7
with SERTS, the VLA,4 and the NASA/National Solar Observatory
spectromagnetograph at the NSO/Kitt Peak Vacuum Telescope. Using
intensity ratios of Fe XVI to Fe XV emission lines, we find that the
coronal plasma temperature is (2.3-2.9) x 10 exp 6 K throughout the
region. The column emission measure ranges from 2.5 x 10 exp 27 to
l.3 x 10 exp 28 cm exp -5. The calculated structure and intensity
of the 20 cm wavelength thermal bremsstrahlung emission from the hot
plasma observed by SERTS is quite similar to the observed structure and
intensity of the 20 cm microwave emission observed by the VLA. Using
the Meyer (1991, 1992) revised coronal iron abundance, we find no
evidence either for cool absorbing plasma or for contributions from
thermal gyroemission. Using the observed microwave polarization and the
SERTS plasma parameters, we calculate a map of the coronal longitudinal
magnetic field. The resulting values, about 30-60 G, are comparable
to extrapolated values of the potential field at heights of 5000 and
10,000 km.
---------------------------------------------------------
Title: Planets and Symbolism
Authors: Jones, H.
1993JBAA..103..109J Altcode:
No abstract at ADS
---------------------------------------------------------
Title: A Magnetograph Comparison Workshop
Authors: Jones, H.; Bogart, R.; Canfield, R.; Chapman, G.; Henney,
C.; Kopp, G.; Lites, B.; Mickey, D.; Montgomery, R.; Pillet, V.;
Rabin, D.; Ulrich, R.; Walton, S.
1993BAAS...25.1216J Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Solar Coronal Plasma and Magnetic Field Diagnostics Using
SERTS and Coordinated VLA Observations
Authors: Brosius, J. W.; Davila, J. M.; Thompson, W. T.; Thomas, R. J.;
Holman, G. D.; Gopalswamy, N.; White, S. M.; Kundu, M. R.; Jones, H. P.
1993BAAS...25.1224B Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Intercomparison of Seven Magnetographs
Authors: Walton, S. R.; Bogart, R. S.; Chapman, G. A.; Henney, C.;
Jones, H.; Kopp, G.; Lites, B.; Mickey, D.; Montgomery, R.; Pillet,
V.; Rabin, D.
1993BAAS...25.1205W Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Analysis of EUV, Microwave and Magnetic Field Observations
of Solar Plage
Authors: Brosius, J. W.; Davila, J. M.; Jones, H. P.; Thompson, W. T.;
Thomas, R. J.; Holman, G. D.; White, S. W.; Gopalswamy, N.; Kundu,
M. R.
1993ASPC...46..291B Altcode: 1993mvfs.conf..291B; 1993IAUCo.141..291B
No abstract at ADS
---------------------------------------------------------
Title: Spectrometer-Based Magnetographs (Invited)
Authors: Jones, H.
1993ASPC...46..156J Altcode: 1993mvfs.conf..156J; 1993IAUCo.141..156J
No abstract at ADS
---------------------------------------------------------
Title: Comparison of Magnetograms by Histogram Equating
Authors: Jones, H. P.
1992AAS...181.8105J Altcode: 1992BAAS...24.1252J
No abstract at ADS
---------------------------------------------------------
Title: The NASA/NSO Spectromagnetograph
Authors: Jones, Harrison P.; Duvall, Thomas L., Jr.; Harvey, John W.;
Mahaffey, Charles T.; Schwitters, Jan D.; Simmons, Jorge E.
1992SoPh..139..211J Altcode:
The NASA/NSO Spectromagnetograph is a new focal plane instrument
for the National Solar Observatory/Kitt Peak Vacuum Telescope which
features real-time digital analysis of long-slit spectra formed on a
two-dimensional CCD detector. The instrument is placed at an exit port
of a Littrow spectrograph and uses an existing modulator of circular
polarization. The new instrument replaces the 512-channel Diode Array
Magnetograph first used in 1973. Commercial video processing boards are
used to digitize the spectral images at video rates and to separate,
accumulate, and buffer the spectra in the two polarization states. An
attached processor removes fixed-pattern bias and gain from the spectra
in cadence with spatial scanning of the image across the entrance
slit. The data control computer performs position and width analysis
of the line profiles as they are acquired and records line-of-sight
magnetic field, Doppler shift, and other computed parameters. The
observer controls the instrument through windowed processes on a
data control console using a keyboard and mouse. Early observations
made with the spectromagnetograph are presented and plans for future
development are discussed.
---------------------------------------------------------
Title: Analysis of EUV, Microwave, and Magnetic Field Observations
of a Solar Active Region
Authors: Brosius, J. W.; Davila, J. M.; Jones, H. P.; Thompson, W. T.;
White, S. M.; Gopalswamy, N.; Kundu, M. R.
1992AAS...180.4002B Altcode: 1992BAAS...24R.792B
No abstract at ADS
---------------------------------------------------------
Title: Calibrating the NASA/NSO Spectromagnetograph
Authors: Jones, H. P.
1992AAS...180.5107J Altcode: 1992BAAS...24..814J
No abstract at ADS
---------------------------------------------------------
Title: New Solar Cycle Data from the NASA/NSO Spectromagnetograph
Authors: Jones, Harrison P.
1992ASPC...27..315J Altcode: 1992socy.work..315J
No abstract at ADS
---------------------------------------------------------
Title: Simultaneous EUV, Microwave, and Magnetic Field Observations
of Solar Active Regions
Authors: Brosius, J. W.; Davila, J. M.; Thompson, W. T.; Gopalswamy,
N.; White, S. M.; Jones, H. P.; Metcalf, T. R.
1991BAAS...23.1388B Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Comparison of SERTS Spectroheliograms with Ground-Based
Observations
Authors: Thompson, W. T.; Neupert, W. M.; Brosius, J. W.; Jones,
H. P.; Schmieder, B.
1991BAAS...23R1061T Altcode:
No abstract at ADS
---------------------------------------------------------
Title: The Bartol/NASA/NSO High-Degree Helioseismometer
Authors: Harvey, J.; Hill, F.; Duvall, T., Jr.; Jones, H.; Jefferies,
S.; Pomerantz, M.
1991BAAS...23.1032H Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Spatial Correlation of Spectrum Line Properties with Magnetic
Flux
Authors: Jones, H. P.
1991BAAS...23.1068J Altcode:
No abstract at ADS
---------------------------------------------------------
Title: First Magnetograms from the NASA/NSO Spectromagnetograph
Authors: Jones, H. P.; Duvall, T. L., Jr.; Mahaffey, C. T.
1990BAAS...22..809J Altcode:
No abstract at ADS
---------------------------------------------------------
Title: High-Resolution Magnetograph for the Southwest Solar Facility
Authors: Jones, Harrison
1990rete.conf...36J Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Formation of fourier phase shifts in the solar Ni i 6768
Å line
Authors: Jones, Harrison P.
1989SoPh..120..211J Altcode:
A formalism is developed to understand better how Doppler shifts
of spectrum lines as inferred from phase shifts in the Fourier
transforms of line profiles are related to the underlying velocity
structures which they are intended to measure. With a standard
model atmosphere and a simplified, quasi-LTE treatment of line
formation, the formalism is applied to the NiI 6768 Å line which
has been selected for use with a network of imaging interferometers
under development by the Global Oscillations Network Group (GONG)
for research in helioseismology. Fourier phase shifts are found to
be a remarkably linear measure of velocity even in the presence of
gradients and unresolved lateral variations in the assumed velocity
field. An assumed outward increase in amplitude of a model oscillatory
velocity is noticeably reflected in the center-to-limb behavior of the
simulated velocity measure, and a sample model of solar granulation is
found to have a strong influence on the formation of the Fourier phase.
---------------------------------------------------------
Title: Digitizing Video Spectra at the NASA/NSO Spectromagnetograph
Authors: Jones, H. P.; Brodzik, D.; Duvall, T. L., Jr.
1989BAAS...21..852J Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Magnetograph Observations During the International Solar Month
Authors: Jones, H. P.
1989BAAS...21..862J Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Preflare activity.
Authors: Priest, E. R.; Gaizauskas, V.; Hagyard, M. J.; Schmahl, E. J.;
Webb, D. F.; Cargill, P.; Forbes, T. G.; Hood, A. W.; Steinolfson,
R. S.; Chapman, G. A.; Deloach, A. C.; Gary, G. A.; Jones, H. P.;
Karpen, J. T.; Martres, M. -J.; Porter, J. G.; Schmieder, B.; Smith,
J. B., Jr.; Toomre, J.; Woodgate, B.; Waggett, P.; Bentley, R.;
Hurford, G.; Schadee, A.; Schrijver, J.; Harrison, R.; Martens, P.
1989epos.conf....1P Altcode:
Contents: 1. Introduction. 2. Magnetohydrodynamic
instability. 3. Preflare magnetic and velocity fields. 4. Coronal
manifestations of preflare activity.
---------------------------------------------------------
Title: Magnetograph group summary
Authors: Jones, Harrison P.
1989dots.work...17J Altcode:
The Magnetograph Group focussed on the techniques and many practical
problems of interleaving ground-based measurements of magnetic
fields from diverse sites and instruments to address the original
scientific objectives. The predominant view of the discussion group
was that present instrumentation and analysis resources do not warrant
immediate, specific plans for further worldwide campaigns of cooperative
magnetograph observing. The several reasons for this view, together
with many caveats, qualifications, and suggestions for future work
are presented.
---------------------------------------------------------
Title: The GONG data reduction and analysis system.
Authors: Pintar, J. A.; Andersen, B.; Anderson, E. R.; Armet, D. B.;
Brown, T. M.; Hathaway, D. H.; Hill, F.; Jones, H. P.; GONG Data Team
1988ESASP.286..217P Altcode:
Each of the six GONG observing stations will produce three, 16-bit,
256×256 images of the Sun every 60 seconds of sunlight. These
data will be transferred from the observing sites to the GONG Data
Management and Analysis Center (DMAC), in Tucson, on high-density tapes
at a combined rate of over 1 gigabyte per day. The contemporaneous
processing of these data will produce several standard data products
and will require a sustained throughput in excess of 7 megaflops. Peak
rates may exceed 50 megaflops. Archives will accumulate at the rate
of approximately 1 terabyte per year, reaching nearly 3 terabytes in
three years of observing. Researchers will access the data products
with a machine-independent GONG Reduction and Analysis Software
Package (GRASP). Based on the Image Reduction and Analysis Facility
(IRAF), this package will include database facilities and helioseismic
analysis tools. Users may access the data as visitors in Tucson, or
may access DMAC remotely through networks, or may process subsets of
the data at their local institutions using GRASP or other systems of
their choice. Elements of the system will reach the prototype stage
by the end of 1988. Full operation is expected in 1992 when data
acquisition begins.
---------------------------------------------------------
Title: The GONG site survey.
Authors: Hill, F.; Ambastha, A.; Ball, W.; Duhalde, O.; Farris,
D.; Fischer, G.; Hieda, L.; Zhen, Huang; Ingram, B.; Jackson, P.;
Jones, H.; Jones, W.; Kennewell, J.; Kunkel, W.; Kupke, R.; Labonte,
B.; Leibacher, J.; Libbrecht, K.; Lu, W.; Morrison, L.; Odell, C.;
Pallé, P.; Saá, O.; Sousa, E.; Stebbins, T.; Xiao, Suming; GONG
Site Survey Team
1988ESASP.286..209H Altcode:
The Global Oscillation Network Group (GONG) project is planning to
place six observing stations around the world to observe the solar
oscillations as continuously as possible. This paper describes the
procedures that are being used to select the six sites. The latest
results of measurements of cloud cover obtained by networks of 6
(out of 10) radiometers show a duty cycle of over 93%, with the first
diurnal sidelobe in the window power spectrum suppressed by a factor
of 400. The results are in good agreement with the predictions of a
computer model of the expected cloud cover at individual sites.
---------------------------------------------------------
Title: Experimental constraints on heating and cooling rates of
refractory inclusions in the early solar system
Authors: Boynton, W. V.; Drake; Hildebrand; Jones; Lewis; Treiman; Wark
1987eprs.nasaQ....B Altcode:
The refractory inclusions in carbonaceous chondrites were the subject of
considerable interest since their discovery. These inclusions contain
minerals that are predicted to be some of the earliest condensates
from the solar nebula, and contain a plethora of isotopic anomalies
of unknown origin. Of particular interest are those coarse-grained
inclusions that contain refractory metal particles (Fe, Ni, Pt,
Ru, Os Ir). Experimental studies of these inclusions in terrestrial
laboratories are, however, complicated because the dense particles tend
to settle out of a molten or partially molten silicate material. Heating
experiments in the Space Station technology and microgravity in order
to observe the effects of metal nuggets (which may act as heterogeneous
nucleation sites) on nucleation rates in silicate systems and to measure
simultaneously the relative volatilization rate of siderophile and
lithophile species. Neither experiment is possible in the terrestrial
environment.
---------------------------------------------------------
Title: Experimental constraints on the origin of chondrules
Authors: Boynton, W. V.; Drake; Hildebrand; Jones; Lewis; Treiman; Wark
1987eprs.nasaR....B Altcode:
Chrondule formation was an important (perhaps ubiguitous) process in
the early solar system, yet their origins remain elusive. Some points,
however, are clear. The precursor material of chondules (dust) was
rapidly heated at rates of perhaps thousands of degrees per second
and was cooled more slowly. It was proposed to investigate chondrule
formation in the Space Station environment via a dust-box (a chamber
in which dust can be suspended, heated, and cooled. A microgravity
environment is conducive to this kind of experiment because of the
significant retardation of settling rates compared with a terrestrial
laboratory environment. These long-duration experiments might require
the development of technologies to counteract even the small, but
finite and permanent gravitation field of the Space Station. Simple,
but interesting experiments on dust suspensions immediately present
themselves.
---------------------------------------------------------
Title: "Underluminous" Lyman-alpha Emission Associated with
Active-Region Magnetic Canopy
Authors: Jones, H. P.; Skumanich, A.; Lemaire, P.
1987BAAS...19..930J Altcode:
No abstract at ADS
---------------------------------------------------------
Title: The NSO/NASA CCD Spectromagnetograph
Authors: Jones, H. P.
1987BAAS...19..929J Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Preflare magnetic and velocity fields
Authors: Hagyard, M. J.; Gaizauskas, V.; Chapman, G. A.; Deloach,
A. C.; Gary, G. A.; Jones, H. P.; Karpen, J. T.; Martres, M. -J.;
Porter, J. G.; Schmeider, B.
1986epos.conf.1.16H Altcode: 1986epos.confA..16H
A characterization is given of the preflare magnetic field, using
theoretical models of force free fields together with observed field
structure to determine the general morphology. Direct observational
evidence for sheared magnetic fields is presented. The role of this
magnetic shear in the flare process is considered within the context
of a MHD model that describes the buildup of magnetic energy, and the
concept of a critical value of shear is explored. The related subject
of electric currents in the preflare state is discussed next, with
emphasis on new insights provided by direct calculations of the vertical
electric current density from vector magnetograph data and on the role
of these currents in producing preflare brightenings. Results from
investigations concerning velocity fields in flaring active regions,
describing observations and analyses of preflare ejecta, sheared
velocities, and vortical motions near flaring sites are given. This
is followed by a critical review of prevalent concepts concerning the
association of flux emergence with flares
---------------------------------------------------------
Title: Magnetic Shear. III. Hale Region 17255
Authors: Athay, R. G.; Jones, H. P.; Zirin, H.
1986ApJ...303..877A Altcode:
Hale active region 17255, which in many respects was the most vigorous
active region observed during the first operational period of SMM,
appears to lie between two large areas of flow (observed in C IV)
converging toward the major axis of the region. In the 6-day period
from November 6-12, 1980, the major axis of the region rotates by
about 25 deg. Several segments of the magnetic neutral line show C
IV flow velocities of opposite sign on either side of the neutral
line. Those segments whose orientation is favorable for measuring
velocity components parallel to the neutral line show evidence that
such flow is present, which is interpreted as evidence for magnetic
shear. This, together with other evidence, suggests that magnetic
shear is widespread in this region, as in the two previous regions
studied. It is concluded that magnetic shear is often associated with
flaring activity but is not a sufficient condition for flaring to occur.
---------------------------------------------------------
Title: Magnetic Shear. IV. Hale Regions 16740, 16815, and 16850
Authors: Athay, R. G.; Klimchuk, J. A.; Jones, H. P.; Zirin, H.
1986ApJ...303..884A Altcode:
Dopplergrams made in C IV 1548 A are studied for evidence of velocity
shear near H-alpha dark filaments and for large-scale flow convergent on
active regions. The three regions studied support earlier conclusions
that shear is a common property of active regions and that active
regions may be the foci of converging plasma flow. Flow patterns
near filaments show divergence or convergence as well as shear. Also
the sense of the shear can be either cyclonic or anticyclonic. No
preference is noted for convergence or divergence or for a particular
sense of shear, and there appears to be no correlation between the
sense of the shear and the sign of the velocity gradient normal to
the filament. The close association of H-alpha dark filaments with
shear lines leads to the suggestion that the filaments may arise from
a cooling instability induced by the Bernoulli effect.
---------------------------------------------------------
Title: Preflare activity.
Authors: Priest, E. R.; Gaizauskas, V.; Hagyard, M. J.; Schmahl, E. J.;
Webb, D. F.; Cargill, P.; Forbes, T. G.; Hood, A. W.; Steinolfson,
R. S.; Chapman, G. A.; Deloach, A. C.; Gary, G. A.; Jones, H. P.;
Karpen, J. T.; Martres, M. -J.; Porter, J. G.; Schmieder, B.; Smith,
J. B., Jr.; Toomre, J.; Woodgate, B.; Waggett, P.; Bentley, R.;
Hurford, G.; Schadee, A.; Schrijver, J.; Harrison, R.; Martens, P.
1986NASCP2439....1P Altcode:
Contents: 1. Introduction: the preflare state - a review of previous
results. 2. Magnetohydrodynamic instability: magnetic reconnection,
nonlinear tearing, nonlinear reconnection experiments, emerging flux and
moving satellite sunspots, main phase reconnection in two-ribbon flares,
magnetic instability responsible for filament eruption in two-ribbon
flares. 3. Preflare magnetic and velocity fields: general morphology of
the preflare magnetic field, magnetic field shear, electric currents in
the preflare active region, characterization of the preflare velocity
field, emerging flux. 4. Coronal manifestations of preflare activity:
defining the preflare regime, specific illustrative events, comparison
of preflare X-rays and ultraviolet, preflare microwave intensity and
polarization changes, non-thermal precursors, precursors of coronal
mass ejections, short-lived and long-lived HXIS sources as possible
precursors.
---------------------------------------------------------
Title: The Interpretation of Spectrum Lines Formed in Small Solar
Structures
Authors: Jones, H. P.
1986ssmf.conf..127J Altcode:
The author reviews some important aspects of radiative transfer
bearing on the interpretation of high-resolution solar data. Recent
developments in techniques for solving transfer problems were discussed
along with some known effects of lateral radiative exchange such as
thermal smoothing and channeling. Also discussed were the effects of
non-uniform fields which must occur along the lines of sight which
traverse small solar flux concentrations.
---------------------------------------------------------
Title: Erratum - a Study of Flare Buildup from Simultaneous
Observations in Microwave Hα and Ultraviolet Wavelengths
Authors: Kundu, M. R.; Gaizauskas, V.; Woodgate, B. E.; Schmahl,
E. J.; Shine, R.; Jones, H. P.
1985ApJS...58..195K Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Magnetic shear. II - Hale region 17244
Authors: Athay, R. G.; Jones, H. P.; Zirin, H.
1985ApJ...291..344A Altcode:
A B-gamma(delta) sunspot group with growing delta-spots of trailing
polarity shows evidence in H-alpha filament structure of a transition
from a state of weak magnetic shear to a state of strong shear. The
shear develops in the chromosphere and transition region to the
corona overlying the photospheric magnetic neutral line separating the
delta-spots from the leading polarity at a time when the delta-spots are
undergoing rapid growth. Several major flares occur along the sheared
portion of the neutral line following the shear development. Other
segments of the neutral line far removed from the delta-spots show
similar evidence of shear in the H-alpha filament structure and in C
IV velocity patterns as well. These 'quiescent' regions of shear are
relatively steady or decaying with time and show very little related
activity.
---------------------------------------------------------
Title: Potential Fields and Magnetic Canopies
Authors: Jones, H. P.
1985BAAS...17..633J Altcode:
No abstract at ADS
---------------------------------------------------------
Title: A study of flare buildup from simultaneous observations in
microwave, H-alpha, and UV wavelengths
Authors: Kundu, M. R.; Gaizauskas, V.; Woodgate, B. E.; Schmahl,
E. J.; Shine, R.; Jones, H. P.
1985ApJS...57..621K Altcode:
The results of high-resolution observations of the solar preflare
activity of June 25, 1980 are analyzed. The observations were carried
out simultaneously in the UV microwave, and H-alpha wavelengths
using the VLA, the Ottawa River photoheliograph, and the Solar Max
spectrometer and polarimeter instruments. Increases were observed in the
intensitiy and polarization of compact sources at a wavelength of 6-cm
during the preflare hour. The increases were associated with rising and
twisting motions in the magnetic loops near the sight of the subsequent
flare. Consistent with this process, analysis of the transverse and
Doppler motions observed in the H-alpha filament before disruption
showed that the filament was activated internally by the motions of
evolving magnetic flux patterns. Ultraviolet data for C IV brightenings
and upflows at the first appearance of the H-alpha filament indicated
the presence of rising magnetic loops and material rising within the
loops. The complete VLA, microwave and H-alpha data sets are given.
---------------------------------------------------------
Title: Full Disk Continuum Photometry with the NSO/Tusson Vacuum
Telescope
Authors: Luttermoser, D. G.; Jones, H. P.
1985BAAS...17..639L Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Magnetic shear. I - Hale region 16918
Authors: Athay, R. G.; Jones, H. P.; Zirin, H.
1985ApJ...288..363A Altcode:
Material motion observed in spectral lines of C IV, C II, and Ca
II formed in the chromosphere-corona transition region and upper
chromosphere exhibits patterns that are closely identified with magnetic
field structure at photospheric levels. Assuming that the fluid flow
follows magnetic lines of force, the authors use chromospheric and
transition region Dopplergrams to infer the broad features of the
magnetic field geometry in these upper layers. For Hale region 16918
they find an area in the transition region and upper chromosphere,
centered roughly over the photospheric magnetic neutral line, in which
the lines of force show a strong tendency to parallel the photospheric
neutral line. The authors interpret this as evidence for magnetic shear,
which is pronounced in the upper layers of the atmosphere.
---------------------------------------------------------
Title: Working group on chromospheric fields - canopies.
Authors: Jones, H. P.
1985cdm..proc...10J Altcode:
Although there are many points of uncertainty and controversy, the
working group on chromospheric fields focussed its discussion on the
concept of canopies; i.e., no one disagreed that a central issue
relating to magnetic fields and chromospheric models is to learn
how the photospheric field spreads with height. However, it quickly
became apparent that in the time available, there was little prospect
of building new unified models of magnetic field phenomena in the
chromosphere beyond the scope of the formal presentations. Thus,
the discussion was devoted to formulating questions which seemed
both possible to address in future work and important for advancing
understanding of the chromosphere. It began by discussing unresolved
physical issues (almost everything) and then proceeded to consider
means, both observational and synthetic, to address them.
---------------------------------------------------------
Title: Recent studies of magnetic canopies
Authors: Jones, H. P.
1985AuJPh..38..919J Altcode:
Two current studies are described which stem from Giovanelli's seminal
studies of the spreading of chromospheric fields near active regions
and active-region network. First, improved observational techniques
are described for obtaining magnetograms in the Ca II 8542 A, Fe
I 8688 A, and C I 9111 A lines which at least in principle allow
for more accurate treatment of instrumental noise and allow better
inference of field orientation. Second, a generalized response
function is developed for calculating theoretical magnetograph
signals from arbitrary line-of-sight variations of magnetic field,
and initial applications to two-dimensional, potential-field models
of network fields are described. Preliminary indications are that
potential-field models can better explain the presence of low-lying,
diffuse horizontal fields than can thin flux-tube models, but fail to
predict a differential response between the different lines.
---------------------------------------------------------
Title: Magnetic canopies and models of the solar chromosphere.
Authors: Jones, H. P.
1985cdm..proc..175J Altcode:
Magnetic canopies are the topologies formed by magnetic field lines
as they spread from compact, nearly vertical concentrations of flux
in the low photosphere into the large-scale organization of the corona
and heliosphere. Analytical techniques for inferring the base-heights
of canopies from magnetographic data are reviewed together with
observational evidence that much of the sun is covered by canopies
which lie two or more pressure scale heights below the level which
is traditionally inferred from thin flux tube models. Implications
of these results for modeling the structure and energetics of the
chromosphere are discussed, and it is argued that future models
should be based upon both spectroscopic and polarimetric data. Recent
improvements in magnetostatic model atmospheres are reviewed, and new
observational data, including C IV Doppler-grams from the Ultraviolet
Spectrometer and Polarimeter on the Solar Maximum Mission, are
considered. Directions for future research in MHD modeling of canopies,
in simulating spectrographic and polarimetric data from such models,
and in observational programs are discussed.
---------------------------------------------------------
Title: Magnetic changes observed in a solar flare
Authors: Moore, R. L.; Hurford, G. J.; Jones, H. P.; Kane, S. R.
1984ApJ...276..379M Altcode:
The authors present observations of a large impulsive flare (1B/M4,
1980 April 10). Observations of the microwave/hard X-ray burst show
the time development of the impulsive energy release. Chromospheric
(Hα) and photospheric (Fe I λ5324) filtergrams and photospheric (Fe I
λ8688) magnetograms, intensitygrams, and velocitygrams show magnetic
structure, flare emission, mass motion, and magnetic changes. These
observations show that strong flare-wrought magnetic changes in the
chromosphere and corona produce observable, sudden, permanent changes
in the photospheric magnetic field. The observations also show that one
of the changes was initiated by transient brightening in Fe I λ5324 and
λ8688 in step with the impulsive energy release and filament eruption.
---------------------------------------------------------
Title: Relationships of a growing magnetic flux region to flares
Authors: Martin, S. F.; Bentley, R. D.; Schadee, A.; Antalova, A.;
Kucera, A.; Dezső, L.; Gesztelyi, L.; Harvey, K. L.; Jones, H.;
Livi, S. H. B.; Wang, J.
1984AdSpR...4g..61M Altcode: 1984AdSpR...4...61M
Some sites for solar flares are known to develop where new magnetic
flux emerges and becomes abutted against opposite polarity pre-existing
magnetic flux (review by Galzauskas/1/). We have identified and analyzed
the evolution of such flare sites at the boundaries of a major new and
growing magnetic flux region within a complex of active regions, Hale
No. 16918. This analysis was done as a part of a continuing study of the
circumstances associated with flares in Hale Region 16918, which was
designated as an FBS target during the interval 18 - 23 June 1980. We
studied the initiation and development of both major and minor flares in
Hα images in relation to the identified potential flare sites at the
boundaries of the growing flux region and to the general development
of the new flux. This study lead to our recognition of a spectrum of
possible relationships of growing flux regions to flares as follows:
(1) intimate interaction with adjacent old flux - flare sites centered
at new/old flux boundary, (2) forced or “intimidated” interaction
in which new flux pushes old field having lower flux density towards a
neighboring old polarity inversion line where a flare then takes place,
(3) “influential” interaction - magnetic lines of force over an old
polarity inversion line, typically containing a filament, reconnect to
the new emerging flux; a flare occurs with erupting filament when the
magnetic field overlying the filament becomes too weak to prevent its
eruption, (4) inconsequential interaction - new flux region is too small
or has wrong orientation for creating flare conditions, (5) incidental -
flare occurs without any significant relationship to new flux regions.
---------------------------------------------------------
Title: Variations of Total Solar Irradiance During Rapid Sunspot
Growth
Authors: Hudson, H. S.; Jones, H.; McIntosh, P.
1983BAAS...15Q.950H Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Solar oscillations with 13-day period
Authors: Duvall, T. L., Jr.; Jones, H. P.; Harvey, J. W.
1983Natur.304..517D Altcode:
Reference is made to the solar observations made by Claverie et
al. (1982) over a three-month period in the summer of 1981 which
show oscillatory velocity with a period of 13.1 days and amplitude
of 6.6 m/s. These investigators reject the possibility that they see
the Doppler shift from a radial oscillation, because the amplitude
is implausibly large. They also do not believe that their signal was
induced by solar magnetic fields, since typical mean solar fields are
too small. Photo-electric drift-scan measurements of the solar diameter
and full-disk magnetograms taken at Kitt Peak National Observatory are
examined here for evidence of variations corresponding to the velocity
oscillations of the 13.1-day period. An upper limit on radius variations
is reported which is a factor of six below the amplitude needed to
explain the velocity observations as a radial oscillation. Attention
is also given to the possible role of the rotation of large-scale
surface magnetic features.
---------------------------------------------------------
Title: Magnetic canopies in unipolar regions.
Authors: Jones, H. P.; Giovanelli, R. G.
1983SoPh...87...37J Altcode:
Base-height statistics are presented for magnetic canopies in six
unipolar magnetic regions which were observed near the limb with the
Kitt Peak Vacuum Telescope and Diode Array Magnetograph during the
period 25 April-3 July, 1980. As in earlier studies, extensive areas
are found to be covered by low-lying canopies.
---------------------------------------------------------
Title: Photospheric, Chromospheric and Transition-Region Flows in
AR 2517
Authors: Athay, R. G.; Jones, H. P.; Zirin, H.
1983BAAS...15Q.719A Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Permafrost melting and dissolution of the landscape of Mars.
Authors: Jones, H. P.
1982ESASP.185...89J Altcode: 1982plma.rept...89J
It is supposed that during or after the updoming of the Noctis
Labyrinthus-/Valles Marineris dome, postulated permafrost either
completely or partly melted. The result was probably a slow sliding
of the overlying volcanic rocks to the east, southeast and south,
according to the inclination of the areas surface.
---------------------------------------------------------
Title: Magnetic Changes Observed in a Flare: True and Flase Transients
and True Permanent Changes
Authors: Moore, R. L.; Hurford, G. J.; Jones, H. P.; Kane, S. R.
1982BAAS...14..899M Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Scaling-Law Equilibria for Calcium in Canopy-Type Models of
the Solar Chromosphere
Authors: Jones, H. P.
1982SoPh...79..279J Altcode:
Scaling laws for resonance line formation are used to obtain approximate
excitation and ionization equilibria for a three-level model of singly
ionized calcium. The method has been developed for and is applied to
the study of magnetograph response in the 8542 Å infrared triplet line
to magnetostatic canopies which schematically model diffuse, nearly
horizontal fields in the low solar chromosphere. For this application,
the method is shown to be efficient and semi-quantitative, and the
results indicate the type and range of effects on calcium-line radiation
which result from reduced gas pressure inside the magnetic regions.
---------------------------------------------------------
Title: The Three-Dimensional Structure of Atmospheric Magnetic Fields
in Two Active Regions
Authors: Giovanelli, R. G.; Jones, H. P.
1982SoPh...79..267G Altcode:
The magnetic field above two unrelated active regions on 11 and 12
September, 1974 has been studied using magnetograms obtained in C I
9111, Fe I 8688, Ca II 8542, and Hα. In C I 9111, originating low in
the photosphere, the fields are strong and sharply defined. In Ca II
8542 and Hα they are very diffuse, with significant diffuseness also in
Fe I 8688, due to the spreading of the field with height to form almost
horizontal magnetic canopies over regions free of field at lower levels.
---------------------------------------------------------
Title: Magnetograph Response to Canopy-Type Fields
Authors: Jones, H. P.; Giovanelli, R. G.
1982SoPh...79..247J Altcode:
The response of longitudinal-field magnetographs to magnetic fields
which are semi-infinite or confined to a horizontal layer is discussed
with respect to the interpretation of solar diffuse fields, observed
towards the limb, in terms of magnetic canopy models. Numerical
results are presented for several reference solar models and typical
`calibration' curves are shown for the C I 9111 Å, Fe I 8688 Å, and
Ca II 8542 Å lines in magnetostatic atmospheres derived from a mean
model. A procedure is developed for determining the base heights of
magnetic canopies from observations with an uncertainty not exceeding
the order of a pressure scale height. Until definitive information
regarding atmospheric structure inside flux tubes can be developed from
theory or observation, reliable field strengths cannot be derived from
the data.
---------------------------------------------------------
Title: Observations of sudden changes of magnetic structure in
a flare.
Authors: Moore, R. L.; Hurford, G. J.; Jones, H. P.; Kane, S. R.
1982BAAS...14Q.572M Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Solar radius measurements
Authors: Duvall, T. L., Jr.; Jones, H. P.
1981NASCP2191..129D Altcode: 1981vsc..conf..129D
Preliminary results of measurements made during 1979-1980 are
discussed. Variability in the radius measurements of 0.4 pi is found,
of unknown origin.
---------------------------------------------------------
Title: Ultramafic blocks from the ocean floor southwest of Australia
Authors: Nicholls, I. A.; Ferguson, John; Jones, H.; Marks, G. P.;
Mutter, J. C.
1981E&PSL..56..362N Altcode:
Samples dredged from the ocean floor near the junction of the
Naturaliste Fracture Zone and the Diamantina Zone, 300 km southwest of
Cape Leeuwin, Western Australia, contain 3- to 10-cm blocks of Cr-spinel
lherzolites and Al-spinel-olivine clinopyroxenites. Both assemblages
show textural evidence for deformation and recrystallization, with
extensive development of kaersutite in one clinopyroxenite. The
blocks are enclosed by clay and Fe-Mn oxide-rich fragmental
material, which also contains a diverse detrital mineral suite and
microfossils. Diopsides in the lherzolites are Na- and Cr-rich, with
marked similarities to those of lherzolite nodules in alkaline basaltic
suites. The Al- and Ti-rich diopsides of the clinopyroxenites are more
magnesium than those of common pyroxene-rich nodules. The lherzolites
are interpreted as upper mantle residues, while the clinopyroxenites
probably represent partly recrystallized cumulates from high-temperature
basaltic magmas traversing the lherzolite mantle. Both are thought to
have been derived from an ultramafic body emplaced into the shallow
crust near the Cretaceous/early Tertiary continent-ocean boundary
off Australia.
---------------------------------------------------------
Title: Solar Radius Measurements
Authors: Duvall, T.; Jones, H.
1981siwn.conf..366D Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Magnetic Canopies in Unipolar Regions
Authors: Jones, H. P.; Giovanelli, R. G.
1981BAAS...13R.881J Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Effects of Field Stratification on Magnetographic Measurements
in the Infrared Triplet Lines of CaII
Authors: Jones, H. P.; Giovanelli, R. G.
1980BAAS...12..807J Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Support of SMM with the Kitt Peak Vacuum Telescope; A Survey
of Active Regions
Authors: Jones, H. P.; Duvall, T. L., Jr.; Recely, F. J.
1980BAAS...12..906J Altcode:
No abstract at ADS
---------------------------------------------------------
Title: A New Method for Measureing the Solar Radius
Authors: Duvall, T. L., Jr.; Jones, H. P.
1980BAAS...12..474D Altcode:
No abstract at ADS
---------------------------------------------------------
Title: The Physical Effects of Radiative Transfer in Multidimensional
Media Including Models of the Solar Atmosphere
Authors: Jones, H. P.; Skumanich, A.
1980ApJS...42..221J Altcode:
We review the astrophysical literature concerning radiative transfer
in multidimensional media where one requires the solution of the
transfer equation under scattering conditions for a medium in which
some combination of boundary configuration, external illumination,
and internal thermodynamic structure causes the radiation field to vary
with more than one spatial dimension. In constant opacity atmospheres,
the radiation field is shown to scale systematically with to a
characteristic geometric scale for a wide variety of configurations
and types of scattering. Some effects of radiative exchange between
different regions of multidimensional media are reviewed, and the
constraining influence of an exponential vertical variation of opacity
is discussed. Particular emphasis is given to recent applications of
multidimensional transfer to the interpretation of the fine spatial
structure on the Sun.
---------------------------------------------------------
Title: Multidimensional Radiative Transfer in Exponential Atmospheres
Authors: Jones, H. P.
1979BAAS...11..405J Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Splines under Tension in Integral Transfer Problems
Authors: Jones, H. P.
1977JQSRT..17..776J Altcode:
No abstract at ADS
---------------------------------------------------------
Title: A possible edge effect in enhanced network.
Authors: Jones, H. P.; Brown, D. R.
1977SoPh...52..337J Altcode:
K-line observations of enhanced network taken with the NASA/SPO
Multichannel Spectrometer on 28 September 1975 in support of OSO-8
are discussed. The data show a correlation between core brightness
and asymmetry for spatial scans which cross enhanced network
boundaries. The implications of this result concerning mass flow in
and near supergranule boundaries are discussed.
---------------------------------------------------------
Title: Space telescope solar array. Feasibility study. Volume 2:
Technical report
Authors: Jones, H.
1976STIN...7719966J Altcode:
The results of a feasibility study of the space telescope solar
array are described and consideration of design is included. The
selected concept with the rationale for its choice is described. A
BISTEM actuated ROSA is chosen on the basis of its general compliance
particularly with the dynamics, comparative simplicity, and mainly
proven technology. Other candidate concepts are described and
evaluated. A design description is given which includes configuration,
mechanical, electrical, dynamic, and thermal aspects.
---------------------------------------------------------
Title: Observations of Enhanced Network from the NASA/SPO Multichannel
Spectrometer in Support of OSO-8
Authors: Jones, H. P.; Brown, D. R.
1976BAAS....8..332J Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Automation of the Solar Multichannel Spectrometer.
Authors: Hobbs, R. W.; Harris, G. D.; Jones, H. P.; Epstein, G. L.;
Brown, D. R.; Wassmund, P.
1975BAAS....7..432H Altcode:
No abstract at ADS
---------------------------------------------------------
Title: A two-layer plus background model for the solar K-line.
Authors: Jones, H. P.
1974BAAS....6..485J Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Splat cooling and metastable phases
Authors: Jones, H.
1973RPPh...36.1425J Altcode:
No abstract at ADS
---------------------------------------------------------
Title: The Formation of Resonance Lines in Multidimensional
Media. II. Radiation Operators and Their Numerical Representation
Authors: Jones, Harrison P.; Skumanich, A.
1973ApJ...185..167J Altcode:
A general integral-operator representation of radiative transfer
in an atmosphere whose properties vary in more than one spatial
dimension is developed together with well-posed procedures for its
discrete numerical representation. This methodology is applied to the
"non-LTE" excitation equilibrium of a two-level impurity species, i.e.,
to the formation of a resonance absorption line. The radiation operator
that appears in the excitation equation is converted into a finite
but large matrix by means of a suitably selected finite set of basis
functions. This matrix-excitation equation is inverted directly to yield
the excitation state and, hence, the impurity absorption characteristics
of the plasma. Illustrative applications to the formation of a resonance
line in a constant-density plasma with several types of two-dimensional
temperature structures are presented. Subject headings: line formation -
radiative transfer
---------------------------------------------------------
Title: The Formation of Resonance Lines in Multidimensional
Media. III. Interpolation Functions, Accuracy, and Stability
Authors: Jones, Harrison P.
1973ApJ...185..183J Altcode:
The accuracy and stability for several specific representations of the
integral-operator technique presented in Paper II (Jones and Skumanich
1973) are discussed. Solutions are tested against independently
calculated results for an effectively thin "embedded slab." It is found
that the cardinal interpolation functions for approximating the source
function along characteristics must be "local," must give accurate
representation of a variety of functions and their second derivatives
on coarse, irregular grids, and must be compatible with interpolation
functions used to map functions of spatial position to functions of path
length. Cubic splines appear to meet these requirements and give good
overall results. Subject headings: line formation - radiative transfer
---------------------------------------------------------
Title: Asymmetries in the Solar K-Line.
Authors: Jones, H. P.
1973BAAS....5..445J Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Observations of the Solar Flare of 7 August 1972
Authors: Epstein, Gabriel L.; Hobbs, Robert W.; Maran, Stephen P.;
Jones, Harrison P.
1973BAAS....5R.272E Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Line Formation in Multidimensional Atmospheres with Rapid
Depth Variation of Absorption Coefficient
Authors: Jones, H. P.
1973BAAS....5R.274J Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Interpolation Functions, Accuracy, and Stability in
Multidimensional Transfer Problems.
Authors: Jones, H. P.
1972BAAS....4..211J Altcode:
No abstract at ADS
---------------------------------------------------------
Title: The Formation of Resonance Lines in Multidimensional
Media. I. Scaling Properties in Two Dimensions
Authors: Jones, Harrison P.
1971ApJ...164..341J Altcode:
A method developed by Rybicki is applied to the non-LTE line-transfer
problem for some simple two-dimensional temperature variations which
crudely represent some aspects of the lateral fine structure of the
solar atmosphere. Approximate scaling formulae are found which describe
the spatial variation of the source function and its dependence on the
geometric properties of the atmosphere. It is shown that the resulting
spatial behavior of the emergent radiation can vary with frequency
within a single profile as well as from line to line even when the
underlying horizontal temperature structure is independent of depth.
---------------------------------------------------------
Title: The Scaling of Resonance-Line Radiation in Two-Dimensional
Imbedded Slabs
Authors: Jones, Harrison P.
1970BAAS....2R.324J Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Line Formation in Multi-Dimensional Media.
Authors: Jones, Harrison Price
1970PhDT.........5J Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Line Formation in Multi-Dimensional Media
Authors: Jones, H. P.; Skumanich, A.
1970sfss.coll..138J Altcode: 1970IAUCo...2..138J
No abstract at ADS
---------------------------------------------------------
Title: Line Formation in Multidimensional Media
Authors: Jones, H. P.; Skumanich, A.
1969BAAS....1S.281J Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Line Formation in Multi-Dimensional Media
Authors: Jones, H. P.; Skumanich, A.
1968rla..conf...79J Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Statistical Equilibrium for a Multilevel Model of Calcium in
the Solar Chromosphere.
Authors: Jones, H. P.; Domenico, B. A.; Skumanich, A.
1968AJS....73S..66J Altcode:
The statistical equilibrium of Ca is studied for collisional and
radiative interactions a~propriate to various states of the solar
chromosphere (cf. Athay and Skumanich, 1967). A model ion with
levels representing the ground states of Ca I, II, and III is used,
including the 4p2P and 3d2D excited states (ignoring fine structure)
of Ca II. Dielectronic recombination from Ca II to Ca I is included in
such a way as to display its maximum effect. For the mean chromosphere
the ratio of continuum to line absorption coefficient, r0, for the
"H-K" line (2P-2S transition) of Ca II is found to be independent
of the radiation fields in the "H-K" and infrared "triplet" (2P-2D)
lines. For other chromospheric conditions (e.g., spicules and plages)
the above is not true and care must be exercised because line transfer
calculations must include a self-consistent treatment of the effect of
line radiation fields on line opacities. Dielectronic recombination
does not affect r0 by more than a factor of 2 to 3. For an optically
thick chromosphere in the "H-K" line ETH~K(Tmin) 3 X 104J such as
used by Athay and Skumanich (1967), Linsky (1967), and Dumont (1967),
studies of the interlocking terms in the "H-K" source function show
the two-level atom to be a useful first approximation. In such a thick
atmosphere the infrared "triplet" saturates to a condition of radiative
detailed balance well before the temperature minimum. This requires the
K1 intensities to yield a temperature minimum of the order of 42000K
regardless of the rate coefficients assumed in the model atom. To
reconcile the K1 intensities with a Tn~jn of 46000K as suggested by
the Bilderberg model (1967) requires an unsaturated infrared "triplet"
and hence a reduction in the "H-K" line optical depth by a factor of
several hundred.
---------------------------------------------------------
Title: Electrons in Nearly Periodic Fields
Authors: Jones, H.
1966RSPSA.294..405J Altcode:
A detailed investigation is made of the change in the energy spectrum of
a single electron in a pure metal brought about by the addition of small
quantities of other elements in solid solution. To obtain numerical
results the foreign atoms are represented by exponentially screened
positive charges. The combined effects of line displacement and line
broadening are determined and the change in the density of states at
the Fermi limit is calculated. It is shown that the distortion of the
energy band depends critically on the nature of the electronic states
in the pure metal. Comparisons are made with the observed electronic
specific heats of silver-based and copper-based solid solutions.
---------------------------------------------------------
Title: The properties of liquid helium
Authors: Jones, H.
1939RPPh....6..280J Altcode:
No abstract at ADS
