Author name code: baker ADS astronomy entries on 2022-09-14 =author:"Baker, D." OR =author:"Baker, Deborah" -title:"Mars" -title:VizieR" ------------------------------------------------------------------------ Title: Stellar FIP effect from the empirical side Authors: Seli, Bálint; Van Driel-Gesztelyi, Lidia; Baker, Deborah; Laming, J. Martin; Kovari, Zsolt; Oláh, Katalin; Kriskovics, Levente; Vida, Krisztián; Balázs, Lajos Bibcode: 2022cosp...44.2585S Altcode: The difference between the elemental abundances of the corona and the photosphere is an apparently common feature of stellar atmospheres. The abundance difference depends on the first ionization potential of the given element, so the phenomenon is known as the FIP effect. Here we explore the variation of the strength of the FIP effect for different types of stars, through the FIP bias parameter. Using a sample of 59 main sequence and evolved stars with known coronal abundances from the literature, we look for macroscopic, measurable parameters that affect the stellar FIP bias, and also re-evaluate the simple dependence on the effective temperature. Title: Investigating of the nature of magnetic oscillations associated with FIP effect Authors: Murabito, Mariarita; Jafarzadeh, Shahin; Van Driel-Gesztelyi, Lidia; Ermolli, Ilaria; Baker, Deborah; Brooks, David; Long, David; Jess, David; Valori, Gherardo; Stangalini, Marco Bibcode: 2022cosp...44.2591M Altcode: Observations of the photosphere, chromosphere, and corona combined with magnetic field modeling of one of the biggest sunspots of the 24 solar cycle, revealed that regions of high FIP bias plasma in the corona were magnetically linked to the locations of the intrinsic magnetic oscillations in the solar chromosphere. In order to characterize the driver of the oscillations, we analyzed the relation between the spatial distribution of the magnetic wave power and the overall field geometry and plasma parameters obtained from the multi-height spectropolarimetric non-local thermodynamic equilibrium (NLTE) inversions. In correspondence with the locations where the magnetic wave energy is observed at chromospheric heights, we found evidence in support of locally excited acoustic waves that, after crossing the equipartition layer located close to the umbra-penumbra boundary at photospheric heights, are converted into magnetic-like waves. These results indicate a direct connection between sunspot chromospheric activity and observable changes in coronal plasma composition, demonstrating the power of high resolution, multi-height studies of the solar atmosphere that will become the gold standard in the era of DKIST. Title: Understanding the Correlation between Solar Coronal Abundances and F10.7 Radio Emission Authors: To, Andy S. H.; Baker, Deborah; Long, David; James, Alexander; Brooks, David; van Driel-Gesztelyi, Lidia; Valori, Gherardo; Bastian, Tim; Lomuscio, Samantha; Stansby, David Bibcode: 2022cosp...44.2592T Altcode: Solar corona plasma composition, derived from full-Sun spectra, and the F10.7 radio flux (2.8 GHz) have been shown to be highly correlated (r = 0.88) during the recent weak solar cycle. However, this correlation becomes nonlinear at times of increased solar magnetic activity. We used co-temporal, high spatial resolution, radio (JVLA), and EUV (Hinode/EIS) images of the Sun taken on the 3 and 7 April 2020 to understand the underlying causes of the non-linearity of the FIP bias-F10.7 solar index correlation. We then calculated differential emission measures from AIA images, and paired them with the observed FIP bias to predict the bremsstrahlung component of F10.7 radio emission. Results of this study provide constraints on the amplitude of composition variability related to solar cycle amplitude, and provide an alternative method to calculate coronal composition. Title: What determines active region coronal plasma composition? Authors: Mihailescu, Teodora; Baker, Deborah; Long, David; Green, Lucie; Brooks, David; van Driel-Gesztelyi, Lidia; To, Andy S. H. Bibcode: 2022cosp...44.2580M Altcode: The chemical composition of the solar corona is different from that of the solar photosphere, with the strongest variation being observed in active regions. Using spectral data from the Extreme Ultraviolet (EUV) Imaging Spectrometer (EIS) on Hinode, we present a survey of coronal elemental composition as expressed in the FIP bias in 28 active regions with a wide range of ages and magnetic flux contents, and at different stages in their evolution. We find no correlation between the FIP bias of an active region and its magnetic flux or age. However, there is a dependence of the FIP bias on the evolutionary stage of the active region. FIP bias shows an increasing trend with average magnetic flux density up to 200 G but this trend does not continue at higher values. In contrast to the single values typically used to characterize the FIP bias in a region, we find that the FIP bias distribution within active regions has a significant spread. The highest spread is observed in very dispersed active regions and active regions that have formed a filament channel along their main polarity inversion lines, which is an indicator of the wide range of physical processes that take place in these active regions. These findings indicate that, while some general trends can be observed, the processes influencing the composition of an active region are complex and specific to its evolution, history and magnetic configuration or environment. The spread of FIP bias values in active regions shows a broad match with that previously observed in situ in the slow solar wind. Title: What have we learned about I-FIP Effect on the Sun from Hinode/EIS? Authors: Baker, Deborah; van Driel-Gesztelyi, Lidia Bibcode: 2022cosp...44.2572B Altcode: Plasma composition in stellar coronae can differ from that of their photospheres, the cause of which is one of the open questions in astrophysics. Elements with a low first ionization potential (FIP) are observed to have either enhanced or depleted abundances relative to that of high FIP elements. The abundance pattern is known as the FIP effect or inverse FIP (I-FIP) effect, depending on whether the low FIP elements are over-/under- (FIP/I-FIP) abundant in coronae. Some stellar coronae are dominated by FIP effect plasma but cooler, more active stars are dominated by I-FIP effect plasma. Our local laboratory, the Sun, has a FIP effect dominated corona, however, short-lived I-FIP patches have occasionally been observed. Analysis of multiple cases of I-FIP effect revealed certain conditions in the magnetic field and flare heating to be necessary for the occurrence of I-FIP effect plasma on the Sun. An overview of what we have learned from sixteen years of spatially resolved spectroscopic observations from Hinode/EIS will be presented. We will demonstrate the power of combining spectroscopic, imaging, and magnetic field observations of our Sun to understand the physical processes on cooler stars which we only observe as point sources. Title: Evolution of Plasma Composition in an Eruptive Flux Rope Authors: Baker, Deborah; Demoulin, Pascal; Long, David; Janvier, Miho; Green, Lucie; Brooks, David; van Driel-Gesztelyi, Lidia; Mihailescu, Teodora; To, Andy S. H.; Yardley, Stephanie; Valori, Gherardo Bibcode: 2022cosp...44.1361B Altcode: Magnetic flux ropes are bundles of twisted magnetic field enveloping a central axis. They harbor free magnetic energy and can be progenitors of coronal mass ejections (CMEs). However, identifying flux ropes on the Sun can be challenging. One of the key coronal observables that has been shown to indicate the presence of a flux rope is a peculiar bright coronal structure called a sigmoid. In this work, we show Hinode EUV Imaging Spectrometer observations of sigmoidal active region (AR) 10977. We analyze the coronal plasma composition in the AR and its evolution as a sigmoid (flux rope) forms and erupts as a CME. Plasma with photospheric composition was observed in coronal loops close to the main polarity inversion line during episodes of significant flux cancellation, suggestive of the injection of photospheric plasma into these loops driven by photospheric flux cancellation. Concurrently, the increasingly sheared core field contained plasma with coronal composition. As flux cancellation decreased and a sigmoid/flux rope formed, the plasma evolved to an intermediate composition in between photospheric and typical AR coronal compositions. Finally, the flux rope contained predominantly photospheric plasma during and after a failed eruption preceding the CME. Hence, plasma composition observations of AR 10977 strongly support models of flux rope formation by photospheric flux cancellation forcing magnetic reconnection first at the photospheric level then at the coronal level. Title: What Determines Active Region Coronal Plasma Composition? Authors: Mihailescu, Teodora; Baker, Deborah; Green, Lucie M.; van Driel-Gesztelyi, Lidia; Long, David M.; Brooks, David H.; To, Andy S. H. Bibcode: 2022ApJ...933..245M Altcode: 2022arXiv220505027M The chemical composition of the solar corona is different from that of the solar photosphere, with the strongest variation being observed in active regions (ARs). Using data from the Extreme Ultraviolet (EUV) Imaging Spectrometer (EIS) on Hinode, we present a survey of coronal elemental composition as expressed in the first ionization potential (FIP) bias in 28 ARs of different ages and magnetic flux content, which are at different stages in their evolution. We find no correlation between the FIP bias of an AR and its total unsigned magnetic flux or age. However, there is a weak dependence of FIP bias on the evolutionary stage, decreasing from 1.9 to 2.2 in ARs with spots to 1.5-1.6 in ARs that are at more advanced stages of the decay phase. FIP bias shows an increasing trend with average magnetic flux density up to 200 G, but this trend does not continue at higher values. The FIP bias distribution within ARs has a spread between 0.4 and 1. The largest spread is observed in very dispersed ARs. We attribute this to a range of physical processes taking place in these ARs, including processes associated with filament channel formation. These findings indicate that, while some general trends can be observed, the processes influencing the composition of an AR are complex and specific to its evolution, magnetic configuration, or environment. The spread of FIP bias values in ARs shows a broad match with that previously observed in situ in the slow solar wind. Title: The identification of magnetic perturbations in the solar atmosphere Authors: Stangalini, Marco; Jafarzadeh, Shahin; Baker, Deborah; Jess, David; Murabito, Mariarita; Valori, Gherardo Bibcode: 2022cosp...44.2590S Altcode: Magneto-hydrodynamic (MHD) waves and, in particular, magnetic perturbations associated with specific wave modes are thought to be important mechanisms not only for the heating of the outer layers of the Sun's atmosphere, but also for the elemental abundance anomaly observed in the corona. High resolution spectropolarimetry is nowadays progressively extending to the upper layers of the solar atmosphere, and this provides invaluable insight into MHD wave processes up to chromospheric heights. However, the identification of real magnetic perturbations remains a difficult task due to a number of spurious effects that can mimic the signals associated with them. In this contribution we will show a novel approach to the identification of real magnetic oscillations potentially linked to FIP and discuss proxies to be used in statistical analyses. Title: Detection of Stellar-like Abundance Anomalies in the Slow Solar Wind Authors: Brooks, David H.; Baker, Deborah; van Driel-Gesztelyi, Lidia; Warren, Harry P.; Yardley, Stephanie L. Bibcode: 2022ApJ...930L..10B Altcode: 2022arXiv220409332B The elemental composition of the Sun's hot atmosphere, the corona, shows a distinctive pattern that is different from the underlying surface or photosphere. Elements that are easy to ionize in the chromosphere are enhanced in abundance in the corona compared to their photospheric values. A similar pattern of behavior is often observed in the slow-speed (<500 km s-1) solar wind and in solar-like stellar coronae, while a reversed effect is seen in M dwarfs. Studies of the inverse effect have been hampered in the past because only unresolved (point-source) spectroscopic data were available for these stellar targets. Here we report the discovery of several inverse events observed in situ in the slow solar wind using particle-counting techniques. These very rare events all occur during periods of high solar activity that mimic conditions more widespread on M dwarfs. The detections allow a new way of connecting the slow wind to its solar source and are broadly consistent with theoretical models of abundance variations due to chromospheric fast-mode waves with amplitudes of 8-10 km s-1, sufficient to accelerate the solar wind. The results imply that M-dwarf winds are dominated by plasma depleted in easily ionized elements and lend credence to previous spectroscopic measurements. Title: Extending the FIP bias sample to magnetically active stars. Challenging the FIP bias paradigm Authors: Seli, B.; Oláh, K.; Kriskovics, L.; Kővári, Zs.; Vida, K.; Balázs, L. G.; Laming, J. M.; van Driel-Gesztelyi, L.; Baker, D. Bibcode: 2022A&A...659A...3S Altcode: 2021arXiv211114735S Context. The different elemental abundances of the photosphere and the corona are striking features of not only the Sun, but of other stars as well. This phenomenon is known as the first ionisation potential (FIP) effect, and its strength can be characterized by the FIP bias, the logarithmic abundance difference between low- and high-FIP elements in the corona, compared to the photosphere. The FIP bias was shown to depend on the surface temperature of the star.
Aims: We aim to extend the Teff−FIP bias relationship to a larger stellar sample and analyse the effect of other astrophysical parameters on the relation (e.g. surface gravity, age, activity indicators).
Methods: We compiled FIP bias and other parameters for 59 stars for which coronal composition is available, now including evolved stars. Using principal component analysis and linear discriminant analysis, we searched for correlations with other astrophysical parameters within the sample that may influence the stellar FIP bias.
Results: Adding stars to the Teff−FIP bias diagram unveiled new features in its structure. In addition to the previously known relationship, there appears to be a second branch: a parallel sequence about 0.5 dex above it. While the Teff remains the main determinant of the FIP bias, other parameters such as stellar activity indicators also have influence. We find three clusters in the FIP bias determinant parameter space. One distinct group is formed by the evolved stars. Two groups contain main sequence stars in continuation separated roughly by the sign change of the FIP-bias value.
Conclusions: The new branch of the Teff−FIP bias diagram contains stars with higher activity level, in terms of X-ray flux and rotational velocity. The Rossby number also seems to be important, indicating possible dependence on the type of dynamo operating in these stars influencing their FIP bias. The two main-sequence clusters run from the earliest spectral types of A-F with shallow convection zones through G-K-early-M stars with gradually deeper convection zones, and they end with the fully convective M dwarf stars, depicting the change of the dynamo type with the internal differences of the main sequence stars in connection with the FIP-bias values. Title: Localizing FRBs through VLBI with the Algonquin Radio Observatory 10 m Telescope Authors: Cassanelli, T.; Leung, Calvin; Rahman, M.; Vanderlinde, K.; Mena-Parra, J.; Cary, S.; Masui, Kiyoshi W.; Luo, Jing; Lin, H. -H.; Bij, A.; Gill, A.; Baker, D.; Bandura, Kevin; Berger, S.; Boyle, P. J.; Brar, Charanjot; Chatterjee, S.; Cubranic, D.; Dobbs, Matt; Fonseca, E.; Good, D. C.; Kaczmarek, J. F.; Kaspi, V. M.; Landecker, T. L.; Lanman, A. E.; Li, Dongzi; McKee, J. W.; Meyers, B. W.; Michilli, D.; Naidu, Arun; Ng, Cherry; Patel, Chitrang; Pearlman, Aaron B.; Pen, U. L.; Pleunis, Ziggy; Quine, Brendan; Renard, A.; Sanghavi, Pranav; Smith, K. M.; Stairs, Ingrid; Tendulkar, Shriharsh P. Bibcode: 2022AJ....163...65C Altcode: 2021arXiv210705659C The Canadian Hydrogen Intensity Mapping Experiment (CHIME)/FRB experiment has detected thousands of fast radio bursts (FRBs) due to its sensitivity and wide field of view; however, its low angular resolution prevents it from localizing events to their host galaxies. Very long baseline interferometry (VLBI), triggered by FRB detections from CHIME/FRB will solve the challenge of localization for non-repeating events. Using a refurbished 10 m radio dish at the Algonquin Radio Observatory located in Ontario Canada, we developed a testbed for a VLBI experiment with a theoretical λ/D ≲ 30 mas. We provide an overview of the 10 m system and describe its refurbishment, the data acquisition, and a procedure for fringe fitting that simultaneously estimates the geometric delay used for localization and the dispersive delay from the ionosphere. Using single pulses from the Crab pulsar, we validate the system and localization procedure, and analyze the clock stability between sites, which is critical for coherently delay referencing an FRB event. We find a localization of ~200 mas is possible with the performance of the current system (single-baseline). Furthermore, for sources with insufficient signal or restricted wideband to simultaneously measure both geometric and ionospheric delays, we show that the differential ionospheric contribution between the two sites must be measured to a precision of 1 × 10-8 pc cm-3 to provide a reasonable localization from a detection in the 400-800 MHz band. Finally we show detection of an FRB observed simultaneously in the CHIME and the Algonquin 10 m telescope, the first non-repeating FRB in this long baseline. This project serves as a testbed for the forthcoming CHIME/FRB Outriggers project. Title: A multi-planetary system orbiting the early-M dwarf TOI-1238 Authors: González-Álvarez, E.; Zapatero Osorio, M. R.; Sanz-Forcada, J.; Caballero, J. A.; Reffert, S.; Béjar, V. J. S.; Hatzes, A. P.; Herrero, E.; Jeffers, S. V.; Kemmer, J.; López-González, M. J.; Luque, R.; Molaverdikhani, K.; Morello, G.; Nagel, E.; Quirrenbach, A.; Rodríguez, E.; Rodríguez-López, C.; Schlecker, M.; Schweitzer, A.; Stock, S.; Passegger, V. M.; Trifonov, T.; Amado, P. J.; Baker, D.; Boyd, P. T.; Cadieux, C.; Charbonneau, D.; Collins, K. A.; Doyon, R.; Dreizler, S.; Espinoza, N.; Fűrész, G.; Furlan, E.; Hesse, K.; Howell, S. B.; Jenkins, J. M.; Kidwell, R. C.; Latham, D. W.; McLeod, K. K.; Montes, D.; Morales, J. C.; O'Dwyer, T.; Pallé, E.; Pedraz, S.; Reiners, A.; Ribas, I.; Quinn, S. N.; Schnaible, C.; Seager, S.; Skinner, B.; Smith, J. C.; Schwarz, R. P.; Shporer, A.; Vanderspek, R.; Winn, J. N. Bibcode: 2022A&A...658A.138G Altcode: 2021arXiv211114602G Context. The number of super-Earth and Earth-mass planet discoveries has increased significantly in the last two decades thanks to the Doppler radial velocity and planetary transit observing techniques. Either technique can detect planet candidates on its own, but the power of a combined photometric and spectroscopic analysis is unique for an insightful characterization of the planets, which in turn has repercussions for our understanding of the architecture of planetary systems and, therefore, their formation and evolution.
Aims: Two transiting planet candidates with super-Earth radii around the nearby (d = 70.64 ± 0.06 pc) K7-M0 dwarf star TOI-1238 were announced by NASA's Transiting Exoplanet Survey Satellite (TESS), which observed the field of TOI-1238 in four different sectors. We aim to validate their planetary nature using precise radial velocities taken with the CARMENES spectrograph.
Methods: We obtained 55 CARMENES radial velocity measurements that span the 11 months between 9 May 2020 and 5 April 2021. For a better characterization of the parent star's activity, we also collected contemporaneous optical photometric observations at the Joan Oró and Sierra Nevada observatories and retrieved archival photometry from the literature. We performed a combined TESS+CARMENES photometric and spectroscopic analysis by including Gaussian processes and Keplerian orbits to account for the stellar activity and planetary signals simultaneously.
Results: We estimate that TOI-1238 has a rotation period of 40 ± 5 d based on photometric and spectroscopic data. The combined analysis confirms the discovery of two transiting planets, TOI-1238 b and c, with orbital periods of 0.764597−0.000011+0.000013 d and 3.294736−0.000036+0.000034 d, masses of 3.76−1.07+1.15 M⊕ and 8.32−1.88+1.90 M⊕, and radii of 1.21−0.10+0.11 R⊕ and 2.11−0.14+0.14 R⊕. They orbit their parent star at semimajor axes of 0.0137 ± 0.0004 au and 0.036 ± 0.001 au, respectively.The two planets are placed on opposite sides of the radius valley for M dwarfs and lie between the star and the inner border of TOI-1238's habitable zone. The inner super-Earth TOI-1238 b is one of the densest ultra-short-period planets ever discovered (ρ = 11.7−3.4+4.2 g cm−3). The CARMENES data also reveal the presence of an outer, non-transiting, more massive companion with an orbital period and radial velocity amplitude of ≥600 d and ≥70 m s−1, which implies a likely mass of M ≥ 2 √(1− e2) MJup and a separation ≥1.1 au from its parent star. Title: Evolution of Plasma Composition in an Eruptive Flux Rope Authors: Baker, D.; Green, L. M.; Brooks, D. H.; Démoulin, P.; van Driel-Gesztelyi, L.; Mihailescu, T.; To, A. S. H.; Long, D. M.; Yardley, S. L.; Janvier, M.; Valori, G. Bibcode: 2022ApJ...924...17B Altcode: 2021arXiv211011714B Magnetic flux ropes are bundles of twisted magnetic field enveloping a central axis. They harbor free magnetic energy and can be progenitors of coronal mass ejections (CMEs). However, identifying flux ropes on the Sun can be challenging. One of the key coronal observables that has been shown to indicate the presence of a flux rope is a peculiar bright coronal structure called a sigmoid. In this work, we show Hinode EUV Imaging Spectrometer observations of sigmoidal active region (AR) 10977. We analyze the coronal plasma composition in the AR and its evolution as a sigmoid (flux rope) forms and erupts as a CME. Plasma with photospheric composition was observed in coronal loops close to the main polarity inversion line during episodes of significant flux cancellation, suggestive of the injection of photospheric plasma into these loops driven by photospheric flux cancellation. Concurrently, the increasingly sheared core field contained plasma with coronal composition. As flux cancellation decreased and a sigmoid/flux rope formed, the plasma evolved to an intermediate composition in between photospheric and typical AR coronal compositions. Finally, the flux rope contained predominantly photospheric plasma during and after a failed eruption preceding the CME. Hence, plasma composition observations of AR 10977 strongly support models of flux rope formation by photospheric flux cancellation forcing magnetic reconnection first at the photospheric level then at the coronal level. Title: Investigating the origin of magnetic perturbations associated with the FIP Effect Authors: Murabito, M.; Stangalini, M.; Baker, D.; Valori, G.; Jess, D. B.; Jafarzadeh, S.; Brooks, D. H.; Ermolli, I.; Giorgi, F.; Grant, S. D. T.; Long, D. M.; van Driel-Gesztelyi, L. Bibcode: 2021A&A...656A..87M Altcode: 2021arXiv210811164M Recently, magnetic oscillations were detected in the chromosphere of a large sunspot and found to be linked to the coronal locations where a first ionization potential (FIP) effect was observed. In an attempt to shed light on the possible excitation mechanisms of these localized waves, we further investigate the same data by focusing on the relation between the spatial distribution of the magnetic wave power and the overall field geometry and plasma parameters obtained from multi-height spectropolarimetric non-local thermodynamic equilibrium (NLTE) inversions of IBIS data. We find, in correspondence with the locations where the magnetic wave energy is observed at chromospheric heights, that the magnetic fields have smaller scale heights, meaning faster expansions of the field lines, which ultimately results in stronger vertical density stratification and wave steepening. In addition, the acoustic spectrum of the oscillations at the locations where magnetic perturbations are observed is broader than that observed at other locations, which suggests an additional forcing driver to the p-modes. Analysis of the photospheric oscillations in the sunspot surroundings also reveals a broader spectrum between the two opposite polarities of the active region (the leading spot and the trailing opposite polarity plage), and on the same side where magnetic perturbations are observed in the umbra. We suggest that strong photospheric perturbations between the two polarities are responsible for this broader spectrum of oscillations, with respect to the p-mode spectrum, resulting in locally excited acoustic waves that, after crossing the equipartition layer, located close to the umbra-penumbra boundary at photopheric heights, are converted into magnetic waves and steepen due to the strong density gradient.

Movie associated to Fig. 1 is available at https://www.aanda.org Title: The high-energy Sun - probing the origins of particle acceleration on our nearest star Authors: Matthews, S. A.; Reid, H. A. S.; Baker, D.; Bloomfield, D. S.; Browning, P. K.; Calcines, A.; Del Zanna, G.; Erdelyi, R.; Fletcher, L.; Hannah, I. G.; Jeffrey, N.; Klein, L.; Krucker, S.; Kontar, E.; Long, D. M.; MacKinnon, A.; Mann, G.; Mathioudakis, M.; Milligan, R.; Nakariakov, V. M.; Pesce-Rollins, M.; Shih, A. Y.; Smith, D.; Veronig, A.; Vilmer, N. Bibcode: 2021ExA...tmp..135M Altcode: As a frequent and energetic particle accelerator, our Sun provides us with an excellent astrophysical laboratory for understanding the fundamental process of particle acceleration. The exploitation of radiative diagnostics from electrons has shown that acceleration operates on sub-second time scales in a complex magnetic environment, where direct electric fields, wave turbulence, and shock waves all must contribute, although precise details are severely lacking. Ions were assumed to be accelerated in a similar manner to electrons, but γ-ray imaging confirmed that emission sources are spatially separated from X-ray sources, suggesting distinctly different acceleration mechanisms. Current X-ray and γ-ray spectroscopy provides only a basic understanding of accelerated particle spectra and the total energy budgets are therefore poorly constrained. Additionally, the recent detection of relativistic ion signatures lasting many hours, without an electron counterpart, is an enigma. We propose a single platform to directly measure the physical conditions present in the energy release sites and the environment in which the particles propagate and deposit their energy. To address this fundamental issue, we set out a suite of dedicated instruments that will probe both electrons and ions simultaneously to observe; high (seconds) temporal resolution photon spectra (4 keV - 150 MeV) with simultaneous imaging (1 keV - 30 MeV), polarization measurements (5-1000 keV) and high spatial and temporal resolution imaging spectroscopy in the UV/EUV/SXR (soft X-ray) regimes. These instruments will observe the broad range of radiative signatures produced in the solar atmosphere by accelerated particles. Title: TOI-1296b and TOI-1298b observed with TESS and SOPHIE: two hot Saturn-mass exoplanets with different densities around metal-rich stars Authors: Moutou, C.; Almenara, J. M.; Hébrard, G.; Santos, N. C.; Stassun, K. G.; Deheuvels, S.; Barros, S.; Benni, P.; Bieryla, A.; Boisse, I.; Bonfils, X.; Boyd, P. T.; Collins, K. A.; Baker, D.; Cortés-Zuleta, P.; Dalal, S.; Debras, F.; Deleuil, M.; Delfosse, X.; Demangeon, O.; Essack, Z.; Forveille, T.; Girardin, E.; Guerra, P.; Heidari, N.; Hesse, K.; Hoyer, S.; Jenkins, J. M.; Kiefer, F.; König, P. C.; Laloum, D.; Latham, D.; Lopez, T.; Martioli, E.; Osborn, H. P.; Ricker, G.; Seager, S.; Vanderspek, R.; Vezie, M.; Villaseñor, J.; Winn, J.; Wohler, B.; Ziegler, C. Bibcode: 2021A&A...653A.147M Altcode: 2021arXiv210909252M We present the discovery of two new transiting extrasolar planet candidates identified as TOI-1296.01 and TOI-1298.01 by the Transiting Exoplanet Survey Satellite (TESS). The planetary nature of these candidates has been secured with the SOPHIE high-precision spectrograph through the measurement of the companion's mass with the radial velocity method. Both planets are similar to Saturn in mass and have similar orbital periods of a few days. They, however, show discrepant radii and therefore different densities. The radius discrepancy might be explained by the different levels of irradiation by the host stars. The subgiant star TOI-1296 hosts a low-density planet with 1.2 RJup while the less luminous, lower-size star TOI-1298 hosts a much denser planet with a 0.84 RJup radius, resulting in bulk densities of 0.198 and 0.743 g cm−3, respectively.In addition, both stars are strongly enriched in heavy elements, having metallicities of +0.44 and +0.49 dex, respectively. The planet masses and orbital periods are 0.298 ± 0.039 MJup and 3.9443715 ± 5.8 ± 10−6 days for TOI-1296b, and 0.356 ± 0.032 MJup and 4.537164 ± 1.2 ± 10−5 days for TOI-1298b. The mass measurements have a relative precision of better than 13%.

Based on observations collected with the SOPHIE spectrograph on the 1.93 m telescope at the Observatoire de Haute-Provence (CNRS), France. Title: Sensitivity of solar wind mass flux to coronal temperature Authors: Stansby, D.; Berčič, L.; Matteini, L.; Owen, C. J.; French, R. J.; Baker, D.; Badman, S. T. Bibcode: 2021A&A...650L...2S Altcode: 2020arXiv200913918S Solar wind models predict that the mass flux carried away from the Sun in the solar wind should be extremely sensitive to the temperature in the corona, where the solar wind is accelerated. We perform a direct test of this prediction in coronal holes and active regions using a combination of in situ and remote sensing observations. For coronal holes, a 50% increase in temperature from 0.8 to 1.2 MK is associated with a tripling of the coronal mass flux. This trend is maintained within active regions at temperatures over 2 MK, with a four-fold increase in temperature corresponding to a 200-fold increase in coronal mass flux.

Code to reproduce the figures presented in this Letter is available at https://github.com/dstansby/publication-code. PSP and WIND data are available from https://spdf.gsfc.nasa.gov/pub/data, GONG data from https://gong2.nso.edu/oQR/zqs/, SDO and SOHO data from http://jsoc.stanford.edu/, and EIS data from http://solarb.mssl.ucl.ac.uk/SolarB/. Title: Widespread occurrence of high-velocity upflows in solar active regions Authors: Yardley, S. L.; Brooks, D. H.; Baker, D. Bibcode: 2021A&A...650L..10Y Altcode: 2021arXiv210601396Y
Aims: We performed a systematic study of 12 active regions (ARs) with a broad range of areas, magnetic fluxes, and associated solar activity in order to determine whether there are upflows present at the AR boundaries and, if these upflows exist, whether there is a high-speed asymmetric blue wing component present in them.
Methods: To identify the presence and locations of the AR upflows, we derive relative Doppler velocity maps by fitting a Gaussian function to Hinode/EIS Fe XII 192.394 Å line profiles. To determine whether there is a high-speed asymmetric component present in the AR upflows, we fit a double Gaussian function to the Fe XII 192.394 Å mean spectrum that is computed in a region of interest situated in the AR upflows.
Results: Upflows are observed at both the eastern and western boundaries of all ARs in our sample, with average upflow velocities ranging between −5 and −26 km s−1. A blue wing asymmetry is present in every line profile. The intensity ratio between the minor high-speed asymmetric Gaussian component compared to the main component is relatively small for the majority of regions; however, in a minority of cases (8/30) the ratios are large and range between 20 and 56 %.
Conclusions: These results suggest that upflows and the high-speed asymmetric blue wing component are a common feature of all ARs. Title: Plasma Upflows Induced by Magnetic Reconnection Above an Eruptive Flux Rope Authors: Baker, Deborah; Mihailescu, Teodora; Démoulin, Pascal; Green, Lucie M.; van Driel-Gesztelyi, Lidia; Valori, Gherardo; Brooks, David H.; Long, David M.; Janvier, Miho Bibcode: 2021SoPh..296..103B Altcode: 2021arXiv210616137B One of the major discoveries of Hinode's Extreme-ultraviolet Imaging Spectrometer (EIS) is the presence of upflows at the edges of active regions. As active regions are magnetically connected to the large-scale field of the corona, these upflows are a likely contributor to the global mass cycle in the corona. Here we examine the driving mechanism(s) of the very strong upflows with velocities in excess of 70 km s−1, known as blue-wing asymmetries, observed during the eruption of a flux rope in AR 10977 (eruptive flare SOL2007-12-07T04:50). We use Hinode/EIS spectroscopic observations combined with magnetic-field modeling to investigate the possible link between the magnetic topology of the active region and the strong upflows. A Potential Field Source Surface (PFSS) extrapolation of the large-scale field shows a quadrupolar configuration with a separator lying above the flux rope. Field lines formed by induced reconnection along the separator before and during the flux-rope eruption are spatially linked to the strongest blue-wing asymmetries in the upflow regions. The flows are driven by the pressure gradient created when the dense and hot arcade loops of the active region reconnect with the extended and tenuous loops overlying it. In view of the fact that separator reconnection is a specific form of the more general quasi-separatrix (QSL) reconnection, we conclude that the mechanism driving the strongest upflows is, in fact, the same as the one driving the persistent upflows of ≈10 - 20 km s−1 observed in all active regions. Title: The Evolution of Plasma Composition during a Solar Flare Authors: To, Andy S. H.; Long, David M.; Baker, Deborah; Brooks, David H.; van Driel-Gesztelyi, Lidia; Laming, J. Martin; Valori, Gherardo Bibcode: 2021ApJ...911...86T Altcode: 2021arXiv210209985T We analyze the coronal elemental abundances during a small flare using Hinode/EIS observations. Compared to the preflare elemental abundances, we observed a strong increase in coronal abundance of Ca XIV 193.84 Å, an emission line with low first ionization potential (FIP < 10 eV), as quantified by the ratio Ca/Ar during the flare. This is in contrast to the unchanged abundance ratio observed using Si X 258.38 Å/S X 264.23 Å. We propose two different mechanisms to explain the different composition results. First, the small flare-induced heating could have ionized S, but not the noble gas Ar, so that the flare-driven Alfvén waves brought up Si, S, and Ca in tandem via the ponderomotive force which acts on ions. Second, the location of the flare in strong magnetic fields between two sunspots may suggest fractionation occurred in the low chromosphere, where the background gas is neutral H. In this region, high-FIP S could behave more like a low-FIP than a high-FIP element. The physical interpretations proposed generate new insights into the evolution of plasma abundances in the solar atmosphere during flaring, and suggests that current models must be updated to reflect dynamic rather than just static scenarios. Title: Upflows in the Upper Solar Atmosphere Authors: Tian, Hui; Harra, Louise; Baker, Deborah; Brooks, David H.; Xia, Lidong Bibcode: 2021SoPh..296...47T Altcode: 2021arXiv210202429T Spectroscopic observations at extreme- and far-ultraviolet wavelengths have revealed systematic upflows in the solar transition region and corona. These upflows are best seen in the network structures of the quiet Sun and coronal holes, boundaries of active regions, and dimming regions associated with coronal mass ejections. They have been intensively studied in the past two decades because they are likely to be closely related to the formation of the solar wind and heating of the upper solar atmosphere. We present an overview of the characteristics of these upflows, introduce their possible formation mechanisms, and discuss their potential roles in the mass and energy transport in the solar atmosphere. Although past investigations have greatly improved our understanding of these upflows, they have left us with several outstanding questions and unresolved issues that should be addressed in the future. New observations from the Solar Orbiter mission, the Daniel K. Inouye Solar Telescope, and the Parker Solar Probe will likely provide critical information to advance our understanding of the generation, propagation, and energization of these upflows. Title: Detection of Transiting Exoplanet Candidates at Austin College's Adams Observatory: Ground-Based Support for NASA's TESS Mission Authors: Baker, D.; O'Dwyer, T.; Schnaible, C.; Skinner, B. Bibcode: 2021BAAS...53c1230B Altcode: NASA's Transiting Exoplanet Survey Satellite (TESS) monitors more than 200,000 stars in the search for transiting exoplanets. One of the primary goals of the TESS mission is to identify 50 planets smaller than four Earth radii with measured masses [1]. Because of the wide field of view and corresponding large pixel size of the TESS telescope, high precision ground-based observations are needed to confirm planetary transits and eliminate false positives [2]. The TESS Follow-up Observing Program Sub Group 1 (TFOP SG1) was developed to coordinate ground-based photometric follow-up observations [3].

The Adams Observatory at Austin College provides ground-based photometric support for the TESS project through TFOP SG1. Located on the roof of the IDEA Center science building, this facility houses the largest research telescope in north Texas and offers outstanding opportunities for research, education, and public outreach. In addition to TFOP, the Adams Observatory contributed to exoplanet transit observations as a member of the KELT Follow-Up Network [2]. The main telescope at the Adams Observatory is a 0.61-m f/8 DFM telescope of Ritchey-Chrétien design. When coupled with a Finger Lakes Instruments (FLI) Proline 16803 imager, this system produces a 26' × 26' field of view and a 0.38" pixel scale. Under optimal conditions, we can detect a minimum transit depth of ~3.0 ppt, which for an M-dwarf star would correspond to an exoplanet with radius ~3 Earth radii.

In summer 2020, we observed 11 stars identified by the TESS Science Team as potentially having exoplanets. Our high-precision follow-up observations offer three possible scenarios for these TESS targets: 1) a light curve from the target star indicating a possible transiting exoplanet, 2) a light curve from a nearby star indicating a nearby eclipsing binary (NEB) star system, and 3) flat light curves for both the target star and nearby stars. Of the 11 stars, four stars exhibit Case 1 behavior and have been verified as planetary candidates. An NEB has been detected near one target star (Case 2), and the star has been "retired" from TESS exoplanet studies. Six observations exhibit flat light curves (Case 3), which could indicate that either the planet is too small (and the corresponding dip in light too shallow) for detection at the Adams Observatory, or that the TESS observation is a false positive. These results may be useful for eliminating other possible causes of light curve variations in the search for small Earth-sized exoplanets.

[1] Ricker G. R. et al. (2015), JATIS 1(1), 014003.

[2] Collins K. A. et al. (2018), AJ 156:234.

[3] Collins K. (2019), AAS Meeting, 2019AAS...23314005C. Title: Spectropolarimetric fluctuations in a sunspot chromosphere Authors: Stangalini, M.; Baker, D.; Valori, G.; Jess, D. B.; Jafarzadeh, S.; Murabito, M.; To, A. S. H.; Brooks, D. H.; Ermolli, I.; Giorgi, F.; MacBride, C. D. Bibcode: 2021RSPTA.37900216S Altcode: 2020arXiv200905302S The instrumental advances made in this new era of 4 m class solar telescopes with unmatched spectropolarimetric accuracy and sensitivity will enable the study of chromospheric magnetic fields and their dynamics with unprecedented detail. In this regard, spectropolarimetric diagnostics can provide invaluable insight into magneto-hydrodynamic (MHD) wave processes. MHD waves and, in particular, Alfvénic fluctuations associated with particular wave modes were recently recognized as important mechanisms not only for the heating of the outer layers of the Sun's atmosphere and the acceleration of the solar wind, but also for the elemental abundance anomaly observed in the corona of the Sun and other Sun-like stars (also known as first ionization potential) effect. Here, we take advantage of state-of-the-art and unique spectropolarimetric Interferometric BIdimensional Spectrometer observations to investigate the relation between intensity and circular polarization (CP) fluctuations in a sunspot chromosphere. Our results show a clear link between the intensity and CP fluctuations in a patch which corresponds to a narrow range of magnetic field inclinations. This suggests the presence of Alfvénic perturbations in the sunspot.

This article is part of the Theo Murphy meeting issue `High-resolution wave dynamics in the lower solar atmosphere'. Title: Alfvénic Perturbations in a Sunspot Chromosphere Linked to Fractionated Plasma in the Corona Authors: Baker, Deborah; Stangalini, Marco; Valori, Gherardo; Brooks, David H.; To, Andy S. H.; van Driel-Gesztelyi, Lidia; Démoulin, Pascal; Stansby, David; Jess, David B.; Jafarzadeh, Shahin Bibcode: 2021ApJ...907...16B Altcode: 2020arXiv201204308B In this study, we investigate the spatial distribution of highly varying plasma composition around one of the largest sunspots of solar cycle 24. Observations of the photosphere, chromosphere, and corona are brought together with magnetic field modeling of the sunspot in order to probe the conditions that regulate the degree of plasma fractionation within loop populations of differing connectivities. We find that, in the coronal magnetic field above the sunspot umbra, the plasma has photospheric composition. Coronal loops rooted in the penumbra contain fractionated plasma, with the highest levels observed in the loops that connect within the active region. Tracing field lines from regions of fractionated plasma in the corona to locations of Alfvénic fluctuations detected in the chromosphere shows that they are magnetically linked. These results indicate a connection between sunspot chromospheric activity and observable changes in coronal plasma composition. Title: Opening pupils' eyes to the Sun Authors: French, Ryan; James, Alexander; Baker, Deborah; Dunn, William; Matthews, Sarah; da Silva Pestana, Brian; Graham, Grace; Shackell, Benjamin; Carretero, Adam Smith; Trindade, Granger Bibcode: 2020A&G....61.6.22F Altcode: Ryan French and colleagues discuss their Hinode/EIS outreach work and the resulting resources available for A-level classes Title: Sensitivity of Solar Wind Mass Flux to Coronal Electron Temperature Authors: Stansby, D.; Bercic, L.; Matteini, L.; Owen, C. J.; French, R.; Baker, D.; Badman, S. T. Bibcode: 2020AGUFMSH0290012S Altcode: Solar wind models predict that the mass flux carried away from the Sun in the solar wind should be extremely sensitive to the temperature in the corona. Using a range of in-situ and remote sensing measurements from Parker Solar Probe, the Solar Dynamics Observatory, and Hinode/EIS, we have tested this hypothesis by measuring the coronal electron temperature and coronal mass flux in both coronal holes and active region outflows.

We find that a three-fold increase in coronal temperature from 0.7 MK to 2.2 MK results in a large increase in coronal mass flux by over a factor of 100. This is in qualitative agreement with current solar wind acceleration models, and provides a new empirical constraint for future models to be tested against. Our work highlights how a wide range of remote and in-situ data sources can be combined to perform new tests of solar wind heating and acceleration theories. Title: Constraint of terrestrial model parameters from ensemble forward simulations Authors: Feng, S.; Lauvaux, T.; Williams, C. A.; Zhou, Y.; Baker, I. T.; Davis, K. J.; Barkley, Z.; Keller, K.; Baker, D.; Schuh, A. E.; Jacobson, A. R.; Liu, J.; Basu, S. Bibcode: 2020AGUFMA128...03F Altcode: Recent estimates of the North American carbon budget have shown a moderate convergence at annual and longer time scales between terrestrial biogeochemical models (BGCMs) and atmospheric inversions. However, multi-BGCM comparisons revealed large discrepancies both spatially and temporally among net ecosystem exchange estimates, illustrating our limited understanding of the underlying mechanisms. To bridge the gap between processes and atmospheric inversions, we propagated process-based errors in a BGCM, here an ensemble of CASA model simulations, into a mesoscale atmospheric system to identify and possibly optimize parameters instead of surface fluxes. Our offline atmospheric-ecosystem coupled model also represent uncertainties from the atmospheric transport in an ensemble-based framework. The unique collection of continental Planetary Boundary Layer measurements of CO2 mixing ratios and meteorological variables from the NASA Atmospheric Carbon and Transport-America (ACT-America) mission provides new perspectives on our understanding of transport and fluxes of greenhouse gases across three regions of the U.S., four seasons, and a variety of synoptic weather conditions. We have assembled a calibrated, continental-scale, 27-km resolution atmospheric model ensemble including biospheric and fossil fuel contributions, prescribing the large-scale inflow of CO2 from several global models. The ensemble system can separate and quantify the uncertainties in modeled CO2 mixing ratios from atmospheric transport, biospheric fluxes, fossil fuel emissions, and boundary inflows. Key parameters of CASA, driving ecosystem respiration and photosynthetic uptake, are constrained using both atmospheric mixing ratio measurements. We identified discrepancies between bottom-up and top-down approaches spatially using aircraft footprints from a backward Lagrangian particle model, to define optimal parameter values for dominant ecosystems across the US. Title: The Solar Orbiter Science Activity Plan. Translating solar and heliospheric physics questions into action Authors: Zouganelis, I.; De Groof, A.; Walsh, A. P.; Williams, D. R.; Müller, D.; St Cyr, O. C.; Auchère, F.; Berghmans, D.; Fludra, A.; Horbury, T. S.; Howard, R. A.; Krucker, S.; Maksimovic, M.; Owen, C. J.; Rodríguez-Pacheco, J.; Romoli, M.; Solanki, S. K.; Watson, C.; Sanchez, L.; Lefort, J.; Osuna, P.; Gilbert, H. R.; Nieves-Chinchilla, T.; Abbo, L.; Alexandrova, O.; Anastasiadis, A.; Andretta, V.; Antonucci, E.; Appourchaux, T.; Aran, A.; Arge, C. N.; Aulanier, G.; Baker, D.; Bale, S. D.; Battaglia, M.; Bellot Rubio, L.; Bemporad, A.; Berthomier, M.; Bocchialini, K.; Bonnin, X.; Brun, A. S.; Bruno, R.; Buchlin, E.; Büchner, J.; Bucik, R.; Carcaboso, F.; Carr, R.; Carrasco-Blázquez, I.; Cecconi, B.; Cernuda Cangas, I.; Chen, C. H. K.; Chitta, L. P.; Chust, T.; Dalmasse, K.; D'Amicis, R.; Da Deppo, V.; De Marco, R.; Dolei, S.; Dolla, L.; Dudok de Wit, T.; van Driel-Gesztelyi, L.; Eastwood, J. P.; Espinosa Lara, F.; Etesi, L.; Fedorov, A.; Félix-Redondo, F.; Fineschi, S.; Fleck, B.; Fontaine, D.; Fox, N. J.; Gandorfer, A.; Génot, V.; Georgoulis, M. K.; Gissot, S.; Giunta, A.; Gizon, L.; Gómez-Herrero, R.; Gontikakis, C.; Graham, G.; Green, L.; Grundy, T.; Haberreiter, M.; Harra, L. K.; Hassler, D. M.; Hirzberger, J.; Ho, G. C.; Hurford, G.; Innes, D.; Issautier, K.; James, A. W.; Janitzek, N.; Janvier, M.; Jeffrey, N.; Jenkins, J.; Khotyaintsev, Y.; Klein, K. -L.; Kontar, E. P.; Kontogiannis, I.; Krafft, C.; Krasnoselskikh, V.; Kretzschmar, M.; Labrosse, N.; Lagg, A.; Landini, F.; Lavraud, B.; Leon, I.; Lepri, S. T.; Lewis, G. R.; Liewer, P.; Linker, J.; Livi, S.; Long, D. M.; Louarn, P.; Malandraki, O.; Maloney, S.; Martinez-Pillet, V.; Martinovic, M.; Masson, A.; Matthews, S.; Matteini, L.; Meyer-Vernet, N.; Moraitis, K.; Morton, R. J.; Musset, S.; Nicolaou, G.; Nindos, A.; O'Brien, H.; Orozco Suarez, D.; Owens, M.; Pancrazzi, M.; Papaioannou, A.; Parenti, S.; Pariat, E.; Patsourakos, S.; Perrone, D.; Peter, H.; Pinto, R. F.; Plainaki, C.; Plettemeier, D.; Plunkett, S. P.; Raines, J. M.; Raouafi, N.; Reid, H.; Retino, A.; Rezeau, L.; Rochus, P.; Rodriguez, L.; Rodriguez-Garcia, L.; Roth, M.; Rouillard, A. P.; Sahraoui, F.; Sasso, C.; Schou, J.; Schühle, U.; Sorriso-Valvo, L.; Soucek, J.; Spadaro, D.; Stangalini, M.; Stansby, D.; Steller, M.; Strugarek, A.; Štverák, Š.; Susino, R.; Telloni, D.; Terasa, C.; Teriaca, L.; Toledo-Redondo, S.; del Toro Iniesta, J. C.; Tsiropoula, G.; Tsounis, A.; Tziotziou, K.; Valentini, F.; Vaivads, A.; Vecchio, A.; Velli, M.; Verbeeck, C.; Verdini, A.; Verscharen, D.; Vilmer, N.; Vourlidas, A.; Wicks, R.; Wimmer-Schweingruber, R. F.; Wiegelmann, T.; Young, P. R.; Zhukov, A. N. Bibcode: 2020A&A...642A...3Z Altcode: 2020arXiv200910772Z Solar Orbiter is the first space mission observing the solar plasma both in situ and remotely, from a close distance, in and out of the ecliptic. The ultimate goal is to understand how the Sun produces and controls the heliosphere, filling the Solar System and driving the planetary environments. With six remote-sensing and four in-situ instrument suites, the coordination and planning of the operations are essential to address the following four top-level science questions: (1) What drives the solar wind and where does the coronal magnetic field originate?; (2) How do solar transients drive heliospheric variability?; (3) How do solar eruptions produce energetic particle radiation that fills the heliosphere?; (4) How does the solar dynamo work and drive connections between the Sun and the heliosphere? Maximising the mission's science return requires considering the characteristics of each orbit, including the relative position of the spacecraft to Earth (affecting downlink rates), trajectory events (such as gravitational assist manoeuvres), and the phase of the solar activity cycle. Furthermore, since each orbit's science telemetry will be downloaded over the course of the following orbit, science operations must be planned at mission level, rather than at the level of individual orbits. It is important to explore the way in which those science questions are translated into an actual plan of observations that fits into the mission, thus ensuring that no opportunities are missed. First, the overarching goals are broken down into specific, answerable questions along with the required observations and the so-called Science Activity Plan (SAP) is developed to achieve this. The SAP groups objectives that require similar observations into Solar Orbiter Observing Plans, resulting in a strategic, top-level view of the optimal opportunities for science observations during the mission lifetime. This allows for all four mission goals to be addressed. In this paper, we introduce Solar Orbiter's SAP through a series of examples and the strategy being followed. Title: The Solar Orbiter EUI instrument: The Extreme Ultraviolet Imager Authors: Rochus, P.; Auchère, F.; Berghmans, D.; Harra, L.; Schmutz, W.; Schühle, U.; Addison, P.; Appourchaux, T.; Aznar Cuadrado, R.; Baker, D.; Barbay, J.; Bates, D.; BenMoussa, A.; Bergmann, M.; Beurthe, C.; Borgo, B.; Bonte, K.; Bouzit, M.; Bradley, L.; Büchel, V.; Buchlin, E.; Büchner, J.; Cabé, F.; Cadiergues, L.; Chaigneau, M.; Chares, B.; Choque Cortez, C.; Coker, P.; Condamin, M.; Coumar, S.; Curdt, W.; Cutler, J.; Davies, D.; Davison, G.; Defise, J. -M.; Del Zanna, G.; Delmotte, F.; Delouille, V.; Dolla, L.; Dumesnil, C.; Dürig, F.; Enge, R.; François, S.; Fourmond, J. -J.; Gillis, J. -M.; Giordanengo, B.; Gissot, S.; Green, L. M.; Guerreiro, N.; Guilbaud, A.; Gyo, M.; Haberreiter, M.; Hafiz, A.; Hailey, M.; Halain, J. -P.; Hansotte, J.; Hecquet, C.; Heerlein, K.; Hellin, M. -L.; Hemsley, S.; Hermans, A.; Hervier, V.; Hochedez, J. -F.; Houbrechts, Y.; Ihsan, K.; Jacques, L.; Jérôme, A.; Jones, J.; Kahle, M.; Kennedy, T.; Klaproth, M.; Kolleck, M.; Koller, S.; Kotsialos, E.; Kraaikamp, E.; Langer, P.; Lawrenson, A.; Le Clech', J. -C.; Lenaerts, C.; Liebecq, S.; Linder, D.; Long, D. M.; Mampaey, B.; Markiewicz-Innes, D.; Marquet, B.; Marsch, E.; Matthews, S.; Mazy, E.; Mazzoli, A.; Meining, S.; Meltchakov, E.; Mercier, R.; Meyer, S.; Monecke, M.; Monfort, F.; Morinaud, G.; Moron, F.; Mountney, L.; Müller, R.; Nicula, B.; Parenti, S.; Peter, H.; Pfiffner, D.; Philippon, A.; Phillips, I.; Plesseria, J. -Y.; Pylyser, E.; Rabecki, F.; Ravet-Krill, M. -F.; Rebellato, J.; Renotte, E.; Rodriguez, L.; Roose, S.; Rosin, J.; Rossi, L.; Roth, P.; Rouesnel, F.; Roulliay, M.; Rousseau, A.; Ruane, K.; Scanlan, J.; Schlatter, P.; Seaton, D. B.; Silliman, K.; Smit, S.; Smith, P. J.; Solanki, S. K.; Spescha, M.; Spencer, A.; Stegen, K.; Stockman, Y.; Szwec, N.; Tamiatto, C.; Tandy, J.; Teriaca, L.; Theobald, C.; Tychon, I.; van Driel-Gesztelyi, L.; Verbeeck, C.; Vial, J. -C.; Werner, S.; West, M. J.; Westwood, D.; Wiegelmann, T.; Willis, G.; Winter, B.; Zerr, A.; Zhang, X.; Zhukov, A. N. Bibcode: 2020A&A...642A...8R Altcode: Context. The Extreme Ultraviolet Imager (EUI) is part of the remote sensing instrument package of the ESA/NASA Solar Orbiter mission that will explore the inner heliosphere and observe the Sun from vantage points close to the Sun and out of the ecliptic. Solar Orbiter will advance the "connection science" between solar activity and the heliosphere.
Aims: With EUI we aim to improve our understanding of the structure and dynamics of the solar atmosphere, globally as well as at high resolution, and from high solar latitude perspectives.
Methods: The EUI consists of three telescopes, the Full Sun Imager and two High Resolution Imagers, which are optimised to image in Lyman-α and EUV (17.4 nm, 30.4 nm) to provide a coverage from chromosphere up to corona. The EUI is designed to cope with the strong constraints imposed by the Solar Orbiter mission characteristics. Limited telemetry availability is compensated by state-of-the-art image compression, onboard image processing, and event selection. The imposed power limitations and potentially harsh radiation environment necessitate the use of novel CMOS sensors. As the unobstructed field of view of the telescopes needs to protrude through the spacecraft's heat shield, the apertures have been kept as small as possible, without compromising optical performance. This led to a systematic effort to optimise the throughput of every optical element and the reduction of noise levels in the sensor.
Results: In this paper we review the design of the two elements of the EUI instrument: the Optical Bench System and the Common Electronic Box. Particular attention is also given to the onboard software, the intended operations, the ground software, and the foreseen data products.
Conclusions: The EUI will bring unique science opportunities thanks to its specific design, its viewpoint, and to the planned synergies with the other Solar Orbiter instruments. In particular, we highlight science opportunities brought by the out-of-ecliptic vantage point of the solar poles, the high-resolution imaging of the high chromosphere and corona, and the connection to the outer corona as observed by coronagraphs. Title: Directly comparing coronal and solar wind elemental fractionation Authors: Stansby, D.; Baker, D.; Brooks, D. H.; Owen, C. J. Bibcode: 2020A&A...640A..28S Altcode: 2020arXiv200500371S Context. As the solar wind propagates through the heliosphere, dynamical processes irreversibly erase the signatures of the near-Sun heating and acceleration processes. The elemental fractionation of the solar wind should not change during transit, however, making it an ideal tracer of these processes.
Aims: We aim to verify directly if the solar wind elemental fractionation is reflective of the coronal source region fractionation, both within and across different solar wind source regions.
Methods: A backmapping scheme was used to predict where solar wind measured by the Advanced Composition Explorer (ACE) originated in the corona. The coronal composition measured by the Hinode Extreme ultraviolet Imaging Spectrometer (EIS) at the source regions was then compared with the in situ solar wind composition.
Results: On hourly timescales, there is no apparent correlation between coronal and solar wind composition. In contrast, the distribution of fractionation values within individual source regions is similar in both the corona and solar wind, but distributions between different sources have a significant overlap.
Conclusions: The matching distributions directly verify that elemental composition is conserved as the plasma travels from the corona to the solar wind, further validating it as a tracer of heating and acceleration processes. The overlap of fractionation values between sources means it is not possible to identify solar wind source regions solely by comparing solar wind and coronal composition measurements, but a comparison can be used to verify consistency with predicted spacecraft-corona connections. Title: Directly Comparing Coronal and Solar Wind Elemental Fractionation Authors: Stansby, D.; Baker, D.; Owen, C.; Brooks, D. Bibcode: 2020SPD....5120801S Altcode: The elemental fractionation of the quasi-collisionless solar wind should not change during transit, making it an ideal tracer of coronal heating and acceleration processes. We aimed to verify directly if the solar wind elemental fractionation is reflective of the coronal source region fractionation, both within and across different solar wind source regions. A backmapping scheme was used to predict where solar wind measured by the Advanced Composition Explorer (ACE) across 15 days originated in the corona. The coronal composition measured by Hinode Extreme ultraviolet Imaging Spectrometer (EIS) at the source regions was then compared with the in-situ solar wind composition. On hourly timescales there was no apparent correlation between coronal and solar wind composition. In contrast, the distribution of fractionation values within individual source regions was similar in both the corona and solar wind, but distributions between different sources had significant overlap. The overlap of fractionation values between sources means it is not possible to identify solar wind source regions solely by comparing solar wind and coronal composition measurements, but a comparison can be used to verify consistency with predicted spacecraft-corona connections. Title: Jupiter's X-ray Emission During the 2007 Solar Minimum Authors: Dunn, W. R.; Branduardi-Raymont, G.; Carter-Cortez, V.; Campbell, A.; Elsner, R.; Ness, J. -U.; Gladstone, G. R.; Ford, P.; Yao, Z.; Rodriguez, P.; Clark, G.; Paranicas, C.; Foster, A.; Baker, D.; Gray, R.; Badman, S. V.; Ray, L. C.; Bunce, E. Â. J.; Snios, B.; Jackman, C. M.; Rae, I. J.; Kraft, R.; Rymer, A.; Lathia, S.; Achilleos, N. Bibcode: 2020JGRA..12527219D Altcode: The 2007-2009 solar minimum was the longest of the space age. We present the first of two companion papers on Chandra and XMM-Newton X-ray campaigns of Jupiter through February-March 2007. We find that low solar X-ray flux during solar minimum causes Jupiter's equatorial regions to be exceptionally X-ray dim (0.21 GW at minimum; 0.76 GW at maximum). While the Jovian equatorial emission varies with solar cycle, the aurorae have comparably bright intervals at solar minimum and maximum. We apply atomic charge exchange models to auroral spectra and find that iogenic plasma of sulphur and oxygen ions provides excellent fits for XMM-Newton observations. The fitted spectral S:O ratios of 0.4-1.3 are in good agreement with in situ magnetospheric S:O measurements of 0.3-1.5, suggesting that the ions that produce Jupiter's X-ray aurora predominantly originate inside the magnetosphere. The aurorae were particularly bright on 24-25 February and 8-9 March, but these two observations exhibit very different spatial, spectral, and temporal behavior; 24-25 February was the only observation in this campaign with significant hard X-ray bremsstrahlung from precipitating electrons, suggesting this may be rare. For 8-9 March, a bremsstrahlung component was absent, but bright oxygen O6+ lines and best-fit models containing carbon, point to contributions from solar wind ions. This contribution is absent in the other observations. Comparing simultaneous Chandra ACIS and XMM-Newton EPIC spectra showed that ACIS systematically underreported 0.45- to 0.6-keV Jovian emission, suggesting quenching may be less important for Jupiter's atmosphere than previously thought. We therefore recommend XMM-Newton for spectral analyses and quantifying opacity/quenching effects. Title: Can Subphotospheric Magnetic Reconnection Change the Elemental Composition in the Solar Corona? Authors: Baker, Deborah; van Driel-Gesztelyi, Lidia; Brooks, David H.; Démoulin, Pascal; Valori, Gherardo; Long, David M.; Laming, J. Martin; To, Andy S. H.; James, Alexander W. Bibcode: 2020ApJ...894...35B Altcode: 2020arXiv200303325B Within the coronae of stars, abundances of those elements with low first ionization potential (FIP) often differ from their photospheric values. The coronae of the Sun and solar-type stars mostly show enhancements of low-FIP elements (the FIP effect) while more active stars such as M dwarfs have coronae generally characterized by the inverse-FIP effect (I-FIP). Here we observe patches of I-FIP effect solar plasma in AR 12673, a highly complex βγδ active region. We argue that the umbrae of coalescing sunspots, and more specifically strong light bridges within the umbrae, are preferential locations for observing I-FIP effect plasma. Furthermore, the magnetic complexity of the active region and major episodes of fast flux emergence also lead to repetitive and intense flares. The induced evaporation of the chromospheric plasma in flare ribbons crossing umbrae enables the observation of four localized patches of I-FIP effect plasma in the corona of AR 12673. These observations can be interpreted in the context of the ponderomotive force fractionation model which predicts that plasma with I-FIP effect composition is created by the refraction of waves coming from below the chromosphere. We propose that the waves generating the I-FIP effect plasma in solar active regions are generated by subphotospheric reconnection of coalescing flux systems. Although we only glimpse signatures of I-FIP effect fractionation produced by this interaction in patches on the Sun, on highly active M stars it may be the dominant process. Title: Preparing for Geophysical Science Enabled by Crewed and Robotic Missions on the Surface of the Moon Authors: Schmerr, N.; Richardson, J.; Ghent, R.; Siegler, M.; Young, K.; Wasser, M.; Whelley, P.; Buczkowski, D.; Carter, L.; Connor, C.; Connor, L.; Bleacher, J.; Fouch, M.; Baker, D.; Hurford, T.; Jozwiak, L.; Kruse, S.; Lekic, V.; Naids, A.; Porter, R.; Montesi, L.; Richardson, D. C.; Rumpf, E.; Schorghofer, N.; Sunshine, J.; Goossens, S.; Whelley, N.; Wyrick, D.; Zhu, W.; Bell, E.; DeMartini, J.; Coan, D.; Akin, D.; Cohen, B.; Mazarico, E.; Neal, C.; Panning, M.; Petro, N.; Strauss, B.; Weber, R.; Glotch, T.; Hendrix, A.; Parker, A.; Wright, S. Bibcode: 2020LPICo2241.5048S Altcode: Geophysics on the Moon will be an important tool for identifying key targets for geological prospecting, scientific sampling, ISRU, assessing hazards and risks to crews and infrastructure, and determining the deep workings of the lunar interior. Title: Geophysical Exploration of the Dynamics and Evolution of the Solar System (GEODES) Authors: Schmerr, N.; Richardson, J.; Ghent, R.; Siegler, M.; Young, K.; Wasser, M.; Whelley, P.; Buczkowski, D.; Carter, L.; Connor, C.; Connor, L.; Bleacher, J.; Fouch, M.; Baker, D.; Hurford, T.; Jozwiak, L.; Kruse, S.; Lekic, V.; Naids, A.; Porter, R.; Montesi, L.; Richardson, D. C.; Rumpf, E.; Schorghofer, N.; Sunshine, J.; Goossens, S.; Whelley, N.; Wyrick, D.; Zhu, W.; Bell, E.; Coan, D.; Akin, D.; Cohen, B.; Mazarico, E.; Neal, C. R.; Panning, M.; Petro, N.; Strauss, B.; Weber, R.; Glotch, T.; Hendrix, A.; Parker, A.; Wright, S.; DeMartini, J. Bibcode: 2020LPI....51.1621S Altcode: GEODES is a SSERVI project that is exploring a suite of natural resources on the Moon, Mars, and asteroids through multidisciplinary geophysical investigations. Title: Photometric Observations of Possible Exoplanet Transits at Austin College's Adams Observatory: Ground-Based Support for NASA's TESS Mission Authors: Baker, D.; Hannon, N.; Martin, A.; Winterrowd, M. Bibcode: 2020LPICo2195.3059B Altcode: The Adams Observatory at Austin College provides ground-based photometric support for the Transiting Exoplanet Survey Satellite (TESS) Follow-up Observing Program (TFOP). Here we present a summary of our follow-up observations through November 2019. Title: Active Region Modulation of Coronal Hole Solar Wind Authors: Macneil, Allan R.; Owen, Christopher J.; Baker, Deborah; Brooks, David H.; Harra, Louise K.; Long, David M.; Wicks, Robert T. Bibcode: 2019ApJ...887..146M Altcode: Active regions (ARs) are a candidate source of the slow solar wind (SW), the origins of which are a topic of ongoing research. We present a case study that examines the processes by which SW is modulated in the presence of an AR in the vicinity of the SW source. We compare properties of SW associated with a coronal hole (CH)-quiet Sun boundary to SW associated with the same CH but one Carrington rotation later, when this region bordered the newly emerged NOAA AR 12532. Differences found in a range of in situ parameters are compared between these rotations in the context of source region mapping and remote sensing observations. Marked changes exist in the structure and composition of the SW, which we attribute to the influence of the AR on SW production from the CH boundary. These unique observations suggest that the features that emerge in the AR-associated wind are consistent with an increased occurrence of interchange reconnection during SW production, compared with the initial quiet Sun case. Title: Achievements of Hinode in the first eleven years Authors: Hinode Review Team; Al-Janabi, Khalid; Antolin, Patrick; Baker, Deborah; Bellot Rubio, Luis R.; Bradley, Louisa; Brooks, David H.; Centeno, Rebecca; Culhane, J. Leonard; Del Zanna, Giulio; Doschek, George A.; Fletcher, Lyndsay; Hara, Hirohisa; Harra, Louise K.; Hillier, Andrew S.; Imada, Shinsuke; Klimchuk, James A.; Mariska, John T.; Pereira, Tiago M. D.; Reeves, Katharine K.; Sakao, Taro; Sakurai, Takashi; Shimizu, Toshifumi; Shimojo, Masumi; Shiota, Daikou; Solanki, Sami K.; Sterling, Alphonse C.; Su, Yingna; Suematsu, Yoshinori; Tarbell, Theodore D.; Tiwari, Sanjiv K.; Toriumi, Shin; Ugarte-Urra, Ignacio; Warren, Harry P.; Watanabe, Tetsuya; Young, Peter R. Bibcode: 2019PASJ...71R...1H Altcode: Hinode is Japan's third solar mission following Hinotori (1981-1982) and Yohkoh (1991-2001): it was launched on 2006 September 22 and is in operation currently. Hinode carries three instruments: the Solar Optical Telescope, the X-Ray Telescope, and the EUV Imaging Spectrometer. These instruments were built under international collaboration with the National Aeronautics and Space Administration and the UK Science and Technology Facilities Council, and its operation has been contributed to by the European Space Agency and the Norwegian Space Center. After describing the satellite operations and giving a performance evaluation of the three instruments, reviews are presented on major scientific discoveries by Hinode in the first eleven years (one solar cycle long) of its operation. This review article concludes with future prospects for solar physics research based on the achievements of Hinode. Title: Comprehensive Determination of the Hinode/EIS Roll Angle Authors: Pelouze, Gabriel; Auchère, Frédéric; Bocchialini, Karine; Harra, Louise; Baker, Deborah; Warren, Harry P.; Brooks, David H.; Mariska, John T. Bibcode: 2019SoPh..294...59P Altcode: 2019arXiv190311923P We present a new coalignment method for the EUV Imaging Spectrometer (EIS) on board the Hinode spacecraft. In addition to the pointing offset and spacecraft jitter, this method determines the roll angle of the instrument, which has never been systematically measured, and which is therefore usually not corrected. The optimal pointing for EIS is computed by maximizing the cross-correlations of the Fe XII 195.119 Å line with images from the 193 Å band of the Atmospheric Imaging Assembly (AIA) on board the Solar Dynamics Observatory (SDO). By coaligning 3336 rasters with high signal-to-noise ratio, we estimate the rotation angle between EIS and AIA and explore the distribution of its values. We report an average value of (−0.387±0.007 ) ∘. We also provide a software implementation of this method that can be used to coalign any EIS raster. Title: Transient Inverse-FIP Plasma Composition Evolution within a Solar Flare Authors: Baker, Deborah; van Driel-Gesztelyi, Lidia; Brooks, David H.; Valori, Gherardo; James, Alexander W.; Laming, J. Martin; Long, David M.; Démoulin, Pascal; Green, Lucie M.; Matthews, Sarah A.; Oláh, Katalin; Kővári, Zsolt Bibcode: 2019ApJ...875...35B Altcode: 2019arXiv190206948B Understanding elemental abundance variations in the solar corona provides an insight into how matter and energy flow from the chromosphere into the heliosphere. Observed variations depend on the first ionization potential (FIP) of the main elements of the Sun’s atmosphere. High-FIP elements (>10 eV) maintain photospheric abundances in the corona, whereas low-FIP elements have enhanced abundances. Conversely, inverse FIP (IFIP) refers to the enhancement of high-FIP or depletion of low-FIP elements. We use spatially resolved spectroscopic observations, specifically the Ar XIV/Ca XIV intensity ratio, from Hinode’s Extreme-ultraviolet Imaging Spectrometer to investigate the distribution and evolution of plasma composition within two confined flares in a newly emerging, highly sheared active region. During the decay phase of the first flare, patches above the flare ribbons evolve from the FIP to the IFIP effect, while the flaring loop tops show a stronger FIP effect. The patch and loop compositions then evolve toward the preflare basal state. We propose an explanation of how flaring in strands of highly sheared emerging magnetic fields can lead to flare-modulated IFIP plasma composition over coalescing umbrae which are crossed by flare ribbons. Subsurface reconnection between the coalescing umbrae leads to the depletion of low-FIP elements as a result of an increased wave flux from below. This material is evaporated when the flare ribbons cross the umbrae. Our results are consistent with the ponderomotive fractionation model for the creation of IFIP-biased plasma. Title: Origins and Properties of Active Region Solar Wind Authors: Macneil, Allan; Owen, Christopher; Baker, Deborah; Harra, Louise; Long, David; Wicks, Robert Bibcode: 2019EGUGA..21.9712M Altcode: A primary goal of both the recently-launched Parker Solar Probe (PSP) and upcoming Solar Orbiter (SolO) missions is to identify and explain the origins of the solar wind. Recent studies have suggested that active regions (ARs) are the source of a significant fraction of the solar wind. Of particular interest is the AR contribution to the slow solar wind; the origins of which are still largely unknown. We present a case study of a rare opportunity to explain how the solar wind may emerge from, or be otherwise altered by, an AR, and also to identify the properties resulting from such a process. A simple backmapping procedure is applied to combine EUV remote sensing (SDO-AIA and Hinode-EIS) and in situ (ACE and WIND) observations of the corona and solar wind for two consecutive Carrington rotations. Contrasting observations during the latter rotation, when an AR is present at a trailing coronal hole (CH) boundary, to those during the former, when the AR is yet to emerge, allows us to isolate the influence of the AR on the solar wind from the CH boundary in a unique way. This observational strategy is particularly timely, as the combination of in situ and remote sensing observations, often from multiple spacecraft, will be critical to the identification of solar wind origins with PSP and SolO. With this methodology we find that, as a result of the presence of the AR, there is significant alteration of solar wind features such as velocity, composition, structure, and magnetic field orientation. The changes observed when the AR is present are consistent with the occurrence of interchange reconnection between AR and CH magnetic fields, which we argue is the likely mechanism by which the AR solar wind is produced. Title: Contribution of ULF Wave Activity to the Global Recovery of the Outer Radiation Belt During the Passage of a High-Speed Solar Wind Stream Observed in September 2014 Authors: Da Silva, L. A.; Sibeck, D.; Alves, L. R.; Souza, V. M.; Jauer, P. R.; Claudepierre, S. G.; Marchezi, J. P.; Agapitov, O.; Medeiros, C.; Vieira, L. E. A.; Wang, C.; Jiankui, S.; Liu, Z.; Gonzalez, W.; Dal Lago, A.; Rockenbach, M.; Padua, M. B.; Alves, M. V.; Barbosa, M. V. G.; Fok, M. -C.; Baker, D.; Kletzing, C.; Kanekal, S. G.; Georgiou, M. Bibcode: 2019JGRA..124.1660D Altcode: Energy coupling between the solar wind and the Earth's magnetosphere can affect the electron population in the outer radiation belt. However, the precise role of different internal and external mechanisms that leads to changes of the relativistic electron population is not entirely known. This paper describes how ultralow frequency (ULF) wave activity during the passage of Alfvénic solar wind streams contributes to the global recovery of the relativistic electron population in the outer radiation belt. To investigate the contribution of the ULF waves, we searched the Van Allen Probes data for a period in which we can clearly distinguish the enhancement of electron fluxes from the background. We found that the global recovery that started on 22 September 2014, which coincides with the corotating interaction region preceding a high-speed stream and the occurrence of persistent substorm activity, provides an excellent scenario to explore the contribution of ULF waves. To support our analyses, we employed ground- and space-based observational data and global magnetohydrodynamic simulations and calculated the ULF wave radial diffusion coefficients employing an empirical model. Observations show a gradual increase of electron fluxes in the outer radiation belt and a concomitant enhancement of ULF activity that spreads from higher to lower L-shells. Magnetohydrodynamic simulation results agree with observed ULF wave activity in the magnetotail, which leads to both fast and Alfvén modes in the magnetospheric nightside sector. The observations agree with the empirical model and are confirmed by phase space density calculations for this global recovery period. Title: Outer Van Allen Radiation Belt Response to Interacting Interplanetary Coronal Mass Ejections Authors: Kilpua, E. K. J.; Turner, D. L.; Jaynes, A. N.; Hietala, H.; Koskinen, H. E. J.; Osmane, A.; Palmroth, M.; Pulkkinen, T. I.; Vainio, R.; Baker, D.; Claudepierre, S. G. Bibcode: 2019JGRA..124.1927K Altcode: We study the response of the outer Van Allen radiation belt during an intense magnetic storm on 15-22 February 2014. Four interplanetary coronal mass ejections (ICMEs) arrived at Earth, of which the three last ones were interacting. Using data from the Van Allen Probes, we report the first detailed investigation of electron fluxes from source (tens of kiloelectron volts) to core (megaelectron volts) energies and possible loss and acceleration mechanisms as a response to substructures (shock, sheath and ejecta, and regions of shock-compressed ejecta) in multiple interacting ICMEs. After an initial enhancement induced by a shock compression of the magnetosphere, core fluxes strongly depleted and stayed low for 4 days. This sustained depletion can be related to a sequence of ICME substructures and their conditions that influenced the Earth's magnetosphere. In particular, the main depletions occurred during a high-dynamic pressure sheath and shock-compressed southward ejecta fields. These structures compressed/eroded the magnetopause close to geostationary orbit and induced intense and diverse wave activity in the inner magnetosphere (ULF Pc5, electromagnetic ion cyclotron, and hiss) facilitating both effective magnetopause shadowing and precipitation losses. Seed and source electrons in turn experienced stronger variations throughout the studied interval. The core fluxes recovered during the last ICME that made a glancing blow to Earth. This period was characterized by a concurrent lack of losses and sustained acceleration by chorus and Pc5 waves. Our study highlights that the seemingly complex behavior of the outer belt during interacting ICMEs can be understood by the knowledge of electron dynamics during different substructures. Title: Solar Cycle Observations of the Neon Abundance in the Sun-as-a-star Authors: Brooks, David H.; Baker, Deborah; van Driel-Gesztelyi, Lidia; Warren, Harry P. Bibcode: 2018ApJ...861...42B Altcode: 2018arXiv180507032B Properties of the Sun’s interior can be determined accurately from helioseismological measurements of solar oscillations. These measurements, however, are in conflict with photospheric elemental abundances derived using 3D hydrodynamic models of the solar atmosphere. This divergence of theory and helioseismology is known as the “solar modeling problem.” One possible solution is that the photospheric neon abundance, which is deduced indirectly by combining the coronal Ne/O ratio with the photospheric O abundance, is larger than generally accepted. There is some support for this idea from observations of cool stars. The Ne/O abundance ratio has also been found to vary with the solar cycle in the slowest solar wind streams and coronal streamers, and the variation from solar maximum to minimum in streamers (∼0.1-0.25) is large enough to potentially bring some of the solar models into agreement with the seismic data. Here we use daily sampled observations from the EUV Variability Experiment on the Solar Dynamics Observatory taken in 2010-2014, to investigate whether the coronal Ne/O abundance ratio shows a variation with the solar cycle when the Sun is viewed as a star. We find only a weak dependence on, and moderate anti-correlation with, the solar cycle with the ratio measured around 0.2-0.3 MK falling from 0.17 at solar minimum to 0.11 at solar maximum. The effect is amplified at higher temperatures (0.3-0.6 MK) with a stronger anti-correlation and the ratio falling from 0.16 at solar minimum to 0.08 at solar maximum. The values we find at solar minimum are too low to solve the solar modeling problem. Title: Coronal Elemental Abundances in Solar Emerging Flux Regions Authors: Baker, Deborah; Brooks, David H.; van Driel-Gesztelyi, Lidia; James, Alexander W.; Démoulin, Pascal; Long, David M.; Warren, Harry P.; Williams, David R. Bibcode: 2018ApJ...856...71B Altcode: 2018arXiv180108424B The chemical composition of solar and stellar atmospheres differs from the composition of their photospheres. Abundances of elements with low first ionization potential (FIP) are enhanced in the corona relative to high-FIP elements with respect to the photosphere. This is known as the FIP effect and it is important for understanding the flow of mass and energy through solar and stellar atmospheres. We used spectroscopic observations from the Extreme-ultraviolet Imaging Spectrometer on board the Hinode observatory to investigate the spatial distribution and temporal evolution of coronal plasma composition within solar emerging flux regions inside a coronal hole. Plasma evolved to values exceeding those of the quiet-Sun corona during the emergence/early-decay phase at a similar rate for two orders of magnitude in magnetic flux, a rate comparable to that observed in large active regions (ARs) containing an order of magnitude more flux. During the late-decay phase, the rate of change was significantly faster than what is observed in large, decaying ARs. Our results suggest that the rate of increase during the emergence/early-decay phase is linked to the fractionation mechanism that leads to the FIP effect, whereas the rate of decrease during the later decay phase depends on the rate of reconnection with the surrounding magnetic field and its plasma composition. Title: A Solar cycle correlation of coronal element abundances in Sun-as-a-star observations Authors: Brooks, David H.; Baker, Deborah; van Driel-Gesztelyi, Lidia; Warren, Harry P. Bibcode: 2017NatCo...8..183B Altcode: 2018arXiv180200563B The elemental composition in the coronae of low-activity solar-like stars appears to be related to fundamental stellar properties such as rotation, surface gravity, and spectral type. Here we use full-Sun observations from the Solar Dynamics Observatory, to show that when the Sun is observed as a star, the variation of coronal composition is highly correlated with a proxy for solar activity, the F10.7 cm radio flux, and therefore with the solar cycle phase. Similar cyclic variations should therefore be detectable spectroscopically in X-ray observations of solar analogs. The plasma composition in full-disk observations of the Sun is related to the evolution of coronal magnetic field activity. Our observations therefore introduce an uncertainty into the nature of any relationship between coronal composition and fixed stellar properties. The results highlight the importance of systematic full-cycle observations for understanding the elemental composition of solar-like stellar coronae. Title: A study of the long term evolution in active region upflows Authors: Harra, Louise K.; Ugarte-Urra, Ignacio; De Rosa, Marc; Mandrini, Cristina; van Driel-Gesztelyi, Lidia; Baker, Deborah; Culhane, J. Leonard; Démoulin, Pascal Bibcode: 2017PASJ...69...47H Altcode: Since their discovery, upflows at the edges of active regions have attracted a lot of interest, primarily as they could potentially contribute to the slow solar wind. One aspect that has not been studied yet is how the long term evolution of active regions impacts the upflows. In this work, we analyze one active region that survives three solar rotations. We track how the flows change with time. We use local and global modeling of the decaying active region to determine how the age of the active region will impact the extent of the open magnetic fields, and then how some of the upflows could become outflows. We finish with a discussion of how these results, set in a broader context, can be further developed with the Solar Orbiter mission. Title: On-Disc Observations of Flux Rope Formation Prior to Its Eruption Authors: James, A. W.; Green, L. M.; Palmerio, E.; Valori, G.; Reid, H. A. S.; Baker, D.; Brooks, D. H.; van Driel-Gesztelyi, L.; Kilpua, E. K. J. Bibcode: 2017SoPh..292...71J Altcode: 2017arXiv170310837J Coronal mass ejections (CMEs) are one of the primary manifestations of solar activity and can drive severe space weather effects. Therefore, it is vital to work towards being able to predict their occurrence. However, many aspects of CME formation and eruption remain unclear, including whether magnetic flux ropes are present before the onset of eruption and the key mechanisms that cause CMEs to occur. In this work, the pre-eruptive coronal configuration of an active region that produced an interplanetary CME with a clear magnetic flux rope structure at 1 AU is studied. A forward-S sigmoid appears in extreme-ultraviolet (EUV) data two hours before the onset of the eruption (SOL2012-06-14), which is interpreted as a signature of a right-handed flux rope that formed prior to the eruption. Flare ribbons and EUV dimmings are used to infer the locations of the flux rope footpoints. These locations, together with observations of the global magnetic flux distribution, indicate that an interaction between newly emerged magnetic flux and pre-existing sunspot field in the days prior to the eruption may have enabled the coronal flux rope to form via tether-cutting-like reconnection. Composition analysis suggests that the flux rope had a coronal plasma composition, supporting our interpretation that the flux rope formed via magnetic reconnection in the corona. Once formed, the flux rope remained stable for two hours before erupting as a CME. Title: Apparent and Intrinsic Evolution of Active Region Upflows Authors: Baker, Deborah; Janvier, Miho; Démoulin, Pascal; Mandrini, Cristina H. Bibcode: 2017SoPh..292...46B Altcode: 2017arXiv170206022B We analyze the evolution of Fe XII coronal plasma upflows from the edges of ten active regions (ARs) as they cross the solar disk using the Hinode Extreme Ultraviolet Imaging Spectrometer (EIS) to do this. Confirming the results of Démoulin et al. (Sol. Phys.283, 341, 2013), we find that for each AR there is an observed long-term evolution of the upflows. This evolution is largely due to the solar rotation that progressively changes the viewpoint of dominantly stationary upflows. From this projection effect, we estimate the unprojected upflow velocity and its inclination to the local vertical. AR upflows typically fan away from the AR core by 40° to nearly vertical for the following polarity. The span of inclination angles is more spread out for the leading polarity, with flows angled from −29° (inclined toward the AR center) to 28° (directed away from the AR). In addition to the limb-to-limb apparent evolution, we identify an intrinsic evolution of the upflows that is due to coronal activity, which is AR dependent. Furthermore, line widths are correlated with Doppler velocities only for the few ARs with the highest velocities. We conclude that for the line widths to be affected by the solar rotation, the spatial gradient of the upflow velocities must be large enough such that the line broadening exceeds the thermal line width of Fe XII. Finally, we find that upflows occurring in pairs or multiple pairs are a common feature of ARs observed by Hinode/EIS, with up to four pairs present in AR 11575. This is important for constraining the upflow-driving mechanism as it implies that the mechanism is not local and does not occur over a single polarity. AR upflows originating from reconnection along quasi-separatrix layers between overpressure AR loops and neighboring underpressure loops is consistent with upflows occurring in pairs, unlike other proposed mechanisms that act locally in one polarity. Title: MMS Super-Conjunction Studies of Chorus Wave Properties and Their Effects on Energetic Electrons Authors: Jaynes, A. N.; Baker, D.; Blake, J. B.; Kletzing, C.; Zhao, H.; Leonard, T. W.; Turner, D. L.; Fennell, J. F.; Wilder, F. D.; Kanekal, S. G.; Schiller, Q.; Mauk, B.; Cohen, I. Bibcode: 2016AGUFMSM43E..07J Altcode: During the first full sweep of NASA's MMS mission through the Earth's magnetotail, referred to as Phase 1x, the active state of the geomagnetic environment allowed many opportunities for new insights into inner magnetospheric dynamics. Of particular interest is the local generation of whistler-mode chorus waves and their subsequent effect on energetic electrons. In this study, we take advantage of conjunctions between MMS and the rest of the Heliospheric System Observatory satellites, including one super-conjunction event on 01 May 2016, when both Van Allen Probes and MMS were all within 1 Re of each other at the same time. Using multipoint measurements, we examine the properties and effects of chorus in fine detail. This concentration of observation points in the chorus generation region unveils new understanding of the wave-particle interactions that accelerate electrons and form the Earth's radiation belts. Title: Evolution of the magnetic field distribution of active regions Authors: Dacie, S.; Démoulin, P.; van Driel-Gesztelyi, L.; Long, D. M.; Baker, D.; Janvier, M.; Yardley, S. L.; Pérez-Suárez, D. Bibcode: 2016A&A...596A..69D Altcode: 2016arXiv160903723D
Aims: Although the temporal evolution of active regions (ARs) is relatively well understood, the processes involved continue to be the subject of investigation. We study how the magnetic field of a series of ARs evolves with time to better characterise how ARs emerge and disperse.
Methods: We examined the temporal variation in the magnetic field distribution of 37 emerging ARs. A kernel density estimation plot of the field distribution was created on a log-log scale for each AR at each time step. We found that the central portion of the distribution is typically linear, and its slope was used to characterise the evolution of the magnetic field.
Results: The slopes were seen to evolve with time, becoming less steep as the fragmented emerging flux coalesces. The slopes reached a maximum value of -1.5 just before the time of maximum flux before becoming steeper during the decay phase towards the quiet-Sun value of -3. This behaviour differs significantly from a classical diffusion model, which produces a slope of -1. These results suggest that simple classical diffusion is not responsible for the observed changes in field distribution, but that other processes play a significant role in flux dispersion.
Conclusions: We propose that the steep negative slope seen during the late-decay phase is due to magnetic flux reprocessing by (super)granular convective cells. Title: Current energetic particle sensors Authors: Fennell, J. F.; Blake, J. B.; Claudepierre, S.; Mazur, J.; Kanekal, S.; O'Brien, P.; Baker, D.; Crain, W.; Mabry, D.; Clemmons, J. Bibcode: 2016JGRA..121.8840F Altcode: Several energetic particle sensors designed to make measurements in the current decade are described and their technology and capabilities discussed and demonstrated. Most of these instruments are already on orbit or approaching launch. These include the Magnetic Electron Ion Spectrometers (MagEIS) and the Relativistic Electron Proton Telescope (REPT) that are flying on the Van Allen Probes, the Fly's Eye Electron Proton Spectrometers (FEEPS) flying on the Magnetospheric Multiscale (MMS) mission, and Dosimeters flying on the AC6 Cubesat mission. We focus mostly on the electron measurement capability of these sensors while providing summary comments of their ion measurement capabilities if they have any. Title: Photospheric Vector Magnetic Field Evolution of NOAA Active Region 11504 and the Ensuing CME Authors: James, Alexander; Green, Lucie; Valori, Gherardo; van Driel-Gesztelyi, Lidia; Baker, Deborah; Brooks, David; Palmerio, Erika Bibcode: 2016SPD....4730305J Altcode: Coronal mass ejections (CMEs) are eruptions of billions of tonnes of plasma from the Sun that drive the most severe space weather effects we observe. In order to be able to produce forecasts of space weather with lead times of the order of days, accurate predictions of the occurrence of CMEs must be developed. The eruptive active-region studied in this work (NOAA 11504) is complex, featuring fragmentation of penumbral magnetic field in the days prior to eruption, as well as rotation of the leading sunspot. SDO/HMI vector photospheric magnetic field measurements are utilised alongside SDO/AIA multi-wavelength extreme ultra-violet (EUV) observations to study the dynamics of the photospheric and coronal structures, as well as Hinode/EIS spectroscopic measurements, including elemental composition data. The EUV data show flare ribbons as well as coronal dimmings, which are used to infer the orientation of the erupting flux rope. This flux rope orientation is then compared to in situ measurements of the flux rope. The vector magnetic field data is used to determine the possible contributions the field fragmentation and sunspot rotation may have made to the formation of the flux rope and the triggering of the CME. Title: Preface: Probing the Sun Inside and Out Authors: Harra, Louise; Baker, Deborah; Howe, Rachel; Leibacher, John; van Driel-Gesztelyi, Lidia Bibcode: 2015SoPh..290.3091H Altcode: 2015SoPh..tmp..167H No abstract at ADS Title: Persistent Near-Surface Flow Structures from Local Helioseismology Authors: Howe, Rachel; Komm, R. W.; Baker, D.; Harra, L.; van Driel-Gesztelyi, L.; Bogart, R. S. Bibcode: 2015SoPh..290.3137H Altcode: 2015arXiv150706525H; 2015SoPh..tmp..115H Near-surface flows measured by the ring-diagram technique of local helioseismology show structures that persist over multiple rotations. We examine these phenomena using data from the Global Oscillation Network Group (GONG) and the Helioseismic and Magnetic Imager (HMI) and show that a correlation analysis of the structures can be used to estimate the rotation rate as a function of latitude, giving a result consistent with the near-surface rate from global helioseismology and slightly slower than that obtained from a similar analysis of the surface magnetic field strength. At latitudes of 60∘ and above, the HMI flow data reveal a strong signature of a two-sided zonal flow structure. This signature may be related to recent reports of "giant cells" in solar convection. Title: A Study of the Coronal Non-thermal Velocity in Polar Regions During the Rise from Solar Minimum to Solar Maximum in Cycle 24 Authors: Harra, L.; Baker, D.; Edwards, S. J.; Hara, H.; Howe, R.; van Driel-Gesztelyi, L. Bibcode: 2015SoPh..290.3203H Altcode: 2015SoPh..tmp....8H We explore the changes in coronal non-thermal velocity (Vnt) measurements at the poles from solar minimum to solar maximum using Hinode EUV Imaging Spectrometer data. We find that although the intensity in the corona at the poles does tend to increase with the cycle, there are no significant changes in the Vnt values. The locations of enhanced Vnt values measured do not always have a counterpart in intensity, and they are sometimes located in weak emission regions. Unipolar magnetic streams, created through diffusion of the following polarity of the decaying active regions, slowly progress towards the poles. These streams are expected to be related to magnetic nulls as locations that indicate an increased likelihood for magnetic reconnection to occur. Through global potential field source-surface modelling, we determine how the number of nulls varied during the cycle and find that those that lie at < 1.1 solar radii vary significantly. We search for a correlation between the variation of the magnetic nulls and the Vnt values, as it may be expected that with an increasing number of nulls, the Vnt values in the corona increase as well. There is no correlation with the Vnt values, however. This indicates that the magnetic structures that create the enhanced Vnt behaviour are small-scale features and hence not easily measurable at the poles. Because they do not change during the solar cycle, they are likely to be created by a local dynamo. The variation of the upper range of Vnt is reduced, which highlights that strongly dynamic behaviour is reduced as the solar maximum approaches. This is likely to be due to the reduced area of the polar coronal hole, which allows fewer opportunities for reconnection to occur between open and closed magnetic fields. Title: Source of a Prominent Poleward Surge During Solar Cycle 24 Authors: Yeates, A. R.; Baker, D.; van Driel-Gesztelyi, L. Bibcode: 2015SoPh..290.3189Y Altcode: 2015SoPh..tmp...18Y; 2015arXiv150204854Y As an observational case study, we consider the origin of a prominent poleward surge of leading polarity, visible in the magnetic butterfly diagram during Solar Cycle 24. A new technique is developed for assimilating individual regions of strong magnetic flux into a surface-flux transport model. By isolating the contribution of each of these regions, the model shows the surge to originate primarily in a single high-latitude activity group consisting of a bipolar active region present in Carrington Rotations 2104 - 05 (November 2010 - January 2011) and a multipolar active region in Rotations 2107 - 08 (February - April 2011). This group had a strong axial dipole moment opposed to Joy's law. On the other hand, the modelling suggests that the transient influence of this group on the butterfly diagram will not be matched by a large long-term contribution to the polar field because it is located at high latitude. This is in accordance with previous flux-transport models. Title: Parallel Evolution of Quasi-separatrix Layers and Active Region Upflows Authors: Mandrini, C. H.; Baker, D.; Démoulin, P.; Cristiani, G. D.; van Driel-Gesztelyi, L.; Vargas Domínguez, S.; Nuevo, F. A.; Vásquez, A. M.; Pick, M. Bibcode: 2015ApJ...809...73M Altcode: 2015arXiv150701264M Persistent plasma upflows were observed with Hinode’s EUV Imaging Spectrometer (EIS) at the edges of active region (AR) 10978 as it crossed the solar disk. We analyze the evolution of the photospheric magnetic and velocity fields of the AR, model its coronal magnetic field, and compute the location of magnetic null-points and quasi-sepratrix layers (QSLs) searching for the origin of EIS upflows. Magnetic reconnection at the computed null points cannot explain all of the observed EIS upflow regions. However, EIS upflows and QSLs are found to evolve in parallel, both temporarily and spatially. Sections of two sets of QSLs, called outer and inner, are found associated to EIS upflow streams having different characteristics. The reconnection process in the outer QSLs is forced by a large-scale photospheric flow pattern, which is present in the AR for several days. We propose a scenario in which upflows are observed, provided that a large enough asymmetry in plasma pressure exists between the pre-reconnection loops and lasts as long as a photospheric forcing is at work. A similar mechanism operates in the inner QSLs; in this case, it is forced by the emergence and evolution of the bipoles between the two main AR polarities. Our findings provide strong support for the results from previous individual case studies investigating the role of magnetic reconnection at QSLs as the origin of the upflowing plasma. Furthermore, we propose that persistent reconnection along QSLs does not only drive the EIS upflows, but is also responsible for the continuous metric radio noise-storm observed in AR 10978 along its disk transit by the Nançay Radio Heliograph. Title: 49 new T dwarfs identified using methane imaging Authors: Cardoso, C. V.; Burningham, B.; Smart, R. L.; van Spaandonk, L.; Baker, D.; Smith, L. C.; Zhang, Z. H.; Andrei, A. H.; Bucciarelli, B.; Dhital, S.; Jones, H. R. A.; Lattanzi, M. G.; Magazzú, A.; Pinfield, D. J.; Tinney, C. G. Bibcode: 2015MNRAS.450.2486C Altcode: 2015arXiv150206503C We present the discovery of 49 new photometrically classified T dwarfs from the combination of large infrared and optical surveys combined with follow-up Telescopio Nazionale Galileo photometry. We used multiband infrared and optical photometry from the United Kingdom Infrared Telescope and Sloan Digital Sky Surveys to identify possible brown dwarf candidates, which were then confirmed using methane filter photometry. We have defined a new photometric conversion between CH4s - CH4l colour and spectral type for T4-T8 brown dwarfs based on a part of the sample that has been followed up using methane photometry and spectroscopy. Using methane differential photometry as a proxy for spectral type for T dwarfs has proved to be a very efficient technique. Of a subset of 45 methane selected brown dwarfs that were observed spectroscopically, 100 per cent were confirmed as T dwarfs. Future deep imaging surveys will produce large samples of faint brown dwarf candidates, for which spectroscopy will not be feasible. When broad wavelength coverage is unavailable, methane imaging offers a means to efficiently classify candidates from such surveys using just a pair of near-infrared images. Title: FIP Bias Evolution in a Decaying Active Region Authors: Baker, D.; Brooks, D. H.; Démoulin, P.; Yardley, S. L.; van Driel-Gesztelyi, L.; Long, D. M.; Green, L. M. Bibcode: 2015ApJ...802..104B Altcode: 2015arXiv150107397B Solar coronal plasma composition is typically characterized by first ionization potential (FIP) bias. Using spectra obtained by Hinode’s EUV Imaging Spectrometer instrument, we present a series of large-scale, spatially resolved composition maps of active region (AR)11389. The composition maps show how FIP bias evolves within the decaying AR during the period 2012 January 4-6. Globally, FIP bias decreases throughout the AR. We analyzed areas of significant plasma composition changes within the decaying AR and found that small-scale evolution in the photospheric magnetic field is closely linked to the FIP bias evolution observed in the corona. During the AR’s decay phase, small bipoles emerging within supergranular cells reconnect with the pre-existing AR field, creating a pathway along which photospheric and coronal plasmas can mix. The mixing timescales are shorter than those of plasma enrichment processes. Eruptive activity also results in shifting the FIP bias closer to photospheric in the affected areas. Finally, the FIP bias still remains dominantly coronal only in a part of the AR’s high-flux density core. We conclude that in the decay phase of an AR’s lifetime, the FIP bias is becoming increasingly modulated by episodes of small-scale flux emergence, i.e., decreasing the AR’s overall FIP bias. Our results show that magnetic field evolution plays an important role in compositional changes during AR development, revealing a more complex relationship than expected from previous well-known Skylab results showing that FIP bias increases almost linearly with age in young ARs. Title: The energetics of a global shock wave in the low solar corona Authors: Long, David; Baker, Deborah; Williams, David; Carley, Eoin; Gallagher, Peter; Zucca, Pietro Bibcode: 2015TESS....140706L Altcode: As the most energetic eruptions in the solar system, coronal mass ejections (CMEs) can produce shock waves at both their front and flanks as they erupt from the Sun into the heliosphere. However, the amount of energy produced in these eruptions, and the proportion of their energy required to produce the waves, is not well characterised. Here we use observations of a solar eruption from 2014 February 25 to estimate the energy budget of an erupting CME and the globally-propagating "EIT wave" produced by the rapid expansion of the CME flanks in the low solar corona. The "EIT wave" is shown using a combination of radio spectra and extreme ultraviolet images to be a shock front with a Mach number greater than one. Its initial energy is then calculated using the Sedov-Taylor blast-wave approximation, which provides an approximation for a shock front propagating through a region of variable density. This approach provides an initial energy estimate of ~2.8 x 10^31 ergs to produce the "EIT wave", which is approximately 10% the kinetic energy of the associated CME (shown to be ~2.5 x 10^32 ergs). These results indicate that the energy of the "EIT wave" may be significant and must be considered when estimating the total energy budget of solar eruptions. Title: The Energetics of a Global Shock Wave in the Low Solar Corona Authors: Long, David M.; Baker, Deborah; Williams, David R.; Carley, Eoin P.; Gallagher, Peter T.; Zucca, Pietro Bibcode: 2015ApJ...799..224L Altcode: 2014arXiv1412.2964L As the most energetic eruptions in the solar system, coronal mass ejections (CMEs) can produce shock waves at both their front and flanks as they erupt from the Sun into the heliosphere. However, the amount of energy produced in these eruptions, and the proportion of their energy required to produce the waves, is not well characterized. Here we use observations of a solar eruption from 2014 February 25 to estimate the energy budget of an erupting CME and the globally propagating "EIT wave" produced by the rapid expansion of the CME flanks in the low solar corona. The "EIT wave" is shown using a combination of radio spectra and extreme ultraviolet images to be a shock front with a Mach number greater than one. Its initial energy is then calculated using the Sedov-Taylor blast-wave approximation, which provides an approximation for a shock front propagating through a region of variable density. This approach provides an initial energy estimate of ≈2.8 × 1031 erg to produce the "EIT wave," which is approximately 10% the kinetic energy of the associated CME (shown to be ≈2.5 × 1032 erg). These results indicate that the energy of the "EIT wave" may be significant and must be considered when estimating the total energy budget of solar eruptions. Title: How Can Active Region Plasma Escape into the Solar Wind from Below a Closed Helmet Streamer? Authors: Mandrini, C. H.; Nuevo, F. A.; Vásquez, A. M.; Démoulin, P.; van Driel-Gesztelyi, L.; Baker, D.; Culhane, J. L.; Cristiani, G. D.; Pick, M. Bibcode: 2014SoPh..289.4151M Altcode: 2014arXiv1409.7369M; 2014SoPh..tmp..115M Recent studies show that active-region (AR) upflowing plasma, observed by the EUV-Imaging Spectrometer (EIS) onboard Hinode, can gain access to open-field lines and be released into the solar wind (SW) via magnetic-interchange reconnection at magnetic null-points in pseudo-streamer configurations. When only one bipolar AR is present on the Sun and is fully covered by the separatrix of a streamer, such as AR 10978 in December 2007, it seems unlikely that the upflowing AR plasma can find its way into the slow SW. However, signatures of plasma with AR composition have been found at 1 AU by Culhane et al. (Solar Phys.289, 3799, 2014) that apparently originated west of AR 10978. We present a detailed topology analysis of AR 10978 and the surrounding large-scale corona based on a potential-field source-surface (PFSS) model. Our study shows that it is possible for the AR plasma to move around the streamer separatrix and be released into the SW via magnetic reconnection, which occurs in at least two main steps. We analyse data from the Nançay Radioheliograph (NRH) in a search for evidence of the chain of magnetic reconnections that we propose. We find a noise storm above the AR and several varying sources at 150.9 MHz. Their locations suggest that they might be associated with particles accelerated during the first-step reconnection process at a null point well outside of the AR. We find no evidence of the second reconnection step in the radio data, however. Our results demonstrate that even when it appears highly improbable for the AR plasma to reach the SW, indirect channels involving a sequence of reconnections can make it possible. Title: Tracking Solar Active Region Outflow Plasma from Its Source to the Near-Earth Environment Authors: Culhane, J. L.; Brooks, D. H.; van Driel-Gesztelyi, L.; Démoulin, P.; Baker, D.; DeRosa, M. L.; Mandrini, C. H.; Zhao, L.; Zurbuchen, T. H. Bibcode: 2014SoPh..289.3799C Altcode: 2014SoPh..tmp...90C; 2014arXiv1405.2949C Seeking to establish whether active-region upflow material contributes to the slow solar wind, we examine in detail the plasma upflows from Active Region (AR) 10978, which crossed the Sun's disc in the interval 8 to 16 December 2007 during Carrington rotation (CR) 2064. In previous work, using data from the Hinode/EUV Imaging Spectrometer, upflow velocity evolution was extensively studied as the region crossed the disc, while a linear force-free-field magnetic extrapolation was used to confirm aspects of the velocity evolution and to establish the presence of quasi-separatrix layers at the upflow source areas. The plasma properties, temperature, density, and first ionisation potential bias [FIP-bias] were measured with the spectrometer during the disc passage of the active region. Global potential-field source-surface (PFSS) models showed that AR 10978 was completely covered by the closed field of a helmet streamer that is part of the streamer belt. Therefore it is not clear how any of the upflowing AR-associated plasma could reach the source surface at 2.5 R⊙ and contribute to the slow solar wind. However, a detailed examination of solar-wind in-situ data obtained by the Advanced Composition Explorer (ACE) spacecraft at the L1 point shows that increases in O7+/O6+, C6+/C5+, and Fe/O - a FIP-bias proxy - are present before the heliospheric current-sheet crossing. These increases, along with an accompanying reduction in proton velocity and an increase in density are characteristic of both AR and slow-solar-wind plasma. Finally, we describe a two-step reconnection process by which some of the upflowing plasma from the AR might reach the heliosphere. Title: VIRUS instrument enclosures Authors: Prochaska, T.; Allen, R.; Mondrik, N.; Rheault, J. P.; Sauseda, M.; Boster, E.; James, M.; Rodriguez-Patino, M.; Torres, G.; Ham, J.; Cook, E.; Baker, D.; DePoy, Darren L.; Marshall, Jennifer L.; Hill, G. J.; Perry, D.; Savage, R. D.; Good, J. M.; Vattiat, Brian L. Bibcode: 2014SPIE.9147E..6UP Altcode: The Visible Integral-Field Replicable Unit Spectrograph (VIRUS) instrument will be installed at the Hobby-Eberly Telescope† in the near future. The instrument will be housed in two enclosures that are mounted adjacent to the telescope, via the VIRUS Support Structure (VSS). We have designed the enclosures to support and protect the instrument, to enable servicing of the instrument, and to cool the instrument appropriately while not adversely affecting the dome environment. The system uses simple HVAC air handling techniques in conjunction with thermoelectric and standard glycol heat exchangers to provide efficient heat removal. The enclosures also provide power and data transfer to and from each VIRUS unit, liquid nitrogen cooling to the detectors, and environmental monitoring of the instrument and dome environments. In this paper, we describe the design and fabrication of the VIRUS enclosures and their subsystems. Title: Coronal Magnetic Reconnection Driven by CME Expansion—the 2011 June 7 Event Authors: van Driel-Gesztelyi, L.; Baker, D.; Török, T.; Pariat, E.; Green, L. M.; Williams, D. R.; Carlyle, J.; Valori, G.; Démoulin, P.; Kliem, B.; Long, D. M.; Matthews, S. A.; Malherbe, J. -M. Bibcode: 2014ApJ...788...85V Altcode: 2014arXiv1406.3153V Coronal mass ejections (CMEs) erupt and expand in a magnetically structured solar corona. Various indirect observational pieces of evidence have shown that the magnetic field of CMEs reconnects with surrounding magnetic fields, forming, e.g., dimming regions distant from the CME source regions. Analyzing Solar Dynamics Observatory (SDO) observations of the eruption from AR 11226 on 2011 June 7, we present the first direct evidence of coronal magnetic reconnection between the fields of two adjacent active regions during a CME. The observations are presented jointly with a data-constrained numerical simulation, demonstrating the formation/intensification of current sheets along a hyperbolic flux tube at the interface between the CME and the neighboring AR 11227. Reconnection resulted in the formation of new magnetic connections between the erupting magnetic structure from AR 11226 and the neighboring active region AR 11227 about 200 Mm from the eruption site. The onset of reconnection first becomes apparent in the SDO/AIA images when filament plasma, originally contained within the erupting flux rope, is redirected toward remote areas in AR 11227, tracing the change of large-scale magnetic connectivity. The location of the coronal reconnection region becomes bright and directly observable at SDO/AIA wavelengths, owing to the presence of down-flowing cool, dense (1010 cm-3) filament plasma in its vicinity. The high-density plasma around the reconnection region is heated to coronal temperatures, presumably by slow-mode shocks and Coulomb collisions. These results provide the first direct observational evidence that CMEs reconnect with surrounding magnetic structures, leading to a large-scale reconfiguration of the coronal magnetic field. Title: Spectroscopic measurements of EUV ejecta in a CME: a high-blueshift trailing thread Authors: Williams, David; Baker, Deborah; van Driel-Gesztelyi, Lidia; Green, Lucie Bibcode: 2014IAUS..300..464W Altcode: The mass of erupting prominence material can be inferred from the obscuration of emission behind this mass of cool plasma thanks to the rapid cadence of SDO/AIA images in the short EUV wavelength range (Carlyle et al. 2013, these proceedings). In comparing this approach with spectral observations from Hinode/EIS, to monitor contributions from emission seen around the erupting prominence material, we have found an intriguing component of blue-shifted emission, trailing the erupting prominence, with Doppler shifts on the order of 350 km s-1 in bright lines of both He ii and Fe xii. Title: FIP bias in a sigmoidal active region Authors: Baker, D.; Brooks, D. H.; Démoulin, P.; van Driel-Gesztelyi, Lidia; Green, L. M.; Steed, K.; Carlyle, J. Bibcode: 2014IAUS..300..222B Altcode: We investigate first ionization potential (FIP) bias levels in an anemone active region (AR) - coronal hole (CH) complex using an abundance map derived from Hinode/EIS spectra. The detailed, spatially resolved abundance map has a large field of view covering 359'' × 485''. Plasma with high FIP bias, or coronal abundances, is concentrated at the footpoints of the AR loops whereas the surrounding CH has a low FIP bias, ~1, i.e. photospheric abundances. A channel of low FIP bias is located along the AR's main polarity inversion line containing a filament where ongoing flux cancellation is observed, indicating a bald patch magnetic topology characteristic of a sigmoid/flux rope configuration. Title: Active region upflow plasma: its relation to small activity and the solar wind Authors: Mandrini, Cristina H.; Culhane, J. Leonard; Cristiani, Germán; Vásquez, Alberto; Van Driel-Gesztelyi, Lidia; Baker, Deborah; Pick, Monique; Demoulin, Pascal; Nuevo, Federico Bibcode: 2014cosp...40E1979M Altcode: Recent studies show that active region (AR) upflowing plasma, observed by the Hinode EUV Imaging Spectrometer (EIS), can gain access to open field lines and be released into the solar wind via magnetic interchange reconnection occurring below the source surface at magnetic null-points in pseudo-streamer configurations. When only one simple bipolar AR is present on the Sun and it is fully covered by the separatrix of a streamer, like AR 10978 on December 2007, it seems unlikely that the upflowing AR plasma could find its way into the slow solar wind. However, signatures of plasma with AR composition at 1 AU that appears to originate from the West of AR 10978 were recently found by Culhane and coworkers. We present a detailed topology analysis of AR 10978 based on a linear force-free magnetic field model at the AR scale, combined with a global PFSS model. This allows us, on one hand, to explain the variations observed in the upflows to the West of the AR as the result of magnetic reconnection at quasi-separatrix layers (QSLs). While at a global scale, we show that reconnection, occurring in at least two main steps, first at QSLs and later at a high-altitude coronal null-point, allows the AR plasma to get around the topological obstacle of the streamer separatrix and be released into the solar wind. Title: Magnetic reconnection driven by filament eruption in the 7 June 2011 event Authors: van Driel-Gesztelyi, L.; Baker, D.; Török, T.; Pariat, E.; Green, L. M.; Williams, D. R.; Carlyle, J.; Valori, G.; Démoulin, P.; Matthews, S. A.; Kliem, B.; Malherbe, J. -M. Bibcode: 2014IAUS..300..502V Altcode: During an unusually massive filament eruption on 7 June 2011, SDO/AIA imaged for the first time significant EUV emission around a magnetic reconnection region in the solar corona. The reconnection occurred between magnetic fields of the laterally expanding CME and a neighbouring active region. A pre-existing quasi-separatrix layer was activated in the process. This scenario is supported by data-constrained numerical simulations of the eruption. Observations show that dense cool filament plasma was re-directed and heated in situ, producing coronal-temperature emission around the reconnection region. These results provide the first direct observational evidence, supported by MHD simulations and magnetic modelling, that a large-scale re-configuration of the coronal magnetic field takes place during solar eruptions via the process of magnetic reconnection. Title: Magnetic Polarity Streams and Subsurface Flows Authors: Howe, R.; Baker, D.; Harra, L.; van Driel-Gesztelyi, L.; Komm, R.; Hill, F.; González Hernández, I. Bibcode: 2013ASPC..478..291H Altcode: An important feature of the solar cycle is the transport of unbalanced magnetic flux from active regions towards the poles, which eventually results in polarity reversal. This transport takes the form of distinct “polarity streams” that are visible in the magnetic butterfly diagram. We compare the poleward migration rate estimated from such streams to that derived from the subsurface meridional flows measured in helioseismic data from the GONG network since 2001, and find that the results are in reasonable agreement. Title: Plasma Composition in a Sigmoidal Anemone Active Region Authors: Baker, D.; Brooks, D. H.; Démoulin, P.; van Driel-Gesztelyi, L.; Green, L. M.; Steed, K.; Carlyle, J. Bibcode: 2013ApJ...778...69B Altcode: 2013arXiv1310.0999B Using spectra obtained by the EUV Imaging Spectrometer (EIS) instrument onboard Hinode, we present a detailed spatially resolved abundance map of an active region (AR)-coronal hole (CH) complex that covers an area of 359'' × 485''. The abundance map provides first ionization potential (FIP) bias levels in various coronal structures within the large EIS field of view. Overall, FIP bias in the small, relatively young AR is 2-3. This modest FIP bias is a consequence of the age of the AR, its weak heating, and its partial reconnection with the surrounding CH. Plasma with a coronal composition is concentrated at AR loop footpoints, close to where fractionation is believed to take place in the chromosphere. In the AR, we found a moderate positive correlation of FIP bias with nonthermal velocity and magnetic flux density, both of which are also strongest at the AR loop footpoints. Pathways of slightly enhanced FIP bias are traced along some of the loops connecting opposite polarities within the AR. We interpret the traces of enhanced FIP bias along these loops to be the beginning of fractionated plasma mixing in the loops. Low FIP bias in a sigmoidal channel above the AR's main polarity inversion line, where ongoing flux cancellation is taking place, provides new evidence of a bald patch magnetic topology of a sigmoid/flux rope configuration. Title: Revisiting the Distribution and Properties of Shatter Cones at the Sudbury Impact Structure, Canada Authors: Osinski, G. R.; Ferrière, L.; Kring, D. A.; Anders, D.; Armstrong, K.; Baker, D.; Bamberg, M.; Beddingfield, C.; Gaither, T.; Harrison, T.; Huber, M. S.; Hurwitz, D.; Jaret, S.; Kramer, G.; Kuriyama, Y.; Lucas, M.; Marion, C. L.; Mercer, C.; Mount, C.; Neish, C.; Nuhn, A.; Ostrach, L.; Pickersgill, A.; Pilles, E.; Potter, R. W. K.; Ryan, A.; Sharp, M.; Swartz, N.; Thomson, O.; Veto, M.; Wielicki, M. M.; Wright, S.; Zanetti, M. Bibcode: 2013LPICo1737.3061O Altcode: Here, we present the first results of a new multi-year research program that aims to systematically map the distribution of shatter cones and their physical properties around the Sudbury structure. Title: 76 T dwarfs from the UKIDSS LAS: benchmarks, kinematics and an updated space density Authors: Burningham, Ben; Cardoso, C. V.; Smith, L.; Leggett, S. K.; Smart, R. L.; Mann, A. W.; Dhital, S.; Lucas, P. W.; Tinney, C. G.; Pinfield, D. J.; Zhang, Z.; Morley, C.; Saumon, D.; Aller, K.; Littlefair, S. P.; Homeier, D.; Lodieu, N.; Deacon, N.; Marley, M. S.; van Spaandonk, L.; Baker, D.; Allard, F.; Andrei, A. H.; Canty, J.; Clarke, J.; Day-Jones, A. C.; Dupuy, T.; Fortney, J. J.; Gomes, J.; Ishii, M.; Jones, H. R. A.; Liu, M.; Magazzú, A.; Marocco, F.; Murray, D. N.; Rojas-Ayala, B.; Tamura, M. Bibcode: 2013MNRAS.433..457B Altcode: 2013arXiv1304.7246B; 2013MNRAS.tmp.1507B We report the discovery of 76 new T dwarfs from the UKIRT Infrared Deep Sky Survey (UKIDSS) Large Area Survey (LAS). Near-infrared broad- and narrow-band photometry and spectroscopy are presented for the new objects, along with Wide-field Infrared Survey Explorer (WISE) and warm-Spitzer photometry. Proper motions for 128 UKIDSS T dwarfs are presented from a new two epoch LAS proper motion catalogue. We use these motions to identify two new benchmark systems: LHS 6176AB, a T8p+M4 pair and HD 118865AB, a T5.5+F8 pair. Using age constraints from the primaries and evolutionary models to constrain the radii, we have estimated their physical properties from their bolometric luminosity. We compare the colours and properties of known benchmark T dwarfs to the latest model atmospheres and draw two principal conclusions. First, it appears that the H - [4.5] and J - W2 colours are more sensitive to metallicity than has previously been recognized, such that differences in metallicity may dominate over differences in Teff when considering relative properties of cool objects using these colours. Secondly, the previously noted apparent dominance of young objects in the late-T dwarf sample is no longer apparent when using the new model grids and the expanded sample of late-T dwarfs and benchmarks. This is supported by the apparently similar distribution of late-T dwarfs and earlier type T dwarfs on reduced proper motion diagrams that we present. Finally, we present updated space densities for the late-T dwarfs, and compare our values to simulation predictions and those from WISE. Title: Are subsurface flows and coronal holes related? Authors: Komm, R.; Howe, R.; González Hernández, I.; Harra, L.; Baker, D.; van Driel-Gesztelyi, L. Bibcode: 2013JPhCS.440a2022K Altcode: We study synoptic maps of solar subsurface flows covering six Carrington rotations (2050 to 2055). The subsurface flows are determined with a ring-diagram analysis of GONG high-resolution Doppler data. We identify the locations of coronal holes in synoptic maps of EUV images at 195Å from the EIT instrument and determine the characteristics of associated subsurface flows. We study two long-lived coronal holes that are present during this epoch. We find that large-scale patterns are present in the subsurface flows but appear to be unrelated to these coronal holes. The horizontal subsurface flows associated with the two long-lived coronal holes are weakly divergent (upflows) with small cyclonic vorticity. These flows are thus similar to subsurface flows of quiet regions with regard to the vertical flows and similar to flows of active regions with regard to vorticity. Title: Can we detect local helioseismic parameter shifts in coronal holes? Authors: Howe, R.; Haber, D. A.; Bogart, R. S.; Zharkov, S.; Baker, D.; Harra, L.; van Driel-Gesztelyi, L. Bibcode: 2013JPhCS.440a2019H Altcode: Changes in helioseismic mode parameters in active regions and across the solar disk are well documented, but local magnetic activity and geometric effects may not account for all of the scatter seen in the results. We use results from the Helioseismic and Magnetic Imager ring-diagram pipeline for Carrington rotation 2113 to look for differences in mode amplitude and frequency between coronal holes and other quiet-Sun regions. While we do not find a systematic difference, the results do suggest that the correlation between magnetic activity index and mode parameters shows less scatter in coronal hole regions than in general quiet Sun. Title: Subsurface flows associated with non-Joy oriented active regions: a case study Authors: González Hernández, Irene; Komm, Rudolf; van Driel-Gesztelyi, Lidia; Baker, Deborah; Harra, Louise; Howe, Rachel Bibcode: 2013JPhCS.440a2050G Altcode: Non-Joy oriented active regions (ARs) are a challenge for solar magnetic field modelers. Although significant deviations from Joy's law are relatively rare for simple bipolar ARs, understanding the causes of their particularity could be critical for the big picture of the solar dynamo. We explore the possibility of the sub-surface local dynamics being responsible for the significant rotation of these ARs. We apply the ring-diagram technique, a local helioseismology method, to infer the flows under and surrounding a non-Joy oriented AR and present the results of a case study in this paper. Title: The 3D Geometry of Active Region Upflows Deduced from Their Limb-to-Limb Evolution Authors: Démoulin, P.; Baker, D.; Mandrini, C. H.; van Driel-Gesztelyi, L. Bibcode: 2013SoPh..283..341D Altcode: 2012arXiv1211.5962D We analyze the evolution of coronal plasma upflows from the edges of AR 10978, which has the best limb-to-limb data coverage with Hinode's EUV Imaging Spectrometer (EIS). We find that the observed evolution is largely due to the solar rotation progressively changing the viewpoint of nearly stationary flows. From the systematic changes in the upflow regions as a function of distance from disc center, we deduce their 3D geometrical properties as inclination and angular spread in three coronal lines (Si VII, Fe XII, and Fe XV). In agreement with magnetic extrapolations, we find that the flows are thin, fan-like structures rooted in quasi separatrix layers (QSLs). The fans are tilted away from the AR center. The highest plasma velocities in these three spectral lines have similar magnitudes and their heights increase with temperature. The spatial location and extent of the upflow regions in the Si VII, Fe XII, and Fe XV lines are different owing to i) temperature stratification and ii) line of sight integration of the spectral profiles with significantly different backgrounds. We conclude that we sample the same flows at different temperatures. Further, we find that the evolution of line widths during the disc passage is compatible with a broad range of velocities in the flows. Everything considered, our results are compatible with the AR upflows originating from reconnections along QSLs between over-pressure AR loops and neighboring under-pressure loops. The flows are driven along magnetic field lines by a pressure gradient in a stratified atmosphere. Our interpretation of the above results is that, at any given time, we observe the superposition of flows created by successive reconnections, leading to a broad velocity distribution. Title: Mass Estimates of Rapidly Moving Prominence Material from High-cadence EUV Images Authors: Williams, David R.; Baker, Deborah; van Driel-Gesztelyi, Lidia Bibcode: 2013ApJ...764..165W Altcode: 2013arXiv1301.4271W We present a new method for determining the column density of erupting filament material using state-of-the-art multi-wavelength imaging data. Much of the prior work on filament/prominence structure can be divided between studies that use a polychromatic approach with targeted campaign observations and those that use synoptic observations, frequently in only one or two wavelengths. The superior time resolution, sensitivity, and near-synchronicity of data from the Solar Dynamics Observatory's Advanced Imaging Assembly allow us to combine these two techniques using photoionization continuum opacity to determine the spatial distribution of hydrogen in filament material. We apply the combined techniques to SDO/AIA observations of a filament that erupted during the spectacular coronal mass ejection on 2011 June 7. The resulting "polychromatic opacity imaging" method offers a powerful way to track partially ionized gas as it erupts through the solar atmosphere on a regular basis, without the need for coordinated observations, thereby readily offering regular, realistic mass-distribution estimates for models of these erupting structures. Title: Plasma outflows at the border of active regions and the solar wind Authors: Nuevo, F. A.; Mandrini, C. H.; Vásquez, A. M.; Deumoulin, P.; Van Driel-Gesztely, L.; Baker, D.; Cristiani, G. D.; Pick, M.; Culhane, J. L. Bibcode: 2013BAAA...56..387N Altcode: We present a detailed topological analysis of active region (AR) 10978; based on a Potential Field Source Surface (PFSS) model. AR 10978 is a standard bipolar region which appears fully covered by the magnetic field lines of a coronal streamer. Despite this simple magnetic configuration; our analysis shows that it is possible for the AR plasma; contained in the outflows observed at the AR borders; to be released into the solar wind via magnetic reconnection. Title: Magnetic Topology of Active Regions and Coronal Holes: Implications for Coronal Outflows and the Solar Wind Authors: van Driel-Gesztelyi, L.; Culhane, J. L.; Baker, D.; Démoulin, P.; Mandrini, C. H.; DeRosa, M. L.; Rouillard, A. P.; Opitz, A.; Stenborg, G.; Vourlidas, A.; Brooks, D. H. Bibcode: 2012SoPh..281..237V Altcode: 2012SoPh..tmp..228V During 2 - 18 January 2008 a pair of low-latitude opposite-polarity coronal holes (CHs) were observed on the Sun with two active regions (ARs) and the heliospheric plasma sheet located between them. We use the Hinode/EUV Imaging Spectrometer (EIS) to locate AR-related outflows and measure their velocities. Solar-Terrestrial Relations Observatory (STEREO) imaging is also employed, as are the Advanced Composition Explorer (ACE) in-situ observations, to assess the resulting impacts on the solar wind (SW) properties. Magnetic-field extrapolations of the two ARs confirm that AR plasma outflows observed with EIS are co-spatial with quasi-separatrix layer locations, including the separatrix of a null point. Global potential-field source-surface modeling indicates that field lines in the vicinity of the null point extend up to the source surface, enabling a part of the EIS plasma upflows access to the SW. We find that similar upflow properties are also observed within closed-field regions that do not reach the source surface. We conclude that some of plasma upflows observed with EIS remain confined along closed coronal loops, but that a fraction of the plasma may be released into the slow SW. This suggests that ARs bordering coronal holes can contribute to the slow SW. Analyzing the in-situ data, we propose that the type of slow SW present depends on whether the AR is fully or partially enclosed by an overlying streamer. Title: Identifying the Main Driver of Active Region Outflows Authors: Baker, D.; van Driel-Gesztelyi, L.; Mandrini, C. H.; Démoulin, P.; Murray, M. J. Bibcode: 2012ASPC..454..425B Altcode: Hinode's EUV Imaging Spectrometer (EIS) has discovered ubiquitous outflows of a few to 50 km s-1 from active regions (ARs). The characteristics of these outflows are very curious in that they are most prominent at the AR boundary and appear over monopolar magnetic areas. They are linked to strong non-thermal line broadening and are stronger in hotter EUV lines. The outflows persist for at least several days. Whereas red-shifted down flows observed in AR closed loops are well understood, to date there is no general consensus for the mechanism(s) driving blue-shifted AR-related outflows. We use Hinode EIS and X-Ray Telescope observations of AR 10942 coupled with magnetic modeling to demonstrate for the first time that the outflows originate from specific locations of the magnetic topology where field lines display strong gradients of magnetic connectivity, namely quasi-separatrix layers (QSLs), or in the limit of infinitely thin QSLs, separatrices. The strongest AR outflows were found to be in the vicinity of QSL sections located over areas of strong magnetic field. We argue that magnetic reconnection at QSLs, separating closed field lines of the AR and either large-scale externally connected or ‘open’ field lines, is a viable mechanism for driving AR outflows which are potentially sources of the slow solar wind. In fact, magnetic reconnection along QSLs (including separatricies) is the first theory to explain the most puzzling characteristics of the outflows, namely their occurrence over monopolar areas at the periphery of ARs and their longevity. Title: Sunspot Light-Bridges - A Bridge Between the Photosphere and the Corona? Authors: Matthews, S.; Baker, D.; Domínguez, S. V. Bibcode: 2012ASPC..454..209M Altcode: 2010arXiv1004.3879M Recent observations of sunspot light-bridges (LBs) have shed new light on the fact that they are often associated with significant chromospheric activity. In particular chromospheric jets (Shimizu et al. 2009) persisting over a period of days have been identified, sometimes associated with large downflows at the photospheric level (Louis et al. 2009). One possible explanation for this activity is reconnection low in the atmosphere. LBs have also been associated with a constant brightness enhancement in the 1600 Å passband of TRACE, and the heating of 1 MK loops. Using data from EIS, SOT and STEREO EUVI we investigate the response of the transition region and lower corona to the presence of a LB. Title: Magnetic topology, coronal outflows, and the solar wind Authors: Mandrini, Cristina H.; Culhane, J. Leonard; Vourlidas, Angelos; Demoulin, Pascal; Stenborg, Guillermo; Opitz, Andrea; Rouillard, Alexis; Van Driel-Gesztelyi, Lidia; Baker, Deborah; DeRosa, Marc; Brooks, David Bibcode: 2012cosp...39.1173M Altcode: 2012cosp.meet.1173M During 2-18 January 2008 a pair of low-latitude opposite polarity coronal holes were observed on the Sun flanked by two ARs with the heliospheric plasma sheet between them. Hinode/EUV Imaging Telescope (EIS) is used to locate AR-related outflows and measure their velocities. The Advanced Composition Explorer (ACE) in-situ observations are employed to assess the resulting impacts on the interplanetary solar wind (SW). Magnetic field extrapolations of the two ARs confirm that AR plasma outflows observed with EIS are co-spatial with quasi-separatrix layer locations, including the separatrix of a null point. Global potential field source-surface modeling indicates that field lines in the vicinity of the null point extend up to the source-surface, enabling a part of the EIS plasma upflows access to the SW. Similar upflow magnitude is also observed within closed field regions. Though part of the plasma upflows observed with EIS remain confined along closed coronal loops, a subset of them are indeed able to make their imprint in the slow SW, making ARs bordering coronal holes a slow SW contributor. Title: Are subsurface flows and coronal holes related? Authors: Komm, Rudolf W.; Howe, R.; González Hernández, I.; Harra, L.; Baker, D.; van Driel-Gesztelyi, L. Bibcode: 2012shin.confE.120K Altcode: We study subsurface flows measured with a ring-diagram analysis of GONG high-resolution Doppler data. In previous studies, we have focused on the relationship between active regions and subsurface flows associated with them. Synoptic subsurface flow maps show also large-scale patterns that are not obviously associated with active regions. It is unknown whether these flow patterns correlate with any large-scale magnetic features. Here, we explore whether there is a relationship between subsurface flows and coronal features. We analyze synoptic maps of subsurface flows covering 18 Carrington rotations during the years 2006 and 2007 (CR 2038-2055). Long-lived coronal holes are present during this epoch at low latitudes, which are accessible by ring-diagram analysis of GONG data. We compare subsurface flow maps with EIT synoptic maps of EUV images at 195A (http://sun.stanford.edu/synop/EIT/) and will present the latest results. Title: Nonlinear Force-Free Extrapolation of Emerging Flux with a Global Twist and Serpentine Fine Structures Authors: Valori, G.; Green, L. M.; Démoulin, P.; Vargas Domínguez, S.; van Driel-Gesztelyi, L.; Wallace, A.; Baker, D.; Fuhrmann, M. Bibcode: 2012SoPh..278...73V Altcode: We study the flux emergence process in NOAA active region 11024, between 29 June and 7 July 2009, by means of multi-wavelength observations and nonlinear force-free extrapolation. The main aim is to extend previous investigations by combining, as much as possible, high spatial resolution observations to test our present understanding of small-scale (undulatory) flux emergence, whilst putting these small-scale events in the context of the global evolution of the active region. The combination of these techniques allows us to follow the whole process, from the first appearance of the bipolar axial field on the east limb, until the buoyancy instability could set in and raise the main body of the twisted flux tube through the photosphere, forming magnetic tongues and signatures of serpentine field, until the simplification of the magnetic structure into a main bipole by the time the active region reaches the west limb. At the crucial time of the main emergence phase high spatial resolution spectropolarimetric measurements of the photospheric field are employed to reconstruct the three-dimensional structure of the nonlinear force-free coronal field, which is then used to test the current understanding of flux emergence processes. In particular, knowledge of the coronal connectivity confirms the identity of the magnetic tongues as seen in their photospheric signatures, and it exemplifies how the twisted flux, which is emerging on small scales in the form of a sea-serpent, is subsequently rearranged by reconnection into the large-scale field of the active region. In this way, the multi-wavelength observations combined with a nonlinear force-free extrapolation provide a coherent picture of the emergence process of small-scale magnetic bipoles, which subsequently reconnect to form a large-scale structure in the corona. Title: Forecasting a CME by Spectroscopic Precursor? Authors: Baker, D.; van Driel-Gesztelyi, L.; Green, L. M. Bibcode: 2012SoPh..276..219B Altcode: Multi-temperature plasma flows resulting from the interaction between a mature active region (AR) inside an equatorial coronal hole (CH) are investigated. Outflow velocities observed by Hinode EIS ranged from a few to 13 km s−1 for three days at the AR's eastern and western edges. However, on the fourth day, velocities intensified up to 20 km s−1 at the AR's western footpoint about six hours prior to a CME. 3D MHD numerical simulations of the observed magnetic configuration of the AR-CH complex showed that the expansion of the mature AR's loops drives persistent outflows along the neighboring CH field (Murray et al. in Solar Phys.261, 253, 2010). Based on these simulations, intensification of outflows observed pre-eruption on the AR's western side where same-polarity AR and CH field interface, is interpreted to be the result of the expansion of a sigmoidal AR, in particular, a flux rope containing a filament that provides stronger compression of the neighboring CH field on this side of the AR. Intensification of outflows in the AR is proposed as a new type of CME precursor. Title: The Research Experience for Undergraduates Program in Solar and Space Physics at the University of Colorado Authors: Snow, M.; Wood, E.; Cobabe-Amman, E.; Baker, D.; Renfrow, S. Bibcode: 2011ASPC..443..332S Altcode: The Research Experience for Undergraduates (REU) program in Solar and Space Physics is a collaboration between the University of Colorado's Laboratory for Atmospheric and Space Physics (LASP), the National Center for Atmospheric Research's High Altitude Observatory (HAO), the National Oceanic and Atmospheric Administration's Space Weather Prediction Center (SWPC), the Southwest Research Institute (SwRI), and Northwest Research Associates' Colorado Research Associates (CoRA). The goal of the program is to give students real-world, hands-on experience doing research with scientist mentors and to further their intended careers.

Our program began in 2007 and is entering its fourth year. Mentors from the member institutions have supervised over fifty research projects dealing with all aspects of Solar and Space Physics. The students begin their eight-week visit to Boulder with a week of classes on the Sun-Earth system as well as practical courses on data analysis and the IDL programming language. The students give a 30 minute oral presentation of their project as well as a poster in a student symposium at the end of the program. Throughout the summer, the students give progress reports at weekly brown-bag lunch meetings. In addition to their own research projects at their host institution, the students tour and meet scientists from the partner institutions as the weekly lunches rotate from site to site. There are also opportunities for students to network with scientists in an informal way at the excursions we organize which include barbecues and weekend outings. Title: The discovery of the T8.5 dwarf UGPS J0521+3640 Authors: Burningham, Ben; Lucas, P. W.; Leggett, S. K.; Smart, R.; Baker, D.; Pinfield, D. J.; Tinney, C. G.; Homeier, D.; Allard, F.; Zhang, Z. H.; Gomes, J.; Day-Jones, A. C.; Jones, H. R. A.; Kovács, G.; Lodieu, N.; Marocco, F.; Murray, D. N.; Sipőcz, B. Bibcode: 2011MNRAS.414L..90B Altcode: 2011arXiv1104.1526B We have carried out a search for late-type T dwarfs in the UKIRT Infrared Deep Sky Survey Galactic Plane Survey 6th Data Release. The search yielded two persuasive candidates, both of which have been confirmed as T dwarfs. The brightest, UGPS J0521+3640, has been assigned the spectral type T8.5 and appears to lie at a distance of 7-9 pc. The fainter of the two, UGPS J0652+0324, is classified as a T5.5 dwarf and lies at an estimated distance of 28-37 pc. Warm-Spitzer observations in IRAC channels 1 and 2, taken as part of the GLIMPSE360 Legacy Survey, are available for UGPS J0521+3640 and we used these data with the near-infrared spectroscopy to estimate its properties. We find best-fitting solar metallicity BT-Settl models for Teff= 600 and 650 K and log g= 4.5 and 5.0. These parameters suggest a mass between 14 and 32MJ for an age between 1 and 5 Gyr. The proximity of this very cool T dwarf, and its location in the Galactic plane, makes it an ideal candidate for high-resolution adaptive optics imaging to search for cool companions. Title: GRB 110112A: WHT candidate afterglow/host galaxy. Authors: Levan, A. J.; Tanvir, N. R.; Baker, D. Bibcode: 2011GCN.11559....1L Altcode: 2011GCN..11559...1L No abstract at ADS Title: Drivers of solar coronal dynamics Authors: Baker, Deborah Bibcode: 2011PhDT.......380B Altcode: No abstract at ADS Title: Using MHD modeling to specify inner heliosphere conditions during the three MESSENGER Mercury flybys Authors: Farr, N. L.; Baker, D.; Odstrcil, D.; Anderson, B. J.; Benna, M.; Gloeckler, G.; Korth, H.; Mayer, L. R.; Raines, J. M.; Schriver, D.; Slavin, J. A.; Solomon, S. C.; Travnicek, P. M.; Zurbuchen, T. Bibcode: 2010AGUFMSH42A..06F Altcode: The three successful flybys of Mercury by the MESSENGER spacecraft occurred, respectively, on 14 January 2008, 6 October 2008, and 29 September 2009. In order to provide contextual information about the solar wind properties and the interplanetary magnetic field (IMF) near the planet at those times, we have used an empirical modeling technique combined with a numerical physics-based solar wind model. The Wang-Sheeley-Arge (WSA) method uses solar photospheric magnetic field observations (from Earth-based instruments) in order to estimate the inner heliospheric radial flow speed and radial magnetic field out to 21.5 solar radii from the Sun. This information is then used as input to the global numerical magnetohydrodynamic model, ENLIL, which calculates solar wind velocity, density, temperature, and magnetic field strength and polarity throughout the inner heliosphere. WSA-ENLIL calculations are presented for the several-week period encompassing each of the flybys. This information in conjunction with available MESSENGER data aid in understanding the Mercury flyby observations and provide a basis for subsequent global magnetospheric modeling. We find that during all three flybys the solar wind conditions were quiescent and would have provided only modest dynamic driving forces for Mercury’s magnetospheric system. We present data-model comparisons for ACE, STEREO-A and -B, and MESSENGER for all of these cases. Title: Extreme Solar System in the Undergraduate Classroom Authors: Baker, D. Bibcode: 2010AGUFMED23A0699B Altcode: One of the greatest challenges for science educators today is to engage non-science students in the scientific process - to help them realize that science is cool, interesting, and fun. With NASA’s Year of the Solar System beginning in October 2010, a course that explores some of the most extreme places in our Solar System may be just the hook needed to improve attitudes toward science. We use three unique inquiry-based approaches in a freshman-level introductory science course to engage non-science students: 1) Emphasis on “extreme” phenomena in our Solar System, 2) Research papers and oral presentations in which “extreme experts” (students) try to convince a mock NASA panel where the next planetary mission should be, and 3) Science Portfolios in which students ask their own scientific questions, design their own scientific experiments, and evaluate their own scientific growth. The effectiveness of these approaches (as determined from pre-/post- surveys, focus groups, and other instruments) will be presented. Preliminary results show that students become less intimidated by science and feel that science has become more important in their everyday lives. Title: Cratering on Mercury: Insights from the MESSENGER Flybys Authors: Chapman, C. R.; Strom, R. G.; Fassett, C. I.; Prockter, L. M.; Head, J. W.; Solomon, S. C.; Banks, M. E.; Baker, D.; Merline, W. J. Bibcode: 2010M&PSA..73.5325C Altcode: No abstract at ADS Title: Outflows at the Edges of an Active Region in a Coronal Hole: A Signature of Active Region Expansion? Authors: Murray, M. J.; Baker, D.; van Driel-Gesztelyi, L.; Sun, J. Bibcode: 2010SoPh..261..253M Altcode: 2009arXiv0912.1246M Outflows of plasma at the edges of active regions surrounded by quiet Sun are now a common observation with the Hinode satellite. While there is observational evidence to suggest that the outflows are originating in the magnetic field surrounding the active regions, there is no conclusive evidence that reveals how they are driven. Motivated by observations of outflows at the periphery of a mature active region embedded in a coronal hole, we have used a three-dimensional simulation to emulate the active region's development in order to investigate the origin and driver of these outflows. We find that outflows are accelerated from a site in the coronal hole magnetic field immediately surrounding the active region and are channelled along the coronal hole field as they rise through the atmosphere. The plasma is accelerated simply as a result of the active region expanding horizontally as it develops. Many of the characteristics of the outflows generated in the simulation are consistent with those of observed outflows: velocities up to 45 km s−1, properties akin to the coronal hole, proximity to the active region's draining loops, expansion with height, and projection over monopolar photospheric magnetic concentrations. Although the horizontal expansion occurs as a consequence of the active region's development in the simulation, expansion is also a general feature of established active regions. Hence, it is entirely possible and plausible that the expansion acceleration mechanism displayed in the simulation is occurring in active regions on the Sun and, in addition to reconnection, is driving the outflows observed at their edges. Title: Magnetic reconnection along QSLs -a major driver of active region outflows Authors: Baker, Deborah; van Driel-Gesztelyi, Lidia; Mandrini, Cristina H.; Demoulin, Pascal Bibcode: 2010cosp...38.2926B Altcode: 2010cosp.meet.2926B The relationship between quasi-separatrix layers (QSLs), or in the limit of infinitely thin QSLs, separatrices, and various activity phenomena has been explored in many different solar magnetic configurations across all scales in recent years. In the absence of magnetic nulls, fast reconnec-tion along QSLs, which are specific locations in the magnetic topology where field lines display strong gradients of magnetic connectivity, was identified as the main physical process at the origin of flares. Recently, it was shown that fast (tens of km/s) persistent hot plasma upflows in active regions (ARs) can also be linked to locations of QSLs. It is likely that these upflows that occur at the edges of ARs over unipolar magnetic field concentrations are accelerated by magnetic reconnection along QSLs. We will show multi-temperature spectral scan observations from Hinode's EIS combined with magnetic modeling of QSLs in two ARs observed on 20-21 February 2007 and 11 January 2008. The latter AR is observed and modeled when it is in the vicinity of the solar central meridian where there are no projection effects, thereby eliminating ambiguity linking the origin of multi-temperature observations of AR upflows to QSLs. We use the Potential Source Surface Model to look for open field lines in the vicinity of upflows and QSL locations in order to demonstrate whether these upflows become outflows and can contribute to the solar wind. Title: Interacting active regions and coronal holes: implications for coronal outflows and solar wind structure Authors: Culhane, J. Leonard; Baker, Deborah; Rouillard, Alexis; van Driel-Gesztelyi, Lidia Bibcode: 2010cosp...38.1863C Altcode: 2010cosp.meet.1863C When active regions are adjacent to coronal holes a variety of magnetic field interactions can result. These may include the interchange reconnection between the closed active region (AR) fields and the open field of the coronal hole (CH), leading to fast and significant evolution of coronal hole boundaries. Outcomes may include variability of -or changes in, active region-associated hot plasma outflows seen with Hinode/EIS and the modulation of the solar wind flows on open field lines. Depending on their relative positions on the Sun, the AR-CH interactions may have their signatures embedded in co-rotating interaction regions (CIRs) or rarefaction regions. During two intervals -8/11 January, 2008 and 7/9 December, 2008, we have made observations with Hinode of two oppositely configured situations on the Sun. For 8/11 January, the coronal hole leads the active region while for 7/9 December the order is reversed. The Hinode EIS instrument is used to locate outflows and measure their velocities while the XRT is used to image the source regions, including the variable nature of the outflows. SOHO EIT imaging is used to follow the longer-term evolution of the coronal hole boundaries while MDI is used to observe changes in the magnetic field. STEREO imaging and in-situ data are also employed -as are ACE observations, to assess the resulting impacts on interplanetary solar wind structures. The contrasting behaviour that results from magnetic interactions in the two different configurations is described and assessed. Title: Intensification of Plasma Upflows in an Active Region---Coronal Hole Complex: A CME Precursor Authors: Baker, D.; van Driel-Gesztelyi, L.; Murray, M. J.; Green, L. M.; Török, T.; Sun, J. Bibcode: 2009ASPC..415...75B Altcode: We investigate the plasma flows resulting from the interaction between a mature active region (AR) and a surrounding equatorial coronal hole (CH) observed by Hinode's EIS and XRT from 15 to 18 October 2007. For 3 days, EIS velocity maps showed upflows at the AR's eastern and western edges that were consistently between 5 and 10 km s-1, whereas downflows of up to 30 km s-1 were seen in AR loops. However, on 18 October, velocity profiles of hotter coronal lines revealed intensification in upflow velocities of up to 18 km s-1 at the AR's western footpoints 4.5 hours prior to a CME. We compare the AR's plasma flows with 2.5D MHD numerical simulations of the magnetic configuration, which show that expansion of the mature AR's loops drives upflows along the neighboring CH field. Further, the intensification of upflows observed on the AR's western side prior to a CME is interpreted to be the result of the expansion of a flux rope containing a filament further compressing the neighboring CH field. Title: Particle Transport and Acceleration in Mercury’s Magnetosphere during the MESSENGER Flybys Authors: Schriver, D.; Travnicek, P. M.; Paral, J.; Slavin, J. A.; Sarantos, M.; Anderson, B. J.; Korth, H.; Zurbuchen, T.; Baker, D.; Benna, M.; Killen, R. M.; McClintock, W. E.; Ho, G. C.; Krimigis, S. M.; McNutt, R. L.; Solomon, S. C. Bibcode: 2009AGUFM.P24A..07S Altcode: The first two MESSENGER flybys on 14 January 2008 and 6 October 2008 encountered very different solar wind interplanetary magnetic field (IMF) conditions. During the first flyby the IMF was northward, while during the second it was southward; in addition, during both flybys the IMF had a large radial (planetward) component. As is well known at the Earth, the orientation of the IMF strongly influences the structure and dynamics of the planetary magnetosphere, and this in turn strongly affects how particles are transported and accelerated as they move through the magnetosphere. To examine the transport, distribution, and energization of plasma (including heavy ions) for the solar wind conditions during the MESSENGER flybys, three-dimensional global hybrid simulations of Mercury’s magnetosphere are used to provide the electric and magnetic field configuration at the time of the flybys, and particle trajectories are then traced through the magnetospheric system. Because electrons are included as a massless fluid in the hybrid simulations, electron transport is also examined using this technique. In particular, these calculations permit an examination of acceleration near reconnection regions, as well as the formation and dynamics of the quasi-stable particle ring around Mercury and sputtering as a source of the planet’s exosphere. Simulation results provide a basis for comparison with MESSENGER data from the first two flybys, as well as from the third flyby on 29 September 2009. Title: MHD modeling of the interaction of the magnetosphere of Mercury with the solar wind during the MESSENGER flybys Authors: Benna, M.; Anderson, B. J.; Baker, D.; Boardsen, S. A.; Killen, R. M.; Korth, H.; Krimigis, S. M.; Purucker, M. E.; McNutt, R. L.; Raines, J. M.; McClintock, W. E.; Sarantos, M.; Slavin, J. A.; Solomon, S. C.; Schriver, D.; Travnicek, P.; Zurbuchen, T. Bibcode: 2009AGUFM.P24A..08B Altcode: The MESSENGER spacecraft flybys of Mercury on 14 January 2008 and 6 October 2008 provided a special opportunity to study the magnetosphere of the innermost planet under different solar wind and interplanetary magnetic field conditions. The model presented in this paper is based on the solution of the three-dimensional, multi-fluid magnetohydrodynamic (MHD) equations for solar wind protons and electrons in the absence of mass loading. In this study we provide new estimates of Mercury’s intrinsic magnetic field and the solar wind conditions that prevailed at the time of these two flybys. We show that the location of the boundary layers and the strength of the magnetic field along the spacecraft trajectory are consistent with a planetary magnetic dipole having a magnitude of 210 RM3 nT and an offset of 0.18 RM to the north of the equator, where RM is Mercury’s radius. A comparison between the magnetospheric structures generated under northward and southward interplanetary magnetic field (IMF) orientations confirms that dayside and nightside reconnections are efficient drivers of energy transfer between the solar wind and the magnetosphere. Analysis of the plasma flow reveals the existence of a stable drift belt around the planet; such a belt can account for the locations of diamagnetic decreases observed during both flybys by the MESSENGER Magnetometer. Moreover, we deduce that the variability in the ion impact rate at the cusps as a result of the very different magnetosphere configurations can provide a possible explanation for the variability in the north-south asymmetry of exospheric sodium observed in Mercury’s neutral tail. Title: MESSENGER X-Ray Spectrometer and Energetic Particle Spectrometer Observations of Energetic Electrons during the Mercury Flybys Authors: Starr, R. D.; Ho, G. C.; Anderson, B. J.; Andrews, G. B.; Baker, D.; Gold, R. E.; Krimigis, S. M.; McNutt, R. L.; Nittler, L.; Rhodes, E. A.; Schlemm, C. E.; Slavin, J. A.; Solomon, S. C. Bibcode: 2009AGUFM.P21A1195S Altcode: The X-Ray Spectrometer (XRS) onboard the MESSENGER spacecraft will determine elemental abundances on the surface of Mercury by measuring fluorescent X-ray emissions induced on the planet’s surface by the incident solar X-ray flux. The most prominent fluorescent lines are the Kα lines from the elements Mg, Al, Si, S, Ca, Ti, and Fe (1-10 keV). The Energetic Particle Spectrometer (EPS) observes both ions and electrons (>35 keV) accelerated in Mercury’s magnetosphere. EPS measurements will help characterize magnetospheric-particle contributions to Mercury’s magnetic field, as well as characterize energy conversion processes in the vicinity of, and within, the magnetosphere. Prior to entering orbit about Mercury in March 2011, MESSENGER has flown by the planet three times for spacecraft-trajectory gravity assists and scientific observations. Solar X-ray emissions during the flybys have been an order of magnitude lower than expected, and no X-ray signal has been detected from the planet. Nevertheless, the XRS has measured several count-rate spikes before (by ~5 minutes) and after (~7 minutes) closest approach whose signatures clearly identify their origin as electrons (~10-30 keV) interacting in the XRS detector material. Electron-induced fluorescence and bremsstrahlung are evident in the XRS gas proportional counters. Measured spectra are well modeled by kappa function electron distributions impinging on the XRS Mg and Al filters, Be windows, and Be-Cu collimator. However, no corresponding signal is observed by the EPS for these events. Modeling of at least one of these events suggests sufficient electron flux above 35 keV to be detectable by EPS. A possible scenario is that the XRS detected highly anisotropic and short-duration electron bursts that were not in the EPS field-of-view, implying an exceptionally narrow pitch angle distribution. The energetic electron observations made by the EPS and XRS provide a basis for assessing the electron distributions at Mercury during MESSENGER flybys. Title: Determining Mean Electron Temperature Variation Along Magnetic Field Lines in the Earth's Plasma-sheet Using Multipoint Measurements From Cluster Authors: Presicci, M. R.; Baker, D. Bibcode: 2009AGUFMSM43A1737P Altcode: Multi-point electron temperature measurements from the Cluster constellation of spacecraft orbiting in tetrahedral formation provide a framework for calculating the local electron temperature dependence on plasma sheet location. Separate parallel and perpendicular temperature components may vary strongly along two or even three dominant directions. Nevertheless, six representative plasma sheet crossings using varying Cluster tetrahedron scale sizes indicate the mean temperature variation in a given direction is dominated by the component along a single direction of maximal temperature change. The temperature variation perpendicular to this dominant direction is relatively small. Because plasma transport occurs preferentially along the direction of the magnetic field, it is reasonable to infer the temperature should be constant along B-field lines. However, the observed magnetic field, and Tsyganenko-modeled field for our crossings have significant component along the dominant direction, and so exhibit large temperature variation along B. Temperature variations may persist regardless of plasma mixing in the plasma sheet. Implications for plasma sheet models, Alfven waves, and field-line resonances will be presented based on plasma, energetic particle and magnetic field line detailed analysis. Title: The Space Environment of Mercury at the Time of the Third MESSENGER Flyby: Solar Wind and IMF Modeling of Upstream Conditions Authors: Odstrcil, D.; Baker, D.; Anderson, B. J.; Mayer, L. R.; Slavin, J. A.; Solomon, S. C. Bibcode: 2009AGUFM.P24A..02O Altcode: The third flyby of Mercury by the MESSENGER spacecraft occurred on 29 September 2009. In order to provide contextual information about the solar wind properties and the interplanetary magnetic field (IMF) near the planet, we have used an empirical modeling technique combined with a numerical-physics-based solar wind model. The Wang-Sheeley-Arge (WSA) method uses solar photospheric magnetic field observations (from Earth-based instruments) to estimate inner heliospheric conditions out to 21.5 solar radii from the Sun. This information is then used as input to the global numerical magnetohydrodynamic model, ENLIL, which calculates solar wind velocity, density, temperature, and magnetic field strength and polarity throughout the inner heliosphere. WSA-ENLIL calculations for the several-week period encompassing MESSENGER’s third Mercury flyby provide a critical context for understanding flyby observations and global magnetospheric modeling results. Title: Systematics of Electron Flux Decay Lifetimes in the Outer Radiation Belts Authors: Kanekal, S. G.; Fennell, J.; Baker, D.; Blake, J. B. Bibcode: 2009AGUFMSM23A1584K Altcode: The fluxes of energetic electrons in the outer belt are highly dynamic often varying by several orders of magnitude in a matter of a few days. This variability is the result of balance between energization and loss processes. Wave-particle interactions have long been known to cause particle precipitation. Some of the types of waves responsible for particle loss include the EMIC, and the VLF chorus waves. The latter are thought to be important outside the plasmapause whereas inside the plasmapause EMIC waves cause particle loss due to pitch angle scattering. Particle interactions with different types of waves may result in differeent decay timescales. We will report on investigations of electron flux decay times. The aim our research is to delineate the role played by various plasma waves such as plasmaspheric hiss, chorus and EMIC in electron precipitation leading to flux depletion. Our preliminary investigations show a clustering of decay time scales with a preponderance of lifetimes of 5, 10.5, and 17.5 days albeit for a limited data set. This study will use data from multiple spacecraft such as SAMPEX, Polar and HEO to measure electron flux decay times over the entire outer zone. We will also examine decay times as a function of electron energy and cover electron events over nearly a solar cycle. Such a full and detailed study has the potential to examine the conditions under which distinct decay processes may operate. Title: Building upon the Electronic Geophysical Year (eGY) Experience: Transitioning Research Results to Operations (Invited) Authors: Baker, D. Bibcode: 2009AGUFMSA34A..06B Altcode: The past 15 years have seen the development of many cost effective ways to acquire, store, and exchange data. We have the potential to expand the exchange of data by allowing working scientists and operational agencies to access and manipulate information and models from large interdisciplinary centers as well as from small, previously isolated, research groups. The key to this technology requires adoption of community-developed standards for data storage and description to form an ''Informatics Commons.'' Scientific societies currently promote the establishment of a system of Virtual Observatories. The Electronic Geophysical Year (eGY) concept (2007-2008) embraced all available and upcoming geophysical data (e.g., atmospheric, geomagnetic, ionospheric, magnetospheric, etc.) and advocated organizing them into a series of virtual geophysical observatories deployed in cyberspace. This concept allows access to all available data through the Internet and World Wide Web, taking advantage of existing networking hardware and software technologies (e.g., Internet, XML, Service-Oriented Architectures, Semantic Web, etc.). The eGY provided an international focus for a resolve to address the issues of data release, data discovery, and data preservation. This effort can help revolutionize the transition of basic research to a state of operational readiness. Title: Energetic electrons response to ULF waves induced by interplanetary shocks in the outer radiation belt Authors: Zong, Q.; Li, X.; Zhou, X.; Pu, Z.; Song, P.; Baker, D.; Fritz, T. A.; Daly, P. W.; Dunlop, M. W. Bibcode: 2009AGUFMSM34A..06Z Altcode: Strong interplanetary shock interactions with the Earth's magnetosphere have great impacts on energetic particle dynamics in the magnetosphere. An interplanetary shock on 7 November 2004 (with the maximum solar wind dynamic pressure of ∼ 70 nPa) was observed by the Cluster constellation to induce significant ULF waves in the plasmasphere boundary, and energetic electrons (up to 2 MeV) were almost simultaneously accelerated when the interplanetary shock impinged upon the magnetosphere. In this paper, the relationship between the energetic electron bursts and the large shock-induced ULF waves is studied. It is shown that the energetic electrons could be accelerated and decelerated by the observed ULF wave electric fields, and the distinct wavenumber of the poloidal and toroidal waves at different locations also indicates the different energy ranges of electrons resonating with these waves. For comparison, a rather weak interplanetary shock on 30 August 2001 (dynamic pressure { ∼} 2.7 nPa) is also investigated. It is found that interplanetary shocks or solar wind pressure pulses with even small dynamic pressure change can have a non-negligible role in the radiation belt dynamics. Title: Mercury’s atmosphere and magnetosphere: MESSENGER third flyby observations (Invited) Authors: Slavin, J. A.; Anderson, B. J.; Baker, D.; Benna, M.; Boardsen, S. A.; Johnson, C. L.; Gloeckler, G.; Gold, R. E.; Killen, R. M.; Korth, H.; Krimigis, S. M.; McClintock, W. E.; McNutt, R. L.; Purucker, M. E.; Sarantos, M.; Schriver, D.; Solomon, S. C.; Sprague, A. L.; Vervack, R. J.; Zurbuchen, T.; Travnicek, P. Bibcode: 2009AGUFM.P24A..01S Altcode: MESSENGER’s third flyby of Mercury en route to orbit insertion about the innermost planet took place on 29 September 2009. The earlier 14 January and 6 October 2008 encounters revealed that Mercury’s magnetic field is highly dipolar and stable over the 35 years since its discovery by Mariner 10; that a structured, temporally variable exosphere extends to great altitudes on the dayside and forms a long tail in the anti-sunward direction; a cloud of planetary ions encompasses the magnetosphere from the dayside bow shock to the downstream magnetosheath and magnetotail; and that the magnetosphere undergoes extremely intense magnetic reconnection in response to variations in the interplanetary magnetic field. Here we report on new results derived from observations from MESSENGER’s Mercury Atmospheric and Surface Composition Spectrometer (MASCS), Magnetometer (MAG), and Energetic Particle and Plasma Spectrometer (EPPS) taken during the third flyby. Title: Mercury's magnetosphere-solar wind interaction under northward and southward interplanetary magnetic field during the MESSENGER flybys Authors: Travnicek, P. M.; Schriver, D.; Hellinger, P.; Hercik, D.; Slavin, J. A.; Sarantos, M.; Anderson, B. J.; Korth, H.; Zurbuchen, T.; Baker, D.; Benna, M.; Sprague, A. L.; Killen, R. M.; McClintock, W. E.; Ho, G. C.; Krimigis, S. M.; McNutt, R. L.; Solomon, S. C. Bibcode: 2009AGUFM.P21A1204T Altcode: Analysis of global hybrid simulations of Mercury's magnetosphere--solar wind interaction under northward and southward interplanetary magnetic field (IMF) orientations provides a context for evaluating observations during MESSENGER's first two encounters with Mercury. The global kinetic simulations reveal the basic structure of this interaction, including a bow shock, ion foreshock, magnetosheath, cusp regions, magnetopause, and a closed ion ring belt formed around the planet within the magnetosphere. The two different IMF orientations induce different locations of ion foreshock and different magnetospheric properties: the dayside magnetosphere is smaller and cusps are at lower latitudes for southward IMF than for northward IMF, whereas for southward IMF the nightside magnetosphere is larger and exhibits a thin current sheet with signatures of magnetic reconnection and plasmoid formation. For the two IMF orientations the ion foreshock and quasi-parallel magnetosheath manifest ion-beam-driven large-amplitude oscillations, whereas the quasi-perpendicular magnetosheath shows ion-temperature-anisotropy-driven wave activity. The ions in Mercury's belt remain quasi-trapped for a limited time before they are either absorbed by Mercury's surface or escape from the magnetosphere. Title: The role of Shabansky orbits in the generation of compression-related EMIC waves Authors: McCollough, J. P.; Elkington, S. R.; Baker, D. Bibcode: 2009AGUFMSM43C..08M Altcode: Electromagnetic ion-cyclotron (EMIC) waves arise from temperature anisotropies in trapped warm plasma populations. In particular, EMIC waves at high L values near local noon are often found to be related to magnetospheric compression events. There are several possible mechanisms that can generate these temperature anisotropies: energizing processes, including adiabatic compression and shock-induced and radial transport; and non-energizing processes, such as drift shell splitting and the effects of off-equatorial minima on particle populations. In this work we investigate the role of off-equatorial minima in the generation of temperature anisotropies both at the magnetic equator and at higher latitudes. There are two kinds of behavior particles undergo in response: particles with high equatorial pitch angles (EPAs) are forced to execute so-called Shabanksy orbits and mirror at high latitudes without passing through the equator, and those with lower EPAs will pass through the equator with higher EPAs than before; as a result, perpendicular energies increase at the cost of parallel energies. By using a 3D particle tracing code in a tunable analytic compressed-dipole field, we parameterize the effects of Shabansky orbits on the anisotropy of the warm plasma. These results as well as evidence from simulations of a real event in which EMIC waves were observed (the compression event of 29 June 2007) are presented. Title: The Impact of the Virtual Observatories on Space Weather Science, Modeling, and Predictions (Invited) Authors: Green, J. C.; Weigel, R. S.; Kihn, E. A.; Baker, D. Bibcode: 2009AGUFMSH54A..04G Altcode: Five years ago, the NASA Living with a Star program funded a group of Virtual Observatories intended to “integrate data and models across many missions, data centers, agencies and countries”. Each observatory was designed to meet the unique needs of specific heliophysics research communities. One of the observatories funded under this program, that will be the main focus of this presentation, was the Virtual Radiation Belt Observatory. This observatory was to accelerate science and modeling by helping scientists overcome research challenges such as the lack of publicly available observational and model data, data inter-calibration differences, and limited access to common analysis tools. The research advancements were expected to feed-back into better models that ultimately would benefit space weather users such as satellite operators and designers. Using ViRBO as the main example, this presentation will demonstrate how the virtual observatories have benefited the space weather community and identify areas for possible improvement. We review the initial vision for the observatories, present their current implementation, and provide example cases describing how the observatories have been successfully used. Title: A Remarkable Natural Experiment: The Extremely Quiet Sun (2007-2009) and its Effect on Earth's Radiation Belts Authors: Farr, N. L.; Baker, D.; Kanekal, S. G.; Li, X. Bibcode: 2009AGUFMSM21B..05F Altcode: In late 2008 and into 2009, the Earth’s electron radiation belts have virtually disappeared. This is unprecedented in the observational record. The Sun has been going through its most profound minimum of activity in the modern era. The paucity of sunspot activity and the associated absence of major solar coronal mass ejections has, in turn, meant that no large geomagnetic storms or other such space weather events have occurred within the Earth’s magnetosphere. The minimum of solar activity has led to an almost complete cessation of external drivers - and the radiation regions around the Earth (the Van Allen radiation belts) have thereby attained their most reduced, quiescent state ever directly witnessed. The events now underway with the quiet Sun offer a rich opportunity to see how quickly, effectively, and completely the radiation belts can naturally be depleted toward their putative ground state. We observe that the electron radiation belt fluxes (E > 2 MeV) in 2009 have been reduced by a factor of 10 4-10 5-compared to 2003-2004. Moreover, the slot region between the inner and outer Van Allen belts has spread outward to L > 4, thereby making a broad region devoid of electrons in what previously was the heart of the outer zone. Title: Severe Space Weather Events: Global Geospace Responses to Powerful Solar Wind Drivers (Invited) Authors: Baker, D. Bibcode: 2009AGUFMSM34A..05B Altcode: Recent international space science programs have made a concerted effort to study activity on the Sun, the propagation of energy bursts from the Sun to near-Earth space, energy coupling into the magnetosphere, and its redistribution and deposition in the upper and middle atmosphere. Extreme solar, geomagnetic and solar wind conditions can be observed by a large international array of satellites and ground-based sensors. We discuss the types of space weather-related problems that have been identified in recent times and consider examples of space weather-induced spacecraft (and ground-based) anomalies and failures that affect both civilian and military systems. Special attention will be given to delineating the specific kinds of geospace responses that occur for different transient solar wind drivers. In this context, we discuss near-term plans to consolidate and integrate understanding as an important component of the community effort to propose technical and operational solutions to space weather problems. I will focus on new scientific advancement that is needed for successful space weather programs and will describe actions that can help assure a good future integrated space weather program. Title: Magnetic Reconnection along Quasi-separatrix Layers as a Driver of Ubiquitous Active Region Outflows Authors: Baker, D.; van Driel-Gesztelyi, L.; Mandrini, C. H.; Démoulin, P.; Murray, M. J. Bibcode: 2009ApJ...705..926B Altcode: 2009arXiv0909.4738B Hinode's EUV Imaging Spectrometer (EIS) has discovered ubiquitous outflows of a few to 50 km s-1 from active regions (ARs). These outflows are most prominent at the AR boundary and appear over monopolar magnetic areas. They are linked to strong non-thermal line broadening and are stronger in hotter EUV lines. The outflows persist for at least several days. Using Hinode EIS and X-Ray Telescope observations of AR 10942 coupled with magnetic modeling, we demonstrate that the outflows originate from specific locations of the magnetic topology where field lines display strong gradients of magnetic connectivity, namely quasi-separatrix layers (QSLs), or in the limit of infinitely thin QSLs, separatrices. We found the strongest AR outflows to be in the vicinity of QSL sections located over areas of strong magnetic field. We argue that magnetic reconnection at QSLs separating closed field lines of the AR and either large-scale externally connected or "open" field lines is a viable mechanism for driving AR outflows which are likely sources of the slow solar wind. Title: Signatures of interchange reconnection: STEREO, ACE and Hinode observations combined Authors: Baker, D.; Rouillard, A. P.; van Driel-Gesztelyi, L.; Démoulin, P.; Harra, L. K.; Lavraud, B.; Davies, J. A.; Opitz, A.; Luhmann, J. G.; Sauvaud, J. -A.; Galvin, A. B. Bibcode: 2009AnGeo..27.3883B Altcode: 2009arXiv0909.5624B Combining STEREO, ACE and Hinode observations has presented an opportunity to follow a filament eruption and coronal mass ejection (CME) on 17 October 2007 from an active region (AR) inside a coronal hole (CH) into the heliosphere. This particular combination of "open" and closed magnetic topologies provides an ideal scenario for interchange reconnection to take place. With Hinode and STEREO data we were able to identify the emergence time and type of structure seen in the in-situ data four days later. On the 21st, ACE observed in-situ the passage of an ICME with "open" magnetic topology. The magnetic field configuration of the source, a mature AR located inside an equatorial CH, has important implications for the solar and interplanetary signatures of the eruption. We interpret the formation of an "anemone" structure of the erupting AR and the passage in-situ of the ICME being disconnected at one leg, as manifested by uni-directional suprathermal electron flux in the ICME, to be a direct result of interchange reconnection between closed loops of the CME originating from the AR and "open" field lines of the surrounding CH. Title: Myths and Mysteries of Solar Wind Speed and MeV Electrons in the Magnetosphere Authors: Li, X.; Baker, D. Bibcode: 2009EGUGA..11.2554L Altcode: The remarkable correlation between high speed solar wind and the enhancement of energetic electrons in the magnetosphere has been identified for over four decades, yet the mystery of this correlation remains. Recently, several interpretations about this correlation have been proposed and most of them are incomplete and some of them may have generated the widespread verdict (or myth) that enhanced ULF waves alone lead to enhanced MeV electrons in the radiation belts. In this presentation, we present a brief review of the association of high speed solar wind and energetic electrons across the entire relevant energy range (10s of keV to multi-MeV) and magnetospheric region (from inner magnetosphere to cental plasmasheet). We discuss the incompleteness of existing interpretations and we describe a more complete picture in understanding this mystery. Title: Simulations of emerging flux in a coronal hole: oscillatory reconnection Authors: Murray, M. J.; van Driel-Gesztelyi, L.; Baker, D. Bibcode: 2009A&A...494..329M Altcode: Context: Observations and simulations show that reconnection will take place when a flux tube emerges into a coronal hole, which is characterised by magnetic fieldlines “open” towards interplanetary space. Although the mechanism by which reconnection is initiated has been thoroughly studied, the long-term evolution of this reconnecting magnetic system remains unreported.
Aims: We aim to understand the long-term evolution of the reconnecting flux tube and coronal hole system and, in particular, to ascertain whether it can reach an equilibrium state in which all reconnection has ceased. By determining the evolution in this particular scenario, we aim to be able to select a subset from the broad spectrum of reconnecting systems, which will undergo the same progression to equilibrium.
Methods: Using a 2.5-dimensional numerical magnetohydrodynamic (MHD) code, we evolve a simple stratified atmospheric domain, which is endowed with a vertical magnetic field, representing the interior of a coronal hole, and a horizontal buoyant flux tube that is placed near the bottom of the domain. To investigate the long-term evolution of the system, we continue to study the domain long after the flux tube has emerged and reconnection has commenced between the magnetic fields of the flux tube and coronal hole.
Results: We find that a series of reconnection reversals (or oscillatory reconnection) takes place, whereby reconnection occurs in distinct bursts and the inflow and outflow magnetic fields of one burst of reconnection become the outflow and inflow fields in the following burst of reconnection, respectively. During each burst of reconnection the gas pressure in the bounded outflow regions increases above the level of that in the inflow regions and, eventually, gives rise to a reconnection reversal. In consecutive bursts of reconnection, the contrast in the gas pressure across the boundaries of the inflow and outflow regions decreases and, over time, the system settles towards equilibrium. Once the equilibrium state is reached, all reconnection ceases. This is the first reported instance of oscillatory reconnection initiated in a self-consistent manner, and the signatures of the mechanism compare favourably with observations of select flux emergence events and with solar and stellar flares.
Conclusions: Across the broader spectrum of reconnecting systems, oscillatory reconnection will only occur if the outflow regions are quasi-bounded during each burst of reconnection. The swaying outflow jet and periodic heating signatures of oscillatory reconnection are exceedingly similar to those exhibited by MHD modes and, in many observations, distinction between the two mechanisms may be impossible. Title: Hinode EIS and XRT Observations of Hot Jets in Coronal Holes - Does the Plasma Escape? Authors: Baker, D.; van Driel-Gesztelyi, L.; Kamio, S.; Culhane, J. L.; Harra, L. K.; Sun, J.; Young, P. R.; Matthews, S. A. Bibcode: 2008ASPC..397...23B Altcode: X-ray jets have been detected in the extreme ultraviolet (EUV) and soft X-ray observations of Hinode's EIS and XRT instruments. Both instruments were used to observe the jets in polar and on-disk coronal holes (CHs). Here, we present a multi-wavelength study of an X-ray jet and its associated bright point found in an equatorial CH on 19 June 2007. Light curves (LCs) in 22 different emission lines were compared to that of Hinode/XRT. As we found in a previous study of two polar X-ray jets, this jet shows a post-jet increase in its EUV LCs. The post-jet enhancement appears cooler than the jet. We suggest this feature arises because the hot plasma of the jet, having failed to reach escape speeds, cools and falls back along the near vertical paths expected to be created by reconnection with open field lines of CHs. In addition to the increase in post-jet EUV intensity, we found tentative evidence of impact heating possibly caused by the fall-back of plasma. Title: Kriging Interpolation Algorithm for Displaying Global SABER Infrared Measurements Authors: Williams, J.; Coakley, H.; Baker, D.; Mlynczak, M.; Russell, J., III Bibcode: 2008AGUSMSA41B..06W Altcode: Three-dimensional atmospheric measurements from satellites are typically unevenly sampled in resolution for both time and space. To create a global representation for atmospheric trends analysis, an interpolation method was implemented using SABER data from the NASA TIMED satellite. A hybrid Kriging processing method was developed and validated. This method shows significant improvements over a linear interpolation model. Hybrid Kriging uses an adaptive statistical least-squares approach to best give a continuous model of the relationship between discrete data points. The algorithm has been rendered less processing intensive, validated using infrared atmospheric data from the SABER multi-channel scanning radiometer, and then displayed for scientific analysis. Title: Outflows at the Edges of Active Regions: Contribution to Solar Wind Formation? Authors: Harra, L. K.; Sakao, T.; Mandrini, C. H.; Hara, H.; Imada, S.; Young, P. R.; van Driel-Gesztelyi, L.; Baker, D. Bibcode: 2008ApJ...676L.147H Altcode: The formation of the slow solar wind has been debated for many years. In this Letter we show evidence of persistent outflow at the edges of an active region as measured by the EUV Imaging Spectrometer on board Hinode. The Doppler velocity ranged between 20 and 50 km s-1 and was consistent with a steady flow seen in the X-Ray Telescope. The latter showed steady, pulsing outflowing material and some transverse motions of the loops. We analyze the magnetic field around the active region and produce a coronal magnetic field model. We determine from the latter that the outflow speeds adjusted for line-of-sight effects can reach over 100 km s-1. We can interpret this outflow as expansion of loops that lie over the active region, which may either reconnect with neighboring large-scale loops or are likely to open to the interplanetary space. This material constitutes at least part of the slow solar wind. Title: Erratum: "Outflows at the Edges of Active Regions: Contribution to Solar Wind Formation?" (ApJ, 676, L147 [2008]) Authors: Harra, L. K.; Sakao, T.; Mandrini, C. H.; Hara, H.; Imada, S.; Young, P. R.; van Driel-Gesztelyi, L.; Baker, D. Bibcode: 2008ApJ...677L.159H Altcode: No abstract at ADS Title: Interaction between emerging flux and coronal hole - observations and simulations Authors: van Driel-Gesztelyi, Lidia; Baker, Deborah; Murray, Michelle; Demoulin, Pascal; Attrill, Gemma; Matthews, Sarah A.; Mandrini, Cristina H.; Toeroek, Tibor Bibcode: 2008cosp...37.3288V Altcode: 2008cosp.meet.3288V Flux emergence in the vicinity of or inside a coronal hole (CH) is expected to induce magnetic reconnection between the closed emerging and open CH magnetic field lines, resulting in an evolution of the CH as formerly closed field lines become topologically open, while at the same time, open field lines close down. Through two case studies we show observational signatures of this (interchange) reconnection process and discuss its implications. First, using SOHO EIT and MDI data, we study a small active region (AR10869) emerging in the close vicinity of a low-latitude coronal hole in April 2006. The interfacing magnetic polarities between the AR and the CH were opposite, favourable for magnetic reconnection. We indeed observe the coupled formation of bright closed loops between the CH and the AR and coronal dimming on the far side of the AR, which we interpret as evidence of interchange reconnection. This process effectively modifies the CH boundary (making it retreat), while simultaneously displacing open field lines to the far side of the AR. In order to study this process in detail, we perform 2.5D MHD simulations, which qualitatively reproduce important aspects of the observations. We expect to find upflows of plasma at the location where previously closed field lines are opening up as well as on the reconnecting side, but since we had no spectroscopic data for this event, we can not verify this. Therefore we analyze Hinode/EIS line-of-sight velocity maps of another low-latitude CH with a small AR in its midst observed on 18 Oct. 2007. We find that while closed loops of the bipole are dominated by downflows in the Fe XII, Fe XIII and Fe XV lines, the strongest coronal plasma upflows are indeed located around and particularly at the "far side" of the bipolar AR, i.e. having the same polarity as the dominant polarity of the CH. The emerging biplole and the series of interchange reconnections it induces create a significant additional plasma upflow in the CH, thus we identify this outflow must contribute to the acceleration of the fast solar wind. Title: In situ observation of radiation belt particle response to an interplanetary shock Authors: Zong, Q.; Zhou, X.; Song, P.; Li, X.; Baker, D.; Fritz, T. Bibcode: 2007AGUFMSM33C..03Z Altcode: Interplanetary shock is one of the most powerful drivers of magnetic storms which often result in strong energetic particles enhancements and the Van Allen radiation belt compression in the magnetosphere. The elevated fluxes of the energetic particles have been proven to be number one threat to space technological systems. How these particles are accelerated is an important and active research subject in space physics. In this study we show that after an interplanetary shock impact on the magnetosphere, the acceleration of the energetic electrons started nearly immediately in the radiation belt and lasted a few hours. Title: Hinode EUV Study of Jets in the Sun's South Polar Corona Authors: Culhane, Len; Harra, Louise K.; Baker, Deborah; van Driel-Gesztelyi, Lidia; Sun, Jian; Doschek, George A.; Brooks, David H.; Lundquist, Loraine L.; Kamio, Suguru; Young, Peter R.; Hansteen, Viggo H. Bibcode: 2007PASJ...59S.751C Altcode: A number of coronal bright points and associated plasma jet features were seen in an observation of the South polar coronal hole during 2007 January. The 40" wide slot was used at the focus of the Hinode EUV Imaging Spectrometer to provide spectral images for two of these events. Light curves are plotted for a number of emission lines that include He II 256Å (0.079MK) and cover the temperature interval from 0.4MK to 5.0MK. Jet speed measurements indicate values less than the escape velocity. The light curves show a post-jet enhancement in a number of the cooler coronal lines indicating that after a few minutes cooling, the plasma fell back to its original acceleration site. This behavior has not been previously observed by e.g., the Yohkoh Soft X-ray Telescope due to the comparatively high temperature cut-off in its response. The observations are consistent with the existing models that involve magnetic reconnection between emerging flux and the ambient open field lines in the polar coronal hole. However we do not have sufficient coverage of lines from lower temperature ion species to register the Hα-emitting surge material that is associated with some of these models. Title: Meteorite Collection on the Lunar Surface Authors: Erikson, L.; Baker, D.; Rance, W. L.; Spahr, E.; Abbud-Madrid, A.; Heeley, M. B. Bibcode: 2007LPICo1371.3052E Altcode: 2007eelo.work.3052E No abstract at ADS Title: Evidence for interchange reconnection between a coronal hole and an adjacent emerging flux region Authors: Baker, D.; van Driel-Gesztelyi, L.; Attrill, G. D. R. Bibcode: 2007AN....328..773B Altcode: Coronal holes are regions of dominantly monopolar magnetic field on the Sun where the field is considered to be `open' towards interplanetary space. Magnetic bipoles emerging in proximity to a coronal hole boundary naturally interact with this surrounding "open" magnetic field. In the case of oppositely aligned polarities between the active region and the coronal hole, we expect interchange reconnection to take place, driven by the coronal expansion of the emerging bipole as well as occasional eruptive events. Using SOHO/EIT and SOHO/MDI data, we present observational evidence of such interchange reconnection by studying AR 10869 which emerged close to a coronal hole. We find closed loops forming between the active region and the coronal hole leading to the retreat of the hole. At the same time, on the far side of the active region, we see dimming of the corona which we interpret as a signature of field line `opening' there, as a consequence of a topological displacement of the `open' field lines of the coronal hole. Title: Hinode Euv Study Of Jets In The Sun’s South Polar Corona Authors: Culhane, J. L.; Brooks, D. H.; Doschek, G. A.; Harra, L. K.; van Driel-Gesztelyi, L.; Baker, D.; Lundquist, L. L.; Hansteen, V. H.; Kamio, S. Bibcode: 2007AAS...210.7201C Altcode: 2007BAAS...39..178C Using the Hinode EUV Imaging Spectrometer coronal jets were observed on 20-JAN-2007 over a range of emission lines and corresponding plasma temperatures using the 40 arc sec wide slot images. In this preliminary analysis, jet plasma temperature and emissivity have been estimated while, based on assumptions about the jet morphology, electron density estimates are given and jet velocity measured. The evolution of the jets will be followed in a number of different EUV emission lines and jet energy input as a function of time will be assessed with reference to the magnetic field topologies involved. Title: Energy Transport, Storage, and Dissipation in the Magnetosphere During Substorms. Authors: Halford, A. J.; Baker, D.; Weygand, J. Bibcode: 2007AGUSMSM53A..04H Altcode: Magnetospheric substorms represent a global interaction between the solar wind, magnetosphere, and ionosphere. Energy transported from the solar wind into the magnetosphere is largely stored in the tail until it is released (primarily into the ionosphere and the ring current). The Akasofu epsilon parameter (ɛ=4π L / μ v B2 sin 4 θ / 2), and multiple empirically determined formulas for energy dissipation into the ionosphere (joule heating and particle precipitation) and the ring current have been considered for such global interactions. An energy budget and estimation of total energy in the tail has been created for 12 isolated substorms that occurred during 2001. Considerable complexity and individuality of substorms is observed with substantial differences in the input and dissipation pattern for individual events. Our analysis is compared with previous published results. Title: The D-CIXS X-ray spectrometer on the SMART-1 mission to the Moon—First results Authors: Grande, M.; Kellett, B. J.; Howe, C.; Perry, C. H.; Swinyard, B.; Dunkin, S.; Huovelin, J.; Alha, L.; D'Uston, L. C.; Maurice, S.; Gasnault, O.; Couturier-Doux, S.; Barabash, S.; Joy, K. H.; Crawford, I. A.; Lawrence, D.; Fernandes, V.; Casanova, I.; Wieczorek, M.; Thomas, N.; Mall, U.; Foing, B.; Hughes, D.; Alleyne, H.; Russell, S.; Grady, M.; Lundin, R.; Baker, D.; Murray, C. D.; Guest, J.; Christou, A. Bibcode: 2007P&SS...55..494G Altcode: The SMART-1 mission has recently arrived at the Moon. Its payload includes D-CIXS, a compact X-ray spectrometer. SMART-1 is a technology evaluation mission, and D-CIXS is the first of a new generation of planetary X-ray spectrometers. Novel technologies enable new capabilities for measuring the fluorescent yield of a planetary surface or atmosphere which is illuminated by solar X-rays. During the extended SMART-1 cruise phase, observations of the Earth showed strong argon emission, providing a good source for calibration and demonstrating the potential of the technique. At the Moon, our initial observations over Mare Crisium show a first unambiguous remote sensing of calcium in the lunar regolith. Data obtained are broadly consistent with current understanding of mare and highland composition. Ground truth is provided by the returned Luna 20 and 24 sample sets. Title: End-to-End Modeling of the Solar Terrestrial System Authors: Wiltberger, M.; Baker, D. Bibcode: 2007sdeh.book..217W Altcode: No abstract at ADS Title: Temporal variability of the MLTI region observed through five years of SABER and TIMED Authors: Remsberg, E. E.; Williams, J.; Turpin, T.; Mlynczak, M. G.; Russell, J. M.; Baker, D. Bibcode: 2006AGUFMSA24A..07R Altcode: The Sounding of the Atmosphere using Broadband Emission Radiometry instrument has achieved nearly five years of flawless operation on the NASA Thermosphere Ionosphere Mesosphere Energetics and Dynamics (TIMED) satellite. The instrument offers an unprecedented data set of over thirty products including, temperature, density, ozone, atomic species, and thermodynamic parameters. The SABER data exhibit clear signals associated with the decline of the current phase of the solar cycle, particularly in the thermosphere and the NO(v) emission at 5.3 um, which is observed to decrease by a factor of 2.5 since early 2002. Also examined are the evolution of the thermal structure and chemical composition during the five years in orbit. Mesospheric temperatures are observed to decrease over the period, with the largest decreases observed at the highest altitudes measured by SABER. These measurements will be reviewed and placed in the context of the atmospheric response to solar variability. Title: The Electric Field Wave Instrument on the Radiation Belt Storm Probe Mission Authors: Wygant, J. R.; Cattell, C. A.; Dombeck, J.; Bonnell, J.; Mozer, F.; Bale, S.; Chaston, C.; Ergun, B.; Baker, D.; Li, X.; Hudson, M. K.; Strangeway, R.; Alpert, J.; Brautigam, D.; Mann, I.; Foster, J. Bibcode: 2006AGUFMSM33A0331W Altcode: The purpose of the Electric Field-Wave Instrument on the two RBSP spacecraft is to investigate the role of plasma structures and waves in the physical processes responsible for the acceleration, transport, and loss of energetic particles in the inner magnetosphere of the Earth. Some of these processes include: prompt acceleration induced by powerful interplanetary shocks, acceleration by the large scale convection electric field, abrupt energization by intense substorm injection fronts propagating in from the tail, coherent and stochastic radial transport by large scale MHD fluctuations, multi-step local energization and cattering by whistler waves, and scattering and energization by kinetic Alfven waves, ion cycltron waves, and other small scale waves and structures. In order to understand the role of these processes in accelerating particles, the EFW instrument measures the three dimensional electric field from dc to greater than 500 kHz. The spin plane electric field vector is obtained from spherical sensors at the ends of two pair of orthogonal booms with tip-to- tip separations of 80 and 100 m. The spin axis measurement is obtained by opposed stacer booms with a tip- to-tip separation of 12 meters or greater. The electric field below 12 Hz is telemetered continuously while higher time resolution is obtained from a programmable burst memory with a maximum sampling rate for six quantities of greater 30,000 samples/s each. DC magnetic fields from the fluxgate magnetometer and wave magnetic fields from the search coil, both associated with the University of Iowa Instrument are input into the EFW instrument for processing in the burst memory and in the Digital Signal Processing Board (DSP). The DSP provides wave spectra and cross spectra of electric and magnetic field data over the frequency range between 50 Hz and 10 kHz with a typical cadence of once per 12 seconds with a maximum rate of ~ 1 Hz in order to provide continuous information on wave properties including: the wave power, the normal direction, the phase velocity, the waves electrostatic or electro-magnetic structure, the longitudinal component of the electric field, the parallel component of the electric field, and Poynting flux. The EFW instrument also provides a wave electric field signal to the University of Iowa Instrument. Title: The Radiation Belt Storm Probes (RBSP) Energetic Particle, Composition, and Thermal Plasma (ECT) Instrument Suite Authors: Spence, H. E.; Kepko, E.; Reeves, G.; Funsten, H.; Thomsen, M.; Henderson, M.; Friedl, R.; Skoug, R.; Jordanova, V.; Fennell, J.; Blake, J. B.; Clemmons, J.; O'Brien, T.; Green, J.; Onsager, T.; Elkington, S.; Baker, D.; Li, X.; Goldstein, J.; Young, D.; Jahn, J.; Thorne, R.; Hudson, M.; Horne, R.; Bourdarie, S.; Mann, I. Bibcode: 2006AGUFMSM33A0335S Altcode: The Energetic particle, Composition, and Thermal plasma (ECT) instrument suite was selected recently by NASA as part of the Radiation Belt Storm Probe (RBSP) mission. In this presentation, we summarize the RBSP-ECT science investigation. The ECT suite contains a well-proven complement of particle instruments to ensure the highest quality measurements in the inner magnetosphere. The coordinated ECT particle measurements, analyzed in combination with fields and waves observations and state-of-the-art theory and modeling, are required for understanding the acceleration, global distribution, and variability of radiation belt electrons and ions, key science objectives of NASA's Living With a Star program and the RBSP mission. ECT has four science objectives, which consolidate the eight prioritized RBSP mission objectives. They are: (1) determine the physical processes that produce radiation belt enhancements; (2) determine the dominant mechanisms for relativistic electron loss; (3) determine how the inner magnetospheric plasma environment controls radiation belt acceleration/loss; and, (4) develop empirical and physical models for understanding/predicting radiation belt space weather effects. In this poster, we present an overview of the science and measurements goals of the ECT suite as well as the instruments required to achieve those goals. Title: Fuel Oxidizer Reaction Products (FORP) Contamination of Service Module and Release of N-Nitrosodimethylamine in a Humid Environment from Crew EVA Suits Contaminated with FORP Authors: Schmidl, W.; Mikatarian, R.; Lam, C. -W.; West, B.; Buchanan, V.; Dee, L.; Baker, D.; Koontz, S. Bibcode: 2006pmss.book..193S Altcode: No abstract at ADS Title: End-to-End Modeling of the Solar Terrestrial System Authors: Wiltberger, M.; Baker, D. Bibcode: 2006SSRv..124..217W Altcode: 2007SSRv..tmp...54W Traditionally modeling for space science has concentrated on developing simulations for individual components of the solar terrestrial system. In reality these regions are coupled together. This coupling can be as simple as the driving of the magnetosphere ionosphere thermosphere system by the solar wind or as a complicated as the feedback of the ionospheric conductivity and currents on the magnetosphere. As part of the CISM project we are beginning a concentrated effort to compressively model the entire system. This approach includes chains of models. In the first chain physics based numerical models are utilized while in the second chain empirical models are coupled together. The first half of this paper discusses the numerical modeling approach by highlighting the coupling of pairs of regions within the system. In the second section we present results from empirical models which are combined to make long term forecasts of conditions in the geospace environment. It is expected that a validated and reliable forecast model for space weather can be obtained by combining the strongest elements of each chain. Title: Modeling the Self-Organized Critical Behavior of Earth's Plasma Sheet Reconnection Dynamics Authors: Klimas, A.; Uritsky, V.; Baker, D. Bibcode: 2006AGUSMSM22A..02K Altcode: Analyses of Polar UVI auroral image data (Uritsky et al. JGR, 2002; GRL, 2003, 2006) show that bright night- side high-latitude UV emissions exhibit so many of the key properties of systems in self-organized criticality that an alternate interpretation has become virtually impossible. It is now necessary to find and model the source of this behavior. We note that the most common models of self-organized criticality are numerical sandpiles. These are, at root, models that govern the transport of some quantity from a region where it is loaded to another where it is unloaded. Transport is enabled by the excitation of a local threshold instability; it is intermittent and bursty, and it exhibits a number of scale-free statistical properties. Searching for a system in the magnetosphere that is analogous and that, in addition, is known to produce auroral signatures, we focus on the reconnection dynamics of the plasma sheet. In our previous work, a driven reconnection model has been constructed and has been under study (Klimas et al. JGR, 2004; GRL 2005). The transport of electromagnetic (primarily magnetic) energy carried by the Poynting flux into the reconnection region of the model has been examined. All of the analysis techniques, and more, that have been applied to the auroral image data have also been applied to this Poynting flux. Here, we report new results showing that this model also exhibits so many of the key properties of systems in self-organized criticality that an alternate interpretation is implausible. Further, we find a strong correlation between these key properties of the model and those of the auroral UV emissions. We suggest that, in general, the driven reconnection model is an important step toward a realistic plasma physical model of self-organized criticality and we conclude, more specifically, that it is also a step in the right direction toward modeling the multiscale reconnection dynamics of the magnetotail. Title: Energetic Particle Modulation in the Radiation Belt Region Authors: Zong, Q.; Fritz, T.; Baker, D.; Li, X.; Balogh, A.; Reme, H. Bibcode: 2006AGUSMSM52A..05Z Altcode: One of open questions in the Earth's radiation belt is to determine which processes dominant in accelerating magnetospheric several keV electrons to MeV energies. In particular recent studies have emphasized the question of the relative dominance of ULF and VLF wave acceleration processes across the outer belt. Energetic electron and ion flux and spectra variations associated with ULF waves in the inner magnetosphere have been examined by using Cluster spacecraft data. The quasi-periodic particle flux (electron 30 keV to 500 keV, proton 30 keV to 1.5 MeV) modulations are observed in the the region of L=5.3 to 11.7 at MLT=8. The relative phase of energetic electron and ion are different in the different location, also, depend on the energy of the particles. The particle fluxes were found to be either 90 or 270 out of phase with the magnetic variations. For the phase difference between the ion density and the magnetic variation, this argues that the time-average Poynting flux of the Pc5 wave along the ambient magnetic field is approximately zero, this indicates that Pc5 waves are standing waves along the field line. In-situ ULF measurements from inside geosynchronous orbit are not commonly available. Multi-point measurements of the ULF wave electric and magnetic field morphology, as well as radiation belt particle flux, are made in this paper to examine the efficiency of the ULF process in the outer belt. Cluster constellation allow to determine wave coherence length and mode structure, which are critical parameters for determining the efficiency of the ULF wave drift-resonance interaction. Title: Open exchange of data: the eGY pathway towards capacity building. Authors: Barton, C.; Baker, D.; Cobabe-Ammann, E.; Fox, P.; Kihn, E.; Peterson, W. K. Bibcode: 2006cosp...36.2387B Altcode: 2006cosp.meet.2387B The Electronic Geophysical Year 2007-2008 eGY uses the 50-year anniversary of the acclaimed International Geophysical Year to advance open access to data information and services The International Polar Years of 1882-1882 and 1932-1933 taught us that free and open exchange of data between nations is cost effective The International Geophysical Year 1957-1958 taught us that free and open exchange of data between scientific disciplines generates new and exciting research The worldwide network of data centers and data standards initiated during IGY continues to foster research to this day And better things lie ahead As we approach the 50th anniversary of the IGY the development of distributed data systems allows worldwide connectivity to data and services at a level never before possible Such systems virtual observatories and so forth expand the free open and cross-disciplinary exchange of data by allowing users worldwide to access and manipulate data from principal data centers as well as from small previously isolated research groups The new information and communication technologies require that we adopt community-developed standards for data storage and description They also demand that we recognize and accommodate the shift in effort from the user to the provider that accompanies a change from the traditional user-pull to a modern provider-push data environment eGY provides an opportunity for coordinated discussions on data storage and description standards These standards have implications for the infrastructure needed to access and Title: Outward radial diffusion during the main phase of a storm Authors: Shprits, Y.; Thorne, R.; Friedel, R.; Reeves, G.; Fennell, J.; Baker, D.; Kanekal, S. Bibcode: 2006cosp...36.1089S Altcode: 2006cosp.meet.1089S The variability of the radiation belt electron fluxes is a result of a competition between various source and loss processes which highly depend on the evolution of the plasmaspheric and ring current plasma populations Relativistic electrons can be accelerated by the inward radial diffusion which is most efficient at higher L-shells and by local acceleration which is most efficient right outside plasmasphere Losses of relativistic electrons may result from pitch angle scattering of electrons by various plasma waves and losses to magnetopause Using observations from CRRES HEO and SAMPEX satellites and radial diffusion modeling we show that magnetopause losses combined with outward radial diffusion may produce significant depletions of the outer radiation belt down to L 4 We also show that radial diffusion driven by gradients in phase space density redistributes radiation belt fluxes and may effectively work as a loss and source process Title: High Resolution Substorm Energetic Electrons seen in the Magnetotail by all 4 CLUSTER satellites Authors: Wu, P.; Fritz, T. A.; Reed, R. S.; Friedel, R.; Reeves, G.; Baker, D.; Daly, P. Bibcode: 2005AGUFMSM32A..04W Altcode: We report our examination of the 3-D pitch angle distributions (PAD) of energetic electrons as the Cluster satellites cross the earth's plasma sheet near their apogee in the nightside magnetosphere during the tail season (July, August, September, October) of year 2005. We identified several energetic electron injections in the tail plasma sheet associated with substorm events. Those events are all associated with continual switching of PADs from field aligned to the peak at 90 degree, which indicated to us that those energetic electrons are accelerated in different manners and they form different populations. The study of the evolution of the PAD gave us an impression that the Fermi and betatron accelerations play different roles along the tail. They compete with each other, depend on the radial distance. However, this idea needs to be further verified with the study of more events. The large separations of the 4 Cluster satellites in this tail season of 2005 provide a good opportunity for us to identify more energetic electron bursts events with better spatial and temporal clarity. Comparing the observation from these 4 different satellites will allow us to visualize the picture in many more dimensions and avoid vagueness as much as we can. Together with our collaboration with LANL and LASP, including more satellite data (e.g. Geosynchronous satellites, POLAR, IMAGE), we will report on a more integrated picture of the magnetotail energetic electron dynamics. Title: Earthward Flowing Plasmoid: Structure and Its Related Auroral Signature Authors: Fritz, T.; Zong, Q.; Baker, D.; Goldstein, M.; Daly, P.; Fu, S.; Frey, H.; Balogh, A.; Reme, H. Bibcode: 2005AGUFMSM24A..03F Altcode: An earthward-moving plasmoid on Oct. 28, 2002 has been observed by the Cluster spacecraft with simultaneous auroral viewing by IMAGE satellite. This offers the opportunity to ascertain the optical signature and its evolution in the ionosphere of an earthward moving plasmoid for the first time. The intensity of the current in the center of the plasmoid is found to be weaker than that in the adjacent region. Also, the directions of the current in the central part of the plasmoid are different from the background cross-tail current: they are more field-aligned. The calculation of J × B demonstrates that the plasmoid is not a highly force-free structure. The unusually large bipolar electric field found in the plasmoid (peak to peak values 6 and 8 mV/m) can be explained as a dawn-dusk polarization electric field is generated to enhance the flows as predicted in the bubble model. Broad-band electrostatic noise (BEN) and bursty electrostatic electron cyclotron waves are found inside the plasmoid which are closely associated with the acceleration of the plasma. Furthermore, IMAGE data show the auroral forms moving to lower latitude, which is when an earthward moving plasmoid observed by the Cluster spacecraft. Such an equatorward auroral motion is consistent well with the observed earthward moving plasmoid. Title: Global statistics of OH layer heights and double layers from SABER limb measurements of OH Meinel emission at 1.6 and 2.0 μm. Authors: Winick, J. R.; Wintersteiner, P. P.; Picard, R. H.; Taylor, M. J.; Baker, D.; Mylnczak, M. G.; Russell, J. M.; Gordley, L. L. Bibcode: 2005AGUFMSA43A1095W Altcode: Two of the 10 radiometers on the SABER instrument aboard the TIMED spacecraft measure the limb profiles from the OH Meinel first-overtone bands at 2.0 μm (OH-A) and at 1.6 μm (OH-B). The OH-A band originates from high-lying vibrational states (v=8-9) of the OH ground electronic state, while the OH-B band originates from low-lying vibrational states (v=3-5). These provide limb radiance profiles continuously over a latitude range 53S-82N or 82N-53S, depending upon the phase of the yaw cycle. We have examined important characteristics of the volume emission rate (VER) profiles of these bands that have been obtained by inverting the radiance profiles. In particular, we characterize the global occurrence probabilities of the heights of both layers as a function of latitude, local time and season and note any differences in behavior between the two bands. Although the OH layer is often considered to be a fixed profile with a narrow peak near 87 km, a significant number of the profiles show distinctly different behavior. Melo et al. (JGR, 2000) reported that double-peaked layers were found in UARS/WINDI data 5-25% of the time. SABER also sees double layers at least 10% of the time and observes the peak VER at times below 80 km, altitudes not observed in the WINDI data. We will examine the occurrence statistics of these features and look for correlations with large tidal amplitudes and temperature inversions that are simultaneously measured by SABER. These correlations may hold clues to what dynamical processes could produce such double peaks and anomalously low-altitude peaks. Title: Contribution of Radial Transport to the Deep Penetration of Outer Belt Electrons During Oct-Nov Magnetic Storm of 2003 Authors: Li, X.; Barker, A.; Baker, D.; Selesnick, R.; Friedel, R. Bibcode: 2005AGUFMSM41D..06L Altcode: During the geomagnetic storm of October/November 2003, the intensity peak of the outer radiation belt electron moved from its nominal position of L=4 to L=2.5 within a day. This event was correlated with extremely high solar wind speeds and enhanced ULF wave power throughout the inner magnetosphere, both are known to be associated with enhanced radial transport of radiation belt electrons. A modeling effort was made, using the measurements of relativistic electrons at geosynchronous orbit as the source population and solar wind parameters as input to a radial diffusion coefficient. We found that the deep penetration of MeV electrons down to L=2.5 could be mostly explained by the fast inward radial transport mechanism. Title: Energetic Particle Modulation by ULF waves in the inner magnetosphere Authors: Zong, Q.; Fritz, T.; Baker, D.; Fu, S.; Xie, L.; Daly, P.; Balogh, A.; Reme, H. Bibcode: 2005AGUFMSM41D..05Z Altcode: One of most important questions in the Earth's radiation belt is to determine the dominant processes which accelerate magnetospheric several keV electrons to MeV energies. In particular recent studies have emphasized the question of the relative dominance of ULF and VLF wave acceleration processes across the outer belt. Energetic electron and ion flux and spectra variations associated with ULF waves in the inner magnetosphere have been examined by using Cluster spacecraft data. The quasi-periodic particle flux (electron 30 keV to 500 keV, proton 30 keV to 1.5 MeV) modulations are observed in the the region of L=5.3 to 11.7 at MLT=8. The relative phase of energetic electron and ion are different in the different location, also, depend on the energy of the particles. The particle fluxes were found to be either 90 or 270 out of phase with the magnetic variations. For the phase difference between the ion density and the magnetic variation, this argues that the time-average Poynting flux of the Pc5 wave along the ambient magnetic field is approximately zero, this indicates that Pc5 waves are standing waves along the field line. In-situ ULF measurements from inside geosynchros orbit are not commonly available. Multi-point measurements of the ULF wave electric and magnetic field morphology, as well as radiation belt particle flux, are made in this paper to examine the efficiency of the ULF process in the outer belt. Cluster constellation allow to determine wave coherence length and mode structure, which are critical parameters for determining the efficiency of the ULF wave drift-resonance interaction. Title: Radial Diffusion as a Potential Source and Loss Mechanism of Relativistic Electrons in the Outer Radiation Belt Authors: Shprits, Y. Y.; Thorne, R.; Friedel, R.; Reeves, G. D.; Fennel, J. F.; Baker, D.; Shrikanth, K.; Horne, R. Bibcode: 2005AGUFMSM51D..06S Altcode: The loss mechanisms responsible for the sudden depletions of the outer electron radiation belt are examined based on observations and radial diffusion modeling. SAMPEX data for October-December 2003, indicates that depletions are correlated with increases in geomagnetic activity and also correlated with sudden increases in the solar wind dynamic pressure. Multi-channel HEO observations show that depletions are seen at energies as low as a few hundred keV. For the same events high energy proton channels also show decrease in fluxes at higher L-values. These observations are consistent with outward radial diffusion driven by the loss to magnetopause. We further examine the viability of the outward radial diffusion loss by comparing CRRES observations with a radial diffusion model simulations. Model-data comparison shows that flux variation near geosynchronous orbit can be effectively propagated by the outward radial diffusion to lower L-values and can account for the main phase storm depletions. The presence of the outward radial diffusion rises an important question: What is the origin of the relativistic electrons at geosynchronous orbit plasma sheet or radiation belts? Title: Plasmaspheric Influence on Radiation Belts During Major Geomagnetic Storms Authors: Goldstein, J.; Baker, D.; Sandel, B. R.; Burch, J. L.; Fennell, J. F. Bibcode: 2005AGUSMSM31A..01G Altcode: We investigate a possible causal relationship between erosion of the plasmasphere and enhancement of the radiation belts during major geomagnetic storms. The Earth's plasmasphere was observed by the IMAGE EUV imager to be drastically reduced in size by the 2003 Halloween geomagnetic storm event. Before the storm the plasmapause was seen at roughly 4 Earth radii (RE) geocentric distance; after the storm, the plasmapause had moved inside 2 RE. This dramatic erosion of the plasmasphere apparently had a profound effect on the global distribution of the Van Allen radiation belts. Wave-particle interactions inside the plasmasphere normally act to remove the radiation belt electrons inside the slot region; however, in the days following the 2003 Halloween storm's drastic plasmasphere erosion, SAMPEX witnessed the formation of an extremely intense new radiation belt in what was formerly the slot region. This chain of events suggests that the plasmasphere configuration can have a primary influence on the global radiation belt distribution. We present preliminary results of the investigation of this possible relationship for three major geomagnetic storms, using global images of the plasmasphere side-by-side with in situ energetic particle data. We discuss likely mechanisms for quickly accelerating electrons to the high levels observed in the slot that normally is devoid of such relativistic electrons. Title: The correlation between the inner edge of outer radiation belt electrons and the location of plasmapause Authors: Li, X.; Barker, A.; Gannon, J.; Baker, D.; Kanekal, S.; Selesnick, R. Bibcode: 2005AGUSMSM23C..02L Altcode: During the period of enhanced geomagnetic activity, both the outer radiation belt electrons and plasmapause move toward the Earth. Are these just a natural consequence of enhanced solar wind interaction with the magnetosphere or are they intrinsically related? Recent studies indicate that the location of the plasmapause may determine the location of the peak in the outer belt electron intensity. Our study of long term satellite measurements shows that the inner edge of the outer belt electrons correlates well with the location of plasmapause. Combining data from SAMPEX, CRRES, Polar, IMAGE, ACE and ground magnetometers and modeling efforts, we will address the role of the plasmasphere in radiation belt acceleration and loss processes. Title: Energetic particle acceleration during a major magnetic storm Authors: Kerttula, R.; Mursula, K.; Asikainen, T.; Friedel, R.; Baker, D.; Søraas, F.; Fennell, J. F.; Blake, J. B.; Grande, M. Bibcode: 2005AdSpR..36.1835K Altcode: We study the global properties of energetic (>30 keV) particles during the main and early recovery phase of a major magnetic storm of March 31, 2001, using data of the NOAA 15 and 16 and the CLUSTER satellites. During the storm main phase the ring current energetic electron and ion fluxes were increased by nearly two orders of magnitude, and the flux maxima were shifted to below L = 3. The maximum ion fluxes were observed at about 07 UT, coinciding with the minimum Dst. However, the highest fluxes of energetic electrons were observed only at about 16-18 UT, indicating significant differences in the acceleration of energetic electrons and ions during the storm. We suggest that the ion maximum at about 07 UT was due to field-aligned acceleration of ions from the ionosphere whereas the electron maximum at 16-18 UT was due to a large injection from the nightside. Title: First results — Lunar X-ray mapping spectrometer on smart-1 Authors: Grande, Manuel; Kellett, B.; Howe, C.; Perry, C. H.; Swinyard, B.; Dunkin, S.; Huovenin, J.; Thomas, N.; Mall, U.; Hughes, D.; Alleyne, H.; Russell, S.; Grady, M.; Lundin, R.; Barabash, S.; Baker, D.; Murray, C. D.; Guest, J. E.; Crawford, I.; Casanova, I.; Maurice, S.; Gasnault, O.; Foing, B.; Lawrence, D.; Fernandez, V. Bibcode: 2005CIBu..163...18G Altcode: 2005SpReT.163...18G No abstract at ADS Title: Hemispheric Differences and Evolution of the Cold Summer Mesopause Observed by the SABER Experiment on the TIMED Satellite Authors: Russell, J. M.; Mlynczak, M. G.; Mertens, C. J.; Gordley, L. L.; Picard, R. H.; Winick, J.; Wintersteiner, P.; Garcia, R.; Siskind, D. E.; Lopez-Puertas, M.; Remsberg, E. E.; Baker, D. Bibcode: 2004AGUFMSA33B..02R Altcode: The Sounding of the Atmosphere using Broadband Emission Radiometry (SABER) experiment was launched on December 7, 2001 into a 74.1 degree inclined, 625 km orbit onboard the TIMED satellite. The primary science goal of SABER is to achieve major advances in understanding the structure, energetics, chemistry, and dynamics in the atmospheric region extending from 60 to 180 km altitude. SABER has been operating almost continuously since activation using the space flight proven experiment approach of spectral broadband limb emission radiometry applied in 10 selected infrared spectral bands ranging from 1.27 micrometers to 17 micrometers wavelength. Observed limb emission profiles are being processed on the ground to provide vertical profiles with 2 km altitude resolution of key constituents, energetics parameters and temperature. Measurements are made both night and day over the latitude range from 52 degrees to 83 degrees with alternating hemisphere coverage every 60 days. During the time SABER has been operating, there have been two major solar storms in April 2002 and October 2003. The temporal and geographic coverage provided by SABER has provided path finding observations on the atmospheric effects of these events. In addition, the battery of measurements made by SABER has yielded new information on atmospheric energetics effects including radiative cooling due to the 15 micrometer band of CO2 and the persistence of heating due to exothermic chemical reactions. SABER observations have also provided new information on the mesopause latitudinal structure and evolution and have revealed the presence of a two-day wave in the mesopause region that previously was known only through modeling. Further, the data have shed light on the global distribution of the effects of nitric oxide vertical descent into the upper stratosphere and on the variability of atomic oxygen. This paper summarizes the major scientific results from SABER up to now using illustrative examples. Title: Cluster Observations of Earthward Flowing Plasmoid in the Tail Authors: Zong, Q.; Fritz, T.; Fu, S.; Pu, Z.; Baker, D.; Zhang, H.; Lui, A.; Glassmeier, K.; Korth, A.; Daly, P.; Balogh, A.; Reme, H. Bibcode: 2004AGUFMSM31A1216Z Altcode: The energetic electrons and ions embedded in Earthward-moving plasmoid structures have been observed. These plasmoids are associated with a rotational local Bz component (bi-polar) signature. Energetic electrons are found to be confined in a smaller spatial region than ions inside the plasmoid. Energetic ions and electrons seem to be a good indicator for the structure boundary. The fleet of Cluster spacecraft cross the plasmoid structure in a "first entry, last out" order (Note: when spacecraft cross a planar discontinuity, e.g. magnetopause, they will be in "first entry, first out" order). This documents the fact that the plasmoid has a non-planar nested structure. The large separation distance (around 1 RE) of the Cluster satellites in October 2002 is an advantage to provide constraints on the size and shape of the plasmoid structure of interest. In addition, the plasmoid (with closed field lines) should preserve the ion composition information where it is formed. The ion composition observed in the plasmoid shows significantly lower O and He than in the ambient plasma. This implies few heavy ions are involved in the reconnection process where the plasmoid is formed. Multiple flux ropes/plasmoids observation presented in this paper can be interpreted as strong evidence for multiple X-lines. Title: Sensitivity Tests of the Temerin-Li Dst Model Authors: Halford, A. J.; Weigel, R.; Baker, D. Bibcode: 2004AGUFMSM43A1146H Altcode: The Dst historically has been used as a measure of the disturbance of the magnetosphere and an indicator of when a geomagnetic storm is occuring. The Temerin-Li [2002] (TL02) model is a semi-empirical Dst model which was trained on five years (1995 - 1999) of data. The TL02 model is the most successful Dst predictor in terms of prediction efficiency, with a reported prediction efficiency of greater then .90. The inputs into this model are the solar wind parameters, solar wind velocity, interplanetary magnetic field, and solar wind density. This model is based on the Burton et al. model, but has many parameters whose physical relavance are not well understood. To better understand the physical relevance of the empirical parameters, we use parameter sensitivity, impulse response, and driver sensitivity analysis. These techniques are used along with seasonal and diurnal analysis of the prediction error to extract a physical understanding of the most influential components of the model. By holding the input parameters constant and comparing this output and the output from sending pulses of delta t = 1 hour at regular intervals over a period of a year to the actual Dst, we can observe the diurnal and seasonal variations due to the individual parameters. Title: CISM Metrics Plan and Initial Model Validation Results Authors: Spence, H. E.; Baker, D.; Burns, A.; Guild, T.; Huang, C.; Siscoe, G.; Weigel, R. Bibcode: 2004AGUSMSM54A..03S Altcode: Metrics and model validation represent two key elements upon which the success of the Center for Integrated Spaceweather Modeling (CISM) hinges. The routine calculation of important operationally- and scientifically-motivated metrics permits us to objectively measure and track the ability of coupled CISM models to predict essential space weather quantities. The rationale for CISM metrics selection is developed and the list of 29 metrics, along with the baseline models, first-generation physics models, and the data sets needed to compute skill scores, are outlined. While metrics provide a means for the objective assessment of long-term model improvement, model validation - the comprehensive, systematic quantitative comparison of model output with observations - is required for identifying and documenting model strengths and weaknesses. Two representative examples of initial validation efforts are summarized. The first uses case study analysis techniques and comparison with in situ observations during real events to explore the range of validity of the Lyon-Fedder-Mobarry (LFM) MHD simulation during magnetic storms. The second uses a statistical approach to compare the climatology of plasma sheet bulk properties (density, temperature, magnetic field, flows) deduced from both spacecraft observation and modeled by the LFM code. Title: Lunar Elemental Composition and Ivestigations with D-CIXS X-Ray Mapping Spectrometer on SMART-1 Authors: Grande, M.; Dunkin, S.; Howe, C.; Browning, R.; Kellett, B.; Perry, C. H.; Swinyard, B.; Waltham, N.; Kent, B.; Huovenin, J.; Thomas, N.; Mal, U.; Hughes, D.; Alleyne, H.; Russell, S.; Grady, M.; Lundin, R.; Barabash, S.; Baker, D.; Murray, C. D.; Guest, J.; Casanova, I.; Maurice, S.; Foing, B. Bibcode: 2004LPI....35.1519G Altcode: The D-CIXS Compact X-ray Spectrometer on ESA SMART-1 successfully launched in Sept 2003 can derive 45 km resolution images of the Moon with a spectral resolution of 185 eV, providing the first high-resolution global map of rock forming element abundances. Title: An Overview Of The SABER Experiment And Science Results Authors: Gordley, L. L.; Russell, J. M.; Mlynczak, M. G.; Mertens, C. J.; Remsberg, E. E.; Picard, R. H.; Lopez-Puertas, M.; Wintersteiner, P.; Winick, J.; Siskind, D. E.; Baker, D.; Garcia, R. Bibcode: 2003AGUFMSA32B..01G Altcode: The Sounding of the Atmosphere using Broadband Emission Radiometry (SABER) experiment was launched on December 7, 2001 into a 74.1o inclined, 625 km orbit onboard the TIMED satellite. The primary science goal of SABER is to achieve major advances in understanding the structure, energetics, chemistry, and dynamics in the atmospheric region extending from 60 to 180 km altitude. SABER has been operating almost continuously since activation using the space flight proven experiment approach of spectral broadband limb emission radiometry. The instrument scans the earth limb in 10 selected spectral bands ranging from 1.27 mm to 17 mm wavelength. The observed limb emission profiles are being processed on the ground to provide vertical profiles with 2 km altitude resolution of the following: temperature, O3, H2O, and CO2 mixing ratios; volume emission rates due to O2 (1D), OH (u=3,4,5), OH (u=7,8,9), and NO; key atmospheric cooling rates, solar heating rates, chemical heating rates, and airglow losses; atomic oxygen, atomic hydrogen and geostrophic winds. Measurements are made both night and day over the latitude range from 54oS to 87oN with alternating hemisphere coverage every 60 days. SABER has provided new information on energetics of the TIMED core region, observed atmospheric effects of major solar storms and made measurements in both northern and southern polar summers. This paper provides an experiment overview, orbital performance, comparisons with correlative observations and an overview of science results. Title: Replication As An Alternative Approach For Large Segmented Telescopes Authors: Farber, M.; Ulmer, M. P.; Graham, M. E.; Vaynman, S.; Varlese, S.; Baker, D.; Echt, J. Bibcode: 2003AAS...203.3819F Altcode: 2003BAAS...35.1263F The next generation of optical/IR telescopes will require large numbers of co-phased mirror segments. Therefore, some form of replication technology is desirable to reduce costs. Eletroforming has the advantage that it is a commercially developed technology for replication, and the technology has been widely used for making X-ray mirrors (e.g. XMM-Newton). Composite materials are appealing, since a great deal of development work has been done with composites as well. There are 3 areas that need to be addressed: replication with minimal stress so as to produce a high quality figure; attachment of support of the mirror segment so as to maintain the figure quality; thermal control requirements. Here we present a discussion of the requirements that lead us to select replication as the fabrication technology and the advantages of replication. We report on our first results of making a concave and flat mirrors.

This work was funded by a NASA Space Grant to Illinois, Ball Aerospace, Northwestern University, NASA Contract NAS1-03007, an AFOSR Contract F4620-C-0073, and a NASA Grant NAG5-03069. Title: Coordinated Energetic Particle Measurements Using Chandra, Cluster, and Polar Authors: Mueller-Mellin, R.; Blake, J. B.; Baker, D. Bibcode: 2003AGUFMSM51E..02M Altcode: It is not well known in the magnetospheric physics community that the Chandra spacecraft carries a multi-element energetic particle telescope called EPHIN (Electron Proton Helium Instrument) fielded by the University of Kiel. For present purposes we are interested in electrons that are measured from greater than 30 keV to greater than 10 MeV. Chandra is in a highly elliptical orbit with a perigee of 16000 km, and apogee of 133,000 km and an inclination of 28 degrees. Fortuitously the line of apsides is relatively close to that of the Cluster constellation. A first use of the Chandra data has been a further examination of a substorm onset that occurred = 0408 UT on 27 August 2001, discussed in a publication by Baker et al. (2002). At that time the s/c coordinates in GSM were Chandra (-6.64, 16.15, 12.82); Cluster 3 (-19.15, -1.40, 1.54); Polar (-7.71, -4.50, 3.32). It can be seen that whereas Cluster and Polar were a bit post midnight and roughly radially aligned, Chandra was well pre-midnight at around 20 hrs. Yet the onset time of energetic electrons at Chandra was very close to that observed at Cluster and Polar. Furthermore, some pre-substorm bursts were also seen to be closely time coincident at Chandra and the other spacecraft. These observations give additional evidence about the scale size of the phenomena and will be discussed in detail along with other coordinated measurements. Baker et al. GRL 29, no. 24, 2190, 2002 Title: Branch Prediction and Speculative Execution in Magnetospheric Forecasting Authors: Doxas, I.; Horton, W.; Baker, D.; McPherron, R.; Weigel, R.; Wiltberger, M. Bibcode: 2003AGUFMSM51B0522D Altcode: Recent advances in the development of integrated models of the Sun-Earth environment are placing increasing emphasis on data assimilation schemes that can maximize the intelligence extracted from our sparse sampling of upwind conditions. One of the schemes proposed is Branch Prediction and Speculative Execution, which consists of making probabilistic estimates of current upstream conditions, and distribute among available machines simulations that assume each of the probabilistically estimated states as initial conditions. As the near-Earth space evolves and near-Earth satellite data are compared with the models, some of the speculatively executed simulations will be proved wrong. At that point the machines that were executing them will be reassigned either to new lines of speculative simulation, or to increase the processing power devoted to more promising simulations already executing. The scheme is particularly suited to Space Weather since our upwind early warning sentries can provide only sparse sampling of the incoming solar wind, while the bulk of our monitors, which can provide significantly better coverage, are located close to Earth and provide much shorter lead times. By the time the data come in from the near-Earth monitors, the forecasts of the speculative simulations are already in hand. CALCHAS is a 3D visualization package that integrates models and data, and is used in the above data assimilation scheme. The package is written in Java 3D, and has a modular design, so that different models and datasets, both real-time and historical, can be seamlessly compared using a variety of goodness-of-fit measures. The scheme gives good results when used with particle simulations and WINDMI, a low-dimensional dynamical model of the coupled Magnetosphere-Ionosphere system (Doxas and Horton, Using Branch Prediction and Speculative Execution to Forecast Space Weather, Geospace Environment Modeling meeting, Telluride, CO, 2002). Numerical perturbation studies of global MHD models will also be presented. Title: The D-CIXS X-ray mapping spectrometer on SMART-1 Authors: Grande, M.; Browning, R.; Waltham, N.; Parker, D.; Dunkin, S. K.; Kent, B.; Kellett, B.; Perry, C. H.; Swinyard, B.; Perry, A.; Feraday, J.; Howe, C.; McBride, G.; Phillips, K.; Huovelin, J.; Muhli, P.; Hakala, P. J.; Vilhu, O.; Laukkanen, J.; Thomas, N.; Hughes, D.; Alleyne, H.; Grady, M.; Lundin, R.; Barabash, S.; Baker, D.; Clark, P. E.; Murray, C. D.; Guest, J.; Casanova, I.; d'Uston, L. C.; Maurice, S.; Foing, B.; Heather, D. J.; Fernandes, V.; Muinonen, K.; Russell, S. S.; Christou, A.; Owen, C.; Charles, P.; Koskinen, H.; Kato, M.; Sipila, K.; Nenonen, S.; Holmstrom, M.; Bhandari, N.; Elphic, R.; Lawrence, D. Bibcode: 2003P&SS...51..427G Altcode: The D-CIXS Compact X-ray Spectrometer will provide high quality spectroscopic mapping of the Moon, the primary science target of the ESA SMART-1 mission. D-CIXS consists of a high throughput spectrometer, which will perform spatially localised X-ray fluorescence spectroscopy. It will also carry a solar monitor, to provide the direct calibration needed to produce a global map of absolute lunar elemental abundances, the first time this has been done. Thus it will achieve ground breaking science within a resource envelope far smaller than previously thought possible for this type of instrument, by exploiting two new technologies, swept charge devices and micro-structure collimators. The new technology does not require cold running, with its associated overheads to the spacecraft. At the same time it will demonstrate a radically novel approach to building a type of instrument essential for the BepiColombo mission and potential future planetary science targets. Title: Scientific rationale for the D-CIXS X-ray spectrometer on board ESA's SMART-1 mission to the Moon Authors: Dunkin, S. K.; Grande, M.; Casanova, I.; Fernandes, V.; Heather, D. J.; Kellett, B.; Muinonen, K.; Russell, S. S.; Browning, R.; Waltham, N.; Parker, D.; Kent, B.; Perry, C. H.; Swinyard, B.; Perry, A.; Feraday, J.; Howe, C.; Phillips, K.; McBride, G.; Huovelin, J.; Muhli, P.; Hakala, P. J.; Vilhu, O.; Thomas, N.; Hughes, D.; Alleyne, H.; Grady, M.; Lundin, R.; Barabash, S.; Baker, D.; Clark, P. E.; Murray, C. D.; Guest, J.; d'Uston, L. C.; Maurice, S.; Foing, B.; Christou, A.; Owen, C.; Charles, P.; Laukkanen, J.; Koskinen, H.; Kato, M.; Sipila, K.; Nenonen, S.; Holmstrom, M.; Bhandari, N.; Elphic, R.; Lawrence, D. Bibcode: 2003P&SS...51..435D Altcode: The D-CIXS X-ray spectrometer on ESA's SMART-1 mission will provide the first global coverage of the lunar surface in X-rays, providing absolute measurements of elemental abundances. The instrument will be able to detect elemental Fe, Mg, Al and Si under normal solar conditions and several other elements during solar flare events. These data will allow for advances in several areas of lunar science, including an improved estimate of the bulk composition of the Moon, detailed observations of the lateral and vertical nature of the crust, chemical observations of the maria, investigations into the lunar regolith, and mapping of potential lunar resources. In combination with information to be obtained by the other instruments on SMART-1 and the data already provided by the Clementine and Lunar Prospector missions, this information will allow for a more detailed look at some of the fundamental questions that remain regarding the origin and evolution of the Moon. Title: The Substorm at 05:45 on October 13, 2001 Observed From the Ground, and the LANL, GOES, Polar, and Cluster Satellites Authors: Peterson, W.; Baker, D.; Su, Y.; Eriksson, S.; Li, X.; Sigwarth, J.; Scudder, J.; Donovan, E.; Korth, A.; Trattner, K.; Slavin, J.; Reme, H.; Dunlop, M.; Andre, M.; Singer, H.; Friedel, R.; Lu, G.; McPherron, R.; Russell, C. Bibcode: 2002AGUFMSM71A0580P Altcode: The substorm at ~05:45 was not the first, last, or most intense of those observed during the first half of October 13, 2001. However the configuration of platforms noted in the title was excellent for obtaining a comprehensive view of the initiation and evolution of a substorm. The combination of Canopus ground magnetograms and Polar VIS images identified onset at 05:45:02 +/- 00:00:22 west and south of Ft. Churchill, Canada. The closest satellite, Polar, was located near geosynchronous altitude at 23:00 MLT. Polar was sampling magnetic fields and plasmas characteristic of the outer plasma sheet before 05:45 UT and characteristic of the central plasma sheet after 05:45 UT. Polar magnetometer data from below the magnetic equator and GOES 12 magnetometer data from above the magnetic equator suggest that the main currents were flowing tailward of near-geosynchronous altitude. The Cluster satellites were located at ~19 Re and ~21:00 MLT on the dusk side of the magnetotail. A coherent dispersion feature in the plasma at several of the Cluster spacecraft was observed at ~05:36 UT, when the Bz (GSM) component on all four spacecraft began decreasing. The Bz component was negative on all four Cluster spacecraft from ~05:42 to ~05:55 UT. We will present these observations and a time line of events derived from them. We will discuss how these observations agree and disagree with current ideas of the initiation and global evolution of substorms. Title: Atmospheric models, GPS and InSAR measurements of the tropospheric water vapour field over Mount Etna Authors: Wadge, G.; Webley, P. W.; James, I. N.; Bingley, R.; Dodson, A.; Waugh, S.; Veneboer, T.; Puglisi, G.; Mattia, M.; Baker, D.; Edwards, S. C.; Edwards, S. J.; Clarke, P. J. Bibcode: 2002GeoRL..29.1905W Altcode: 2002GeoRL..29s..11W Dynamic models of atmospheric movement over the Mount Etna volcano are used to calculate the path delays affecting radar caused by variable water vapour in the troposphere. We compare these model results with the equivalent differential radar interferogram generated by two ERS-2 SAR images taken 35 days apart and the water vapour delay retrievals from a network of fourteen GPS stations distributed over the volcano. The atmospheric model delay field agrees well with the long-wavelength spatial differences measured by InSAR and those measured by GPS. Title: The SABER Experiment on the TIMED Mission: Overview and Preliminary Science Results Authors: Russell, J. M.; Mlynczak, M. G.; Gordley, L. L.; Mertens, C. J.; Picard, R. H.; Lopez-Puertas, M.; Wintersteiner, P.; Winick, J.; Siskind, D. E.; Baker, D.; Ulwick, J.; Remsberg, E. E.; Garcia, R.; Espy, P. J.; Roble, R. G.; Solomon, S. Bibcode: 2002AGUSMSA51A..04R Altcode: The Sounding of the Atmosphere using Broadband Emission Radiometry (SABER) experiment was launched onboard the TIMED satellite at 7:07:35 am PST on December 7, 2001 from the Western Test Range. The satellite was placed in a 74.1o inclined, 625 km orbit by a Delta II rocket. The primary science goal of SABER is to achieve major advances in understanding the structure, energetics, chemistry, and dynamics in the atmospheric region extending from 60 to 180 km altitude. This will be accomplished using the space flight proven experiment approach of spectral broadband limb emission radiometry. The SABER instrument scans the earth limb in 10 selected spectral bands ranging from 1.27 mm to 17 mm wavelength. The observed limb emission profiles are being processed on the ground to provide vertical profiles with 2 km altitude resolution the following: temperature, O3, H2O, and CO2 mixing ratios; volume emission rates due to O2 (1D), OH (u=3,4,5), OH (u=7,8,9), and NO; key atmospheric cooling rates, solar heating rates, chemical heating rates, and airglow losses; atomic oxygen, atomic hydrogen and geostrophic winds. Measurements are made both night and day over the latitude range from 54oS to 87oN with alternating hemisphere coverage every 60 days. SABER measurements taken just after activation include data on the cold summer mesopause in the southern hemisphere and observations of the dynamically active northern hemisphere winter. This paper provides an experiment overview, orbital performance, example data products, and preliminary comparisons with correlative observations. Science implications of the data will be discussed. Title: Self-Organized Criticality and Intermittent Turbulence in the Plasma Sheet Authors: Klimas, A.; Uritsky, V.; Vassiliadis, D.; Weigel, R.; Baker, D. Bibcode: 2002AGUSMSM31B..06K Altcode: Our recent analysis of Polar UVI image data has now made the evidence for self-organized criticality (SOC) in the magnetospheric dynamics difficult to interpret in any other way. The results support our earlier suggestion that this SOC component of the dynamics is centered in the plasma sheet and that it is related to the flow bursts and associated localized reconnections that have been observed there. It is necessary now to develop an interpretation of SOC in a plasma physical context. Numerical simulations of a 2-D plasma sheet model that may evolve into SOC will be discussed. Chang has suggested that intermittent turbulence may be associated with SOC in the plasma sheet. Angelopolous et al. [Phys. Plasmas, 1999], taking advantage of a rare conjunction of the Geotail and Wind spacecraft in the plasma sheet, have shown that relative cross-tail plasma velocities at the spatially separated spacecraft positions exhibit a Castaing distribution, indicative of intermittent turbulence. It will be shown that relative velocities in the numerical solutions of the 2-D plasma sheet model also exhibit this type of distribution when the model appears to be evolving in the neighborhood of the SOC limit. Based on the model behavior, the relationship between intermittent turbulence and SOC will be discussed. Title: The D-CIXS X-ray spectrometer, and its capabilities for lunar science Authors: Grande, M.; Dunkin, S.; Heather, D.; Kellett, B.; Perry, C. H.; Browning, R.; Waltham, N.; Parker, D.; Kent, B.; Swinyard, B.; Fereday, J.; Howe, C.; Huovelin, J.; Muhli, P.; Hakala, P. J.; Vilhu, O.; Thomas, N.; Hughes, D.; Alleyne, H.; Grady, M.; Russell, S.; Lundin, R.; Barabash, S.; Baker, D.; Clark, P. E.; Murray, C. D.; Christou, A.; Guest, J.; Casanova, I.; d'Uston, L. C.; Maurice, S.; Foing, B.; Kato, M. Bibcode: 2002AdSpR..30.1901G Altcode: The purpose of the D-CIXS (Demonstration of a Compact Imaging X-ray Spectrometer) instrument on the ESA SMART-1 mission is to provide high quality spectroscopic mapping of the Moon by imaging fluorescence X-rays emitted from the lunar surface. In order to obtain adequate statistics for what can be very weak sources, it is essential to have a large effective area, while maintaining a low mass. The solution is to make a thin, low profile detector, essentially a modern version of "X-ray detecting paper". D-CIXS will achieve a spatial resolution on the ground of 42km from a spacecraft at 300 km altitude, with a spectral resolution of 200 eV or better. The instrument is based around the use of advanced dual microstructure collimator and Swept Charge Device X-ray detector technologies. Swept Charge Device X-ray detectors, a novel architecture based on proven CCD technology, have the virtue of providing superior X-ray detection and spectroscopic measurement capabilities, while also operating at room temperature. Thus we avoid the need for the large passive cooling radiator that was previously required to cool large X-ray focal plane CCDs. The advanced low profile microstructure collimation and filter design builds on expertise developed in solid state and microwave technology to enable us to dramatically reduce the instrument mass. The total mass of D-CIXS, including an X-ray solar monitor is ∼4.6 kg. D-CIXS will provide the first global map of the Moon in X-rays. During normal solar conditions, it will be able to detect absolute elemental abundances of Fe, Mg, Al and Si on the lunar surface, using the on-board solar monitor to obtain a continuous measurement of the input solar spectrum. During solar flare events, it will also be possible to detect other elements such as Ca, Ti, V, Cr, Mn, Co, K, P and Na. The global mapping of Mg, Al and Si, and in particular deriving Mg#, the magnesium number (MgO/[MgO+FeO]), represents the prime goal of the D-CIXS experiment. Title: New results on the structure and dynamics of the radiation belts Authors: Vassiliadis, D.; Weigel, R.; Klimas, A.; Fung, S.; Kanekal, S.; Mewaldt, R.; Baker, D.; Rigler, E. Bibcode: 2002cosp...34E2936V Altcode: 2002cosp.meetE2936V Earlier solar wind-magnetosphere coupling studies tell us that the MeV electron pop- ulation in the outer zone responds to the solar wind speed V_SW, IMF B_z, and B_tot. The most geoeffective profiles of these quantities are associated with high- speed streams and magnetic clouds. What is less known is that different L shell re- gions of the inner magnetosphere respond to very different, sometimes diametrically so, interplanetary conditions. Using the response to the solar wind driving we iden- tify four regions: L=1-2, 2-3 (slot), 3-4 (P0, responding to shock- and cloud-like solar wind), 4-7 (P1, responding to high-speed stream conditions), and 7-15 (P2, responding to dV_SW/dt<0 and IMF B_z>0). We find that a) omnidirectional fluxes in a given L shell are strongly correlated with fluxes in the same region, but much less so with fluxes in other regions, giving further support to the hypothesis of magnetospheric coherence. b) The boundaries between regions (especially between P1 and P2 which determines overall trapping capacity) vary with the solar cycle and season. c) The re- sponse in each region increases with activity level, but each region has a different rate of increase. d) The P2 region is characterized by lower fluxes (typically >2 orders of magnitude below P1) organized in a fine structure of long-lived (days-weeks-long), narrow (DeltaL=0.1-0.3) regions with generally different dynamics than P0 or P1. The most prominent of these regions are located at L=9.4 and 7.5. These effects were stud- ied with SAMPEX and EXOS-C (OHZORA) particle fluxes and the OMNIweb solar wind database. Title: Solar wind driven radiation belt response functions at 100-min time scales using SAMPEX orbit-averaged electron fluxes Authors: Baker, D.; Rigler, J.; Vassiliadis, D. Bibcode: 2002cosp...34E2198B Altcode: 2002cosp.meetE2198B Characterizations of radiation belt dynamics using linear prediction filters (LPFs) were first published by Nagai (1988) and Baker et al. (1990). These studies focused primarily on short-term predictions of daily-averaged radiation fluxes at geostationary orbit using global magnetospheric indices and the speed of the so la r wind impinging on the Earth's magnetosphere. Using solar wind data from the NSSDC OMNI database and SAMPEX 2 6MeV omn idirectional electron fluxes at- various magnetic L-shells, new analyses have combined linear response functions to provide a three dimensional view (relative time, L-shell, and impulse response) describing the linear response of relativistic radiation belt electrons to solar wind input. Several physical interpretations and implications are gleaned by applying this novel data analysis technique. This includes the demonstration of strong seasonal and solar cycle-dependent variatio ns in the global response function, as well as the existence of a quasi-adiabatic peak in the response functions just outside of the slot region. Our analyses have demonstrated the ability of autoregressive(AR) filters to remove the diurnal variation observed in radiation belt data sets. This paper extends prior work by removing diurnal variations in SAMPEX orbit-averaged electron data and analyzing the linear prediction filters at the 100-min time scales of the SAMPEX orbit. Title: Cluster Observations of Magnetospheric Substorm Behavior In The Near- and Mid-tail Regions Authors: Baker, D.; Blake, J.; Burch, J. L.; Daly, P.; Dunlop, M.; Ergun, R.; Friedel, R.; Fritz, T. Bibcode: 2002EGSGA..27.6639B Altcode: The Cluster constellation of spacecraft have returned a wealth of new data on particle and field variations in the near- and mid-magnetotail regions of Earth's magnetosphere. Using the Research with Adaptive Particle Imaging Detectors (RAPID) systems onboard the four Cluster vehicles, we have identified substorm- related energetic (E > 20 keV) electron enhancement events during the period March 2001 through October 2001 in the geocentric radial range of 4 to 19 Earth radii. We have used concurrent data from other Cluster instruments as well as from the IMAGE, FAST, OPS, and geostationary orbit spacecraft in order to understand particle injection and transport phenomena throughout this key region of the magnetotail. One particularly striking event during a major geomagnetic storm on 31 March 2001 showed a dispersionless electron injection event in as close to the Earth as 4 Re. More normal electron enhancements in the plasma sheet at intermediate radial distances are also studied in a global substorm context. Title: Cluster observations of geomagnetic storms and of magnetospheric substorm behavior in the near- and mid-tail regions Authors: Baker, D. Bibcode: 2002cosp...34E.234B Altcode: 2002cosp.meetE.234B The Cluster constellation of spacecraft have returned a wealth of new data on particle and field variations in the near- and mid-magnetotail regions of Earth's magnetosphere. Using the Research with Adaptive Particle Imaging Detectors (RAPID) systems onboard the four Cluster vehicles, we have identified substorm- related energetic (E > 20 keV) electron enhancement events during the period March 2001 through October 2001 in the geocentric radial range of 4 to 19 Earth radii. We have used concurrent data from other Cluster instruments as well as from the IMAGE, FAST, GPS, and geostationary orbit spacecraft in order to understand particle injection and transport phenomena throughout this key region of the magnetotail. One particularly striking event during a major geomagnetic storm on 31 March 2001 showed a dispersionless electron injection event in as close to the Earth as 4 Re. More normal electron enhancements in the plasma sheet at intermediate radial distances are also studied in a global substorm context. A particularly well- observed substorm case occurred on August 27, 2001 when CLUSTER was almost exactly in the midnight meridian and complementary data were available from IMAGE, POLAR, GOES-8, and the LANL satellites. We find evidence that CLUSTER was very near the near-Earth substorm neutral line and that magnetic reconnection began some seven minutes prior to the substorm auroral brightening of the expansive phase onset. Title: Energetic particle boundaries and injections during the main phase of a major magnetic storm Authors: Kerttula, R.; Mursula, K.; Asikainen, T.; Friedel, R.; Baker, D.; Soeraas, F.; Daly, P.; Fritz, T.; Blake, J.; Carter, M. Bibcode: 2002cosp...34E2702K Altcode: 2002cosp.meetE2702K We study energetic particle observations during the main phase of the March 31, 2001, storm using the low-altitude NOAA satellites and the four Cluster satellites. The NOAA satellites are used to monitor the change of the global magnetospheric configuration. At the start of the main phase, the polar cap boundaries extend equatorwards and energetic particle densities in the polar cap region are reduced. The boundaries return polewards soon after the end of the main phase. Strong injections of energetic particles are observed during and soon after the main phase whose development is followed by the NOAA satellite observations. Also during the main phase, an intense population of energetic electrons is established at very low altitudes in the equatorial region. During one of the most intense injections at about 0640 UT, when Cluster is close to its perigee in the post-midnight sector, the energetic particle fluxes of the Rapid instruments are increased in two steps separated by about 3 minutes. Using Cluster observations we will examine whether the increases are due to spatial gradients formed after one major injection or whether they correspond to two separate injections, and determine the motion of the injection boundary. Title: Status of Project GRAND's Proportional Wire Chamber Array Authors: Poirier, J.; Baker, D.; Barchie, J.; D'Andrea, C.; Dunford, M.; Green, M.; Gress, J.; Lin, T.; Race, D.; Skibba, R.; VanLaecke, G.; Wysocki, M. Bibcode: 2001astro.ph..9489P Altcode: Project GRAND is an extensive air shower array of proportional wire chambers. It has 64 stations in a 100m x 100m area; each station has eight planes of proportional wire chambers with a 50 mm steel absorber plate above the bottom two planes. This arrangement of planes, each 1.25 square meters of area, allow an angular measurement for each track to 0.25 degrees in each of two projections. The steel absorber plate allows a measurement of the identity of each muon track to 96% accuracy. Two data-taking triggers allow data to be simultaneously taken for a) extensive air showers (multiple coincidence station hits) at about 1 Hz and b) single muons (single tracks of identified muons) at 2000 Hz. Eight on-line computers pre-analyze the single track data and store the results on magnetic tape in compacted form with a minimum of computer dead-time. One additional computer reads data from the shower triggers and records this raw data on a separate magnetic tape with no pre-analysis. Title: Project GRAND's status: an array of proportional wire chambers Authors: Poirier, J.; Baker, D.; Barchie, J.; D'Andrea, C.; Dunford, M.; Green, M.; Gress, J.; Lin, T.; Race, D.; Skibba, R.; Vanlaecke, G.; Wysocki, J. Bibcode: 2001ICRC....2..602P Altcode: 2001ICRC...27..602P Project GRAND is an extensive air shower array of proportional wire chambers. It has 64 stations in a 100 m x 100 m area; each station has eight planes of proportional wire chambers with a 50 mm steel absorber plate above the bottom two planes. This arrangement of planes, each 1.25 square meters of area, allow an angular measurement for each track to 0.25° in each of two projections. The steel absorber plate allows a measurement of the identity of each muon track to 96% accuracy. Two data-taking triggers allow data to be simultaneously taken for a) extensive air showers (multiple coincidence station hits) at about 1 Hz and b) single muons (single tracks of identified muons) at 2000 Hz. Eight on-line computers pre-analyze the single track data and store the results on magnetic tape in compacted form with a minimum of computer dead-time. One additional computer reads data from the shower triggers and records this raw data on a separate magnetic tape with no pre-analysis. Title: Solar-Terrestrial Connection: Coupling Between Solar Wind, Magnetosphere, Ionosphere, and Neutral Atmosphere Authors: Baker, D. Bibcode: 2000eaa..bookE2239B Altcode: The particle flux from the Sun and the magnetosphere represents a large source of energy and ionization for the lower thermosphere and ionosphere. The energy flux, which ranges from <10-3 J m-2 s-1 to over 0.1 J m-2 s-1, is deposited by particles with energies that range from hundreds of eV to several hundred MeV. The intensity, spectrum, and localization of the precipitation are functions of sol... Title: The D-CIXS X-Ray Spectrometer on ESA's SMART-1 Mission to the Moon Authors: Grande, M.; Browning, R.; Dunkin, S.; Parker, D.; Kent, B.; Kellett, B.; Perry, H. C.; Swinyard, B.; Phillips, K.; Huovenin, J.; Thomas, N.; Hughes, D.; Alleyne, H.; Grady, M.; Lundin, R.; Barabash, S.; Baker, D.; Murray, D. C.; Guest, J.; Casanova, I.; D'Uston, C. L.; Maurice, S.; Foing, B.; Heather, D.; Clark, E. P.; Kato, M. Bibcode: 2000ESASP.462...97G Altcode: 2000eum..conf...97G No abstract at ADS Title: Lunar Elemental Composition and Investigations with D-CIXS X-Ray Mapping Spectrometer on Smart-1 Authors: Grande, M.; Browning, R.; Waltham, N.; Kent, B.; Kellett, B.; Perry, C. H.; Phillips, B. Swinyard K.; Huovenin, J.; Thomas, N.; Livi, S.; Mal, U.; Hughes, D.; Alleyne, H.; Lundin, M. Grady R.; Barabash, S.; Baker, D.; Murray, C. D.; Guest, J.; Dunkin, S. K.; Maurice, I. Casanova S.; Foing, B. Bibcode: 2000LPI....31.1442G Altcode: No abstract at ADS Title: A Multi-Spacecraft Synthesis of Relativistic Electrons in the Inner Magnetosphere using LANL, GOES, GPS, SAMPEX, HEO and POLAR Authors: Friedel, R. H. W.; Reeves, G.; Belian, D.; Cayton, T.; Mouikis, C.; Korth, A.; Blake, B.; Fennell, J.; Selesnick, R.; Baker, D.; Onsager, T.; Kanekal, S. Bibcode: 2000AdSpR..26...93F Altcode: One of the Brussels Radiation Belt Workshop recommendations was the establishment of a near-real-time data driven model of the inner magnetospheric energetic particle population (L < 8). Although the ``ideal'' missions and data sets for such a model do not exist at present, more spacecraft than ever before are currently sampling the inner magnetosphere. We attempt here in a case study of the January 10, 1997 magnetic cloud event to construct such a model with the energetic electron data available from 5 geosynchronous and 5 elliptically orbiting satellites. We examine the constraints and difficulties of putting together a large number of datasets which are measured near-simultaneously at very different locations in the inner magnetosphere. First results indicate that we can achieve a time resolution of about 3 hours for a given ``snapshot'' of the inner magnetosphere, and that large azimuthal asymmetries of the energetic electron population can be observed during large storms Title: D-CIXS: Lunar investigation using the Compact X-Ray Spectrometer on SMART-1 Authors: Grande, M.; Browning, R.; Waltham, N.; Kent, B.; Kellett, B.; Perry, C. H.; Swinyard, B.; Phillips, K.; Huovenin, J.; Thomas, N.; Livi, S.; Wilken, B.; Hughes, D.; Alleyne, H.; Grady, M.; Lundin, R.; Barabash, S.; Baker, D.; Murray, C. D.; Guest, J.; Dunkin, S. Bibcode: 1999DPS....31.0808G Altcode: The D-CIXS Compact X-ray Spectrometer will provide high quality spectroscopic mapping of the Moon, the primary science target of the SMART-1 mission. At the same time it will demonstrate a radically novel approach to building a type of instrument essential for the Mercury cornerstone mission. It will achieve ground breaking science within a resource envelope far smaller than previously thought possible for this type of instrument, using new technology which does not require cold running, with its associated overheads to the spacecraft, and which is radiation tolerant, essential to many potential and future science targets. It consists of a high throughput spectrometer, which will perform spatially localised X-ray fluorescence spectroscopy, and a solar monitor to provide the calibration of the illumination necessary to produce global map of absolute Lunar elemental abundances. Title: D-CIXS: lunar investigation using the compact X-Ray spectrometer on SMART-1. Authors: Grande, M.; Browning, R.; Waltham, N.; Kent, B.; Kellett, B.; Perry, C. H.; Swinyard, B. M.; Phillips, K.; Huovenin, J.; Thomas, N.; Livi, S.; Wilken, B.; Hughes, D.; Alleyne, H.; Grady, M.; Lundin, R.; Barabash, S.; Baker, D.; Murray, C. D.; Guest, J. E.; Dunkin, S. Bibcode: 1999BAAS...31R1083G Altcode: No abstract at ADS Title: Solar-terrestrial symposium examines coupling processes Authors: Daglis, I.; Baker, D.; Sarris, E.; Wilken, B. Bibcode: 1998EOSTr..79..139D Altcode: Exploration of the space environment has revealed a dynamic and complex system of interacting plasmas, magnetic fields, and electrical currents. Plasma physics determines the behavior of matter in space on spatial and temporal scales vastly different from those that can be duplicated in Earth-based laboratories. The near-Earth space environment has traditionally been studied as a system of independent component parts in the interplanetary region, the magnetosphere, the ionosphere, and the upper atmosphere. From such early explorations, it was known that “geospace” is a complex system composed of highly interactive parts. While previous programs advanced the understanding of these geospace components individually, an understanding of geospace as a whole required a planned program of simultaneous space and ground-based observations and theoretical studies keyed to a global assessment of the production, transfer, storage, and dissipation of energy throughout the solar-terrestrial system. Prior understanding of the various geospace components plus the availability of advanced instrumentation has allowed, for the first time, a comprehensive, quantitative study of the solar-terrestrial energy chain to be planned: the International Solar Terrestrial Physics (ISTP) Program. Title: RAPID - The Imaging Energetic Particle Spectrometer on Cluster Authors: Wilken, B.; Axford, W. I.; Daglis, I.; Daly, P.; Guttler, W.; Ip, W. H.; Korth, A.; Kremser, G.; Livi, S.; Vasyliunas, V. M.; Woch, J.; Baker, D.; Belian, R. D.; Blake, J. B.; Fennell, J. F.; Lyons, L. R.; Borg, H.; Fritz, T. A.; Gliem, F.; Rathje, R.; Grande, M.; Hall, D.; Kecsuemety, K.; McKenna-Lawlor, S.; Mursula, K.; Tanskanen, P.; Pu, Z.; Sandahl, I.; Sarris, E. T.; Scholer, M.; Schulz, M.; Sorass, F.; Ullaland, S. Bibcode: 1997SSRv...79..399W Altcode: No abstract at ADS Title: The Clementine mission - initial results from Lunar mapping. Authors: Spudis, P. D.; Shoemaker, E.; Davies, M.; Acton, C.; Burratti, B.; Duxbury, T.; Eliason, E.; McEwen, A.; Baker, D.; Smith, D.; Lucey, P.; Blamont, J.; Pieters, C. Bibcode: 1994ESASP1170...91S Altcode: 1994luna.work...91S No abstract at ADS Title: The Clementine Mission: Initial Results from lunar mapping Authors: Spudis, P. D.; Shoemaker, E.; Acton, C.; Burratti, B.; Duxbury, T.; Baker, D.; Smith, D.; Blamont, J.; Davies, M.; Eliason, E. Bibcode: 1994STIN...9524994S Altcode: Clementine was a mission designed to test the space-worthiness of a variety of advanced sensors for use on military surveillance satellites while, at the same time, gathering useful scientific information on the composition and structure of the Moon and a near-Earth asteroid. Conducted jointly by the Ballistic Missile Defense Organization (BMDO, formerly the Strategic Defense Initiative Organization) of the US Department of Defense and NASA, Clementine was dispatched for an extended stay in the vicinity of Earth's moon on 25 January 1994 and arrived at the Moon on 20 February 1994. The spacecraft started systematic mapping on 26 February, completed mapping on 22 April, and left lunar orbit on 3 May. The entire Clementine project, from conception through end-of-mission, lasted approximately 3 years. Title: One Small Step for Mankind Authors: Baker, D. Bibcode: 1989NewSc.123...52B Altcode: No abstract at ADS Title: Earth-based Radio Observations of the Planet Mercury Authors: Ledlow, M. J.; Burns, J. O.; Zhao, J. H.; Gisler, G.; Zeilik, M.; Baker, D. Bibcode: 1989LPI....20..564L Altcode: No abstract at ADS Title: Observation of OH Meinel (7,4) P(N''=13) transitions in the night airglow Authors: Pendleton, W., Jr.; Espy, P.; Baker, D.; Steed, A.; Fetrow, M.; Henriksen, K. Bibcode: 1989JGR....94..505P Altcode: Improved spectral measurements of the OH Meinel Δv=3 night airglow emissions have revealed unexpectedly intense transitions from high rotational levels. The example selected for this communication involves the previously unreported P(N''=13) transitions in the OH M (7,4) band. Under the extant conditions, the column emission rates associated with these new features exceeded by factors ~104 those expected on the basis of the assumption of rotational-kinetic equilibrium for the v=7 rotational manifold. We present the key observations and discuss some of the implications. Title: Book-Review - the History of Manned Space Flight Authors: Baker, D.; Fraknoi, A. Bibcode: 1983Mercu..12T..91B Altcode: No abstract at ADS Title: Book-Review - the History of Manned Space Flight Authors: Baker, D.; Michaud, M. A. G. Bibcode: 1983S&T....66...30B Altcode: No abstract at ADS Title: Astronomia. Authors: Baker, D. Bibcode: 1980astr.book.....B Altcode: No abstract at ADS Title: Book-Review - the Rocket Authors: Baker, D.; Watts, R. N., Jr. Bibcode: 1980S&T....60..141B Altcode: No abstract at ADS Title: Book-Review - Space Shuttle Authors: Baker, D.; Michaud, M. A. G. Bibcode: 1980S&T....59..150B Altcode: No abstract at ADS Title: Book-Review - Space Shuttle Authors: Baker, D. Bibcode: 1980Sci...208..394B Altcode: No abstract at ADS Title: Der Kosmos-Sternführer. Planeten, Sterne, Galaxien. Authors: Baker, D.; Hardy, D. A. Bibcode: 1979dkps.book.....B Altcode: No abstract at ADS Title: Space Shuttle. Authors: Baker, D. Bibcode: 1979spsh.book.....B Altcode: No abstract at ADS Title: The rocket_- the history and development of rocket and missile technology. Authors: Baker, D. Bibcode: 1978rhdr.book.....B Altcode: No abstract at ADS Title: The Hamlyn guide to astronomy. Authors: Baker, D. Bibcode: 1978hgta.book.....B Altcode: No abstract at ADS Title: Behind the Viking scene. 4, 5. Authors: Baker, D. Bibcode: 1977SpFl...19..166B Altcode: Engineering problems encountered early in the mission of Viking Lander 1 are discussed. These include the refusal of the seismometer to uncage itself, failure of the low-gain No. 1 receiver, and trouble in retracting the surface-sampler boom. The way in which the boom problem was overcome is described in detail. It is noted that the seismometer was rendered virtually inoperable and that the low-gain receiver could not be coaxed back into operation. Title: Near-infrared spectrum of an aurora Authors: Baker, D.; Pendleton, W., Jr.; Steed, A.; Huppi, R.; Stair, A. T., Jr. Bibcode: 1977JGR....82.1601B Altcode: The spectrum of an aurora has been obtained at moderately high resolution by using a wide-field interferometer-spectrometer. The free spectral range was from 0.83 to 1.67 µm at a midrange resolving power of about 1800. The principal auroral features observed during an IBC III+ breakup on the night of April 19, 1974, at Chatanika, Alaska, were the N2+ Meinel bands, the N2 first positive bands, and certain atomic O and N emission lines. Comparisons of the auroral spectra are made with both high-latitude airglow and laboratory spectra taken by the same instrument. Title: Behind the Viking scene. 1 - 3. Authors: Baker, D. Bibcode: 1977SpFl...19...75B Altcode: No abstract at ADS Title: Viking: lander science equipment - 2. Authors: Baker, D. Bibcode: 1976SpFl...18..241B Altcode: The soil collector carried aboard the Viking Mars Lander and the instruments and procedures that will be used to investigate samples of the surface soil of Mars are described. The collector, stored in a collapsed, coiled configuration during flight, deploys to form a rigid arm capable of collecting materials from 90 cm to 3 m from the Lander itself within an azimuth arc of 120 deg. Screens limit the passage of particles larger than 1 mm. Soil samples delivered to the bio-lab will be subjected to pyrolytic release, labelled release, and gas exchange tests to detect the presence of metabolic products or of organic compounds indicative of the present or past existence of life. The GCMS, which is capable of performing six organic tests and up to 60 atmospheric analyses, will be used to search for compounds in the surface soil. Inorganic chemical analyses will be performed by an X-ray fluorescence spectrometer. Title: Viking: Orbiter science equipment. Authors: Baker, D. Bibcode: 1976SpFl...18..124B Altcode: The instrumentation aboard the Viking orbiter for obtaining a photographic record of geological changes, high resolution imagery of selected areas of the Martian surface, information on the distribution of water vapor, and details on the thermal environment is described. The spacecraft will carry two TV cameras incorporating 38 mm selenium vidicon tube, and catadioptric Cassegrain lenses. An infrared spectrometer will detect water vapor at 1.38 micrometers. A four-channel infrared radiometer operating at wavelengths of 6-8, 8-9.5, 9.5-13, and 18-24 microns will be used to determine surface temperature profiles, measure atmospheric temperature, and detect frost or condensation levels. Additional spectral bands at 0.3-3 and 16 microns will measure atmospheric temperature and planetary albedo. Bimetallic thermocouples will measure infrared radiation in the spectral gaps between filter settings. The aeroshell protecting the Lander will contain a mass spectrometer, retarding potential analyzer, and pressure and temperature sensors to measure gross characteristics of the atmosphere of Mars. Title: Viking: lander science equipment - 1. Authors: Baker, D. Bibcode: 1976SpFl...18..211B Altcode: No abstract at ADS Title: Viking: the orbiter. Authors: Baker, D. Bibcode: 1976SpFl...18...84B Altcode: No abstract at ADS Title: Surveyor on the moon. 6. Authors: Baker, D. Bibcode: 1976SpFl...18..228B Altcode: No abstract at ADS Title: The voyages of Viking - 3. Viking: the lander. Authors: Baker, D. Bibcode: 1976SpFl...18..158B Altcode: No abstract at ADS Title: Mariner-Venus-Mercury 1973 project history. Authors: Baker, D. Bibcode: 1975SpFl...17..298B Altcode: The significant advances made by the Mariner-Venus-Mercury 1973 project include the gravity-assist fly-by of a second planet from the deflected trajectory induced by a primary target, TV views of Venus, investigation of Mercury, the planetary re-visit on a fly-by profile, and effective manipulation of real-time planning (using solar-sailing to effect attitude stabilization). The flight of Mariner 10 is described from June 6, 1974, when the spacecraft had moved around the sun to superior conjunction and the dual S-band and X-band radio signals from the high-gain antenna passed within 1.67 deg of the solar surface as viewed from earth, until the conclusion of the operational phase on March 24, 1975. The second and third Mercury encounters, allowed a full frontal scan of the sunlit side plus slant-angle examination of the south pole and transmitted images of 60% of the total surface area of Mercury. Title: Twilight transition spectra of atmospheric O2 Ir emissions Authors: Baker, D.; Steed, A.; Huppi, R.; Baker, K. Bibcode: 1975GeoRL...2..235B Altcode: Resolved spectra have been obtained from the ground of the O2(a¹Δg) emissions from the upper atmosphere utilizing a wide-field interferometer with a cryogenically cooled germanium detector. The rotational structure of both the (0, 0) band at 1.27 µm and the (0, 1) band at 1.58 µm are clearly separable from the hydroxyl airglow. The decay rate of the O2(a¹Δg) during the twilight transition has been observed. Title: Mariner-Venus-Mercury 1973 project history. Part 2. Authors: Baker, D. Bibcode: 1975SpFl...17..191B Altcode: During December, 1973, as Mariner 10 continued on its course toward Venus, recurrent problems were encountered with the feed system of the spacecraft's steerable dish antenna. The final trajectory correction maneuver, TCM-2, was accomplished on January 21, 1975, and the spacecraft passed Venus at a distance of 3585 miles on February 5, 1974. After the TCM-3 burn on March 16, Mariner 10 passed within 460 miles of Mercury on March 29. The second Mercury encounter occurred on September 21, 1974. Title: Mariner-Venus-Mercury 1973 project history. Part 1. Authors: Baker, D. Bibcode: 1975SpFl...17..131B Altcode: Mariner-Venus-Mercury 1973 (MVM 73) was officially endorsed by the Space Science Board of the National Academy of Science in 1968. In February 1970, the initial Program Authorization Document was signed and a project office was set up. NASA plans for MVM-73 anticipated a launch during the period from November 1 to December 15, 1973. The actual launch took place on November 3, 1973. On November 28, Mariner 10 was 5.5 million miles from earth and 48.1 million miles from Venus. Title: A history of the Saturn I/IB launchers Authors: Baker, D. Bibcode: 1975SpFl...17..146B Altcode: Studies concerning the development of a liquid propellant booster using a cluster of conventional rocket motors to produce a total thrust of 1.5 million pounds began in April 1957. By November 1958 four flight test vehicles had been approved. On January 18, 1960, the Saturn project was approved as a program of highest national priority. Attention is given to handling problems concerning the various Saturn stages, questions of payload capability, major changes to the Saturn C-1 program in connection with the Apollo program, the first C-1 launching on October 27, 1961, and plans for Nova. Title: Report from Jupiter - 2. Authors: Baker, D. Bibcode: 1975SpFl...17..102B Altcode: The exploration of the planet Jupiter with the aid of the spacecraft Pioneer 10 is discussed. Pioneer 10 had been launched on Mar. 2, 1972. The closest approach of the spacecraft to Jupiter came on Dec. 3, 1973, when Pioneer 10 passed within 81,000 miles of the cloud tops of the gigantic planet. The journey of Pioneer 10 through the asteroid belt is briefly reviewed and the various stages of the encounter of the spacecraft with Jupiter are described. The characteristics of the Jovian environment are considered along with details regarding the Galilean satellites, the Jovian radiation belts, and the new perspective on Jupiter obtained as a result of the Pioneer-10 data. Title: Skylab: the three month vigil. Part 3. Authors: Baker, D. Bibcode: 1975SpFl...17...11B Altcode: No abstract at ADS Title: The Russian Venus probes. Authors: Baker, D. Bibcode: 1975SpFl...17..446B Altcode: No abstract at ADS Title: Ranger 7. Authors: Baker, D. Bibcode: 1974SpFl...16..276B Altcode: No abstract at ADS Title: Skylab: the three month vigil. II. Authors: Baker, D. Bibcode: 1974SpFl...16..456B Altcode: No abstract at ADS Title: Report from Jupiter. Part 1. Authors: Baker, D. Bibcode: 1974SpFl...16..140B Altcode: No abstract at ADS Title: The large space telescope. Authors: Baker, D. Bibcode: 1974SpFl...16....7B Altcode: No abstract at ADS Title: Skylab: 59 days in space. Part four. Authors: Baker, D. Bibcode: 1974SpFl...16..305B Altcode: No abstract at ADS Title: Skylab: 59 days in space. Part three. Authors: Baker, D. Bibcode: 1974SpFl...16..206B Altcode: No abstract at ADS Title: Skylab: 59 days in space. Part 1, 2. Authors: Baker, D. Bibcode: 1974SpFl...16...55B Altcode: No abstract at ADS Title: Mariner 4. Authors: Baker, D. Bibcode: 1974SpFl...16..418B Altcode: No abstract at ADS Title: Skylab: the three month vigil. Authors: Baker, D. Bibcode: 1974SpFl...16..412B Altcode: No abstract at ADS Title: The last Apollo - 1, 2, 3. Authors: Baker, D. Bibcode: 1973SpFl...15...42B Altcode: No abstract at ADS Title: Skylab - the diary of a rescue mission. Part 1. Authors: Baker, D. Bibcode: 1973SpFl...15..334B Altcode: No abstract at ADS Title: Skylab - The diary of a rescue mission. Part 2, 3. Authors: Baker, D. Bibcode: 1973SpFl...15..377B Altcode: No abstract at ADS Title: Negative Ion Composition of the D and E-Regions During a PCA Authors: Narcisi, R. S.; Sherman, C.; Philbrick, C. R.; Thomas, D. M.; Bailey, A. D.; Wlodyka, L. E.; Wlodyka, R. A.; Baker, D.; Federico, G. Bibcode: 1972spen.conf..411N Altcode: No abstract at ADS Title: Positive Ion Composition of the D and E-Regions During a PCA Authors: Narcisi, R. S.; Philbrick, C. R.; Thomas, D. M.; Bailey, A. D.; Wlodyka, L. E.; Baker, D.; Federico, G.; Wlodyka, R.; Gardner, M. E. Bibcode: 1972spen.conf..421N Altcode: No abstract at ADS Title: Mission to Descartes - 1. Authors: Baker, D. Bibcode: 1972SpFl...14..246B Altcode: No abstract at ADS Title: Pioneers to Jupiter. Authors: Baker, D. Bibcode: 1972SpFl...14..111B Altcode: No abstract at ADS Title: Mission to Descartes - 2. Authors: Baker, D. Bibcode: 1972SpFl...14..287B Altcode: No abstract at ADS Title: Lunar roving vehicle: Design report. Authors: Baker, D. Bibcode: 1971SpFl...13..234B Altcode: No abstract at ADS Title: Space Station Situation Report - 2. The McDonnell-Douglas proposal. Authors: Baker, D. Bibcode: 1971SpFl...13..344B Altcode: No abstract at ADS Title: Skylab. Authors: Baker, D. Bibcode: 1971SpFl...13..335B Altcode: No abstract at ADS Title: Expedition to Hadley-Apennine - 3. Authors: Baker, D. Bibcode: 1971SpFl...13..468B Altcode: No abstract at ADS Title: Apollo 14: A visit to Fra Mauro - 3. Authors: Baker, D. Bibcode: 1971SpFl...13..373B Altcode: No abstract at ADS Title: Orbitas bases. Space Station Situation Report - 1: The North American Rockwell proposal. Authors: Baker, D. Bibcode: 1971SpFl...13..318B Altcode: No abstract at ADS Title: Apollo 14: A visit to Fra Mauro, 1, 2. Authors: Baker, D. Bibcode: 1971SpFl...13..164B Altcode: No abstract at ADS Title: a Large Aperture, High-Resolution Field-Widened Interferometer-Spectrometer for Airglow Studies Authors: Despain, A.; Brown, F., Jr.; Steed, A.; Baker, D. Bibcode: 1971fosp.conf..293D Altcode: No abstract at ADS Title: Expedition to Hadley-Apennine - 1. Authors: Baker, D. Bibcode: 1971SpFl...13..358B Altcode: No abstract at ADS Title: Expedition to Hadley-Apennine - 2. Authors: Baker, D. Bibcode: 1971SpFl...13..431B Altcode: No abstract at ADS Title: NASA explores the solar system. Authors: Baker, D. Bibcode: 1971SpFl...13...42B Altcode: No abstract at ADS Title: Apollo 11: A systems analysis. Authors: Baker, D. Bibcode: 1970SpFl...12...35B Altcode: No abstract at ADS Title: Lunar landing dust. Authors: Baker, D. Bibcode: 1970SpFl...12..336B Altcode: No abstract at ADS Title: The Apollo spacecraft: Guidance and navigation. Authors: Baker, D. Bibcode: 1969SpFl...11..386B Altcode: No abstract at ADS