Author: "Lockheed Martin Advanced Technology Center (ATC)" / Topic: 0105 earth and related environmental sciences - Searchworks@Jio Institute Digital Library Search Results

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19 results on '"Lockheed Martin Advanced Technology Center (ATC)"'

1. Ion chemistry in the coma of comet 67P near perihelion

Author: Martin Rubin, Michael G. Rinaldi, J. De Keyser, Peter Wurz, Michael R. Combi, Stephen A. Fuselier, Thierry Sémon, Kathrin Altwegg, Kirk C. Hansen, Ulrich Mall, Myrtha Hässig, Erik Vigren, B. Fiethe, Jean-Jacques Berthelier, C. Y. Tzou, Tamas I. Gombosi, Gaël Cessateur, H. Rème, C. Briois, Léna Le Roy, J. H. Waite, James L. Burch, Arnaud Beth, Hans Balsiger, Karlheinz Trattner, S. M. Petrinec, André Bieler, Kathleen Mandt, Marina Galand, Herbert Gunell, K. L. Heritier, Ursina Calmonte, Adrienn Luspay-Kuti, A. Korth, T. W. Broiles, Sébastien Gasc, Space Science Division [San Antonio], Southwest Research Institute [San Antonio] ( SwRI ), UTSA Department of Physics and Astronomy [San Antonio], The University of Texas at San Antonio ( UTSA ), Physikalisches Institut [Bern], Universität Bern [Bern], IMPEC - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales ( LATMOS ), Université de Versailles Saint-Quentin-en-Yvelines ( UVSQ ) -Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ) -Université de Versailles Saint-Quentin-en-Yvelines ( UVSQ ) -Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ), Department of Physics [London], Imperial College London, Department of Atmospheric, Oceanic, and Space Sciences [Ann Arbor] ( AOSS ), University of Michigan [Ann Arbor], Laboratoire de Physique et Chimie de l'Environnement et de l'Espace ( LPC2E ), Institut national des sciences de l'Univers ( INSU - CNRS ) -Université d'Orléans ( UO ) -Centre National de la Recherche Scientifique ( CNRS ), Belgian Institute for Space Aeronomy / Institut d'Aéronomie Spatiale de Belgique ( BIRA-IASB ), Institute of Computer and Network Engineering [Braunschweig] ( IDA ), Technische Universität Braunschweig [Braunschweig], Max-Planck-Institut für Sonnensystemforschung ( MPS ), Lockheed Martin Advanced Technology Center ( ATC ), Institut de recherche en astrophysique et planétologie ( IRAP ), Université Paul Sabatier - Toulouse 3 ( UPS ) -Observatoire Midi-Pyrénées ( OMP ) -Centre National de la Recherche Scientifique ( CNRS ), Laboratory for Atmospheric and Space Physics [Boulder] ( LASP ), University of Colorado Boulder [Boulder], Swedish Institute of Space Physics [Uppsala] ( IRF ), Southwest Research Institute [San Antonio] (SwRI), The University of Texas at San Antonio (UTSA), PLANETO - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Department of Physics [Imperial College London], Department of Atmospheric, Oceanic, and Space Sciences [Ann Arbor] (AOSS), University of Michigan System-University of Michigan System, Laboratoire de Physique et Chimie de l'Environnement et de l'Espace (LPC2E), Observatoire des Sciences de l'Univers en région Centre (OSUC), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Belgian Institute for Space Aeronomy / Institut d'Aéronomie Spatiale de Belgique (BIRA-IASB), Institute of Computer and Network Engineering [Braunschweig] (IDA), Technische Universität Braunschweig = Technical University of Braunschweig [Braunschweig], Max-Planck-Institut für Sonnensystemforschung (MPS), Max-Planck-Gesellschaft, Lockheed Martin Advanced Technology Center (ATC), Institut de recherche en astrophysique et planétologie (IRAP), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Laboratory for Atmospheric and Space Physics [Boulder] (LASP), University of Colorado [Boulder], Swedish Institute of Space Physics [Uppsala] (IRF), Universität Bern [Bern] (UNIBE), Max-Planck-Institut für Sonnensystemforschung = Max Planck Institute for Solar System Research (MPS), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), and Science and Technology Facilities Council (STFC)
Subjects: 010504 meteorology & atmospheric sciences, 530 Physics, individual [comets], Comet, [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], Coma (optics), Astrophysics, Equinox, Astronomy & Astrophysics, Mass spectrometry, 01 natural sciences, Ion, general [comets], Fusion, plasma och rymdfysik, Comet nucleus, 0103 physical sciences, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, Physics, 520 Astronomy, Astronomy, Astronomy and Astrophysics, Plasma, 620 Engineering, plasmas, Fusion, Plasma and Space Physics, [ SDU.ASTR.EP ] Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], 0201 Astronomical And Space Sciences, Solar wind, solar wind, 13. Climate action, Space and Planetary Science
Abstract: The ESLAB 50 Symposium - spacecraft at comets from 1P/Halley to 67P/Churyumov-Gerasimenko; International audience; The coma and the comet-solar wind interaction of comet 67P/Churyumov-Gerasimenko changed dramatically from the initial Rosetta spacecraft encounter in August 2014 through perihelion in August 2015. Just before equinox (at 1.6 AU from the Sun), the solar wind signal disappeared and two regions of different cometary ion characteristics were observed. These “outer” and “inner” regions have cometary ion characteristics similar to outside and inside the ion pileup region observed during the Giotto approach to comet 1P/Halley. Rosetta/DFMS ion mass spectrometer observations are used here to investigate the H3O+/H2O+ ratio in the outer and inner regions at 67P/ Churyumov-Gerasimenko. The H3O+/H2O+ ratio and the H3O+ signal are observed to increase in the transition from the outer to the inner region and the H3O+ signal appears to be weakly correlated with cometary ion energy. These ion composition changes are similar to the ones observed during the 1P/Halley flyby. Modeling is used to determine the importance of neutral composition and transport of neutrals and ions away from the nucleus. This modeling demonstrates that changes in the H3O+/H2O+ ratio appear to be driven largely by transport properties and only weakly by neutral composition in the coma.
Published: 2016
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2. Changes in granulation scales over the solar cycle seen with SDO/HMI and Hinode/SOT

Author: Jérôme Ballot, J. M. Malherbe, Z. Frank, Th. Roudier, Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Laboratoire d'études spatiales et d'instrumentation en astrophysique = Laboratory of Space Studies and Instrumentation in Astrophysics (LESIA), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Lockheed Martin Solar and Astrophysics Laboratory (LMSAL), Lockheed Martin Advanced Technology Center (ATC), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA (UMR_8109)), and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP)
Subjects: Convection, 010504 meteorology & atmospheric sciences, Granule (solar physics), FOS: Physical sciences, Context (language use), Astrophysics, 01 natural sciences, Sun: granulation, Granulation, Sun: activity, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), 0105 earth and related environmental sciences, Physics, integumentary system, [SDU.ASTR.SR]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], food and beverages, Astronomy and Astrophysics, Solar maximum, Solar cycle, Astrophysics - Solar and Stellar Astrophysics, Convection zone, 13. Climate action, Space and Planetary Science, Physics::Space Physics, Maximum density, Astrophysics::Earth and Planetary Astrophysics
Abstract: The Sun is the only star where the superficial turbulent convection can be observed at very high spatial resolution. The Solar Dynamics Observatory (SDO) has continuously observed the full Sun from space with multi-wavelength filters since July 2010. In particular, the Helioseismic and Magnetic Imager (HMI) instrument takes high-cadence frames (45 seconds) of continuum intensity in which solar granulation is visible. We aimed to follow the evolution of the solar granules over an activity cycle and look for changes in their spatial properties. We investigated the density of granules and their mean area derived directly from the segmentation of deconvolved images from SDO/HMI. To perform the segmentation, we define granules as convex elements of images. We measured an approximately 2% variation in the density and the mean area of granules over the cycle, the density of granules being greater at solar maximum with a smaller granule mean area. The maximum density appears to be delayed by about one year compared to classical activity indicators, such as the sunspot number. We complemented this study with high-spatial-resolution observations obtained with Hinode/SOTBFI (Solar Optical Telescope Broadband Filter Imager), which are consistent with our results. The observed variations in solar granulation at the disc centre reveal a direct insight into the change in the physical properties that occur in the upper convective zone during a solar cycle. These variations can be due to interactions between convection and magnetic fields, either at the global scale or, locally, at the granulation scale., Comment: 10 pages, 17 figures, accepted for publication in Astronomy and Astrophysics
Published: 2021
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3. On the Ubiquity of Magnetic Reconnection Inside Flux Transfer Event‐Like Structures at the Earth's Magnetopause

Author: Michael O. Chandler, Elena Grigorenko, S. M. Petrinec, Hiroshi Hasegawa, Charlie J. Farrugia, Victoria N. Coffey, W. R. Paterson, C. Schiff, John C. Dorelli, Thomas E. Moore, Marit Øieroset, S. Fadanelli, K. J. Trattner, Sergio Toledo-Redondo, Jonathan Eastwood, S. A. Fuselier, T. D. Phan, C. J. Pollock, J. A. Sauvaud, Benoit Lavraud, Yoshitaka Saito, Q. Lenouvel, C. Jacquey, Philippe Garnier, James L. Burch, D. J. Gershman, R. Kieokaew, N. Fargette, D. L. A. Avanov, S. E. Smith, Vincent Génot, Emmanuel Penou, Barbara L. Giles, Science and Technology Facilities Council (STFC), Institut de recherche en astrophysique et planétologie (IRAP), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Space Sciences Laboratory [Berkeley] (SSL), University of California [Berkeley], University of California-University of California, Centre de physique moléculaire optique et hertzienne (CPMOH), Centre National de la Recherche Scientifique (CNRS)-Université Sciences et Technologies - Bordeaux 1, Space Science Division [San Antonio], Southwest Research Institute [San Antonio] (SwRI), Lockheed Martin Advanced Technology Center (ATC), Institute of Space and Astronautical Science (ISAS), Japan Aerospace Exploration Agency [Sagamihara] (JAXA), Laboratoire de microbiologie et génétique moléculaires (LMGM), Centre de Biologie Intégrative (CBI), Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Centre National de la Recherche Scientifique (CNRS), NASA Goddard Space Flight Center (GSFC), Laboratoire de Parasitologie-Mycologie, Assistance publique - Hôpitaux de Paris (AP-HP) (AP-HP)-Hôpital Henri Mondor-Université Paris-Est Créteil Val-de-Marne - Paris 12 (UPEC UP12), NASA Headquarters, Space Research Institute of the Russian Academy of Sciences (IKI), Russian Academy of Sciences [Moscow] (RAS), Hokkaido University [Sapporo, Japan], Centre d'Immunologie de Marseille - Luminy (CIML), Institut National de la Santé et de la Recherche Médicale (INSERM)-Centre National de la Recherche Scientifique (CNRS)-Aix Marseille Université (AMU), Joint Global Change Research Institute, Pacific Northwest National Laboratory (PNNL)-University of Maryland [College Park], University of Maryland System-University of Maryland System, Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), University of California [Berkeley] (UC Berkeley), University of California (UC)-University of California (UC), Université Sciences et Technologies - Bordeaux 1 (UB)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de microbiologie et génétique moléculaires - UMR5100 (LMGM), Université de Toulouse (UT)-Université de Toulouse (UT)-Centre National de la Recherche Scientifique (CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Centre National de la Recherche Scientifique (CNRS), Aix Marseille Université (AMU)-Institut National de la Santé et de la Recherche Médicale (INSERM)-Centre National de la Recherche Scientifique (CNRS), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Université Sciences et Technologies - Bordeaux 1-Centre National de la Recherche Scientifique (CNRS), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), and Génot, Vincent
Subjects: Physics, 010504 meteorology & atmospheric sciences, [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], [SDU.ASTR.EP] Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], Magnetic reconnection, Geophysics, 01 natural sciences, Physics::Space Physics, 0103 physical sciences, Meteorology & Atmospheric Sciences, General Earth and Planetary Sciences, Magnetopause, Flux transfer event, 010303 astronomy & astrophysics, ComputingMilieux_MISCELLANEOUS, Earth (classical element), 0105 earth and related environmental sciences
Abstract: Flux transfer events (FTEs) are transient phenomena frequently observed at the Earth's magnetopause. Their usual interpretation is a flux rope moving away from the reconnection region. However, the Magnetospheric Multiscale Mission revealed that magnetic reconnection sometimes occurs inside these structures, questioning their flux rope configuration. Here we investigate 229 FTE‐type structures and find reconnection signatures inside 19% of them. We analyze their large‐scale magnetic topology using electron heat flux and find that it is significantly different across the FTE reconnecting current sheets, demonstrating that they are constituted of two magnetically disconnected structures. We also find that the interplanetary magnetic field (IMF) associated with reconnecting FTEs presents a strong By component. We discuss several formation mechanisms to explain these observations. In particular, the maximum magnetic shear model predicts that for large IMF By, two spatially distinct X lines coexist at the magnetopause. They can generate separate magnetic flux tubes that may become interlaced.
Published: 2020
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4. Mass Loading the Earth's Dayside Magnetopause Boundary Layer and Its Effect on Magnetic Reconnection

Author: Paul Tenfjord, Robert J. Strangeway, Daniel B. Graham, Stein Haaland, Thomas E. Moore, S. A. Fuselier, Benoit Lavraud, Michael Hesse, Wenya Li, James L. Burch, Sarah K. Vines, K. J. Trattner, Jérémy Dargent, S. M. Petrinec, Mats André, Katariina Nykyri, Alex Glocer, Sergio Toledo-Redondo, C. R. Chappell, L. M. Kistler, Michael H. Denton, N. Aunai, L. Alm, Lockheed Martin Advanced Technology Center (ATC), European Space Agency (ESA), Swedish Institute of Space Physics [Uppsala] (IRF), Laboratoire de Physique des Plasmas (LPP), Université Paris-Saclay-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris-Sud - Paris 11 (UP11)-École polytechnique (X)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), Max-Planck-Institut für Extraterrestrische Physik (MPE), NASA Goddard Space Flight Center (GSFC), EOS Space Science Center [Durham], University of New Hampshire (UNH), Institut de recherche en astrophysique et planétologie (IRAP), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), CFD Lab [Montréal], Department of Mechanical Engineering [Montréal], McGill University = Université McGill [Montréal, Canada]-McGill University = Université McGill [Montréal, Canada], Agence Spatiale Européenne = European Space Agency (ESA), Université Paris-Sud - Paris 11 (UP11)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École polytechnique (X)-Sorbonne Université (SU)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), and Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS)
Subjects: Physics, 010504 meteorology & atmospheric sciences, Field line, [SDU.STU.GP]Sciences of the Universe [physics]/Earth Sciences/Geophysics [physics.geo-ph], Magnetic reconnection, 010502 geochemistry & geophysics, 01 natural sciences, Computational physics, Magnetic field, Boundary layer, Geophysics, Magnetosheath, Physics::Plasma Physics, Physics::Space Physics, General Earth and Planetary Sciences, Magnetopause, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Ionosphere, Interplanetary magnetic field, 0105 earth and related environmental sciences
Abstract: International audience; When the interplanetary magnetic field is northward for a period of time, O + from the high-latitude ionosphere escapes along reconnected magnetic field lines into the dayside magnetopause boundary layer. Dual-lobe reconnection closes these field lines, which traps O + and mass loads the boundary layer. This O + is an additional source of magnetospheric plasma that interacts with magnetosheath plasma through magnetic reconnection. This mass loading and interaction is illustrated through analysis of a magnetopause crossing by the Magnetospheric Multiscale spacecraft. While in the O +-rich boundary layer, the interplanetary magnetic field turns southward. As the Magnetospheric Multiscale spacecraft cross the high-shear magnetopause, reconnection signatures are observed. While the reconnection rate is likely reduced by the mass loading, reconnection is not suppressed at the magnetopause. The high-latitude dayside ionosphere is therefore a source of magnetospheric ions that contributes often to transient reduction in the reconnection rate at the dayside magnetopause.
Published: 2019
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5. Comparison of neutral outgassing of comet 67P/Churyumov-Gerasimenko inbound and outbound beyond 3 AU from ROSINA/DFMS

Author: S. M. Petrinec, S. A. Fuselier, O. Mousis, Urs Mall, Arnaud Beth, Jean-Jacques Berthelier, Kathleen Mandt, K. J. Trattner, Myrtha Hässig, George Livadiotis, Peter Wurz, B. Fiethe, Tamas I. Gombosi, Adrienn Luspay-Kuti, Kirk C. Hansen, Chia-Yu Tzou, Kathrin Altwegg, Frederik Dhooghe, Martin Rubin, Johns Hopkins University Applied Physics Laboratory [Laurel, MD] (APL), Physikalisches Institut [Bern], Universität Bern [Bern], Center for Space and Habitability (CSH), University of Bern, PLANETO - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), Sorbonne Université (SU)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), Department of Physics [Imperial College London], Imperial College London, Belgian Institute for Space Aeronomy / Institut d'Aéronomie Spatiale de Belgique (BIRA-IASB), Centre for Mathematical Plasma-Astrophysics [Leuven] (CmPA), Catholic University of Leuven - Katholieke Universiteit Leuven (KU Leuven), Institute of Computer and Network Engineering [Braunschweig] (IDA), Technische Universität Braunschweig = Technical University of Braunschweig [Braunschweig], Southwest Research Institute [San Antonio] (SwRI), Department of Climate and Space Sciences and Engineering (CLaSP), University of Michigan [Ann Arbor], University of Michigan System-University of Michigan System, Max-Planck-Institut für Sonnensystemforschung (MPS), Max-Planck-Gesellschaft, Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Lockheed Martin Advanced Technology Center (ATC), Laboratory for Atmospheric and Space Physics [Boulder] (LASP), University of Colorado [Boulder], Universität Bern [Bern] (UNIBE), Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), and Max-Planck-Institut für Sonnensystemforschung = Max Planck Institute for Solar System Research (MPS)
Subjects: Insolation, Physics, 010504 meteorology & atmospheric sciences, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 520 Astronomy, Comet, Astronomy and Astrophysics, Context (language use), Coma (optics), Equinox, Astrophysics, 620 Engineering, 01 natural sciences, Article, On board, Outgassing, 13. Climate action, Space and Planetary Science, 0103 physical sciences, 010303 astronomy & astrophysics, Southern Hemisphere, 0105 earth and related environmental sciences
Abstract: Context.Pre-equinox measurements of comet 67P/Churyumov-Gerasimenko with the mass spectrometer ROSINA/DFMS on board the Rosetta spacecraft revealed a strongly heterogeneous coma. The abundances of major and various minor volatile species were found to depend on the latitude and longitude of the nadir point of the spacecraft. The observed time variability of coma species remained consistent for about three months up to equinox. The chemical variability could be generally interpreted in terms of surface temperature and seasonal effects superposed on some kind of chemical heterogeneity of the nucleus.Aims.We compare here pre-equinox (inbound) ROSINA/DFMS measurements from 2014 to measurements taken after the outbound equinox in 2016, both at heliocentric distances larger than 3 AU. For a direct comparison we limit our observations to the southern hemisphere.Methods.We report the similarities and differences in the concentrations and time variability of neutral species under similar insolation conditions (heliocentric distance and season) pre- and post-equinox, and interpret them in light of the previously published observations. In addition, we extend both the pre- and post-equinox analysis by comparing species concentrations with a mixture of CO2and H2O.Results.Our results show significant changes in the abundances of neutral species in the coma from pre- to post-equinox that are indicative of seasonally driven nucleus heterogeneity.Conclusions.The observed pre- and post-equinox patterns can generally be explained by the strong erosion in the southern hemisphere that moves volatile-rich layers near the surface.
Published: 2019
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6. Nonlobe Reconnection at the Earth's Magnetopause for Northward IMF

Author: K. J. Trattner, S. M. Petrinec, S. A. Fuselier, J. Mukherjee, Benoit Lavraud, Lockheed Martin Advanced Technology Laboratories (ATL), Lockheed Martin Advanced Technology Laboratories, Lockheed Martin Advanced Technology Center (ATC), Institut de recherche en astrophysique et planétologie (IRAP), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), and Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS)
Subjects: Physics, 010504 meteorology & atmospheric sciences, Field line, [PHYS.ASTR.EP]Physics [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], Magnetosphere, Magnetic reconnection, Geophysics, 010502 geochemistry & geophysics, 01 natural sciences, Solar wind, Current sheet, Magnetosheath, Space and Planetary Science, Physics::Space Physics, Magnetopause, Astrophysics::Solar and Stellar Astrophysics, Interplanetary magnetic field, 0105 earth and related environmental sciences
Abstract: International audience; Under northward interplanetary magnetic field conditions, magnetic reconnection at the Earth's magnetopause is usually thought to operate through the merging of magnetosheath magnetic field lines and open magnetic field lines from the magnetospheric lobe. However, reconnection also occurs between magnetosheath field lines and closed magnetic field lines in the magnetosphere. Under certain conditions, this nonlobe field line reconnection has distinct plasma and magnetic field signatures that distinguish it from reconnection of lobe field lines. A survey of these conditions suggests that nonlobe reconnection at the Earth's magnetopause may be common even for relatively strong northward IMF. Plain Language Summary Magnetic reconnection interconnects magnetic field lines across a current sheet like that at the Earth's magnetopause or like that in the solar corona. This paper describes a type of interconnection of magnetic field lines at the magnetopause that was first reported for the solar corona. It appears that this type of reconnection is fairly common at the magnetopause. The different topology of this reconnection suggests a different type of interaction between the magnetic field lines in the solar wind and the field lines of the Earth.
Published: 2018
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7. Solar Ultraviolet Bursts

Author: Shin Toriumi, Chris J. Nelson, Luc Rouppe van der Voort, Kevin Reardon, Hardi Peter, Peter R. Young, Maria S. Madjarska, Sanja Danilovic, Petr Heinzel, Brigitte Schmieder, Gregal J. M. Vissers, Zhenghua Huang, Lakshmi Pradeep Chitta, Yukio Katsukawa, A. Berlicki, Robert J. Rutten, C. A. Madsen, Mark C. M. Cheung, Hui Tian, Centre for Research on Environmental Systems and Statistics (CRES), Lancaster University, Shandong Agricultural University (SDAU), Observatoire de Paris - Site de Paris (OP), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA (UMR_8109)), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), NASA Goddard Space Flight Center (GSFC), School of Earth and Space Sciences [Beijing], Peking University [Beijing], Max Planck Institute for Solar System Research (MPS), Max-Planck-Gesellschaft, Institute of Theoretical Astrophysics [Oslo], University of Oslo (UiO), Astrophysics Research Centre [Belfast] (ARC), Queen's University [Belfast] (QUB), Albanova University Centre, National Astronomical Observatory of Japan (NAOJ), Astronomical Institute [Wroclaw], University of Wrocław [Poland] (UWr), Lockheed Martin Solar and Astrophysics Laboratory (LMSAL), Lockheed Martin Advanced Technology Center (ATC), Harvard-Smithsonian Center for Astrophysics (CfA), Smithsonian Institution-Harvard University [Cambridge], Centre National de la Recherche Scientifique (CNRS)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Institut national des sciences de l'Univers (INSU - CNRS), and PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)
Subjects: 010504 meteorology & atmospheric sciences, FEATURES, Flux, Astrophysics, medicine.disease_cause, 01 natural sciences, transition region [Sun], MAGNETIC RECONNECTION, Astrophysics::Solar and Stellar Astrophysics, activity [Sun], Sun: transition region, 010303 astronomy & astrophysics, ComputingMilieux_MISCELLANEOUS, EXPLOSIVE EVENTS, [PHYS]Physics [physics], Physics, Astrophysics - Solar and Stellar Astrophysics, Physical Sciences, Physics::Space Physics, SI-IV, Space Science, atmosphere [Sun], H-ALPHA, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astronomy & Astrophysics, Atmosphere, ELLERMAN BOMBS, Sun: activity, 0103 physical sciences, medicine, Solar and Stellar Astrophysics (astro-ph.SR), TRANSITION-REGION BLINKERS, 0105 earth and related environmental sciences, UV radiation [Sun], Photosphere, Sunspot, Science & Technology, Astronomy and Astrophysics, Magnetic reconnection, IV BURSTS, Sun: UV radiation, Planetary science, QUIET-SUN, 13. Climate action, Space and Planetary Science, EMERGING FLUX, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Sun: atmosphere, Ultraviolet
Abstract: The term "ultraviolet (UV) burst" is introduced to describe small, intense, transient brightenings in ultraviolet images of solar active regions. We inventorize their properties and provide a definition based on image sequences in transition-region lines. Coronal signatures are rare, and most bursts are associated with small-scale, canceling opposite-polarity fields in the photosphere that occur in emerging flux regions, moving magnetic features in sunspot moats, and sunspot light bridges. We also compare UV bursts with similar transition-region phenomena found previously in solar ultraviolet spectrometry and with similar phenomena at optical wavelengths, in particular Ellerman bombs. Akin to the latter, UV bursts are probably small-scale magnetic reconnection events occurring in the low atmosphere, at photospheric and/or chromospheric heights. Their intense emission in lines with optically thin formation gives unique diagnostic opportunities for studying the physics of magnetic reconnection in the low solar atmosphere. This paper is a review report from an International Space Science Institute team that met in 2016-2017., Review article accepted for publication in Space Science Reviews
Published: 2018
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8. Two sources of magnetosheath ions observed by Cluster in the mid-altitude polar cusp

Author: C. P. Escoubet, Andrew Fazakerley, Matthew Taylor, M. W. Dunlop, Arnaud Masson, Frederic Pitout, H. E. Laakso, C. Vallat, H. Rème, J. M. Bosqued, Jean Berchem, Karlheinz Trattner, Iannis Dandouras, European Space Research and Technology Centre (ESTEC), European Space Agency (ESA), Institute of Geophysics and Planetary Physics [Los Angeles] (IGPP), University of California [Los Angeles] (UCLA), University of California-University of California, Centre d'étude spatiale des rayonnements (CESR), Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées, Lockheed Martin Advanced Technology Center (ATC), Max-Planck-Institut für Extraterrestrische Physik (MPE), Space Science and Technology Department [Didcot] (RAL Space), STFC Rutherford Appleton Laboratory (RAL), Science and Technology Facilities Council (STFC)-Science and Technology Facilities Council (STFC), Mullard Space Science Laboratory (MSSL), and University College of London [London] (UCL)
Subjects: Atmospheric Science, 010504 meteorology & atmospheric sciences, Mathematics::Number Theory, Population, Aerospace Engineering, Magnetosphere, Subsolar point, Astrophysics, Atmospheric sciences, 01 natural sciences, Magnetosheath, 0103 physical sciences, Interplanetary magnetic field, education, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, Physics, education.field_of_study, Astronomy and Astrophysics, Magnetic reconnection, Magnetopause, Geophysics, 13. Climate action, Space and Planetary Science, Magnetospheric physics, Physics::Space Physics, General Earth and Planetary Sciences, Cusp (anatomy), Cusp and boundary layers
Abstract: International audience; Double cusps have been observed on a few occasions by polar orbiting spacecraft and ground-based observatories. The four Cluster spacecraft observed two distinct regions, showing characteristics of a double cusp, during a mid-altitude cusp pass on 7 August 2004. The Wind spacecraft detected a southward turning of the Interplanetary Magnetic Field (IMF) at the beginning of the cusp crossings and IMF-Bz stayed negative throughout. Cluster 4 observed a high energy step in the ion precipitation around 1 keV on the equatorward side of the cusp and a dense ion population in the cusp centre. Cluster 1, entering the cusp around 1 min later, observed only a partial ion dispersion with a low energy cutoff reaching 100 eV, together with the dense ion population in the cusp centre. About 9 min later, Cluster 3 entered the cusp and observed full ion dispersion from a few keV down to around 50 eV, together with the dense ion population in the centre of the cusp. The ion flow was directed poleward and eastward in the step/dispersion, whereas in the centre of the cusp the flow was directed poleward and westward. In addition the altitude of the source region of ion injection in the step/dispersion was found 50% larger than in the cusp centre. This event could be explained by the onset of dayside reconnection when the IMF turned southward. The step would be the first signature of component reconnection near the subsolar point, and the injection in the centre of the cusp a result of anti-parallel reconnection in the northern dusk side of the cusp. A three-dimensional magnetohydrodynamic (MHD) simulation is used to display the topology of the magnetic field and locate the sources of the ions during the event.
Published: 2008
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9. Rosina – Rosetta Orbiter Spectrometer for Ion and Neutral Analysis

Author: T Magoncelli, E. G. Shelley, Jenny Müller, E. Arijs, Christian Mazelle, Peter Bochsler, C. Aoustin, J. M. Illiano, Timm-Emanuel Riesen, H. Lauche, A. Loose, Stefano Livi, B. Fiethe, Tamas I. Gombosi, J. De Keyser, J. Fischer, Stephan Graf, Lennard A. Fisk, H. Rème, J. L. Medale, Jean-Jacques Berthelier, S. Scherer, Hermann Wollnik, Bruce P. Block, Peter Wurz, Annette Jäckel, Sandra Wüthrich, Kathrin Altwegg, Jean-André Sauvaud, S. Delanoye, U. Langer, Eernest Kopp, Eddy Neefs, D. T. Young, Fritz Gliem, Jean-Loup Bertaux, A. G. Ghielmetti, J. H. Waite, D. Nevejans, B. Wilken, A. Korth, M. Mildner, L. Duvet, Martin Rubin, Hans Balsiger, Peter Eberhardt, K Heerlein, G. R. Carignan, Stephen A. Fuselier, Ulrich Mall, Physikalisches Institut [Bern], Universität Bern [Bern], Belgian Institute for Space Aeronomy / Institut d'Aéronomie Spatiale de Belgique (BIRA-IASB), Centre d'étude spatiale des rayonnements (CESR), Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées, Centre d'étude des environnements terrestre et planétaires (CETP), Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Service d'aéronomie (SA), Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Lockheed Martin Advanced Technology Center (ATC), Max-Planck-Institut für Sonnensystemforschung (MPS), Max-Planck-Gesellschaft, Technische Universität Braunschweig = Technical University of Braunschweig [Braunschweig], Space Physics Research Laboratory [Ann Arbor] (SPRL), University of Michigan [Ann Arbor], University of Michigan System-University of Michigan System, Southwest Research Institute [San Antonio] (SwRI), Physikalisches Institut [Gießen], Justus-Liebig-Universität Gießen (JLU), Universität Bern [Bern] (UNIBE), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Max-Planck-Institut für Sonnensystemforschung = Max Planck Institute for Solar System Research (MPS), and Justus-Liebig-Universität Gießen = Justus Liebig University (JLU)
Subjects: [PHYS.PHYS.PHYS-AO-PH]Physics [physics]/Physics [physics]/Atmospheric and Oceanic Physics [physics.ao-ph], Physics, 010504 meteorology & atmospheric sciences, Spectrometer, Comet, Astronomy and Astrophysics, Mass spectrometry, 7. Clean energy, 01 natural sciences, Ion, law.invention, Astrobiology, Nuclear physics, Orbiter, Planetary science, Fragmentation (mass spectrometry), 13. Climate action, Space and Planetary Science, law, 0103 physical sciences, Formation and evolution of the Solar System, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences
Abstract: The Rosetta Orbiter Spectrometer for Ion and Neutral Analysis (ROSINA) will answer important questions posed by the mission's main objectives. After Giotto, this will be the first time the volatile part of a comet will be analyzed in situ. This is a very important investigation, as comets, in contrast to meteorites, have maintained most of the volatiles of the solar nebula. To accomplish the very demanding objectives through all the different phases of the comet's activity, ROSINA has unprecedented capabilities including very wide mass range (1 to >300 amu), very high mass resolution (m/Δ m > 3000, i.e. the ability to resolve CO from N2 and 13C from 12CH), very wide dynamic range and high sensitivity, as well as the ability to determine cometary gas velocities, and temperature. ROSINA consists of two mass spectrometers for neutrals and primary ions with complementary capabilities and a pressure sensor. To ensure that absolute gas densities can be determined, each mass spectrometer carries a reservoir of a calibrated gas mixture allowing in-flight calibration. Furthermore, identical flight-spares of all three sensors will serve for detailed analysis of all relevant parameters, in particular the sensitivities for complex organic molecules and their fragmentation patterns in our electron bombardment ion sources.
Published: 2007
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10. Solar Magnetic Field Reversals and the Role of Dynamo Families

Author: Marc L. DeRosa, Allan Sacha Brun, J. T. Hoeksema, Lockheed Martin Solar and Astrophysics Laboratory (LMSAL), Lockheed Martin Advanced Technology Center (ATC), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Hansen Experimental Physics Lab [Stanford] (HEPL), Stanford University, STARS2, European Project: 207430,EC:FP7:ERC,ERC-2007-StG,STARS2(2008), Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Hansen Experimental Physics Laboratory (HEPL), and Stanford University [Stanford]
Subjects: 010504 meteorology & atmospheric sciences, Polarity (physics), FOS: Physical sciences, Astrophysics, 7. Clean energy, 01 natural sciences, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), 0105 earth and related environmental sciences, Earth and Planetary Astrophysics (astro-ph.EP), Coupling, Physics, Solar observatory, Time evolution, Astronomy and Astrophysics, Magnetic field, Astrophysics - Solar and Stellar Astrophysics, 13. Climate action, Space and Planetary Science, Dynamo theory, Physics::Space Physics, Harmonic, Astrophysics - Earth and Planetary Astrophysics, Dynamo
Abstract: The variable magnetic field of the solar photosphere exhibits periodic reversals as a result of dynamo activity occurring within the solar interior. We decompose the surface field as observed by both the Wilcox Solar Observatory and the Michelson Doppler Imager into its harmonic constituents, and present the time evolution of the mode coefficients for the past three sunspot cycles. The interplay between the various modes is then interpreted from the perspective of general dynamo theory, where the coupling between the primary and secondary families of modes is found to correlate with large-scale polarity reversals for many examples of cyclic dynamos. Mean-field dynamos based on the solar parameter regime are then used to explore how such couplings may result in the various long-term trends in the surface magnetic field observed to occur in the solar case., Comment: Accepted to ApJ; comments/corrections to this article are welcome via e-mail, even after publication
Published: 2013
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11. Computer Vision for The Solar Dynamics Observatory

Author: Kelly E. Korreck, N.-E. Raouafi, Jean-François Hochedez, Manolis K. Georgoulis, S. Farid, A. Engell, Craig DeForest, Steven H. Saar, Thomas Wiegelmann, Yingna Su, Rafal A. Angryk, M. J. Wills-Davey, P. C. Grigis, R. Timmons, Antonia Savcheva, Jonathan Cirtain, I. De Moortel, Paola Testa, G. D. R. Attrill, Pietro N. Bernasconi, A. R. Davey, Justin C. Kasper, R. T. J. McAteer, Petrus C. Martens, Véronique Delouille, Harvard-Smithsonian Center for Astrophysics (CfA), Harvard University-Smithsonian Institution, Department of Physics [Bozeman], Montana State University (MSU), Department of Astronomy [Boston], Boston University [Boston] (BU), Johns Hopkins University Applied Physics Laboratory [Laurel, MD] (APL), Royal Observatory of Belgium [Brussels] (ROB), HELIOS - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), NASA Marshall Space Flight Center (MSFC), Southwest Research Institute [Boulder] (SwRI), Department of Computer Science [Bozeman], School of Mathematics and Statistics [St Andrews], University of St Andrews [Scotland], Max-Planck-Institut für Sonnensystemforschung = Max Planck Institute for Solar System Research (MPS), Max-Planck-Gesellschaft, Research Center for Astronomy and Applied Mathematics [Athens], Academy of Athens, Trinity College Dublin, Lockheed Martin Advanced Technology Center (ATC), Smithsonian Institution-Harvard University [Cambridge], and Max-Planck-Institut für Sonnensystemforschung (MPS)
Subjects: 010504 meteorology & atmospheric sciences, ComputingMethodologies_IMAGEPROCESSINGANDCOMPUTERVISION, Coronal hole, 01 natural sciences, Software, Heliophysics, Observatory, 0103 physical sciences, Coronal mass ejection, Astrophysics::Solar and Stellar Astrophysics, Computer vision, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, Physics, Sunspot, Solar observatory, business.industry, [SDU.ASTR.SR]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], Astronomy, Astronomy and Astrophysics, [PHYS.ASTR.SR]Physics [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], 13. Climate action, Space and Planetary Science, Physics::Space Physics, Large Angle and Spectrometric Coronagraph, Artificial intelligence, business
Abstract: International audience; In Fall 2008 NASA selected a large international consortium to produce a comprehensive automated feature-recognition system for the Solar Dynamics Observatory (SDO). The SDO data that we consider are all of the Atmospheric Imaging Assembly (AIA) images plus surface magnetic-field images from the Helioseismic and Magnetic Imager (HMI). We produce robust, very efficient, professionally coded software modules that can keep up with the SDO data stream and detect, trace, and analyze numerous phenomena, including flares, sigmoids, filaments, coronal dimmings, polarity inversion lines, sunspots, X-ray bright points, active regions, coronal holes, EIT waves, coronal mass ejections (CMEs), coronal oscillations, and jets. We also track the emergence and evolution of magnetic elements down to the smallest detectable features and will provide at least four full-disk, nonlinear, force-free magnetic field extrapolations per day. The detection of CMEs and filaments is accomplished with Solar and Heliospheric Observatory (SOHO)/Large Angle and Spectrometric Coronagraph (LASCO) and ground-based Hα data, respectively. A completely new software element is a trainable feature-detection module based on a generalized image-classification algorithm. Such a trainable module can be used to find features that have not yet been discovered (as, for example, sigmoids were in the pre-Yohkoh era). Our codes will produce entries in the Heliophysics Events Knowledgebase (HEK) as well as produce complete catalogs for results that are too numerous for inclusion in the HEK, such as the X-ray bright-point metadata. This will permit users to locate data on individual events as well as carry out statistical studies on large numbers of events, using the interface provided by the Virtual Solar Observatory. The operations concept for our computer vision system is that the data will be analyzed in near real time as soon as they arrive at the SDO Joint Science Operations Center and have undergone basic processing. This will allow the system to produce timely space-weather alerts and to guide the selection and production of quicklook images and movies, in addition to its prime mission of enabling solar science. We briefly describe the complex and unique data-processing pipeline, consisting of the hardware and control software required to handle the SDO data stream and accommodate the computer-vision modules, which has been set up at the Lockheed-Martin Space Astrophysics Laboratory (LMSAL), with an identical copy at the Smithsonian Astrophysical Observatory (SAO).
Published: 2012
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12. In situ mass spectrometry during the Lutetia flyby

Author: S. A. Fuselier, Henri Rème, Myrtha Hässig, Peter Wurz, J. De Keyser, Annette Jäckel, L. Hofer, B. Fiethe, B. Schläppi, Jean-Jacques Berthelier, Kathrin Altwegg, Ursina Calmonte, Urs Mall, Martin Rubin, Hans Balsiger, Physikalisches Institut [Bern], Universität Bern [Bern], HELIOS - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Belgian Institute for Space Aeronomy / Institut d'Aéronomie Spatiale de Belgique (BIRA-IASB), Institute of Computer and Network Engineering [Braunschweig] (IDA), Technische Universität Braunschweig = Technical University of Braunschweig [Braunschweig], Lockheed Martin Advanced Technology Center (ATC), Max-Planck-Institut für Sonnensystemforschung (MPS), Max-Planck-Gesellschaft, Centre d'étude spatiale des rayonnements (CESR), Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées, Institut de recherche en astrophysique et planétologie (IRAP), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), University of Michigan [Ann Arbor], University of Michigan System, Universität Bern [Bern] (UNIBE), Max-Planck-Institut für Sonnensystemforschung = Max Planck Institute for Solar System Research (MPS), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), and Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS)
Subjects: In situ, [PHYS.ASTR.IM]Physics [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], 010504 meteorology & atmospheric sciences, Spacecraft outgassing, [PHYS.ASTR.EP]Physics [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], ROSINA, Mass spectrometry, 01 natural sciences, Astrobiology, 0103 physical sciences, Rosetta, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, Physics, Spacecraft, business.industry, Astronomy, Astronomy and Astrophysics, Lutetia, in situ mass spectrometry, [SDU.ASTR.IM]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], Outgassing, 13. Climate action, Space and Planetary Science, Asteroid, Aspect angle, business, Exosphere
Abstract: International audience; During the Rosetta flyby at asteroid Lutetia the ROSINA instrument tried to detect a thin exosphere of the asteroid. Although the instrument is sensitive enough to detect even very tenuous gases at a density level of 1 cm−3 the Lutetia exosphere could not be unambiguously detected due to spacecraft outgassing, which was not constant because of the changing solar aspect angle. An upper limit for a water exosphere density at the flyby distance of 3160 km of (3.5±1.0)*103 cm−3 was deduced from the measurements.
Published: 2012
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13. Sun Earth Connection Coronal and Heliospheric Investigation (SECCHI)

Author: O. C. St. Cyr, Jeffrey S. Newmark, S. Cooper, T. Carter, C. J. Eyles, W. Deutsch, Simon Plunkett, James R. Lemen, E. Mentzell, Franck Delmotte, J. W. Cook, Christopher J. Davis, Richard A. Harrison, Dennis G. Socker, Joseph M. Davila, Kimberly I. Mehalick, Volker Bothmer, A. Moore, Jean-Pierre Wuelser, Russell A. Howard, V. Stephens, Marie-Françoise Ravet, R. Baugh, Jean-Philippe Halain, H. Mapson-Menard, N. Rich, Nicholas R. Waltham, C. J. Wolfson, A. Hurley, Dexter W. Duncan, Jean-Pierre Delaboudiniere, F. Auchère, Clarence M. Korendyke, William T. Thompson, Jean-Marc Defise, Emmanuel Mazy, G. Maahs, Pierre Rochus, Raymond Mercier, G. M. Simnett, J. Lang, D. R. McMullin, John D. Moses, T. D. Tarbell, Angelos Vourlidas, Dennis Wang, E. O. Hulburt Center for Space Research, Naval Research Laboratory (NRL), NASA Goddard Space Flight Center (GSFC), Lockheed Martin Solar and Astrophysics laboratory (LMSAL), Lockheed Martin Advanced Technology Center (ATC), Space Science and Technology Department [Didcot] (RAL Space), STFC Rutherford Appleton Laboratory (RAL), Science and Technology Facilities Council (STFC)-Science and Technology Facilities Council (STFC), Astrophysics and Space Research group [Birmingham], University of Birmingham [Birmingham], Centre Spatial de Liège (CSL), Université de Liège, Laboratoire Charles Fabry de l'Institut d'Optique / Scop, Laboratoire Charles Fabry de l'Institut d'Optique (LCFIO), Centre National de la Recherche Scientifique (CNRS)-Institut d'Optique Graduate School (IOGS)-Université Paris-Sud - Paris 11 (UP11)-Centre National de la Recherche Scientifique (CNRS)-Institut d'Optique Graduate School (IOGS)-Université Paris-Sud - Paris 11 (UP11), Institut d'astrophysique spatiale (IAS), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Sud - Paris 11 (UP11), Max-Planck-Institut für Sonnensystemforschung (MPS), Max-Planck-Gesellschaft, Interferometrics, Inc, HYTEC Inc., PRAXIS Inc., PRAXIS Inc, and Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)
Subjects: Solar System, 010504 meteorology & atmospheric sciences, 7. Clean energy, 01 natural sciences, law.invention, Telescope, Observatory, law, 0103 physical sciences, Coronal mass ejection, 14. Life underwater, 010303 astronomy & astrophysics, ComputingMilieux_MISCELLANEOUS, 0105 earth and related environmental sciences, Remote sensing, Physics, [PHYS.PHYS.PHYS-OPTICS]Physics [physics]/Physics [physics]/Optics [physics.optics], Spacecraft, business.industry, Astronomy, Astronomy and Astrophysics, Coronal loop, Space and Planetary Science, Large Angle and Spectrometric Coronagraph, business, Heliosphere
Abstract: The Sun Earth Connection Coronal and Heliospheric Investigation (SECCHI) is a five telescope package, which has been developed for the Solar Terrestrial Relation Observatory (STEREO) mission by the Naval Research Laboratory (USA), the Lockheed Solar and Astrophysics Laboratory (USA), the Goddard Space Flight Center (USA), the University of Birmingham (UK), the Rutherford Appleton Laboratory (UK), the Max Planck Institute for Solar System Research (Germany), the Centre Spatiale de Leige (Belgium), the Institut d’Optique (France) and the Institut d’Astrophysique Spatiale (France). SECCHI comprises five telescopes, which together image the solar corona from the solar disk to beyond 1 AU. These telescopes are: an extreme ultraviolet imager (EUVI: 1–1.7 R⊙), two traditional Lyot coronagraphs (COR1: 1.5–4 R⊙ and COR2: 2.5–15 R⊙) and two new designs of heliospheric imagers (HI-1: 15–84 R⊙ and HI-2: 66–318 R⊙). All the instruments use 2048×2048 pixel CCD arrays in a backside-in mode. The EUVI backside surface has been specially processed for EUV sensitivity, while the others have an anti-reflection coating applied. A multi-tasking operating system, running on a PowerPC CPU, receives commands from the spacecraft, controls the instrument operations, acquires the images and compresses them for downlink through the main science channel (at compression factors typically up to 20×) and also through a low bandwidth channel to be used for space weather forecasting (at compression factors up to 200×). An image compression factor of about 10× enable the collection of images at the rate of about one every 2–3 minutes. Identical instruments, except for different sizes of occulters, are included on the STEREO-A and STEREO-B spacecraft.
Published: 2008

14. Temporal evolution of a staircase ion signature observed by Cluster in the mid-altitude polar cusp

Author: Jean Berchem, Andrew Fazakerley, Karlheinz Trattner, Frederic Pitout, J. M. Bosqued, Arnaud Masson, H. Rème, C. P. Escoubet, H. E. Laakso, Iannis Dandouras, Matthew Taylor, Malcolm Dunlop, European Space Research and Technology Centre (ESTEC), European Space Agency (ESA), Centre d'étude spatiale des rayonnements (CESR), Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées, Institute of Geophysics and Planetary Physics [Los Angeles] (IGPP), University of California [Los Angeles] (UCLA), University of California-University of California, Lockheed Martin Advanced Technology Center (ATC), Max-Planck-Institut für Extraterrestrische Physik (MPE), STFC Rutherford Appleton Laboratory (RAL), Science and Technology Facilities Council (STFC), Mullard Space Science Laboratory (MSSL), University College of London [London] (UCL), Agence Spatiale Européenne = European Space Agency (ESA), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), and University of California (UC)-University of California (UC)
Subjects: 010504 meteorology & atmospheric sciences, INTERPLANETARY MAGNETIC-FIELD, Magnetosphere, Electron precipitation, Astrophysics, 01 natural sciences, Ion, FLUX-TRANSFER EVENTS, MAGNETOPAUSE RECONNECTION, 0103 physical sciences, Cluster (physics), Interplanetary magnetic field, Dispersion (water waves), LOW-ALTITUDE OBSERVATIONS, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, Physics, Cusp (singularity), Geophysics, 13. Climate action, EDGE, [SDU]Sciences of the Universe [physics], PRECIPITATION, Physics::Space Physics, General Earth and Planetary Sciences, Polar, AURORA
Abstract: International audience; We use the Cluster string of pearls configuration to investigate temporal variations of ion precipitation in the mid-altitude polar cusp. On 7 Aug. 2004, Cluster 4 was moving poleward through the Northern cusp, followed by Cluster 1, Cluster 2, and finally Cluster 3. The Wind spacecraft detected a Southward turning of the Interplanetary Magnetic Field (IMF) at the beginning of the cusp crossings and IMF-Bz stayed negative throughout. Cluster 4 observed a high energy step in the ion dispersion around 1 keV on the equatorward side of the cusp. C1, entering the cusp around 1 minute later, did not observe the high energy step anymore but a partial dispersion with a low energy cut-off reaching 100 eV. About 9 min later, C3 entered the cusp and observed a full ion dispersion from a few keV down to around 50 eV. The open-closed boundary, identified by electron precipitation, was initially moving equatorward at a rate of −0.43° ILAT/minute at the beginning of the event and then slowed down to −0.16° ILAT/minute, suggesting the erosion of the dayside magnetosphere under IMF Southward. This event is explained by the onset of dayside reconnection when the IMF turned southward; the step being the first signature of the reconnection that would then evolve as a full dispersion as reconnection goes on. We observed 1–3 keV ions near the open-closed boundary on the three spacecraft crossings that suggests a continuous reconnection during about 9 minutes.
Published: 2006
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15. Coordinated polar spacecraft, geosynchronous spacecraft, and ground-based observations of magnetopause processes and their coupling to the ionosphere

Author: Chao-Song Huang, T. E. Moore, Christopher T. Russell, K. Yumoto, Y. Zheng, S.-H. Chen, S. M. Petrinec, James A. Slavin, Guan Le, Howard J. Singer, John C. Samson, GSFC Laboratory for Extraterrestrial Physics, NASA Goddard Space Flight Center (GSFC), Universities Space Research Association (USRA), Institute of Geophysics and Planetary Physics [Los Angeles] (IGPP), University of California [Los Angeles] (UCLA), University of California-University of California, MIT Haystack Observatory, Massachusetts Institute of Technology (MIT), Space Physics Laboratory, Lockheed Martin Advanced Technology Center (ATC), Department of Physics [Edmonton], University of Alberta, NOAA Space Environment Center, National Oceanic and Atmospheric Administration (NOAA), Space Environment Research Center [Kyushu] (SERC), and Kyushu University [Fukuoka]
Subjects: Atmospheric Science, 010504 meteorology & atmospheric sciences, Field line, Magnetosphere, [SDU.STU]Sciences of the Universe [physics]/Earth Sciences, 01 natural sciences, Current sheet, Magnetosheath, 0103 physical sciences, Earth and Planetary Sciences (miscellaneous), lcsh:Science, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, Physics, [SDU.OCEAN]Sciences of the Universe [physics]/Ocean, Atmosphere, lcsh:QC801-809, Geology, Astronomy and Astrophysics, Geophysics, lcsh:QC1-999, Solar wind, lcsh:Geophysics. Cosmic physics, Polar wind, 13. Climate action, Space and Planetary Science, Physics::Space Physics, Magnetopause, lcsh:Q, Magnetohydrodynamics, lcsh:Physics
Abstract: In this paper, we present in-situ observations of processes occurring at the magnetopause and vicinity, including surface waves, oscillatory magnetospheric field lines, and flux transfer events, and coordinated observations at geosynchronous orbit by the GOES spacecraft, and on the ground by CANOPUS and 210° Magnetic Meridian (210MM) magnetometer arrays. On 7 February 2002, during a high-speed solar wind stream, the Polar spacecraft was skimming the magnetopause in a post-noon meridian plane for ~3h. During this interval, it made two short excursions and a few partial crossings into the magnetosheath and observed quasi-periodic cold ion bursts in the region adjacent to the magnetopause current layer. The multiple magnetopause crossings, as well as the velocity of the cold ion bursts, indicate that the magnetopause was oscillating with an ~6-min period. Simultaneous observations of Pc5 waves at geosynchronous orbit by the GOES spacecraft and on the ground by the CANOPUS magnetometer array reveal that these magnetospheric pulsations were forced oscillations of magnetic field lines directly driven by the magnetopause oscillations. The magnetospheric pulsations occurred only in a limited longitudinal region in the post-noon dayside sector, and were not a global phenomenon, as one would expect for global field line resonance. Thus, the magnetopause oscillations at the source were also limited to a localized region spanning ~4h in local time. These observations suggest that it is unlikely that the Kelvin-Helmholz instability and/or fluctuations in the solar wind dynamic pressure were the direct driving mechanisms for the observed boundary oscillations. Instead, the likely mechanism for the localized boundary oscillations was pulsed reconnection at the magnetopause occurring along the X-line extending over the same 4-h region. The Pc5 band pressure fluctuations commonly seen in high-speed solar wind streams may modulate the reconnection rate as an indirect cause of the observed Pc5 pulsations. During the same interval, two flux transfer events were also observed in the magnetosphere near the oscillating magnetopause. Their ground signatures were identified in the CANOPUS data. The time delays of the FTE signatures from the Polar spacecraft to the ground stations enable us to estimate that the longitudinal extent of the reconnection X-line at the magnetopause was ~43° or ~5.2 RE. The coordinated in-situ and ground-based observations suggest that FTEs are produced by transient reconnection taking place along a single extended X-line at the magnetopause, as suggested in the models by Scholer(1988) and Southwood et al.(1988). The observations from this study suggest that the reconnection occurred in two different forms simultaneously in the same general region at the dayside magnetopause: 1) continuous reconnection with a pulsed reconnection rate, and 2) transient reconnection as flux transfer events. Key words. Magnetospheric physics (Magnetopause, cusp and boundary layers; Magnetosphere-ionosphere interactions; MHD waves and instabilities)
Published: 2004

16. Rosina’s Scientific Perspective at Comet Churyumov-Gerasimenko

Author: Tamas I. Gombosi, Fritz Gliem, Jean-Jacques Berthelier, H. Rème, Kathrin Altwegg, E. Arijs, Hans Balsiger, Annette Jäckel, A. Korth, S. A. Fuselier, Physikalisches Institut [Bern], Universität Bern [Bern], Belgian Institute for Space Aeronomy / Institut d'Aéronomie Spatiale de Belgique (BIRA-IASB), Centre d'étude des environnements terrestre et planétaires (CETP), Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Lockheed Martin Advanced Technology Center (ATC), Technische Universität Braunschweig = Technical University of Braunschweig [Braunschweig], Space Physics Research Laboratory [Ann Arbor] (SPRL), University of Michigan [Ann Arbor], University of Michigan System-University of Michigan System, Max-Planck-Institut für Aeronomie (MPI Aeronomie), Max-Planck-Gesellschaft, Centre d'étude spatiale des rayonnements (CESR), Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées, Colangeli L., Epifani E.M., and Palumbo P. (eds)
Subjects: Physics, Molecular composition, 010504 meteorology & atmospheric sciences, Comet, Astronomy, 01 natural sciences, law.invention, Astrobiology, On board, Orbiter, law, [SDU]Sciences of the Universe [physics], 0103 physical sciences, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences
Abstract: International audience; The Rosetta Orbiter Spectrometer for Ion and Neutral Analysis (ROSINA) on board Rosetta is designed to analyze the volatile material of comet 67P/Churyumov-Gerasimenko. We show in this paper that the scientific requirements related to the volatile material of comets in general and specifically to the present Rosetta target can be met by the three ROSINA sensors. ROSINA will answer scientifically important questions concerning the elemental, isotopic and molecular composition of Churyumov-Gerasimenko.
Published: 2004

17. Stratosphere over Dumont d'Urville, Antarctica, in winter 1992

Author: J. L. Mergenthaler, Sophie Godin, Jean-Pierre Pommereau, Florence Goutail, E. Monnier, Lucien Froidevaux, Martyn P. Chipperfield, Joe W. Waters, Christine David, Philippe Ricaud, Aidan E. Roche, Hugh C. Pumphrey, Observatoire Bordeaux, Université Sciences et Technologies - Bordeaux 1, Service d'aéronomie (SA), Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Jet Propulsion Laboratory (JPL), California Institute of Technology (CALTECH)-NASA, Lockheed Martin Advanced Technology Center (ATC), School of Geosciences [Edinburgh], University of Edinburgh, Department of Chemistry [Cambridge, UK], University of Cambridge [UK] (CAM), Université Sciences et Technologies - Bordeaux 1 (UB), and NASA-California Institute of Technology (CALTECH)
Subjects: Atmospheric Science, 010504 meteorology & atmospheric sciences, Chemical transport model, Total Ozone Mapping Spectrometer, Soil Science, Aquatic Science, 010502 geochemistry & geophysics, Oceanography, Atmospheric sciences, 01 natural sciences, Atmosphere, chemistry.chemical_compound, Geochemistry and Petrology, Earth and Planetary Sciences (miscellaneous), Stratosphere, 0105 earth and related environmental sciences, Earth-Surface Processes, Water Science and Technology, [PHYS.PHYS.PHYS-AO-PH]Physics [physics]/Physics [physics]/Atmospheric and Oceanic Physics [physics.ao-ph], Ecology, Chlorine nitrate, Paleontology, Forestry, Vortex, Microwave Limb Sounder, Geophysics, chemistry, 13. Climate action, Space and Planetary Science, Environmental science, Chlorine monoxide
Abstract: International audience; We present an analysis of the temporal evolution of stratospheric constituents above the station of Dumont d'Urville in Antarctica (67°S, 140°E) from August 14 to September 20, 1992. Data sets include temperature profiles and H2O, ClO, O3, NO2, ClONO2, HNO3, N2O, and CH4 mixing ratios and aerosol extinction coefficients from 46 to 1 hPa measured by the Microwave Limb Sounder (MLS) and the Cryogenic Limb Array Etalon Spectrometer (CLAES) instruments aboard the Upper Atmosphere Research Satellite (UARS). At the station, aerosol extinction coefficients and O3 profiles are obtained by a lidar together with O3 profiles provided by sondes. Integrated O3 and NO2 column amounts are given by a Système d'Analyse par Observation Zénithale (SAOZ) spectrometer located at the station. Column O3 is also provided by the Total Ozone Mapping Spectrometer (TOMS) instrument aboard the NIMBUS 7 satellite, complemented with potential vorticity derived from the U.K. Meteorological Office assimilated data set and temperature fields provided by the European Centre for Medium-Range Weather Forecasts. Time evolution of these measurements is interpreted by comparison with results from the SLIMCAT three-dimensional chemical transport model. We show that the site is near the vortex edge on average and is alternately inside the vortex or just outside in the region referred to as the "collar" region. There are no observations of polar stratospheric clouds (PSCs) over the station above 46 hPa (∼18 km). In fact, PSCs mainly appear over the Palmer Peninsula area at 46 hPa. The rates of change of chemical species are evaluated at 46 hPa when the station is conservatively inside the vortex collar region. The ozone loss rate is 0.04 ppmv d-1 (∼1.3% d-1), which is consistent with other analyses of southern vortex ozone loss rates; chlorine monoxide tends to decrease by 0.03 ppbv d-1, while chlorine nitrate increases by 0.025 ppbv d-1. These negative ClO and positive ClONO2 trends are only observed in the collar region of the vortex where O3 amounts are far from near zero, and little denitrification is observed. Loss and production rates as measured by UARS are more pronounced than the ones deduced from the SLIMCAT model, probably because of the moderate model horizontal resolution (3.75° × 3.75°), which is not high enough to resolve the vortex crossings above Dumont d'Urville and which leads to a larger extent of denitrified air than indicated by the UARS data. The analysis also shows activated ClO inside the vortex at 46 hPa, a dehydrated vortex at 46 hPa, and rehydrated above, with no trace of denitrification in the lower stratosphere. Good agreement between coincident measurements of O3 profiles by UARS/MLS, lidar, and sondes is also observed. Finally, the agreement between UARS and SLIMCAT data sets is much better in the middle stratosphere (4.6 hPa) than in the lower stratosphere (46 hPa).
Published: 1998
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18. Rosetta Orbiter Spectrometer for Ion and Neutral Analysis—ROSINA

Author: B. Wilken, E. Kopp, Stefano Livi, E. G. Shelley, D. T. Young, J. H. Waite, Lennard A. Fisk, Fritz Gliem, Hermann Wollnik, Peter Wurz, Tamas I. Gombosi, Joachim Woch, G. R. Carignan, Stephen A. Fuselier, H. Rème, A. G. Ghielmetti, J. L. Bertaux, E. Arijs, A. Korth, Hans Balsiger, Jean-Jacques Berthelier, Kathrin Altwegg, Christian Mazelle, J. A. Sauvaud, Peter Bochsler, Peter Eberhardt, Physikalisches Institut [Bern], Universität Bern [Bern], Belgian Institute for Space Aeronomy / Institut d'Aéronomie Spatiale de Belgique (BIRA-IASB), Service d'aéronomie (SA), Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Centre d'étude des environnements terrestre et planétaires (CETP), Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Space Physics Research Laboratory [Ann Arbor] (SPRL), University of Michigan [Ann Arbor], University of Michigan System-University of Michigan System, Lockheed Martin Advanced Technology Center (ATC), Technische Universität Braunschweig = Technical University of Braunschweig [Braunschweig], Max-Planck-Institut für Aeronomie (MPI Aeronomie), Max-Planck-Gesellschaft, Centre d'étude spatiale des rayonnements (CESR), Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées, Lockheed Martin Palo Alto Research Laboratories, Lockheed Martin Corporation, Space Science Division [San Antonio], Southwest Research Institute [San Antonio] (SwRI), Physikalisches Institut [Gießen], Justus-Liebig-Universität Gießen (JLU), Universität Bern [Bern] (UNIBE), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), and Justus-Liebig-Universität Gießen = Justus Liebig University (JLU)
Subjects: Physics, Atmospheric Science, Ion flow, 010504 meteorology & atmospheric sciences, Resolution (mass spectrometry), Spectrometer, Aerospace Engineering, Astronomy and Astrophysics, 7. Clean energy, 01 natural sciences, law.invention, Astrobiology, Ion, Orbiter, Geophysics, 13. Climate action, Space and Planetary Science, law, [SDU]Sciences of the Universe [physics], 0103 physical sciences, Wide dynamic range, High mass, General Earth and Planetary Sciences, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences
Abstract: International audience; The Rosetta Orbiter Spectrometer for Ion and Neutral Analysis (ROSINA) will answer outstanding questions concerning the main objectives of the mission. To accomplish the very demanding objectives, ROSINA will have unprecedented capabilities, including: very wide mass range from 1 amu to >300 amu; very high mass resolution (ability to resolve CO from N2 and 13C from 12CH); very wide dynamic range and high sensitivity; the ability to determine cometary gas and ion flow velocities and temperatures.
Published: 1998
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19. Accuracy and precision of cryogenic limb array etalon spectrometer (CLAES) temperature retrievals

Author: Michael R. Gross, Aidan E. Roche, David P. Edwards, John C. Gille, Ian S. McDermid, Upendra N. Singh, Alain Hauchecorne, Paul L. Bailey, Thomas J. McGee, Alvin J. Miller, Steven T. Massie, John B. Kumer, Lawrence V. Lyjak, John L. Mergenthaler, Phillip Keckhut, National Center for Atmospheric Research [Boulder] (NCAR), Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), Lockheed Martin Advanced Technology Center (ATC), Department of Geological Sciences [Gainesville] (UF|Geological), University of Florida [Gainesville] (UF), Service d'aéronomie (SA), Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Scripps Institution of Oceanography (SIO), University of California [San Diego] (UC San Diego), University of California-University of California, NASA Langley Research Center [Hampton] (LaRC), Scripps Institution of Oceanography (SIO - UC San Diego), and University of California (UC)-University of California (UC)
Subjects: Atmospheric Science, Accuracy and precision, 010504 meteorology & atmospheric sciences, Soil Science, Aquatic Science, 010502 geochemistry & geophysics, Oceanography, Atmospheric sciences, 01 natural sciences, law.invention, Mesosphere, Atmosphere, Geochemistry and Petrology, law, Earth and Planetary Sciences (miscellaneous), Stratosphere, 0105 earth and related environmental sciences, Earth-Surface Processes, Water Science and Technology, Remote sensing, [PHYS.PHYS.PHYS-AO-PH]Physics [physics]/Physics [physics]/Atmospheric and Oceanic Physics [physics.ao-ph], Ecology, Spectrometer, Paleontology, Forestry, Wavelength, Geophysics, 13. Climate action, Space and Planetary Science, Radiosonde, Environmental science, Satellite
Abstract: International audience; The Cryogenic Limb Array Etalon Spectrometer (CLAES) measured emission from the 792 cm−1 Q branch of CO2, from which temperature distributions in the stratosphere and low mesosphere were derived. Here we briefly review the measurement technique, concentrating on aspects that affect the temperature determination. Comparison of many pairs of retrievals at the same location (near 32°N or 32°S) measured on sequential orbits (time separation of 96 min) shows a precision ranging from approximately 0.8 K at 68 mbar to about 3.5 K at 0.2 mbar, which agrees with simulations incorporating random noise and short‐period spacecraft motions. Comparisons of globally analyzed CLAES data with National Meteorological Center (NMC) and U.K. Meteorological Office (UKMO) analyses show general agreement, with CLAES tending to be cooler by about 2 K, except in the tropics and high‐latitude winter conditions. This is supported by comparisons with individual radiosondes and several lidars that indicate that the agreement is within 2 K throughout the profile (except for a narrow layer around 3 mbar). An error analysis also indicates that systematic errors should be roughly 2 K, independent of altitude. The systematic differences at low latitudes appear to be due to tropical waves, which have vertical wavelengths too short to be seen by the TIROS Operational Vertical Sounder (TOVS) instruments. There are no correlative rocketsondes or lidars to help resolve the reasons for the high‐latitude differences. Comparisons with other Upper Atmosphere Research Satellite (UARS) data should shed additional light on this question.
Published: 1996
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19 results on '"Lockheed Martin Advanced Technology Center (ATC)"'

1. Ion chemistry in the coma of comet 67P near perihelion

2. Changes in granulation scales over the solar cycle seen with SDO/HMI and Hinode/SOT

3. On the Ubiquity of Magnetic Reconnection Inside Flux Transfer Event‐Like Structures at the Earth's Magnetopause

4. Mass Loading the Earth's Dayside Magnetopause Boundary Layer and Its Effect on Magnetic Reconnection

5. Comparison of neutral outgassing of comet 67P/Churyumov-Gerasimenko inbound and outbound beyond 3 AU from ROSINA/DFMS

6. Nonlobe Reconnection at the Earth's Magnetopause for Northward IMF

7. Solar Ultraviolet Bursts

8. Two sources of magnetosheath ions observed by Cluster in the mid-altitude polar cusp

9. Rosina – Rosetta Orbiter Spectrometer for Ion and Neutral Analysis

10. Solar Magnetic Field Reversals and the Role of Dynamo Families

11. Computer Vision for The Solar Dynamics Observatory

12. In situ mass spectrometry during the Lutetia flyby

13. Sun Earth Connection Coronal and Heliospheric Investigation (SECCHI)

14. Temporal evolution of a staircase ion signature observed by Cluster in the mid-altitude polar cusp

15. Coordinated polar spacecraft, geosynchronous spacecraft, and ground-based observations of magnetopause processes and their coupling to the ionosphere

16. Rosina’s Scientific Perspective at Comet Churyumov-Gerasimenko

17. Stratosphere over Dumont d'Urville, Antarctica, in winter 1992

18. Rosetta Orbiter Spectrometer for Ion and Neutral Analysis—ROSINA

19. Accuracy and precision of cryogenic limb array etalon spectrometer (CLAES) temperature retrievals

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19 results on '"Lockheed Martin Advanced Technology Center (ATC)"'

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