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1. The BepiColombo Planetary Magnetometer MPO-MAG: What Can We Learn from the Hermean Magnetic Field?

Author

Johannes Z. D. Mieth, Rumi Nakamura, H. U. Auster, Johannes Wicht, Ferdinand Plaschke, Ayako Matsuoka, Karl-Heinz Fornacon, Werner Magnes, Chris Carr, Susanne Vennerstrøm, G. Berghofer, Yasuhito Narita, Magda Delva, Mioara Mandea, Karl-Heinz Glassmeier, Adam Masters, Patrick Kolhey, M. K. Dougherty, Daniel Heyner, Timothy S. Horbury, W. Exner, James A. Slavin, André Balogh, Wolfgang Baumjohann, Uwe Motschmann, Beatriz Sánchez-Cano, B. Langlais, Ingo Richter, David Fischer, Martin Volwerk, J. S. Oliveira, Joachim Vogt, Laboratoire de Planétologie et Géodynamique [UMR 6112] (LPG), Université d'Angers (UA)-Université de Nantes - UFR des Sciences et des Techniques (UN UFR ST), Université de Nantes (UN)-Université de Nantes (UN)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), The Royal Society, Science and Technology Facilities Council, and Science and Technology Facilities Council (STFC)

Subjects
010504 meteorology & atmospheric sciences, Magnetometer, Polar orbit, [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], Magnetosphere, Astronomy & Astrophysics, Fluxgate, 01 natural sciences, law.invention, Orbiter, law, 0103 physical sciences, 0201 Astronomical and Space Sciences, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, Physics, Astronomy, Astronomy and Astrophysics, Mercury, Solar wind, Planetary science, Magnetic field, Space and Planetary Science, Physics::Space Physics, Magnetopause, Satellite, Astrophysics::Earth and Planetary Astrophysics
Abstract

The magnetometer instrument MPO-MAG on-board the Mercury Planetary Orbiter (MPO) of the BepiColombo mission en-route to Mercury is introduced, with its instrument design, its calibration and scientific targets. The instrument is comprised of two tri-axial fluxgate magnetometers mounted on a 2.9 m boom and are 0.8 m apart. They monitor the magnetic field with up to 128 Hz in a $\pm 2048$ ± 2048 nT range. The MPO will be injected into an initial $480 \times 1500$ 480 × 1500 km polar orbit (2.3 h orbital period). At Mercury, we will map the planetary magnetic field and determine the dynamo generated field and constrain the secular variation. In this paper, we also discuss the effect of the instrument calibration on the ability to improve the knowledge on the internal field. Furthermore, the study of induced magnetic fields and field-aligned currents will help to constrain the interior structure in concert with other geophysical instruments. The orbit is also well-suited to study dynamical phenomena at the Hermean magnetopause and magnetospheric cusps. Together with its sister instrument Mio-MGF on-board the second satellite of the BepiColombo mission, the magnetometers at Mercury will study the reaction of the highly dynamic magnetosphere to changes in the solar wind. In the extreme case, the solar wind might even collapse the entire dayside magnetosphere. During cruise, MPO-MAG will contribute to studies of solar wind turbulence and transient phenomena.

Published
2021

2. Dynamic field line draping at comet 67P/Churyumov-Gerasimenko during the Rosetta dayside excursion

Author

Magda Delva, Niklas J. T. Edberg, Martin Volwerk, Hans Nilsson, Charlotte Goetz, Etienne Behar, Pierre Henri, Karl-Heinz Glassmeier, Gabriella Stenberg Wieser, Kristie LLera, Anders Eriksson, Ingo Richter, Space Research Institute of Austrian Academy of Sciences (IWF), Austrian Academy of Sciences (OeAW), Technische Universität Braunschweig = Technical University of Braunschweig [Braunschweig], Swedish Institute of Space Physics [Kiruna] (IRF), Institut für Weltraumforschung [Graz] (IWF), Osterreichische Akademie der Wissenschaften (ÖAW), Swedish Institute of Space Physics [Uppsala] (IRF), 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), and Institut für Geophysik und Extraterrestrische Physik [Braunschweig] (IGEP)

Subjects
Physics, 010504 meteorology & atmospheric sciences, [PHYS.ASTR.EP]Physics [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], Excursion, Comet, Astronomy and Astrophysics, Context (language use), Astrophysics, Plasma, [PHYS.ASTR.SR]Physics [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], 01 natural sciences, [PHYS.PHYS.PHYS-SPACE-PH]Physics [physics]/Physics [physics]/Space Physics [physics.space-ph], Magnetic field, Solar wind, 13. Climate action, Space and Planetary Science, 0103 physical sciences, Interplanetary magnetic field, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, Line (formation)
Abstract

Context. The Rosetta dayside excursion took place in September–October 2015 when comet 67P/Churyumov-Gerasimenko (67P/CG) was located at ~1.36 AU from the Sun after it had passed perihelion on 13 August 2015 at ~1.25 AU. At this time, the comet was near its most active period, and its interaction with the solar wind was expected to be at its most intense, with ion pickup and magnetic field line draping. The dayside excursion was planned to move through different regions that were expected upstream of the cometary nucleus, and to possibly detect the location of the bow shock. Aims. The goal of this study is to describe the dynamic field line draping that takes place around the comet and the plasma processes that are connected to this. Methods. The data from the full Rosetta Plasma Consortium (RPC) were used to investigate the interaction of solar wind and comet, starting from boxcar-averaged magnetic field data in order to suppress high-frequency noise in the data. Through calculating the cone and clock angle of the magnetic field, we determined the draping pattern of the magnetic field around the nucleus of the comet. Then we studied the particle data in relation to the variations that are observed in the magnetic field. Results. During the dayside excursion, the magnetic field cone angle changed several times, which means that the magnetic field direction changes from pointing sunward to anti-sunward. This is caused by the changing directions of the interplanetary magnetic field that is transported toward the comet. The cone-angle direction shows that mass-loading of the interplanetary magnetic field of the solar wind leads to dynamic draping. The ion velocity and the magnetic field strength are correlated because the unmagnetized ions are accelerated more (less) strongly by the increasing (decreasing) magnetic field strength. There is an indication of an anticorrelation between the electron density and the magnetic field strength, which might be caused by the magnetized electrons being mirrored out of the strong field regions. The Rosetta RPC has shown that (dynamic) draping also occurs as mildly active comets, as was found at highly active comets such as 1P/Halley and 21P/Giacobini-Zinner, but also that determining both dynamic and nested draping will require a combination of fast flybys and slow excursions for future missions.

Published
2019

3. Astronomy Unusually high magnetic fields in the coma of 67P/Churyumov-Gerasimenko during its high-activity phase

Author

Anne Wellbrock, Niklas J. T. Edberg, Raymond Goldstein, Etienne Behar, Prachet Mokashi, Bruce T. Tsurutani, P. Henri, Karl-Heinz Glassmeier, Martin Volwerk, Ingo Richter, Anders Eriksson, C. Goetz, Hans Nilsson, Service de Biophysique et Médecine Nucléaire, CHU Strasbourg-Université Louis Pasteur - Strasbourg I-Hôpital de Hautepierre [Strasbourg], Jet Propulsion Laboratory (JPL), California Institute of Technology (CALTECH)-NASA, 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), Space Research Institute of Austrian Academy of Sciences (IWF), Austrian Academy of Sciences (OeAW), IFP Energies nouvelles (IFPEN), Swedish Institute of Space Physics [Uppsala] (IRF), Swedish Institute of Space Physics [Kiruna] (IRF), Space Sciences Laboratory [Berkeley] (SSL), University of California [Berkeley], University of California-University of California, Mullard Space Science Laboratory (MSSL), University College of London [London] (UCL), Institut für Geophysik und Extraterrestrische Physik [Braunschweig] (IGEP), Technische Universität Braunschweig = Technical University of Braunschweig [Braunschweig], Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université d'Orléans (UO)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université d'Orléans (UO)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Centre National d’Études Spatiales [Paris] (CNES), and Technische Universität Braunschweig [Braunschweig]

Subjects
Physics, 010504 meteorology & atmospheric sciences, Magnetic field magnitude, [SDU.ASTR.SR]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], Comet, Phase (waves), [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], Astronomy and Astrophysics, Coma (optics), Plasma, Astrophysics, 01 natural sciences, Magnetic field, 13. Climate action, Space and Planetary Science, 0103 physical sciences, Physics::Space Physics, High activity, Astrophysics::Earth and Planetary Astrophysics, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences
Abstract

Aims. On July 3, 2015, an unprecedented increase in the magnetic field magnitude was measured by the Rosetta spacecraft orbiting comet 67P/Churyumov-Gerasimenko (67P). This increase was accompanied by large variations in magnetic field and ion and electron density and energy. To our knowledge, this unusual event marks the highest magnetic field ever measured in the plasma environment of a comet. Our goal here is to examine possible physical causes for this event, and to explain this reaction of the cometary plasma and magnetic field and its trigger. Methods. We used observations from the entire Rosetta Plasma Consortium as well as energetic particle measurements from the Standard Radiation Monitor on board Rosetta to characterize the event. To provide context for the solar wind at the comet, observations at Earth were compared with simulations of the solar wind. Results. We find that the unusual behavior of the plasma around 67P is of solar wind origin and is caused by the impact of an interplanetary coronal mass ejection, combined with a corotating interaction region. This causes the magnetic field to pile up and increase by a factor of six to about 300 nT compared to normal values of the enhanced magnetic field at a comet. This increase is only partially accompanied by an increase in plasma density and energy, indicating that the magnetic field is connected to different regions of the coma.

Published
2019

4. Dynamic unmagnetized plasma in the diamagnetic cavity around comet 67P/Churyumov–Gerasimenko

Author

James L. Burch, Hans Nilsson, Martin Rubin, Herbert Gunell, Jérôme Moré, Charlotte Goetz, Bruce T. Tsurutani, Gaëtan Wattieaux, X. Vallières, Pierre Henri, Rajkumar Hajra, Zoltán Németh, Ingo Richter, N. Gilet, Anders Eriksson, 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), Plasmas Réactifs Hors Equilibre (LAPLACE-PRHE), LAboratoire PLasma et Conversion d'Energie (LAPLACE), Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut National Polytechnique (Toulouse) (Toulouse INP), Université Fédérale Toulouse Midi-Pyrénées-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées, Technische Universität Braunschweig = Technical University of Braunschweig [Braunschweig], Jet Propulsion Laboratory (JPL), California Institute of Technology (CALTECH)-NASA, Belgian Institute for Space Aeronomy / Institut d'Aéronomie Spatiale de Belgique (BIRA-IASB), Swedish Institute of Space Physics [Kiruna] (IRF), Swedish Institute of Space Physics [Uppsala] (IRF), Wigner Research Centre for Physics [Budapest], Hungarian Academy of Sciences (MTA), Southwest Research Institute [Boulder] (SwRI), Physikalisches Institut [Bern], and Universität Bern [Bern]

Subjects
010504 meteorology & atmospheric sciences, 530 Physics, Comet, Electron, 01 natural sciences, law.invention, Orbiter, law, Ionization, 0103 physical sciences, Relative density, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, Plasma density, Physics, comets: individual: 67P/Churyumov–Gerasimenko, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 520 Astronomy, comets: general, Astronomy and Astrophysics, Plasma, 620 Engineering, methods: data analysis, Space and Planetary Science, Diamagnetism, Atomic physics, methods: observational
Abstract

International audience; The Rosetta orbiter witnessed several hundred diamagnetic cavity crossings (unmagnetized regions) around comet 67P/Churyumov–Gerasimenko during its two year survey of the comet. The characteristics of the plasma environment inside these diamagnetic regions are studied using in situ measurements by the Rosetta Plasma Consortium instruments. Although the unmagnetized plasma density has been observed to exhibit little dynamics compared to the very dynamical magnetized cometary plasma, we detected several localized dynamic plasma structures inside those diamagnetic regions. These plasma structures are not related to the direct ionization of local cometary neutrals. The structures are found to be steepened, asymmetric plasma enhancements with typical rising-to-descending slope ratio of ∼2.8 (±1.9), skewness ∼0.43 (±0.36), mean duration of ∼2.7 (±0.9) min and relative density variation ΔN/N of ∼0.5 (±0.2), observed close to the electron exobase. Similar steepened plasma density enhancements were detected at the magnetized boundaries of the diamagnetic cavity as well as outside the diamagnetic region. The plausible scalelength and propagation direction of the structures are estimated from simple plasma dynamics considerations. It is suggested that they are large-scale unmagnetized plasma enhancements, transmitted from the very dynamical outer magnetized region to the inner magnetic field-free cavity region.

Published
2018

5. Lower hybrid waves at comet 67P/Churyumov–Gerasimenko

Author

Erik Vigren, F. L. Johansson, C. Norgren, G. Stenberg Wieser, Anders Eriksson, Ingo Richter, Tomas Karlsson, Daniel B. Graham, Mats André, Martin Rubin, Elias Odelstad, P. Henri, Swedish Institute of Space Physics [Uppsala] (IRF), Department of Space and Plasma Physics [Stockholm], KTH School of Electrical Engineering, Royal Institute of Technology [Stockholm] (KTH )-Royal Institute of Technology [Stockholm] (KTH ), 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), Physikalisches Institut [Bern], Universität Bern [Bern], Institut für Geophysik und Extraterrestrische Physik [Braunschweig] (IGEP), and Technische Universität Braunschweig = Technical University of Braunschweig [Braunschweig]

Subjects
010504 meteorology & atmospheric sciences, Energy transfer, Comet, Electron, 01 natural sciences, Ion, Physics::Plasma Physics, 0103 physical sciences, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, Physics, Range (particle radiation), 520 Astronomy, Astronomy, Astronomy and Astrophysics, Plasma, Ion acoustic wave, Lower hybrid oscillation, 620 Engineering, Computational physics, 13. Climate action, Space and Planetary Science, [SDU]Sciences of the Universe [physics], Physics::Space Physics, Astrophysics::Earth and Planetary Astrophysics, plasmas –waves – comets: general
Abstract

International audience; We investigate the generation of waves in the lower hybrid frequency range by density gradients in the near plasma environment of comet 67P/Churyumov–Gerasimenko. When the plasma is dominated by water ions from the comet, a situation with magnetized electrons and unmagnetized ions is favourable for the generation of lower hybrid waves. These waves can transfer energy between ions and electrons and reshape the plasma environment of the comet. We consider cometocentric distances out to a few hundred km. We find that when the electron motion is not significantly interrupted by collisions with neutrals, large average gradients within tens of km of the comet, as well as often observed local large density gradients at larger distances, are often likely to be favourable for the generation of lower hybrid waves. Overall, we find that waves in the lower hybrid frequency range are likely to be common in the near plasma environment.

Published
2017

6. Structure and evolution of the diamagnetic cavity at comet 67P/Churyumov–Gerasimenko

Author

Hans Nilsson, Christoph Koenders, Charlotte Goetz, Bruce T. Tsurutani, Chris Carr, Holger Sierks, Pierre Henri, Dennis Frühauff, Kirk C. Hansen, Ingo Richter, Anders Eriksson, Martin Volwerk, Martin Rubin, Karl-Heinz Glassmeier, Carsten Güttler, James L. Burch, Institut für Geophysik und Extraterrestrische Physik [Braunschweig] (IGEP), Technische Universität Braunschweig = Technical University of Braunschweig [Braunschweig], Department of Atmospheric, Oceanic, and Space Sciences [Ann Arbor] (AOSS), University of Michigan [Ann Arbor], University of Michigan System-University of Michigan System, Southwest Research Institute [San Antonio] (SwRI), Space and Atmospheric Physics Group [London], Blackett Laboratory, Imperial College London-Imperial College London, Swedish Institute of Space Physics [Uppsala] (IRF), Max-Planck-Institut für Sonnensystemforschung (MPS), Max-Planck-Gesellschaft, 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), Jet Propulsion Laboratory (JPL), California Institute of Technology (CALTECH)-NASA, and Science and Technology Facilities Council (STFC)

Subjects
010504 meteorology & atmospheric sciences, 530 Physics, ROSETTA PLASMA CONSORTIUM, Comet, Astrophysics, Astronomy & Astrophysics, ROSINA, magnetic fields, 01 natural sciences, REGION, Fusion, plasma och rymdfysik, comets: individual: 67P, individual: 67P [comets], 0103 physical sciences, data analysis [methods], ION, PROBE, 010303 astronomy & astrophysics, Short duration, HALLEY, MAGNETOMETER, 0105 earth and related environmental sciences, Physics, Science & Technology, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 520 Astronomy, Astronomy, Astronomy and Astrophysics, Plasma, 620 Engineering, plasmas, Fusion, Plasma and Space Physics, methods: data analysis, [PHYS.PHYS.PHYS-SPACE-PH]Physics [physics]/Physics [physics]/Space Physics [physics.space-ph], Magnetic field, 0201 Astronomical And Space Sciences, 13. Climate action, Space and Planetary Science, SOLAR-WIND, Physical Sciences, MAGNETIC CAVITY, Diamagnetism, Astrophysics::Earth and Planetary Astrophysics, PERIHELION
Abstract

International audience; The long duration of the Rosetta mission allows us to study the evolution of the diamagnetic cavity at comet 67P/Churyumov–Gerasimenko in detail. From 2015 April to 2016 February 665 intervals could be identified where Rosetta was located in a zero-magnetic-field region. We study the temporal and spatial distribution of this cavity and its boundary and conclude that the cavity properties depend on the long-term trend of the outgassing rate, but do not respond to transient events at the spacecraft location, such as outbursts or high neutral densities. Using an empirical model of the outgassing rate, we find a functional relationship between the outgassing rate and the distance of the cavity to the nucleus. There is also no indication that this unexpectedly large distance is related to unusual solar wind conditions. Because the deduced shape of the cavity boundary is roughly elliptical on small scales and the distances of the boundary from the nucleus are much larger than expected we conclude that the events observed by Rosetta are due to a moving instability of the cavity boundary itself.

Published
2017

7. RPC observation of the development and evolution of plasma interaction boundaries at 67P/Churyumov-Gerasimenko

Author

T. W. Broiles, Andrew J. Coates, Jean-Pierre Lebreton, Chris Carr, Arnaud Beth, Niklas J. T. Edberg, Martin Volwerk, Pierre Henri, Christoph Koenders, Charlotte Goetz, Adrienn Luspay-Kuti, Prachet Mokashi, Esa Kallio, Kirk C. Hansen, Hans Nilsson, Markku Alho, N. Biver, Kathleen Mandt, S. A. Fuselier, James L. Burch, J. D. Haiducek, Zoltán Németh, Karoly Szego, Marina Galand, Karl-Heinz Glassmeier, K. Chae, G. Stenberg Wieser, Andrea Opitz, Anders Eriksson, Marilia Samara, C. Simon Wedlund, Ingo Richter, Raymond Goldstein, Chia-Yu Tzou, Emanuele Cupido, UTSA Department of Physics and Astronomy [San Antonio], The University of Texas at San Antonio (UTSA), Space Science Division [San Antonio], Southwest Research Institute [San Antonio] (SwRI), Swedish Institute of Space Physics [Uppsala] (IRF), Technische Universität Braunschweig = Technical University of Braunschweig [Braunschweig], 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), Wigner Research Centre for Physics [Budapest], Hungarian Academy of Sciences (MTA), School of Electrical Engineering [Aalto Univ], Aalto University, Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), Université Pierre et Marie Curie - Paris 6 (UPMC)-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 Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Department of Physics [Imperial College London], Imperial College London, Blackett Laboratory, Mullard Space Science Laboratory (MSSL), University College of London [London] (UCL), Centre for Planetary Sciences [UCL/Birkbeck] (CPS), Department of Climate and Space Sciences and Engineering (CLaSP), University of Michigan [Ann Arbor], University of Michigan System-University of Michigan System, University of Michigan, Department of Atmospheric, 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 Research and Planetary Sciences [Bern) (WP), Physikalisches Institut [Bern], Universität Bern [Bern]-Universität Bern [Bern], Space Research Institute of Austrian Academy of Sciences (IWF), Austrian Academy of Sciences (OeAW), Department of Physics [Oslo], Faculty of Mathematics and Natural Sciences [Oslo], University of Oslo (UiO)-University of Oslo (UiO), Southwest Research Institute, Swedish Institute of Space Physics, Technical University of Braunschweig, Laboratoire de Physique et Chimie de l’Environnement et de l’Espace, Wigner Research Centre for Physics, Department of Radio Science and Engineering, Observatoire de Paris, University College London, University of Michigan, Ann Arbor, NASA Goddard Space Flight Center, University of Bern, Austrian Academy of Sciences, University of Oslo, Aalto-yliopisto, 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), Universität Bern [Bern] (UNIBE)-Universität Bern [Bern] (UNIBE), and Science and Technology Facilities Council (STFC)

Subjects
010504 meteorology & atmospheric sciences, 530 Physics, Comet, Electron, Astrophysics, Astronomy & Astrophysics, 01 natural sciences, Ion, general [comets], Fusion, plasma och rymdfysik, Physics::Plasma Physics, 0103 physical sciences, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, Physics, ta115, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 520 Astronomy, comets: general, Astronomy and Astrophysics, Plasma, 620 Engineering, plasmas, Fusion, Plasma and Space Physics, [PHYS.PHYS.PHYS-SPACE-PH]Physics [physics]/Physics [physics]/Space Physics [physics.space-ph], Magnetic field, Solar wind, 0201 Astronomical And Space Sciences, solar wind, 13. Climate action, Space and Planetary Science, Physics::Space Physics, Diamagnetism, Dynamic pressure, Astrophysics::Earth and Planetary Astrophysics, Atomic physics
Abstract

International audience; One of the primary objectives of the Rosetta Plasma Consortium, a suite of five plasma instruments on-board the Rosetta spacecraft, is to observe the formation and evolution of plasma interaction regions at the comet 67P/Churyumov-Gerasimenko (67P/CG). Observations made between 2015 April and 2016 February show that solar wind–cometary plasma interaction boundaries and regions formed around 2015 mid-April and lasted through early 2016 January. At least two regions were observed, separated by an ion-neutral collisionopause boundary. The inner region was located on the nucleus side of the boundary and was characterized by low-energy water-group ions, reduced magnetic field pileup and enhanced electron densities. The outer region was located outside of the boundary and was characterized by reduced electron densities, water-group ions that are accelerated to energies above 100 eV and enhanced magnetic field pileup compared to the inner region. The boundary discussed here is outside of the diamagnetic cavity and shows characteristics similar to observations made on-board the Giotto spacecraft in the ion pileup region at 1P/Halley. We find that the boundary is likely to be related to ion-neutral collisions and that its location is influenced by variability in the neutral density and the solar wind dynamic pressure.

Published
2016

8. Charged particle signatures of the diamagnetic cavity of comet 67P/Churyumov–Gerasimenko

Author

Christoph Koenders, James L. Burch, Prachet Mokashi, Charlotte Goetz, Raymond Goldstein, H. Madanian, Kathleen Mandt, Ingo Richter, Pierre Henri, Zoltán Németh, Aniko Timar, Karoly Szego, Wigner Research Centre for Physics [Budapest], Hungarian Academy of Sciences (MTA), Space Science Division [San Antonio], Southwest Research Institute [San Antonio] (SwRI), Institut für Geophysik und Extraterrestrische Physik [Braunschweig] (IGEP), Technische Universität Braunschweig = Technical University of Braunschweig [Braunschweig], Department of Applied Mathematics and Theoretical Physics [Cambridge] (DAMTP), Faculty of mathematics Centre for Mathematical Sciences [Cambridge] (CMS), University of Cambridge [UK] (CAM)-University of Cambridge [UK] (CAM), 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), Department of Physics and Astronomy [Lawrence Kansas], University of Kansas [Lawrence] (KU), UTSA Department of Physics and Astronomy [San Antonio], The University of Texas at San Antonio (UTSA), and ANR-15-CE31-0009,SPECTRA,Sonder le Plasma dans l'Environnement d'une ComètE avec RosettA(2015)

Subjects
Physics, comets: individual: 67P/Chuyumov-Gerasimenko plasmas methods: data analysis magnetic fields, 010504 meteorology & atmospheric sciences, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Magnetometer, Comet, Astronomy and Astrophysics, Electron, Plasma, 01 natural sciences, Charged particle, law.invention, Ion, Magnetic field, Space and Planetary Science, law, 0103 physical sciences, Diamagnetism, Atomic physics, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences
Abstract

International audience; One of the scientific objectives of the Rosetta mission is to investigate the diamagnetic cavity of comet 67P/Churyumov–Gerasimenko. We employed combined data of several instruments of the Rosetta Plasma Consortium (RPC) to identify and study diamagnetic cavity crossing events. Using electron data from the Ion Electron Sensor (IES) to complement the Magnetometer (MAG) data enabled us to work out a search criterion for the cavity crossing events based on a unique signature we identified in the electron spectrum. Although this search criterion is insufficient to find all the cavity events, we were able to find an abundance of more than one hundred cavity crossings in the data obtained in the summer of 2015. This unexpectedly high number of events allowed us to study their common features, as well as the shape and extent of the diamagnetic cavity in the terminator plane. The results suggest that in the summer of 2015 there was a cavity around comet 67P, which had a highly variable outer boundary. We present the effects of the diamagnetic cavity on the thermal and suprathermal electron and suprathermal ion content of the plasma, and also the probable mechanisms responsible for these charged particle signatures.

Published
2016

9. Birth of a comet magnetosphere: A spring of water ions

Author

Emanuele Cupido, Stas Barabash, Rickard Lundin, Martin Rubin, Etienne Behar, Pierre Henri, Masatoshi Yamauchi, Raymond Goldstein, Cyril Simon Wedlund, J. A. Sauvaud, Hannu Koskinen, Prachet Mokashi, Niklas J. T. Edberg, Chris Carr, Gabriella Stenberg Wieser, Hans Nilsson, Ingo Richter, Herbert Gunell, Esa Kallio, Andrei Fedorov, Karoly Szego, Christoph Koenders, Anders Eriksson, Martin Volwerk, James L. Burch, Claire Vallat, Martin Wieser, Zoltán Németh, Jean-Pierre Lebreton, Swedish Institute of Space Physics [Uppsala] (IRF), Belgian Institute for Space Aeronomy / Institut d'Aéronomie Spatiale de Belgique (BIRA-IASB), Blackett Laboratory, Imperial College London, Space Science Division [San Antonio], Southwest Research Institute [San Antonio] (SwRI), 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), Finnish Meteorological Institute (FMI), School of Electrical Engineering [Aalto Univ], Aalto University, 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), Swedish Institute of Space Physics [Kiruna] (IRF), Technische Universität Braunschweig = Technical University of Braunschweig [Braunschweig], Wigner Research Centre for Physics [Budapest], Hungarian Academy of Sciences (MTA), Austrian Academy of Sciences (OeAW), Rosetta Science Ground Segment (European Space Astronomy Centre), European Space Agency (ESA), Physikalisches Institut [Bern], Universität Bern [Bern], Science and Technology Facilities Council (STFC), Science and Technology Facilities Council [2006-2012], 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), Rosetta Science Ground Segment, European Space Astronomy Centre (ESAC), Agence Spatiale Européenne = European Space Agency (ESA)-Agence Spatiale Européenne = European Space Agency (ESA), and Universität Bern [Bern] (UNIBE)

Subjects
010504 meteorology & atmospheric sciences, General Science & Technology, ROSETTA PLASMA CONSORTIUM, ta221, Astronomical unit, Population, ta1171, Magnetosphere, Atmospheric-pressure plasma, 01 natural sciences, 7. Clean energy, SOLAR-WIND INTERACTION, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, ta216, education, 010303 astronomy & astrophysics, HALLEY, 0105 earth and related environmental sciences, Physics, education.field_of_study, ENVIRONMENT, ta115, Multidisciplinary, Science & Technology, ta213, ta114, Energetic neutral atom, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Comet tail, Astronomy, 67P/CHURYUMOV-GERASIMENKO, Plasma, Multidisciplinary Sciences, Solar wind, 13. Climate action, Physics::Space Physics, Science & Technology - Other Topics, RPC, Astrophysics::Earth and Planetary Astrophysics, PLANETS
Abstract

http://science.sciencemag.org/content/347/6220/aaa0571.full; International audience; The Rosetta mission shall accompany comet 67P/Churyumov-Gerasimenko from a heliocentric distance of >3.6 astronomical units through perihelion passage at 1.25 astronomical units, spanning low and maximum activity levels. Initially, the solar wind permeates the thin comet atmosphere formed from sublimation, until the size and plasma pressure of the ionized atmosphere define its boundaries: A magnetosphere is born. Using the Rosetta Plasma Consortium ion composition analyzer, we trace the evolution from the first detection of water ions to when the atmosphere begins repelling the solar wind (similar to 3.3 astronomical units), and we report the spatial structure of this early interaction. The near-comet water population comprises accelerated ions (

Published
2015

10. Evolution of the ion environment of comet 67P/Churyumov-Gerasimenko Observations between 3.6 and 2.0 AU

Author

P. Fox, Niklas J. T. Edberg, Kathleen Mandt, Emanuele Cupido, Etienne Behar, Christoph Koenders, Andrei Fedorov, Claire Vallat, Martin Volwerk, Karoly Szego, Ingo Richter, Martin Wieser, Herbert Gunell, Bernhard Geiger, S. Barabash, James L. Burch, Hannu Koskinen, G. Stenberg Wieser, Jean-Pierre Lebreton, Zoltán Németh, Rickard Lundin, Raymond Goldstein, J. A. Sauvaud, Esa Kallio, Chris Carr, Anders Eriksson, Prachet Mokashi, Masatoshi Yamauchi, C. Simon Wedlund, Pierre Henri, Hans Nilsson, Swedish Institute of Space Physics [Uppsala] (IRF), School of Electrical Engineering [Aalto Univ], Aalto University, Belgian Institute for Space Aeronomy / Institut d'Aéronomie Spatiale de Belgique (BIRA-IASB), Swedish Institute of Space Physics [Kiruna] (IRF), Technische Universität Braunschweig = Technical University of Braunschweig [Braunschweig], Southwest Research Institute [San Antonio] (SwRI), Blackett Laboratory, Imperial College London, Wigner Research Centre for Physics [Budapest], Hungarian Academy of Sciences (MTA), 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), Finnish Meteorological Institute (FMI), 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), Austrian Academy of Sciences (OeAW), Rosetta Science Ground Segment, European Space Astronomy Centre (ESAC), Agence Spatiale Européenne = European Space Agency (ESA)-Agence Spatiale Européenne = European Space Agency (ESA), PRODEX/ROSETTA/ROSINA PEA 4000107705. CSW and EK are supported by the Academy of Finland, CDDP and IC for the use of AMDA and the RPC Quicklook database (provided by a collaboration between the Centre de Données de la Physique des Plasmas (CDPP) supported by CNRS, CNES, Observatoire de Paris and Université Paul Sabatier, Toulouse and Imperial College London, supported by the UK Science and Technology Facilities Council)., 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), Rosetta Science Ground Segment (European Space Astronomy Centre), and European Space Agency (ESA)

Subjects
Physics, Comet tail, Astrophysics::High Energy Astrophysical Phenomena, comets: general, comets: individual: 67P/Churyumov-Gerasimenko, Astronomy and Astrophysics, Plasma, Astrophysics, Mass spectrometry, plasmas, 7. Clean energy, Spectral line, Ion, Solar wind, 13. Climate action, Space and Planetary Science, Sputtering, Physics::Plasma Physics, [SDU]Sciences of the Universe [physics], Comet nucleus, Physics::Space Physics, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, acceleration of particles
Abstract

International audience; Context. The Rosetta spacecraft is escorting comet 67P/Churyumov-Gerasimenko from a heliocentric distance of >3.6 AU, where the comet activity was low, until perihelion at 1.24 AU. Initially, the solar wind permeates the thin comet atmosphere formed from sublimation. Aims. Using the Rosetta Plasma Consortium Ion Composition Analyzer (RPC-ICA), we study the gradual evolution of the comet ion environment, from the first detectable traces of water ions to the stage where cometary water ions accelerated to about 1 keV energy are abundant. We compare ion fluxes of solar wind and cometary origin. Methods. RPC-ICA is an ion mass spectrometer measuring ions of solar wind and cometary origins in the 10 eV–40 keV energy range. Results. We show how the flux of accelerated water ions with energies above 120 eV increases between 3.6 and 2.0 AU. The 24 h average increases by 4 orders of magnitude, mainly because high-flux periods become more common. The water ion energy spectra also become broader with time. This may indicate a larger and more uniform source region. At 2.0 AU the accelerated water ion flux is frequently of the same order as the solar wind proton flux. Water ions of 120 eV–few keV energy may thus constitute a significant part of the ions sputtering the nucleus surface. The ion density and mass in the comet vicinity is dominated by ions of cometary origin. The solar wind is deflected and the energy spectra broadened compared to an undisturbed solar wind. Conclusions. The flux of accelerated water ions moving from the upstream direction back toward the nucleus is a strongly nonlinear function of the heliocentric distance.

Published
2015

11. Possible evidence for partial differentiation of asteroid Lutetia from Rosetta

Author

Linda T. Elkins-Tanton, Ingo Richter, Marcello Fulchignoni, Benjamin P. Weiss, M. Antonietta Barucci, Colin Snodgrass, Richard P. Binzel, Jean-Baptiste Vincent, Martin Pätzold, Paul R. Weissman, Simone Marchi, Rita Schulz, Holger Sierks, Department of Earth, Atmospheric and Planetary Sciences [MIT, Cambridge] (EAPS), Massachusetts Institute of Technology (MIT), Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), Université Pierre et Marie Curie - Paris 6 (UPMC)-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 Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Max-Planck-Institut für Sonnensystemforschung = Max Planck Institute for Solar System Research (MPS), Max-Planck-Gesellschaft, Solar System Exploration Research Virtual Institute (SSERVI), Southwest Research Institute [Boulder] (SwRI), Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), Rhenish Institute for Environmental Research (RIU), University of Cologne, Institut de Mécanique Céleste et de Calcul des Ephémérides (IMCCE), 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 de Lille-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), European Space Research and Technology Centre (ESTEC), Agence Spatiale Européenne = European Space Agency (ESA), Max-Planck-Institut für Sonnensystemforschung (MPS), Max Planck Institute for Solar System Research (MPS), and European Space Agency (ESA)

Subjects
[PHYS]Physics [physics], Planetesimal, 010504 meteorology & atmospheric sciences, Metamorphic rock, Astronomy and Astrophysics, Crust, engineering.material, 01 natural sciences, Astrobiology, Meteorite, Space and Planetary Science, Chondrite, Asteroid, 0103 physical sciences, Enstatite, engineering, Asteroid belt, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], 010303 astronomy & astrophysics, Geology, ComputingMilieux_MISCELLANEOUS, 0105 earth and related environmental sciences
Abstract

The petrologic diversity of meteorites demonstrates that planetesimals ranged from unmelted, variably metamorphosed aggregates to fully molten, differentiated bodies. However, partially differentiated bodies have not been unambiguously identified in the asteroid belt. New constraints on the density, composition, and morphology of 21 Lutetia from the Rosetta spacecraft indicate that the asteroid's high bulk density exceeds that of most known chondritic meteorite groups, yet its surface properties resemble those of some carbonaceous and enstatite chondrite groups. This indicates that Lutetia likely experienced early compaction processes like metamorphic sintering. It may have also partially differentiated, forming a metallic core overlain by a primitive chondritic crust.

Published
2012

12. Rosetta and Mars Express observations of the influence of high solar wind pressure on the Martian plasma environment

Author

Niklas J. T. Edberg, David Brain, Stanley W. H. Cowley, Markus Fränz, A. Bößwetter, James L. Burch, Rickard Lundin, Jean-Gabriel Trotignon, S. Barabash, U. Auster, Hans Nilsson, Karl-Heinz Glassmeier, Firdevs Duru, M. Samara, Ronan Modolo, Emanuele Cupido, Anders Eriksson, Ingo Richter, Raymond Goldstein, Mark Lester, Chris Carr, Swedish Institute of Space Physics [Uppsala] (IRF), Department of Physics and Astronomy [Leicester], University of Leicester, Institut für Geophysik und Extraterrestrische Physik [Braunschweig] (IGEP), Technische Universität Braunschweig = Technical University of Braunschweig [Braunschweig], Swedish Institute of Space Physics [Kiruna] (IRF), Institut für Theoretische Physik [Braunschweig], Space Sciences Laboratory [Berkeley] (SSL), University of California [Berkeley], University of California-University of California, Southwest Research Institute [San Antonio] (SwRI), Blackett Laboratory, Imperial College London, Department of Physics and Astronomy [Iowa City], University of Iowa [Iowa City], Max-Planck-Institut für Sonnensystemforschung (MPS), Max-Planck-Gesellschaft, 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), Laboratoire de physique et chimie de l'environnement (LPCE), Université d'Orléans (UO)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), University of California [Berkeley] (UC Berkeley), University of California (UC)-University of California (UC), Max-Planck-Institut für Sonnensystemforschung = Max Planck Institute for Solar System Research (MPS), and Institut national des sciences de l'Univers (INSU - CNRS)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)

Subjects
Atmospheric Science, 010504 meteorology & atmospheric sciences, Planetary bow shocks, [PHYS.ASTR.EP]Physics [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], Astrophysics::High Energy Astrophysical Phenomena, Magnetosphere, 01 natural sciences, 0103 physical sciences, Earth and Planetary Sciences (miscellaneous), Astrophysics::Solar and Stellar Astrophysics, Interplanetary physics, Interplanetary magnetic field, lcsh:Science, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, Physics, Martian, lcsh:QC801-809, Geology, Astronomy and Astrophysics, Geophysics, Mars Exploration Program, Magnetosheath, Bow shocks in astrophysics, lcsh:QC1-999, Solar wind, lcsh:Geophysics. Cosmic physics, Polar wind, 13. Climate action, Space and Planetary Science, [SDU]Sciences of the Universe [physics], Physics::Space Physics, Magnetospheric physics, Magnetopause, lcsh:Q, Astrophysics::Earth and Planetary Astrophysics, lcsh:Physics, Solar wind interactions
Abstract

We report on new simultaneous in-situ observations at Mars from Rosetta and Mars Express (MEX) on how the Martian plasma environment is affected by high pressure solar wind. A significant sharp increase in solar wind density, magnetic field strength and turbulence followed by a gradual increase in solar wind velocity is observed during ~24 h in the combined data set from both spacecraft after Rosetta's closest approach to Mars on 25 February 2007. The bow shock and magnetic pileup boundary are coincidently observed by MEX to become asymmetric in their shapes. The fortunate orbit of MEX at this time allows a study of the inbound boundary crossings on one side of the planet and the outbound crossings on almost the opposite side, both very close to the terminator plane. The solar wind and interplanetary magnetic field (IMF) downstream of Mars are monitored through simultaneous measurements provided by Rosetta. Possible explanations for the asymmetries are discussed, such as crustal magnetic fields and IMF direction. In the same interval, during the high solar wind pressure pulse, MEX observations show an increased amount of escaping planetary ions from the polar region of Mars. We link the high pressure solar wind with the observed simultaneous ion outflow and discuss how the pressure pulse could also be associated with the observed boundary shape asymmetry.

Published
2009

13. RPC: The rosetta plasma consortium

Author

Hans Nilsson, Karl-Heinz Glassmeier, A. Balogh, Jean-Gabriel Trotignon, T. Beek, G. Musmann, C. J. Pollock, J. L. Michau, Raymond Goldstein, C. G. Y. Lee, D. Lagoutte, Emanuele Cupido, Anders Eriksson, Chris Carr, K. Lundin, Bjørn Lybekk, Rickard Lundin, Ingo Richter, Reine Gill, James L. Burch, C. N. Dunford, Southwest Research Institute [San Antonio] (SwRI), Space and Atmospheric Physics Group [London], Blackett Laboratory, Imperial College London-Imperial College London, Swedish Institute of Space Physics [Uppsala] (IRF), Institut für Geophysik und Extraterrestrische Physik [Braunschweig] (IGEP), Technische Universität Braunschweig = Technical University of Braunschweig [Braunschweig], 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), Swedish Institute of Space Physics [Kiruna] (IRF), University of Oslo (UiO), and Institute for Geophysics and Meteorology [Braunschweig]

Subjects
010504 meteorology & atmospheric sciences, Magnetometer, Interface (computing), Comet, Analyser, Coma (optics), 7. Clean energy, 01 natural sciences, law.invention, Rosetta plasma consortium, symbols.namesake, space physics, law, 0103 physical sciences, Rosetta, Langmuir probe, comets, Aerospace engineering, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, Remote sensing, Physics, instrumentation, Spacecraft, business.industry, plasma physics, solar-wind comet interaction, Astronomy and Astrophysics, Plasma, Space and Planetary Science, [SDU]Sciences of the Universe [physics], symbols, RPC, business
Abstract

International audience; The Rosetta Plasma Consortium (RPC) will make in-situ measurements of the plasma enviromnent of comet 67P/Churyumov-Gerasimenko. The consortium will provide the complementary data sets necessary for an understanding of the plasma processes in the inner coma, and the structure and evolution of the coma with the increasing cometary activity. Five sensors have been selected to achieve this: the Ion and Electron Sensor (IES), the Ion Composition Analyser (ICA), the Langmuir Probe (LAP), the Mutual Impedance Probe (MIP) and the Magnetometer (MAG). The sensors interface to the spacecraft through the Plasma Interface Unit (PIU). The consortium approach allows for scientific, technical and operational coordination, and makes Optimum use of the available mass and power resources.

Published
2007

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