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1. Induced Magnetic Fields and Plasma Motions in the Inner Part of the Martian Magnetosphere

Author

E. Dubinin, M. Fraenz, R. Modolo, M. Pätzold, S. Tellmann, O. Vaisberg, S. Shuvalov, L. Zelenyi, L. Chai, Y. Wei, J. McFadden, G. DiBraccio, J. Espley, Max-Planck-Institut für Sonnensystemforschung (MPS), Max-Planck-Gesellschaft, HELIOS - 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), Rheinisches Institut für Umweltforschung (RIU), Universität zu Köln, Space Research Institute of the Russian Academy of Sciences (IKI), Russian Academy of Sciences [Moscow] (RAS), Institute of Geology and Geophysics [Beijing] (IGG), Chinese Academy of Sciences [Beijing] (CAS), Space Sciences Laboratory [Berkeley] (SSL), University of California [Berkeley], University of California-University of California, NASA Goddard Space Flight Center (GSFC), Fraenz, M., 1 Max‐Planck‐Institute for Solar System Research Göttingen Germany, Modolo, R., 2 Rheinisches Institut Fuer Umweltforschung Cologne Germany, Pätzold, M., 3 LATMOS/IPSL UVSQ Universite UPMC University Paris CNRS Guyancourt France, Tellmann, S., Vaisberg, O., 4 Institute of Space Research Moscow Russia, Shuvalov, S., Zelenyi, L., Chai, L., 5 Key Lab of Earth and Planetary Physics Institute of Geology and Geophysics Beijing People Republic of China, Wei, Y., McFadden, J., 6 Space Sciences Laboratory U. C. Berkeley Berkeley CA USA, DiBraccio, G., 7 NASA Goddard Space Flight Center Greenbelt MD USA, and Espley, J.

Subjects
ddc:523, 010504 meteorology & atmospheric sciences, 01 natural sciences, ddc:551.5, Geophysics, Physics::Plasma Physics, [SDU]Sciences of the Universe [physics], [PHYS.PHYS.PHYS-PLASM-PH]Physics [physics]/Physics [physics]/Plasma Physics [physics.plasm-ph], 13. Climate action, Space and Planetary Science, Physics::Space Physics, 0103 physical sciences, Astrophysics::Earth and Planetary Astrophysics, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences
Abstract

Analysis of Mars Atmosphere and Volatile Evolution (MAVEN)/Supra‐Thermal And Thermal Ion Composition observations in the Martian upper atmosphere, bounded at higher altitudes by the shocked solar wind, shows that the draping of interplanetary magnetic field penetrates down to low altitudes (∼200−250 km) and governs dynamics of the ionosphere. The upper ionospheric plasma is driven into motion flowing around Mars similar to the shocked solar wind in the adjacent magnetosheath. Such a fluid‐like motion is accompanied by ion acceleration caused by the bending of the magnetic field, leading to ion extraction and finally to ion pickup. Extraction of ions and their acceleration produces a recoil effect of the bulk ionosphere in the opposite direction. This provides a strong asymmetry in ion dynamics in two different hemispheres, accompanied by wrapping of the magnetic field lines around Mars and respective reconnection., Plain Language Summary: Although the Martian magnetosphere is hybrid and contains components of the induced and intrinsic magnetosphere, is possible to display these components by using the specific coordinate systems. Here we study the properties of the induced magnetosphere using the data obtained by MAVEN spacecraft. The interplanetary magnetic field penetrates deep into the Martian ionosphere draping around Mars and drive to the motion dense ionospheric plasma. Draping features and the induced plasma motions occur different in two hemispheres determined by the direction of the motional electric field in the solar wind. Ion acceleration and extraction is accompanied by a recoil effect that leads to a shift and asymmetry of the ionosphere., Key Points: Draping of the interplanetary magnetic field around Mars penetrates deep to the ionosphere enveloping the planet and driving the ionosphere to the bulk motion. Draping and motion of the ionospheric plasma is characterized by asymmetry by the direction of the motional electric field in solar wind. Ion acceleration and extraction from the ionosphere is accompanied by a shift of the bulk ionosphere in the opposite direction., National Aeronautics and Space Administration http://dx.doi.org/10.13039/100000104, DFG http://dx.doi.org/10.13039/501100001659, Russian Science Foundation http://dx.doi.org/10.13039/501100006769

Published
2021
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2. Mars Express science highlights and future plans

Author

Dmitrij Titov, Jean-Pierre Bibring, Alejandro Cardesin, John Carter, Thomas Duxbury, Francois Forget, Marco Giuranna, Francisco González-Galindo, Mats Holmström, Ralf Jaumann, Anni Määttänen, Patrick Martin, Franck Montmessin, Roberto Orosei, Martin Pätzold, Jeffrey Plaut, Mex Sgs Team, European Space Research and Technology Centre (ESTEC), European Space Agency (ESA), Institut d'astrophysique spatiale (IAS), Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), European Space Astronomy Centre (ESAC), George Mason University [Fairfax], Laboratoire de Météorologie Dynamique (UMR 8539) (LMD), Institut national des sciences de l'Univers (INSU - CNRS)-École polytechnique (X)-École des Ponts ParisTech (ENPC)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Département des Géosciences - ENS Paris, École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), Istituto di Astrofisica e Planetologia Spaziali - INAF (IAPS), Istituto Nazionale di Astrofisica (INAF), Instituto de Astrofísica de Andalucía (IAA), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Swedish Institute of Space Physics [Kiruna] (IRF), Free University of Berlin (FU), 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), Istituto di Radioastronomia [Bologna] (IRA), Rheinisches Institut für Umweltforschung (RIU), Universität zu Köln, Jet Propulsion Laboratory (JPL), and NASA-California Institute of Technology (CALTECH)

Subjects
Meridiani Planum, Martian, Amazonian, Mars, MARSIS, Mars Exploration Program, 7. Clean energy, the martian climate, SPICAM, Solar cycle, Astrobiology, HRSC, Planetengeologie, Solar wind, [SDU]Sciences of the Universe [physics], 13. Climate action, Mars Express, Ionosphere, ComputingMilieux_MISCELLANEOUS, Geology
Abstract

21st EGU General Assembly, EGU2019, proceedings from the conference held 7-12 April, 2019 in Vienna, Austria, id.11100, After 15 years in orbit Mars Express remains one of ESA's most scientifically productive Solar System missions whose publication record now exceeds 1200 papers. Characterization of the geological processes on a local-to-regional scale by HRSC, OMEGA and partner experiments on NASA spacecraft has allowed constraining land-forming processes in space and time. Recent results suggest episodic geological activity as well as the presence of large bodies of liquid water in several provinces (e.g. Eridania Planum, Terra Chimeria) in the early and middle Amazonian epoch and formation of vast sedimentary plains north of the Hellas basin. Mars Express observations and experimental teams provided essential contribution to the selection of the Mars-2020 landing sites. Recent discovery of subglacial liquid water underneath the Southern polar cap has proven that the mission science potential is still not exhausted. More than a decade-long record of the atmospheric parameters such as temperature, dust loading, water vapor and ozone abundance, water ice and CO2 clouds distribution, collected by SPICAM, PFS, OMEGA, HRSC and VMC together with subsequent modeling have provided key contributions to our understanding of the martian climate. Recent spectroscopic monitoring of the 2018 dust storm revealed dust properties, their spatial and temporal variations and atmospheric circulation. More than 10,000 crossings of the bow shock by Mars Express allowed ASPERA-3 to characterize complex behavior of the magnetic boundary topology as function of the solar EUV flux. Observations of the ion escape during complete solar cycle revealed important dependencies of the atmospheric erosion rate on parameters of the solar wind and EUV flux and established global energy balance between the solar wind and escaping ion flow. The observations showed that ion escape can be responsible for removal of about 10 mbar over the Mars history that implies existence of other more effective escape channels. The structure of the ionosphere sounded by the MARSIS radar and the MaRS radio science experiment was found to be significantly affected by the solar activity, the crustal magnetic field, as well as by the influx of meteorite and cometary dust. MARSIS and ASPERA-3 observations suggest that the sunlit ionosphere over the regions with strong crustal fields is denser and extends to higher altitudes as compared to the regions with no crustal anomalies. Several models of the upper atmosphere and plasma environment are being developed based on and in support of the collected experimental data. The models aim at creating user-friendly data base of plasma parameters similar to the Mars Climate Database that would be of great service to the planetary community. A significant recent achievement was the flawless transition to the >gyroless> attitude control and operations mode on the spacecraft, that would allow mitigating the onboard gyros aging and extending the mission lifetime. In November 2018 ESA's Science Programme Committee (SPC) confirmed the mission operations till the end of 2020 and notionally approved its extension till the end of 2022. The talk will give the Mars Express status, review the recent science highlights, and outline future plans focusing on synergistic science with TGO.

Published
2021
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3. The gravity field and internal structure of Comet 67P/Churyumov-Gerasimenko

Author

Andert, Tom, Barriot, Jean-Pierre, Pätzold, Martin, Jacob, Robert, Tellmann, Silvia, Häusler, Bernd, Marty, Jean-Charles, LAURENT-VARIN, Julien, Sierks, Holger, Guttler, Carsten, Tubiana, Cecilia, Hahn, Matthias, Universität der Bundeswehr München [Neubiberg], Université de la Polynésie Française (UPF), Géopôle du Pacifique Sud (GePaSUD), Rheinisches Institut für Umweltforschung (RIU), Universität zu Köln, Géosciences Environnement Toulouse (GET), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-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), Max Planck Institute for Solar System Research (MPS), and Max-Planck-Gesellschaft

Subjects
[SPI]Engineering Sciences [physics], [SDU]Sciences of the Universe [physics], ComputingMilieux_MISCELLANEOUS
Abstract

International audience

Published
2019

4. The induced magnetosphere of Mars. Asymmetrical topology of the magnetic field lines

Author

Lev Zelenyi, John E. P. Connerney, Joachim Woch, Yong Wei, J. P. McFadden, Ronan Modolo, Markus Fraenz, Gina A. DiBraccio, Lihui Chai, Elena Grigorenko, Martin Paetzold, Eduard Dubinin, Jared Espley, Max-Planck-Institut für Sonnensystemforschung (MPS), Max-Planck-Gesellschaft, 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), Rheinisches Institut für Umweltforschung (RIU), Universität zu Köln, CAS Key Laboratory of Earth and Planetary Physics (EPP), Institute of Geology and Geophysics [Beijing] (IGG), Chinese Academy of Sciences [Beijing] (CAS)-Chinese Academy of Sciences [Beijing] (CAS), NASA Goddard Space Flight Center (GSFC), Space Sciences Laboratory [Berkeley] (SSL), University of California [Berkeley], University of California-University of California, GSFC Solar System Exploration Division, Space Research Institute of the Russian Academy of Sciences (IKI), and Russian Academy of Sciences [Moscow] (RAS)

Subjects
Physics, 010504 meteorology & atmospheric sciences, Field line, Magnetosphere, Plasma, Mars Exploration Program, 010502 geochemistry & geophysics, 01 natural sciences, Magnetic field, Computational physics, Geophysics, [SDU]Sciences of the Universe [physics], Electric field, Physics::Space Physics, General Earth and Planetary Sciences, Astrophysics::Earth and Planetary Astrophysics, Ionosphere, Interplanetary magnetic field, 0105 earth and related environmental sciences
Abstract

International audience; An asymmetrical pileup of the interplanetary magnetic field (IMF) leads to an additional draping of the field lines in the opposite direction to the motional electric field. Such a draping and the associated magnetic field forces push the ionosphere plasma in the transverse direction opening a passage for an ion trail which contains dense and slowly moving plasma. We found that wrapping of the field lines around Mars starts in the hemisphere pointing in the direction of the motional electric field and propagates to the opposite hemisphere where the cross‐flow component of the draped IMF changes sign in a broad area accompanied by the formation of loops of closed field lines. Reconnection near Mars accompanied by the generation of plasma vortices imposes serious constraints on the ion dynamics and their escape through the tail. The existence of all these features is confirmed by hybrid simulations.

Published
2019
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5. Mars Express science highlights and future plans

Author

Dmitrij V. Titov, Francisco Gonzalez-Galindo, Mats Holmström, Thomas C. Duxbury, Ralf Jaumann, Alejandro Cardesin, Patrick Martin, Jeffrey J. Plaut, Roberto Orosei, Marco Giuranna, Anni Määttänen, Jean-Pierre Bibring, François Forget, Franck Montmessin, Martin Pätzold, European Space Research and Technology Centre (ESTEC), European Space Agency (ESA), Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), European Space Astronomy Centre (ESAC), George Mason University [Fairfax], Laboratoire de Météorologie Dynamique (UMR 8539) (LMD), Institut national des sciences de l'Univers (INSU - CNRS)-École polytechnique (X)-École des Ponts ParisTech (ENPC)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Département des Géosciences - ENS Paris, École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), Istituto di Astrofisica e Planetologia Spaziali - INAF (IAPS), Istituto Nazionale di Astrofisica (INAF), Instituto de Astrofísica de Andalucía (IAA), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Swedish Institute of Space Physics [Kiruna] (IRF), DLR Institut für Planetenforschung, Deutsches Zentrum für Luft- und Raumfahrt [Berlin] (DLR), 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), Space Applications Center (SAC), Indian Space Research Organisation (ISRO), Istituto di Radioastronomia [Bologna] (IRA), Rhenish Institute for Environmental Research (RIU), University of Cologne, Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), Cardon, Catherine, Agence Spatiale Européenne = European Space Agency (ESA), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-École polytechnique (X)-École des Ponts ParisTech (ENPC)-Centre National de la Recherche Scientifique (CNRS)-Département des Géosciences - ENS Paris, École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École normale supérieure - Paris (ENS-PSL), DLR Institute of Planetary Research, German Aerospace Center (DLR), 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), Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), Rheinisches Institut für Umweltforschung (RIU), Universität zu Köln, 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), Département des Géosciences - ENS Paris, and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-École des Ponts ParisTech (ENPC)-École polytechnique (X)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC)

Subjects
Solar System, Spacecraft, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], business.industry, Earth science, Amazonian, [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], MARSIS, Mars Exploration Program, Structural basin, [SDU.ASTR] Sciences of the Universe [physics]/Astrophysics [astro-ph], law.invention, law, 13. Climate action, [SDU]Sciences of the Universe [physics], Sedimentary rock, Radar, business, Geology
Abstract

After 16 years in orbit Mars Express remains one of ESA’s most scientifically productive Solar System missions which publication record now exceeds 1270 papers. Characterization of the geological processes on a local-to-regional scale by HRSC, OMEGA and partner experiments on NASA spacecraft has allowed constraining land-forming processes in space and time. Recent studies suggest geological evidence of a planet-wide groundwater system on Mars and surface clay formation during short-term warmer and wetter conditions on a largely cold ancient Mars that might indicate a change in our understanding of early Mars climate. HRSC team released first set of multi-orbit Digital Elevation Model (DEM) of the MC-11 quadrangle and the Southern polar cap with 50 m/px resolution. Mars Express observations and experimental teams provided essential contribution to the selection of the Mars-2020 landing sites and supporting characterization of potential landing sites for the Chinese HX-1 mission. Following recent discovery of subglacial liquid water underneath the Southern polar layered deposits the MARSIS radar continues searching for subsurface water pockets.One-and-half decade of monitoring of atmospheric parameters such as temperature, dust loading, water vapor and ozone abundance, water ice and CO2 clouds distribution, collected by SPICAM, PFS, OMEGA, HRSC and VMC together with subsequent modeling have provided key contributions to our understanding of the Martian climate. The observed ozone climatology demonstrate significant discrepancies with model predictions indicating the need for models improvement. In 2018 PFS confirmed observations of a methane abundance “spike” in the Gale crater observed in situ by the Curiosity Rover. Recent similar quasi-simultaneous observations were in disagreement, thus indicating that the methane “enigma” continues. This poses a significant challenge to both observers and modelers. The radio-science experiment MaRS revealed fine structure of the boundary layer. Its depth varies from 2 km in topographic lows to ~10 km over highlands.Observations of the ion escape during complete solar cycle revealed that ion escape can be responsible for removal of about 10 mbar over Mars history that implies existence of other more effective escape channels. The structure of the ionosphere derived from MARSIS and MaRS sounding was found to be significantly affected by the solar activity, the crustal magnetic field. The observations suggest that the sunlit ionosphere over the regions with strong crustal fields is denser and extends to higher altitudes as compared to the regions with no crustal anomalies. Expansion of the ionosphere was also observed during the global dust storm. Ionospheric models aim at creating user-friendly data base of plasma parameters that would be of great service to the planetary community.The “gyroless” attitude control and operations mode of the spacecraft operates flawlessly since April 2018. Aging batteries impose more and more limitations on science operations during eclipse seasons. The mission is now confirmed till the end of 2020 and notionally extended till the end of 2022. The talk will give the Mars Express status, review the recent science highlights, and outline future plans including synergistic science with TGO.

Published
2019

6. The low-degree gravity field of Phobos from two Mars Express flybys

Author

Yang, Xuan, Yan, Jianguo, Andert, Thomas, Ye, Mao, Pätzold, Martin, Hahn, Matthias, Jin, Weitong, Li, Fei, Barriot, Jean-Pierre, Rheinisches Institut für Umweltforschung (RIU), Universität zu Köln, Géopôle du Pacifique Sud (GePaSUD), and Université de la Polynésie Française (UPF)

Subjects
[PHYS]Physics [physics], Physics::Space Physics, Astrophysics::Earth and Planetary Astrophysics
Abstract

International audience; Several close spacecraft flybys of Phobos have been performed over the past 40 years in order to determine the gravity field of this tiny Martian moon. In this work, the gravity field of Phobos is derived from the radio tracking data of two combined MEX flybys (2010 and 2013) applying a least squares inverse technique, by using as a first guess the gravity field modelled from the shape model and a constant density hypothesis. The result shows a good agreement with previous publications and the precision of GM as well as C20 increased by two to three times.

Published
2019

7. Internal structure of the nucleus of 67P/Churyumov-Gerasimenko from its gravity field

Author

Hahn, Matthias, Pätzold, Martin, Tellmann, Silvia, Häusler, Bernd, Andert, Tom, Barriot, Jean-Pierre, Rheinisches Institut für Umweltforschung (RIU), Universität zu Köln, Institut für Raumfahrttechnik, Universität der Bundeswehr München [Neubiberg], Géopôle du Pacifique Sud (GePaSUD), and Université de la Polynésie Française (UPF)

Subjects
[PHYS]Physics [physics]
Abstract

International audience; Various models of the interior nucleus structure and density distributions are used to compute simulated values of the gravity field coefficients. A comparison with the observed coefficients yields the feasibility of the theoretical interior structure. Thus, the gravity field helps constraining models of the internal structure, the composition and also of the origin and formation of the comets' nucleus. Another approach was applied with a model of the nucleus using mass concentrations. This results in a more precise representation of the highly irregular gravity field. It also enables to model various different density structures within the nucleus and test them with an orbit determination procedure.

Published
2019

8. The Nucleus of Comet 67P/Churyumov-Gerasimenko from RSI observations

Author

Hahn, Matthias, Tellmann, Silvia, Häusler, Bernd, Andert, Tom, Barriot, Jean-Pierre, Asmar, Sami W., Bird, Michael K., Oschlisniok, Janusz, Peter, Kerstin, Rheinisches Institut für Umweltforschung (RIU), Universität zu Köln, Institut für Raumfahrttechnik, Universität der Bundeswehr München [Neubiberg], Géopôle du Pacifique Sud (GePaSUD), Université de la Polynésie Française (UPF), Jet Propulsion Laboratory (JPL), California Institute of Technology (CALTECH)-NASA, Argelander-Institut für Astronomie (AlfA), and Rheinische Friedrich-Wilhelms-Universität Bonn

Subjects
[PHYS]Physics [physics], ComputingMilieux_MISCELLANEOUS
Abstract

International audience

Published
2019

9. A dynamic atmosphere revealed by the Venus Express mission

Author

Wilson, Colin, Svedhem, Håkan, Drossart, Pierre, Piccioni, Giuseppe, Markiewicz, Wojciech J., Pätzold, M., Titov, Dmitry V., Bertaux, Jean-Loup, Department of Atmospheric, Oceanic and Planetary Physics [Oxford] (AOPP), University of Oxford, European Space Research and Technology Centre (ESTEC), Agence Spatiale Européenne = European Space Agency (ESA), 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), Pôle Planétologie du LESIA, 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)-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), Istituto di Astrofisica Spaziale e Fisica cosmica - Roma (IASF-Roma), Istituto Nazionale di Astrofisica (INAF), Max-Planck-Institut für Sonnensystemforschung = Max Planck Institute for Solar System Research (MPS), Max-Planck-Gesellschaft, Rheinisches Institut für Umweltforschung (RIU), Universität zu Köln = University of Cologne, PLANETO - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), and 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)

Subjects
[PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract

International audience; ESA’s Venus Express orbiter has achieved a mission lifetime of eight years, well in excess of its original nominal science mission duration of 500 days. The science payload was selected to focus on atmospheric investigations from the deep atmosphere - probed using near-infrared spectral windows - up to the mesosphere and exosphere. While initial analyses focussed on first detections and mean atmospheric states, subsequent analyses have revealed variability on timescales ranging from diurnal to seasonal to multiannual. In the upper atmosphere, VEx/VIRTIS shows dramatic maps of O_{2} nightglow spatial distribution changing location on scales of minutes to hours, as well as gravity waves high in polar regions high above the core of the polar vortex. Thermospheric and mesospheric densities, revealed through solar and stellar occultation as well as by the VEx Atmospheric Drag Experiment, are observed to vary by over 100% on a day-to-day basis. The Southern polar vortex was revealed to change shape on a day-to-day basis, taking sometimes the previously observed wavenumber-2 shape (“polar dipole”) but changing rapidly also to wavenumber-1 or wavenumber-3 shapes. In the lower / middle cloud layer Venus Express was able to map the formation and dissipation of regions of thin and thick cloud on timescales of hours to days. But it is the long-term changes on periods of several years which are perhaps the most intriguing. Mean zonal wind speed at low latitudes at cloud-top altitude, as revealed by cloud tracking in UV imagery, is found to have increased by 30% over the period 2007-2013. Mesospheric sulphur dioxide abundances were found to increase fourfold during 2006-2008 followed by a tenfold decrease in 2008-2012, echoing a pattern seen earlier from Pioneer Venus and Hubble observations. There may also be associated long-term changes in the UV albedo of Venus - this is still under investigation. But to date no long-term trend has been observed in the abundance of other trace gas species, notably of water vapour, which might be expected to vary alongside mesospheric sulphur dioxide abundances. Explaining this combination of observations provides constraints and challenges for our understanding of the Venus atmosphere. In this presentation we review the highlights of Venus Express atmospheric science results, with particular focus on temporal variability.

Published
2014

10. Transiting exoplanets from the CoRoT space mission. XXI. CoRoT-19b: a low density planet orbiting an old inactive F9V-star

Author

Aldo S. Bonomo, Magali Deleuil, M. Ollivier, Lev Tal-Or, Stefan Dreizler, Guillaume Hébrard, Helmut Lammer, Hannu Parviainen, François Bouchy, J. Weingrill, Laurent Jorda, Annie Baglin, C. Moutou, B. Tingley, Rudolf Dvorak, Michaël Gillon, Sylvio Ferraz-Mello, Roi Alonso, Rodrigo F. Díaz, J. M. Almenara, B. Samuel, Alexandre Santerne, S. Carpano, Michel Auvergne, Emmanuel Jehin, Neale P. Gibson, Lisa Nortmann, Anders Erikson, Pierre Barge, Davide Gandolfi, A. Léger, Daniel Rouan, Sz. Csizmadia, Pascal Bordé, Hans J. Deeg, Martin Paetzold, Didier Queloz, Aviv Ofir, Hans Bruntt, E. W. Guenther, Tristan Guillot, Ludmila Carone, M. Havel, G. Wuchterl, Jean Schneider, Heike Rauer, T. Pasternacki, Tsevi Mazeh, M. Fridlund, Artie P. Hatzes, J. C. Gazzano, Suzanne Aigrain, Juan Cabrera, C. Cavarroc, Thüringer Landessternwarte Tautenburg (TLS), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Observatoire de Haute-Provence (OHP), Institut Pythéas (OSU PYTHEAS), Institut de Recherche pour le Développement (IRD)-Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Institut de Recherche pour le Développement (IRD)-Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE), Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA), School of Physics and Astronomy [Tel Aviv] (TAU), Raymond and Beverly Sackler Faculty of Exact Sciences [Tel Aviv] (TAU), Tel Aviv University (TAU)-Tel Aviv University (TAU), 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), Department of Physics [Oxford], University of Oxford, DLR Institute of Planetary Research, German Aerospace Center (DLR), Observatoire Astronomique de l'Université de Genève (ObsGE), Université de Genève = University of Geneva (UNIGE), Instituto de Astrofisica de Canarias (IAC), 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), Institut d'astrophysique spatiale (IAS), Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Department of Physics and Astronomy [Aarhus], Aarhus University [Aarhus], Rheinisches Institut für Umweltforschung (RIU), Universität zu Köln = University of Cologne, European Space Research and Technology Centre (ESTEC), Agence Spatiale Européenne = European Space Agency (ESA), Georg-August-University = Georg-August-Universität Göttingen, University of Vienna [Vienna], Universidade Federal de São Paulo, Institut d'Astrophysique et de Géophysique [Liège], Université de Liège, Laboratoire de Cosmologie, Astrophysique Stellaire & Solaire, de Planétologie et de Mécanique des Fluides (CASSIOPEE), Université Nice Sophia Antipolis (1965 - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Space Research Institute of Austrian Academy of Sciences (IWF), Austrian Academy of Sciences (OeAW), German Aerospace Centre (DLR), Institute of Aerodynamics & Flow Technology, Technical University of Berlin / Technische Universität Berlin (TU), Laboratoire Univers et Théories (LUTH (UMR_8102)), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Université Nice Sophia Antipolis (... - 2019) (UNS), Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Laboratoire des technologies de la microélectronique (LTM), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS), 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), School of Physics, University of Exeter, Departamento de Matemàtica, PUC RIO, Institut de Recherche pour le Développement (IRD)-Aix Marseille Université (AMU)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Aix Marseille Université (AMU)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Centre National de la Recherche Scientifique (CNRS), Stellar Astrophysics Centre [Aarhus] (SAC), Institut de Radioprotection et de Sûreté Nucléaire (IRSN), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), ON/MCT (ON/MCT, 20921-030, Rio de Janeiro, Brazil)), ON/MCT, Instituto de Astronomia, Geofísica e Ciências Atmosféricas [São Paulo] (IAG), Universidade de São Paulo = University of São Paulo (USP), Research and Scientific Support Department, ESTEC (RSSD), Agence Spatiale Européenne = European Space Agency (ESA)-Agence Spatiale Européenne = European Space Agency (ESA), Department of Brain and Behavioural Sciences, Università degli Studi di Pavia = University of Pavia (UNIPV), Joseph Louis LAGRANGE (LAGRANGE), Université Joseph Fourier - Grenoble 1 (UJF)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Centre National de la Recherche Scientifique (CNRS), Rhenish Institute for Environmental Research (RIU), University of Cologne, DLR Institut für Planetenforschung, Deutsches Zentrum für Luft- und Raumfahrt [Berlin] (DLR), and Institut für Astrophysik [Göttingen]

Subjects
transits, photometry, planetary systems, photometric, radial velocities, spectroscopic, [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], FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Ephemeris, 01 natural sciences, Jupiter, Planet, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Transit (astronomy), 010303 astronomy & astrophysics, ComputingMilieux_MISCELLANEOUS, Astrophysics::Galaxy Astrophysics, Earth and Planetary Astrophysics (astro-ph.EP), [PHYS]Physics [physics], Physics, 010308 nuclear & particles physics, Giant planet, Astronomy, Astronomy and Astrophysics, Radius, Exoplanet, Corot, Radial velocity, exoplanets, Space and Planetary Science, Astrophysics::Earth and Planetary Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Earth and Planetary Astrophysics
Abstract

Observations of transiting extrasolar planets are of key importance to our understanding of planets because their mass, radius, and mass density can be determined. The CoRoT space mission allows us to achieve a very high photometric accuracy. By combining CoRoT data with high-precision radial velocity measurements, we derive precise planetary radii and masses. We report the discovery of CoRoT-19b, a gas-giant planet transiting an old, inactive F9V-type star with a period of four days. After excluding alternative physical configurations mimicking a planetary transit signal, we determine the radius and mass of the planet by combining CoRoT photometry with high-resolution spectroscopy obtained with the echelle spectrographs SOPHIE, HARPS, FIES, and SANDIFORD. To improve the precision of its ephemeris and the epoch, we observed additional transits with the TRAPPIST and Euler telescopes. Using HARPS spectra obtained during the transit, we then determine the projected angle between the spin of the star and the orbit of the planet. We find that the host star of CoRoT-19b is an inactive F9V-type star close to the end of its main-sequence life. The host star has a mass M*=1.21+/-0.05 Msun and radius R*=1.65+/-0.04 Rsun. The planet has a mass of Mp=1.11+/-0.06 Mjup and radius of Rp=1.29+/-0.03 Rjup. The resulting bulk density is only rho=0.71+/-0.06 gcm-3, which is much lower than that for Jupiter. The exoplanet CoRoT-19b is an example of a giant planet of almost the same mass as Jupiter but a 30% larger radius., 6 pages, 7 figures

Published
2012
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11. Transiting exoplanets from the CoRoT space mission

Author

Bouchy, F., Deleuil, M., Guillot, T., Aigrain, S., Carone, L., Cochran, W., Almenara, J., Alonso, R., Auvergne, M., Baglin, A., Barge, P., Bonomo, A., Bordé, P., Csizmadia, Sz., de Bondt, K., Deeg, H., Díaz, R., Dvorak, R., Endl, M., Erikson, A., Ferraz-Mello, S., Fridlund, M., Gandolfi, D., Gazzano, J., Gibson, N., Gillon, M., Guenther, E., Hatzes, A., Havel, M., Hébrard, G., Jorda, L., Léger, A., Lovis, C., Llebaria, A., Lammer, H., Macqueen, P., Mazeh, T., Moutou, C., Ofir, A., Ollivier, M., Parviainen, H., Pätzold, M., Queloz, D., Rauer, H., Rouan, Daniel, Santerne, A., Schneider, J., Tingley, B., Wuchterl, G., Observatoire de Haute-Provence (OHP), Institut Pythéas (OSU PYTHEAS), Institut de Recherche pour le Développement (IRD)-Aix Marseille Université (AMU)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Aix Marseille Université (AMU)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Centre National de la Recherche Scientifique (CNRS), Institut d'Astrophysique de Paris (IAP), 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 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), Laboratoire de Cosmologie, Astrophysique Stellaire & Solaire, de Planétologie et de Mécanique des Fluides (CASSIOPEE), Université Nice Sophia Antipolis (1965 - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Department of Physics [Oxford], University of Oxford, Rheinisches Institut für Umweltforschung (RIU), Universität zu Köln = University of Cologne, McDonald Observatory, University of Texas at Austin [Austin], Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), Observatoire Astronomique de l'Université de Genève (ObsGE), Université de Genève = University of Geneva (UNIGE), Observatoire de Paris, Université Paris sciences et lettres (PSL), Institut d'astrophysique spatiale (IAS), Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), DLR Institute of Planetary Research, German Aerospace Center (DLR), Institut de Planétologie et d'Astrophysique de Grenoble (IPAG ), Observatoire des Sciences de l'Univers de Grenoble (OSUG), Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de physique et chimie des nano-objets (LPCNO), Institut National des Sciences Appliquées - Toulouse (INSA Toulouse), Institut National des Sciences Appliquées (INSA)-Université de Toulouse (UT)-Institut National des Sciences Appliquées (INSA)-Université de Toulouse (UT)-Institut de Chimie de Toulouse (ICT), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS)-Institut National Polytechnique (Toulouse) (Toulouse INP), Université de Toulouse (UT)-Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS)-Institut National Polytechnique (Toulouse) (Toulouse INP), Université de Toulouse (UT)-Institut de Recherche sur les Systèmes Atomiques et Moléculaires Complexes (IRSAMC), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Centre National de la Recherche Scientifique (CNRS)-Centre National de la Recherche Scientifique (CNRS), Institute of Astronomy, University of Vienna [Vienna], McDonald Observatory, University of Texas, Institute of Astronomy, Geophysics and Atmospheric Sciences (IAG), Universidade de São Paulo = University of São Paulo (USP), Research and Scientific Support Department, ESTEC (RSSD), European Space Research and Technology Centre (ESTEC), Agence Spatiale Européenne = European Space Agency (ESA)-Agence Spatiale Européenne = European Space Agency (ESA), Thüringer Landessternwarte Tautenburg (TLS), Université de Liège, Université de Nice Sophia-Antipolis (UNSA), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Institut für Weltraumforschung = Space Research institute [Graz] (IWF), Osterreichische Akademie der Wissenschaften (ÖAW), School of Physics and Astronomy [Tel Aviv] (TAU), Raymond and Beverly Sackler Faculty of Exact Sciences [Tel Aviv] (TAU), Tel Aviv University (TAU)-Tel Aviv University (TAU), Instituto de Astrofisica de Canarias (IAC), Universidad de La Laguna [Tenerife - SP] (ULL), Tech Univ Berlin, Inst Opt & Atom Phys, Hardenbergstr 36, D-10623 Berlin, Germany, 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), Laboratoire Univers et Théories (LUTH (UMR_8102)), and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)

Subjects
[PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract

International audience

Published
2011
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12. The Assimilation of Envisat data (ASSET) project

Author

S. Rharmili, Marco Ridolfi, Boris Khattatov, A. F. Vik, Slimane Bekki, T. von Clarmann, D. Fonteyn, Sebastien Massart, Simone Ceccherini, Alan J. Geer, O. Talagrand, Quentin Errera, Arjo Segers, William Lahoz, David Jackson, H. E. Thornton, Niels Bormann, Vincent-Henri Peuch, Marion Marchand, Henk Eskes, Hendrik Elbern, Data Assimilation Research Centre [Reading] (DARC), University of Reading (UOR), 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), European Centre for Medium-Range Weather Forecasts (ECMWF), Istituto di Fisica Applicata 'Nello Carrara' (IFAC), Consiglio Nazionale delle Ricerche [Roma] (CNR), Rheinisches Institut für Umweltforschung (RIU), Universität zu Köln, Belgian Institute for Space Aeronomy / Institut d'Aéronomie Spatiale de Belgique (BIRA-IASB), Royal Netherlands Meteorological Institute (KNMI), United Kingdom Met Office [Exeter], Fusion Numerics, Inc, Centre Européen de Recherche et de Formation Avancée en Calcul Scientifique (CERFACS), CERFACS, Météo-France [Paris], Météo France, Alma Mater Studiorum Università di Bologna [Bologna] (UNIBO), Laboratoire de Météorologie Dynamique (UMR 8539) (LMD), Département des Géosciences - ENS Paris, École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-École des Ponts ParisTech (ENPC)-École polytechnique (X)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Norsk Institutt for Luftforskning (NILU), Forschungszentrum Karlsruhe, ASSET, COST, ISSI, European Project: EVK2-CT-2002-00137, National Research Council of Italy | Consiglio Nazionale delle Ricerche (CNR), Universität zu Köln = University of Cologne, Météo-France, Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-École polytechnique (X)-École des Ponts ParisTech (ENPC)-Centre National de la Recherche Scientifique (CNRS)-Département des Géosciences - ENS Paris, École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), Norwegian Institute for Air Research (NILU), W. A. Lahoz, A. J. Geer, S. Bekki, N. Bormann, S. Ceccherini, H. Elbern, Q. Errera, H. J. Eske, D. Fonteyn, D. R. Jackson, B. Khattatov, S. Massart, V. H. Peuch, S. Rharmili, M. Ridolfi, A. Seger, O. Talagrand, H. E. Thornton, A. F. Vik, and T. von Clarmann

Subjects
Atmospheric Science, Earth observation, Meteorological reanalysis, Meteorology, 010504 meteorology & atmospheric sciences, Asset (computer security), 7. Clean energy, 01 natural sciences, Troposphere, 010309 optics, lcsh:Chemistry, Atmospheric composition and structure, Data assimilation, 0103 physical sciences, ddc:550, Inversione, Data archival, 0105 earth and related environmental sciences, [SDU.OCEAN]Sciences of the Universe [physics]/Ocean, Atmosphere, Atmospheric composition, Assimilation (biology), Remote sensing, Numerical weather prediction, lcsh:QC1-999, lcsh:QD1-999, 13. Climate action, Assimilation, Environmental science, lcsh:Physics
Abstract

International audience This paper discusses the highlights of the EU-funded "Assimilation of Envisat data" (ASSET) project, which has involved assimilation of Envisat atmospheric constituent and temperature data into systems based on Numerical Weather Prediction (NWP) models and chemical transport models (CTMs). Envisat was launched in 2002 and is one of the largest Earth Observation (EO) satellites ever built. It carries several sophisticated EO instruments providing insights into chemistry and dynamics of the atmosphere. In this paper we focus on the assimilation of temperature and constituents from Envisat. The overarching theme of the ASSET project has been to bring together experts from all aspects of the data assimilation problem. This has allowed ASSET to address several themes comprehensively: enhancement of NWP analyses by assimilation of research satellite data; studies of the distribution of stratospheric chemical species by assimilation of research satellite data into CTM systems; objective assessment of the quality of ozone analyses; studies of the spatial and temporal evolution of tropospheric pollutants; enhanced retrievals of Envisat data; and data archival and dissemination. Among the results from the ASSET project, many of which are firsts in their field, we can mention: a positive impact on NWP analyses from assimilation of height-resolved stratospheric humidity and temperature data, and assimilation of limb radiances; the extraction of temperature information from the assimilation of chemical species into CTMs; a first intercomparison between ozone assimilation systems; the extraction of information on tropospheric pollution from assimilation of Envisat data; and the large potential of the Envisat MIPAS dataset. This paper discusses these, often novel, developments and results. Finally, achievements of, and recommendations from, the ASSET project are presented.

Published
2007
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