Author: "HELIOS - LATMOS" - Searchworks@Jio Institute Digital Library Search Results

Your search keyword '"HELIOS - LATMOS"' showing total 835 results

Start Over Author "HELIOS - LATMOS"

835 results on '"HELIOS - LATMOS"'

1. Connecting Coronal 3D Electron Density from Tomographic Reconstruction to In-situ Measurements from Parker Solar Probe

Author: Philippe Lamy, Julien Wojak, Aix Marseille Université (AMU), HELIOS - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), and Cardon, Catherine
Subjects: [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], [SDU.ASTR] Sciences of the Universe [physics]/Astrophysics [astro-ph]
Abstract: There are few possibilities to put the in-situ measurements of the coronal electron density such as obtained by the Parker Solar Probe (PSP) in the context of the 3D configuration of the corona and its structure. One of them consists in using MHD models relying on synoptic maps of the photospheric magnetic field, but their accuracy is subject to questions, especially in the case of complex coronae of the maximum type. The 2D inversion of white-light coronagraphic images requires the simplified assumption of spherical symmetry of the corona which basically washes out the longitudinal variations. We will present preliminary results of a new method which makes use of the 3D time-dependent tomographic reconstruction of the coronal electron density based on accurately corrected and calibrated LASCO-C2 images of the polarized brightness of the corona. It is performed over a sliding window of 14 days (half a Carrington rotation) centered at the times of the PSP perihelion with a time interval of 4 days. The resulting “cubes” of the 3D electron density Ne are visualized from six different vantage points and with movies. The orbit of PSP is projected on a synoptic map of Ne extracted from the cubes at a heliocentric distance of 5.5 Rs; the track extends from Perihelion-5 days to Perihelion+5 days. The electron density at the heliocentric distances of PSP is extrapolated radially from the values at 5.5 Rs using an inverse square law and compared with the in-situ measurements collected by PSP/FIELDS. We will present results from the first PSP encounters.
Published: 2023

2. Exploring Fundamental Particle Acceleration and Loss Processes in Heliophysics through an Orbiting X-ray Instrument in the Jovian System (A White Paper for the 2024-2033 Solar and Space Physics (Heliophysics) Decadal Survey)

Author: Dunn, W, Berland, G, Roussos, E, Clark, G, Kollmann, P, Turner, D, Feldman, C, Stallard, T, Branduardi-Raymont, G, Woodfield, E, Rae, I, Ray, L, Carter, J, Lindsay, S, Yao, Z, Marshall, R, Jaynes, A, Ezoe, Y, Numazawa, M, Hospodarsky, G, Wu, X, Weigt, D, Jackman, C, Mori, K, Nénon, Quentin, Desai, R, Blum, L, Nordheim, T, Ness, J, Bodewits, D, Kimura, T, Li, W, Smith, H, Millas, D, Wibisono, A, Achilleos, N, Koutroumpa, Dimitra, Mcentee, S, Collier, H, Bhardwaj, A, Martindale, A, Wolk, S, Badman, S, Kraft, R, University College of London [London] (UCL), Centre for Planetary Sciences [UCL/Birkbeck] (CPS), University of Colorado [Boulder], Max-Planck-Institut für Sonnensystemforschung = Max Planck Institute for Solar System Research (MPS), Max-Planck-Gesellschaft, Johns Hopkins University Applied Physics Laboratory [Laurel, MD] (APL), University of Leicester, Mullard Space Science Laboratory (MSSL), British Antarctic Survey (BAS), Natural Environment Research Council (NERC), University of Northumbria at Newcastle [United Kingdom], Lancaster University, Chinese Academy of Sciences [Beijing] (CAS), University of Iowa [Iowa City], Tokyo Metropolitan University [Tokyo] (TMU), Université de Genève = University of Geneva (UNIGE), Dublin Institute for Advanced Studies (DIAS), Columbia University [New York], 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), Imperial College London, University of Warwick [Coventry], Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), European Space Astronomy Centre (ESAC), Agence Spatiale Européenne = European Space Agency (ESA), Auburn University (AU), Tokyo University of Science [Tokyo], Boston University [Boston] (BU), HELIOS - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), 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), Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich), University of Applied Sciences and Arts Northwestern Switzerland (FHNW), Physical Research Laboratory [Ahmedabad] (PRL), Indian Space Research Organisation (ISRO), Smithsonian Astrophysical Observatory, and Smithsonian Institution
Subjects: [SDU.ASTR.SR]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR]
Published: 2023

3. Space Plasma Physics Science Opportunities for the Lunar Orbital Platform - Gateway

Author: Iannis Dandouras, Matt G. G. T. Taylor, Johan De Keyser, Yoshifumi Futaana, Ruth A. Bamford, Graziella Branduardi-Raymont, Jean-Yves Chaufray, Dragos Constantinescu, Elisabetta De Angelis, Pierre Devoto, Jonathan Eastwood, Marius Echim, Philippe Garnier, Benjamin Grison, David Hercik, Helmut Lammer, André Laurens, François Leblanc, Anna Milillo, Rumi Nakamura, Lubomír Přech, Elias Roussos, Štěpán Štverák, Julien Forest, Arnaud Trouche, Sébastien L. G. Hess, Jean-Charles Mateo-Vélez, James Carpenter, Josef Winter, Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-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 Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), ESA, CNES, Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), 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), European Space Research and Technology Centre (ESTEC), Agence Spatiale Européenne = European Space Agency (ESA), Belgian Institute for Space Aeronomy / Institut d'Aéronomie Spatiale de Belgique (BIRA-IASB), Swedish Institute of Space Physics [Kiruna] (IRF), STFC Rutherford Appleton Laboratory (RAL), Science and Technology Facilities Council (STFC), Mullard Space Science Laboratory (MSSL), University College of London [London] (UCL), HELIOS - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), 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), Technische Universität Braunschweig = Technical University of Braunschweig [Braunschweig], Istituto di Astrofisica e Planetologia Spaziali - INAF (IAPS), Istituto Nazionale di Astrofisica (INAF), Imperial College London, Institute of Space Science [Bucharest-Măgurele] (ISS), Institute of Atmospheric Physics [Prague] (IAP), Czech Academy of Sciences [Prague] (CAS), Scibit [Liberec], Space Research Institute of Austrian Academy of Sciences (IWF), Austrian Academy of Sciences (OeAW), Centre National d'Études Spatiales [Toulouse] (CNES), Charles University [Prague] (CU), Max-Planck-Institut für Sonnensystemforschung = Max Planck Institute for Solar System Research (MPS), Max-Planck-Gesellschaft, Astronomical Institute of Charles University, artenum SARL, ONERA / DPHY, Université de Toulouse [Toulouse], and ONERA-PRES Université de Toulouse
Subjects: Earth and Planetary Astrophysics (astro-ph.EP), Space weather, Moon Gateway deep space space plasmas heliophysics space weather, [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], FOS: Physical sciences, Astronomy and Astrophysics, Deep space, Physics - Plasma Physics, Space Physics (physics.space-ph), [SDU.ASTR.IM]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], Plasma Physics (physics.plasm-ph), Physics - Space Physics, [SDU]Sciences of the Universe [physics], Space plasmas, Astrophysics - Instrumentation and Methods for Astrophysics, Moon, Instrumentation and Methods for Astrophysics (astro-ph.IM), Astrophysics - Earth and Planetary Astrophysics, Gateway, Heliophysics
Abstract: International audience; The Lunar Orbital Platform-Gateway (LOP-Gateway, or simply Gateway) is a crewed platform that will be assembled and operated in the vicinity of the Moon by NASA and international partner organizations, including ESA, starting from the mid-2020s. It will offer new opportunities for fundamental and applied scientific research. The Moon is a unique location to study the deep space plasma environment. Moreover, the lunar surface and the surface-bounded exosphere are interacting with this environment, constituting a complex multi-scale interacting system. This paper examines the opportunities provided by externally mounted payloads on the Gateway in the field of space plasma physics, heliophysics and space weather, but also examines the impact of the space environment on an inhabited platform in the vicinity of the Moon. It then presents the conceptual design of a model payload, required to perform these space plasma measurements and observations. It results that the Gateway is very well-suited for space plasma physics research. It allows a series of scientific objectives with a multidisciplinary dimension to be addressed.
Published: 2023

4. Investigating the impact of different Interplanetary Coronal Mass Ejection parameters on the Venusian atmospheric escape

Author: Maria Chloi Katrougkalou, Sae Aizawa, Moa Persson, Nicolas André, Ronan Modolo, 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), HELIOS - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), and 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)
Subjects: [SDU]Sciences of the Universe [physics]
Abstract: Venus lacks an intrinsic magnetic filed, as a result, the incoming solar wind interacts directly with its atmosphere, creating an induced magnetosphere. Venus is believed to have once held a significant amount of water, which has since then disappeared from the planet as evidence by the increased, compared to Earth's, Deuterium-Hydrogen ratio measured by Pioneer Venus (Donahue et al. 1982). Its disappearance is mainly contributed to the interaction of the solar wind with the planet's induced magnetosphere. This interaction is the primary cause of atmospheric escape for elements heavier than Hydrogen, such as Oxygen (Futaana et al. 2017). Measurements from Venus Express have shown that the majority of the escape is taking place at the magnetotail, with the ration of Hydrogen to Oxygen escape being approximately equal to two during solar minimum and equal to one during solar maximum (Persson et al. 2018), indicating the escape of water from the nightside. This effect can bring rise to the question: what happens to the atmospheric loss under extreme solar wind conditions, such as under the influence of Interplanetary Coronal Mass Ejections (ICMEs)? Understanding those processes can give us valuable information on the evolution of the planet. Previous works have provided answers by investigating the impact of ICMEs on the Venusian atmospheric escape compared to nominal conditions with observations (Luhmann et al. 2007, McEnulty et al. 2010, Edberg et al. 2011, Collinson et al. 2015) and simulations (Luhmann et al. 2008, Dimmock et al. 2017) to name a few. In this study, we contribute to this subject by using observations taken from Venus Express and simulations to explore the influence of different ICME parameters on the escape. The simulation used is a global hybrid model, called LatHyS, first developed for Mars (Modolo et al. 2017) and adapted for Venus (Aizawa et al. 2022), that has the advantage of having a self consistently calculated ionosphere. Magnetic field and particle data taken from Venus Express upstream of the bowshock are used as reference for the initial conditions of the simulations. Two ICME events are selected. The first impacted Venus on the 5th of November 2011 and created the highest observed magnetic obstacle at the planet. Upstream of the bowshock it had a temperature of 200 eV and a velocity of 900 km/s. The second event occurred on the 27th of October 2013 and had similar plasma and magnetic field parameters to the first one, but had significantly different temperature of 35 eV and velocity of 600 km/s. Idealized models of the events are simulated and compared. In order to discuss the parameter dependence, for each comparison the simulation inputs of the two events are forced to be the same, imposing either temperature or velocity to be identical, and leaving the studied variable as the only difference. We find an increase of the dayside Oxygen escape for the event with the higher velocity, but a decrease on the nightside outgoing ion flux. Since both of the selected events can be considered as fast solar wind, to better investigate the dependency of the velocity we perform an additional simulation with a much lower solar wind speed of 300 km/s. To study further the effect of the ICME parameters, in a more model driven approach, the second selected event is kept as a reference and additional simulations are performed to examine variables such as the magnetic field strength and cone angle. Finally, the results are compared with statistical data of the mean solar wind conditions on Venus and their corresponding calculated atmospheric escape. References: Aizawa et al. 2022, doi: https://doi.org/10.1016/j.pss.2022.105499 Collinson et al. 2015, doi: https://doi.org/10.1002/2014JA020616 Dimmock et al. 2018, doi: https://doi.org/10.1029/2017JA024852 Donahue et al. 1982, doi: https://doi.org/10.1126/science.216.4546.630 Edberg et al. 2011, doi: https://doi.org/10.1029/2011JA016749 Futaana et al. 2017, doi: https://doi.org/10.1007/s11214-017-0362-8 Luhmann et al. 2007, doi: https://doi.org/10.1029/2006JE002820 Luhmann et al. 2008, doi: https://doi.org/10.1029/2008JE003092 McEnulty et al. 2010, doi: https://doi.org/10.1016/j.pss.2010.07.019 Modolo et al. 2016, doi: https://doi.org/10.1002/2015JA022324 Persson et al. 2018, doi: https://doi.org/10.1029/2018GL079454
Published: 2022

5. Evidence of the nonstationarity of the terrestrial bow shock from multi-spacecraft observations: methodology, results, and quantitative comparison with particle-in-cell (PIC) simulations

Author: Bertrand Lembège, Christian Mazelle, 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), 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), Financial support. This research has been supported by the Centre This research has been supported by the Centre National d'Études Spatiales (CNES, grant nos. APR-W-EEXP/10-01-01-05 and APR-Z-ETP-E-0010/01-01-05)., Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), and 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)
Subjects: Atmospheric Science, 010504 meteorology & atmospheric sciences, Science, QC1-999, media_common.quotation_subject, Geophysics. Cosmic physics, Inertia, 01 natural sciences, 0103 physical sciences, Earth and Planetary Sciences (miscellaneous), Bow shock (aerodynamics), 010306 general physics, Scaling, 0105 earth and related environmental sciences, media_common, [SDU.OCEAN]Sciences of the Universe [physics]/Ocean, Atmosphere, Physics, Computer simulation, QC801-809, Front (oceanography), Geology, Astronomy and Astrophysics, Mechanics, Shock (mechanics), Magnetic field, Space and Planetary Science, Particle-in-cell
Abstract: The nonstationarity of the terrestrial bow shock is analyzed in detail from in situ magnetic field measurements issued from the fluxgate magnetometer (FGM) experiment of the Cluster mission. Attention is focused on statistical analysis of quasi-perpendicular supercritical shock crossings. The present analysis stresses for the first time the importance of a careful and accurate methodology in the data processing, which can be a source of confusion and misunderstanding if not treated properly. The analysis performed using 96 shock front crossings shows evidence of a strong variability of the microstructures of the shock front (foot and ramp), which are analyzed in great detail. The main results are that (i) most statistics clearly show that the ramp thickness is very narrow and can be as low as a few c/ωpe (electron inertia length); (ii) the width is narrower when the angle θBn (between the shock normal and the upstream magnetic field) approaches 90∘; (iii) the foot thickness strongly varies, but its variation has an upper limit provided by theoretical estimates given in previous studies (e.g., Schwartz et al., 1983; Gosling and Thomsen, 1985; Gosling and Robson, 1985); and (iv) the presence of foot and overshoot, as shown in all front profiles, confirms the importance of dissipative effects. Present results indicate that these features can be signatures of the shock front self-reformation among a few mechanisms of nonstationarity identified from numerical simulation and theoretical studies. A comparison with 2D particle-in-cell (PIC) simulation for a perpendicular supercritical shock (used as reference) has been performed and shows the following: (a) the ramp thickness varies only slightly in time over a large fraction of the reformation cycle and reaches a lower-bound value on the order of a few electron inertial length; (b) in contrast, the foot width strongly varies during a self-reformation cycle but always stays lower than an upper-bound value in agreement with the value given by Woods (1971); and (c) as a consequence, the time variability of the whole shock front is depending on both ramp and foot variations. Moreover, a detailed comparative analysis shows that many elements of analysis were missing in previous reported studies concerning both (i) the important criteria used in the data selection and (ii) the different and careful steps of the methodology used in the data processing itself. The absence of these precise elements of analysis makes the comparison with the present work difficult; worse, it makes some final results and conclusive statements quite questionable at the present time. At least, looking for a precise estimate of the shock transition thickness presents nowadays a restricted interest, since recent results show that the terrestrial shock is rather nonstationary, and one unique typical spatial scaling of the microstructures of the front (ramp, foot) must be replaced by some “variation ranges” (with lower-bound and upper-bound values) within which the spatial scales of the fine structures can extend.
Published: 2021

6. Electron dynamics in small magnetospheres: insights from global fully-kinetic plasma simulations of planet Mercury

Author: Lavorenti, Federico, Henri, P., Califano, Francesco, Deca, Jan, Aizawa, Sae, André, Nicolas, Benkhoff, Johannes, Joseph Louis LAGRANGE (LAGRANGE), 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), Dipartimento di Fisica 'E. Fermi', University of Pisa - Università di Pisa, 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), Laboratory for Atmospheric and Space Physics [Boulder] (LASP), University of Colorado [Boulder], HELIOS - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), 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), Institute for Modeling Plasma, Atmospheres and Cosmic Dust (IMPACT), NASA, 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), European Space Research and Technology Centre (ESTEC), and Agence Spatiale Européenne = European Space Agency (ESA)
Subjects: Mercury, Magnetosphere, Plasma, Electron Dynamics, BepiColombo, [SDU]Sciences of the Universe [physics]
Abstract: International audience; Context. The planet Mercury possesses a small but highly dynamic magnetosphere in which the role and dynamics of electrons are still largely unknown. Aims. We aim to model the global dynamics of solar-wind electrons impinging on Mercury’s magnetosphere. Particular relevance is given to local acceleration processes and the global circulation patterns. Methods. The goals of this work are pursued by means of three-dimensional, fully kinetic particle-in-cell simulations modeling the interaction of the solar wind with the Hermean magnetosphere. This method allows a self-consistent representation of the plasma dynamics from the large planetary scale down to the electron kinetic scale. We carried out numerical simulations using two different solar-wind conditions: purely northward or purely southward interplanetary magnetic field direction. Results. We find a high plasma current (of the order of few μA m −2 ) flowing at the magnetospheric boundaries (bow shock and magnetopause) dominated by electrons. This current is driven by the small-scale electron physics resolved in our model. Furthermore, we observe strong electron acceleration up to tens of keV as a consequence of magnetic reconnection when the interplanetary magnetic field is directed southward. Such energetic electrons are partially trapped in the dipolar magnetic field of the planet mainly at nightside. Finally, by studying the distribution of electrons in our simulations along Mariner10 and BepiColombo first-Mercury-flyby trajectories, we propose that both spacecraft observed this energetic quasi-trapped electron population around closest approach.
Published: 2022

7. On the origins of backscattered solar wind energetic neutral hydrogen from the Moon and Mercury

Author: Leblanc, François, Deborde, Robin, Tramontina, D., Bringa, E., Chaufray, Jean-Yves, Aizawa, S., Modolo, Ronan, Morrissey, L., Woodson, A., Verkercke, Sébastien, Dukes, C., HELIOS - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), 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), 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), Universidad Nacional de Cuyo [Mendoza] (UNCUYO), 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), Memorial University of Newfoundland = Université Memorial de Terre-Neuve [St. John's, Canada] (MUN), and University of Virginia
Subjects: [SDU]Sciences of the Universe [physics], Space and Planetary Science, Astronomy and Astrophysics
Abstract: International audience; The surfaces of planetary airless bodies are directly bombarded by solar particles. The most abundant of those particles are solar wind protons. In the case of the Moon, many in situ observations have shown that a significant portion of these incident solar-wind protons are backscattered as energetic neutral hydrogen atoms (ENA). Measurements of the energy flux distribution of these neutral particles provide a clue regarding the processes occurring in the surface regolith when impacting protons collide with the surface grains.In this work, we developed a model to describe the fate of protons through a regolith model and compared our results with Chandrayaan-1 ENA measurements. We combined a Monte Carlo approach to reconstruct the motion of these particles into a layer of grains with molecular dynamics to parametrize the interaction of an incident proton with a grain. Using simultaneous measurements of the incident plasma by Chandrayaan-1 SWIM, this detailed modelling allowed us to analyse the measurements performed by the Chandrayaan-1 CENA instrument when the Moon is in the solar wind and in the Earth's magnetosheath, and to highlight what could control the flux and energy properties of these backscattered neutral hydrogen particles. Predictions of the intensity and shape of the backscattered neutral hydrogen distribution at Mercury are derived from this calculation.
Published: 2023

8. Observations of Solar Type III radio bursts by Cassini/RPWS experiment

Author: Mohammed Y. Boudjada, Ahmed Abou el-Fadl, Helmut Lammer, Eimad Al-Haddad, Patrick H. M. Galopeau, Space Research Institute of Austrian Academy of Sciences (IWF), Austrian Academy of Sciences (OeAW), 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), and University of Applied Sciences [Graz]
Subjects: Astrophysics::High Energy Astrophysical Phenomena, Magnetosphere, 02 engineering and technology, Astrophysics, Radiation, 01 natural sciences, 7. Clean energy, Saturn, 0103 physical sciences, 0202 electrical engineering, electronic engineering, information engineering, 010303 astronomy & astrophysics, Physics, Spacecraft, Relative intensity, Waves in plasmas, business.industry, 020206 networking & telecommunications, General Medicine, Plasma, [SDU]Sciences of the Universe [physics], 13. Climate action, lcsh:TA1-2040, Physics::Space Physics, Astrophysics::Earth and Planetary Astrophysics, business, lcsh:Engineering (General). Civil engineering (General)
Abstract: In this study, we report on the occurrence of solar Type III radio bursts recorded by radio and plasma wave experiment (RPWS) experiment onboard Cassini spacecraft. This instrument is designed to investigate the Saturn's plasma environment and sub-auroral radio missions. RPWS/Cassini experiment allows to measure electric field over a frequency range from 1 Hz to 16 MHz (Gurnett et al., 2004). The essential observed emission is associated to the Saturnian Kilometric Radiation (SKR) which is generated in the sub-auroral regions of the magnetosphere. The capability of this experiment leads to detect Solar Type III radio bursts recorded during the increase phase of the solar activity, i.e. January 2008 to December 2014. Hence we have found more than 300 Type III solar bursts when the distance of Cassini to the Sun was about 10 AU. Observational parameters like the time occurrence, the emission frequency and the relative intensity are considered in this analysis. Those features lead us to characterize the detection conditions and to estimate the occurrence variabilities of Type III bursts.
Published: 2020

9. Modeling the variability of Martian O+ ion escape due to Solar Wind forcing

Author: Ronan Modolo, Francois Leblanc, Jean-Yves Chaufray, Norberto Romanelli, Eduard Dubinin, Vincent Génot, Claire Baskevitch, David Brain, Shannon Curry, Robert Lillis, HELIOS - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), 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), NASA Goddard Space Flight Center (GSFC), Center for Research and Exploration in Space Science and Technology [Baltimore] (CRESST), University of Maryland [Baltimore County] (UMBC), University of Maryland System-University of Maryland System, Max-Planck-Institut für Sonnensystemforschung = Max Planck Institute for Solar System Research (MPS), Max-Planck-Gesellschaft, 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), Laboratory for Atmospheric and Space Physics [Boulder] (LASP), University of Colorado [Boulder], Space Sciences Laboratory [Berkeley] (SSL), University of California [Berkeley] (UC Berkeley), and University of California (UC)-University of California (UC)
Subjects: [SDU]Sciences of the Universe [physics], Physics::Space Physics, Solar Wind, Planetary Ion Fluxes, Astrophysics::Solar and Stellar Astrophysics, Mars, Astrophysics::Earth and Planetary Astrophysics
Abstract: During the last decade, MAVEN space mission have emphasized a widespread spatial distribution of escaping O+ ions (Brain et al., 2015; Dong et al., 2015; Curry et al., 2015). Statistical studies have demonstrated that such structure is constant and present an asymmetry with respect to the solar wind convective electric field direction. In the Mars Solar Ecliptic coordinate system, continuous large O+ ion fluxes have been observed from the Martian wake to the Northward hemisphere. Global hybrid models have been developed since more than fiffteen years (Modolo et al., 2005, 2016; Brecht and Ledvina, 2006; Kallio et al., 2006) predicting and reproducing successfully the main characteristics of these escaping ion signatures. To further characterize this heavy-ion escape and its variability due to the solar wind forcing, global hybrid simulations have been performed with different set of upstream solar wind parameters. The impact of the solar wind drivers on the dynamics of O+ ion fluxes are reported and compared to the statistical ion fluxes maps derived from MAVEN/STATIC observations (Dong et al., 2015).Brain, D. A., McFadden, J. P., Halekas, J. S., Connerney, J. E. P., Bougher, S. W., Curry, S., et al. (2015). The spatial distribution of planetary ion fluxes near Mars observed by MAVEN. Geophys. Res. Lett. 42, 9142–9148. doi:10.1002/2015GL065293Dong, Y., Fang, X., Brain, D. A., McFadden, J. P., Halekas, J. S., Connerney, J. E., et al. (2015). Strong plume fluxes at Mars observed by MAVEN: An important planetary ion escape channel. Geophys. Res. Lett. 42, 8942–8950. doi:10.1002/2015GL065346Curry, S. M., Luhmann, J. G., Ma, Y. J., Dong, C. F., Brain, D., Leblanc, F., et al. (2015). Response of Mars O+ pickup ions to the 8 March 2015 ICME: Inferences from MAVEN data-based models. Geophys. Res. Lett. 42, 9095–9102. doi:10.1002/2015GL065304Modolo, R., Chanteur, G. M., Dubinin, E., and Matthews, A. P. (2005). Influence of the solar EUV flux on the Martian plasma environment. Annales Geophysicae 23, 433–444. doi:10.5194/angeo-23-433-2005 Brecht, S. H. and Ledvina, S. A. (2006). The Solar Wind Interaction With the Martian Ionosphere/Atmosphere 126, 15–38. doi:10.1007/s11214-006-9084-zKallio, E., Fedorov, A., Budnik, E., Sa¨les, T., Janhunen, P., Schmidt, W., et al. (2006). Ion escape at Mars: Comparison of a 3-D hybrid simulation with Mars Express IMA/ASPERA-3 measurements 182, 350–359. doi:10.1016/j.icarus.2005.09.018
Published: 2022

10. HiRISE - High-Resolution Imaging and Spectroscopy Explorer - ultrahigh resolution, interferometric and external occulting coronagraphic science

Author: Erdélyi, Robertus, Damé, Luc, Fludra, Andrzej, Mathioudakis, Mihalis, Amari, T., Belucz, B., Berrilli, F., Bogachev, S., Bolsée, D., Bothmer, V., Brun, S., Dewitte, S., de Wit, T. Dudok, Faurobert, M., Gizon, L., Gyenge, N., Korsós, M. B., Labrosse, Nicolas, Matthews, S., Meftah, M., Morgan, H., Pallé, P., Rochus, P., Rozanov, E., Schmieder, B., Tsinganos, K., Verwichte, E., Zharkov, S., Zuccarello, F., Wimmer-Schweingruber, R., Solar Physics and Space Plasma Research Centre, School of Mathematics and Statistics [Sheffield] (SoMaS), University of Sheffield [Sheffield]-University of Sheffield [Sheffield], Eötvös Loránd University (ELTE), Hungarian Solar Physics Foundation (HSPF), HELIOS - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), 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), STFC Rutherford Appleton Laboratory (RAL), Science and Technology Facilities Council (STFC), Astrophysics Research Centre [Belfast] (ARC), Queen's University [Belfast] (QUB), Centre de Physique Théorique [Palaiseau] (CPHT), École polytechnique (X)-Centre National de la Recherche Scientifique (CNRS), Università degli Studi di Roma Tor Vergata [Roma], P. N. Lebedev Physical Institute of the Russian Academy of Sciences [Moscow] (LPI RAS), Russian Academy of Sciences [Moscow] (RAS), Belgian Institute for Space Aeronomy / Institut d'Aéronomie Spatiale de Belgique (BIRA-IASB), Georg-August-University = Georg-August-Universität Göttingen, Département d'astrophysique, Géophysique et Océanographie (AGO), Université de Liège, Institut Royal Météorologique de Belgique [Bruxelles] - Royal Meteorological Institute (IRM), 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), Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Laboratoire Universitaire d'Astrophysique de Nice (LUAN), 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)-Centre National de la Recherche Scientifique (CNRS), Max-Planck-Institut für Sonnensystemforschung = Max Planck Institute for Solar System Research (MPS), Max-Planck-Gesellschaft, Aberystwyth University, SUPA School of Physics and Astronomy [Glasgow], University of Glasgow, Mullard Space Science Laboratory (MSSL), University College of London [London] (UCL), STRATO - LATMOS, Instituto de Astrofisica de Canarias (IAC), Centre Spatial de Liège (CSL), Physikalisch-Meteorologisches Observatorium Davos/World Radiation Center (PMOD/WRC), Observatoire de Paris - Site de Meudon (OBSPM), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS), National and Kapodistrian University of Athens (NKUA), University of Warwick [Coventry], University of Hull [United Kingdom], Dipartimento di Fisica e Astronomia [Catania], Università degli studi di Catania = University of Catania (Unict), Christian-Albrechts-Universität zu Kiel (CAU), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), and Max-Planck-Institut für Sonnensystemforschung (MPS)
Subjects: Solar atmosphere, Astronomy & Astrophysics, CORONA, Solar physics mission, LIMITS, LEAKAGE, Photosphere, SDG 13 - Climate Action, Ultra-high resolution, Astrophysics::Solar and Stellar Astrophysics, Interferometry, Coronagraph, Chromosphere, Corona, QC, QB, Science & Technology, [SDU.ASTR.SR]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], Astrophysics::Instrumentation and Methods for Astrophysics, MAGNETIC-FIELD, SUN, Astronomy and Astrophysics, IRRADIANCE, VARIABILITY, Space and Planetary Science, OUTFLOWS, Physics::Space Physics, Physical Sciences, ALFVEN WAVES, Astrophysics::Earth and Planetary Astrophysics, Settore FIS/06 - Fisica per il Sistema Terra e Il Mezzo Circumterrestre, SOLAR DIAMETER
Abstract: Recent solar physics missions have shown the definite role of waves and magnetic fields deep in the inner corona, at the chromosphere-corona interface, where dramatic and physically dominant changes occur. HiRISE (High Resolution Imaging and Spectroscopy Explorer), the ambitious new generation ultra-high resolution, interferometric, and coronagraphic, solar physics mission, proposed in response to the ESA Voyage 2050 Call, would address these issues and provide the best-ever and most complete solar observatory, capable of ultra-high spatial, spectral, and temporal resolution observations of the solar atmosphere, from the photosphere to the corona, and of new insights of the solar interior from the core to the photosphere. HiRISE, at the L1 Lagrangian point, would provide meter class FUV imaging and spectro-imaging, EUV and XUV imaging and spectroscopy, magnetic fields measurements, and ambitious and comprehensive coronagraphy by a remote external occulter (two satellites formation flying 375 m apart, with a coronagraph on a chaser satellite). This major and state-of-the-art payload would allow us to characterize temperatures, densities, and velocities in the solar upper chromosphere, transition zone, and inner corona with, in particular, 2D very high resolution multi-spectral imaging-spectroscopy, and, direct coronal magnetic field measurement, thus providing a unique set of tools to understand the structure and onset of coronal heating. HiRISE’s objectives are natural complements to the Parker Solar Probe and Solar Orbiter-type missions. We present the science case for HiRISE which will address: i) the fine structure of the chromosphere-corona interface by 2D spectroscopy in FUV at very high resolution; ii) coronal heating roots in the inner corona by ambitious externally-occulted coronagraphy; iii) resolved and global helioseismology thanks to continuity and stability of observing at the L1 Lagrange point; and iv) solar variability and space climate with, in addition, a global comprehensive view of UV variability.
Published: 2022

11. Low-altitude frequency-banded equatorial emissions observed below the electron cyclotron frequency

Author: Sami Sawas, Valery V. Denisenko, Patrick H. M. Galopeau, Helmut Lammer, Werner Magnes, Hans Eichelberger, Konrad Schwingenschuh, Bruno P. Besser, Mohammed Y. Boudjada, Space Research Institute of Austrian Academy of Sciences (IWF), Austrian Academy of Sciences (OeAW), 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), Institute of communications and wave propagation [Graz], Graz University of Technology [Graz] (TU Graz), Institute of Computational Modelling of the Russian Academy of Sciences (ICM SB RAS), Siberian Branch of the Russian Academy of Sciences (SB RAS), Institut für Weltraumforschung [Graz] (IWF), and Osterreichische Akademie der Wissenschaften (ÖAW)
Subjects: Atmospheric Science, 010504 meteorology & atmospheric sciences, Cyclotron, 0211 other engineering and technologies, Plasmasphere, 02 engineering and technology, Astrophysics, Plasma oscillation, 01 natural sciences, Physics::Geophysics, Latitude, law.invention, law, Earth and Planetary Sciences (miscellaneous), lcsh:Science, Southern Hemisphere, 021101 geological & geomatics engineering, 0105 earth and related environmental sciences, [PHYS.PHYS.PHYS-AO-PH]Physics [physics]/Physics [physics]/Atmospheric and Oceanic Physics [physics.ao-ph], Physics, lcsh:QC801-809, Northern Hemisphere, Resonance, Geology, Astronomy and Astrophysics, lcsh:QC1-999, lcsh:Geophysics. Cosmic physics, 13. Climate action, Space and Planetary Science, Physics::Space Physics, lcsh:Q, Astrophysics::Earth and Planetary Astrophysics, Ionosphere, lcsh:Physics
Abstract: The ICE (Instrument Champ Électrique) experiment on board the DEMETER (Detection of Electro-Magnetic Emissions Transmitted from Earthquake Regions) satellite recorded frequency-banded wave emissions below the electron cyclotron frequency, with band spacing ≳ frequency low-hybrid resonance, in the vicinity of the magnetic equatorial plane. Those radiations were observed in the beginning of the year 2010 on the night side of Earth and rarely on the day side. We distinguish two components: one appears as frequency bands continuous in time between a few kilohertz and up to 50 kHz, and the other one is from 50 to 800 kHz. The first component exhibits positive and negative frequency drift rates in the Southern Hemisphere and Northern Hemisphere, at latitudes between 40 and 20∘. The second one displays multiple spaced frequency bands. Such bands mainly occur near the magnetic equatorial plane with a particular enhancement of the power level when the satellite latitude is close to the magnetic equatorial plane. We show in this study the similarities and the discrepancies between the non-free-space DEMETER frequency-banded emissions and the well-known free-space terrestrial kilometric radiation. The hollow cones of the DEMETER frequency-banded wave emissions are oriented towards Earth's ionosphere. We suggest that the source region is localized in regions poleward of the plasmapause where the ratio of the plasma frequency to gyro-frequency is smaller than one.
Published: 2020

12. Ion density and phase space density distribution of planetary ions Na+, O+ and He+ in Mercury’s magnetosphere

Author: Jean-Yves Chaufray, S. Aizawa, Ronan Modolo, François Leblanc, W. Exner, A. L. E. Werner, Carl Schmidt, Jim M. Raines, Uwe Motschmann, 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), 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), Department of Climate and Space Sciences and Engineering (CLaSP), University of Michigan [Ann Arbor], University of Michigan System-University of Michigan System, Institut für Geophysik und Extraterrestrische Physik [Braunschweig] (IGEP), Technische Universität Braunschweig = Technical University of Braunschweig [Braunschweig], Institut für Theoretische Physik [Braunschweig], DLR Institut für Planetenforschung, Deutsches Zentrum für Luft- und Raumfahrt [Berlin] (DLR), Center for Space Physics [Boston] (CSP), Boston University [Boston] (BU), 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), 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), A.L.E.W., F.L., J.-Y.C. and R.M acknowledges the support by ANR,France of the TEMPETE project (grant ANR-17-CE31-0016). S.A., F.L.,J.-Y.C., R.M and A.L.E.W. would like to acknowledge the supportof CNES, France for the BepiColombo mission. W.E. was supportedby DFG (German Research Foundation) under contract HE8016/1-1.C.S. acknowledges NASA, USA’s support of this study under grant80NSSC19K0790., and ANR-17-CE31-0016,TEMPETE,Évolutions temporelles des environnements planétaires magnétisés pendant des tempêtes solaires(2017)
Subjects: 010504 meteorology & atmospheric sciences, Solar wind, Population, Magnetosphere, 01 natural sciences, 7. Clean energy, Ion, Atmosphere, 0103 physical sciences, Interplanetary magnetic field, education, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, Physics, education.field_of_study, Astronomy and Astrophysics, Plasma, Mercury, Ionospheres, 13. Climate action, Space and Planetary Science, Magnetospheres, [SDU]Sciences of the Universe [physics], Physics::Space Physics, atmosphere, Astrophysics::Earth and Planetary Astrophysics, Atomic physics, Exosphere
Abstract: Photo-ionization of Mercury’s tenuous exosphere contributes to the heavy ion population in the Hermean environment. Observations with the MESSENGER Fast Imaging Plasma Spectrometer (FIPS) have revealed the ion density and spatial distribution of the three most abundant planetary ions or ion groups around Mercury: The Na+-group (mass-per-charge ratio m / q = 21 – 30 amu / e ), O+-group ( m / q = 16 – 20 amu / e ) and He+. We developed a test-particle model coupled to a neutral exosphere model and two different models of the magnetosphere to simulate the ion density distribution of Na+, He+ and O+. We compare the modeled ion density distribution at aphelion for northward interplanetary magnetic field (IMF) with FIPS observations from the entire orbital phase (23 March 2011 to 30 April 2015). Our model reproduces several observed features but the average ion density is up to 18x too high. However, we find that the discrepancy is less than 3x for other solar wind and exosphere conditions. Comparison with previous simulation studies of the Na+ ion density and magnetic field line resonance observations give an average Na+ density which is on the same order as our estimate. Finally, we model the phase space density (PSD) distribution in four different regions. We find that in three out of four regions only a fraction of the PSD distribution can typically be observed by FIPS. This is mainly due the obstruction of the field-of-view caused by the spacecraft’s sun shield, which blocks plasma with a high v x / v z ratio from entering the instrument.
Published: 2022

13. Modeling of Diffuse Auroral Emission at Mars: Contribution of MeV Protons

Author: Yuki Nakamura, Naoki Terada, François Leblanc, Ali Rahmati, Hiromu Nakagawa, Shotaro Sakai, Sayano Hiruba, Ryuho Kataoka, Kiyoka Murase, Graduate School of Science [Sendai], Tohoku University [Sendai], 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), PLANETO - LATMOS, Space Sciences Laboratory [Berkeley] (SSL), University of California [Berkeley], University of California-University of California, Planetary Plasma and Atmospheric Research Center [Sendai] (PPARC), National Institute of Polar Research [Tokyo] (NiPR), Graduate University for Advanced Studies [Hayama] (SOKENDAI), and ANR-09-BLAN-0223,HELIOSARES,Relation Soleil ? Mars: description et analyse des échanges présents et passés entre magnétosphère et atmosphère(2009)
Subjects: Geophysics, 010504 meteorology & atmospheric sciences, [SDU]Sciences of the Universe [physics], 13. Climate action, Space and Planetary Science, Physics::Space Physics, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, 010303 astronomy & astrophysics, 01 natural sciences, 7. Clean energy, 0105 earth and related environmental sciences
Abstract: International audience; The Solar Energetic Particle and Imaging UltraViolet Spectrograph (IUVS) instruments onboard the Mars Atmosphere and Volatile EvolutioN (MAVEN) spacecraft discovered diffuse aurora that span across the nightside of Mars due to the interaction of solar energetic particles (SEPs) with the Martian atmosphere. However, it is unclear whether the diffuse aurora originates from energetic electrons or protons. We have developed a Monte Carlo model to calculate the limb intensity profile of the CO2+ ultraviolet doublet (UVD) due to precipitation of energetic electrons and protons with energy ranges from 100 eV to 100 keV and from 50 keV to 5 MeV, respectively. We used electron and proton fluxes observed by MAVEN during the December 2014 SEP event and the September 2017 SEP event. Our results showed that proton-induced CO2+ UVD emission has a lower peak altitude than electron-induced CO2+ UVD emission. The calculated peak altitudes of the CO2+ UVD limb profiles are 76 km and 68 km in the December 2014 event and the September 2017 event, respectively. Extending the energy to 500 keV for electrons and 20 MeV for protons further improved our comparison to the IUVS observations. We have succeeded in reproducing peak altitudes and shapes of the observed CO2+ UVD limb profiles using the SEP flux observed by MAVEN. This was possible by taking into account the contribution of energetic protons, indicating that both energetic electrons and protons contribute to producing the observed diffuse aurora.
Published: 2022

14. Reflectivity of Venus' dayside disk during the 2020 observation campaign: outcomes and future perspectives

Author: Lee, Yeon Joo, Muñoz, Antonio García, Yamazaki, Atsushi, Quémerais, Eric, Mottola, Stefano, Hellmich, Stephan, Granzer, Thomas, Bergond, Gilles, Roth, Martin, Gallego Cano, Eulalia, Chaufray, Jean-Yves, Robidel, Rozenn, Murakami, Go, Masunaga, Kei s, Kaplan, Murat, Erece, Orhan, Hueso, Ricardo, Kabáth, Petr, Špoková, Magdaléna, Sánchez-Lavega, Agustín, Kim, Myung-Jin, Mangano, Valeria, Jessup, Kandis-Lea, Widemann, Thomas, Sugiyama, Ko-ichiro, Watanabe, Shigeto, Yamada, Manabu, Satoh, Takehiko, Nakamura, Masato, Imai, Masataka se, Cabrera, Juan, DLR Institut für Planetenforschung, Deutsches Zentrum für Luft- und Raumfahrt [Berlin] (DLR), Pioneer Research Center for Climate and Earth Science (PRC), Institute of Basic Science (IBS), Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Institute of Space and Astronautical Science (ISAS), Japan Aerospace Exploration Agency [Sagamihara] (JAXA), Graduate School of Science [Tokyo], The University of Tokyo (UTokyo), HELIOS - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), 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), Laboratoire d'Astrophysique [Versoix] (LASTRO), Ecole Polytechnique Fédérale de Lausanne (EPFL), Leibniz Institute for Astrophysics Potsdam (AIP), Centro Astronómico Hispano Alemán, Observatorio de Calar Alto (CAHA), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Instituto de Astrofísica de Andalucía (IAA), Akdeniz University, Departamento de Fisica Aplicada [Bilbao], Universidad del Pais Vasco / Euskal Herriko Unibertsitatea [Espagne] (UPV/EHU), Ondřejov Observatory of the Prague Astronomical Institute, Czech Academy of Sciences [Prague] (CAS), Department of Theoretical Physics and Astrophysics [Brno], Masaryk University [Brno] (MUNI), Korea Astronomy and Space Science Institute (KASI), Istituto di Astrofisica e Planetologia Spaziali - INAF (IAPS), Istituto Nazionale di Astrofisica (INAF), Southwest Research Institute [Boulder] (SwRI), 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), Matsue National College of Technology, Hokkaido Information University, Planetary Exploration Research Center [Chiba] (PERC), Chiba Institute of Technology (CIT), Kyoto Sangyo University, Ministerio de Ciencia e Innovación (España), and European Commission
Subjects: atmospheric clouds, fourier-transform measurements, Earth and Planetary Astrophysics (astro-ph.EP), sulfur-dioxide, uv absorption, solar system astronomy, FOS: Physical sciences, absorption cross-sections, Venus, cloud-top, valence-shell, observational astronomy, s 2p, planetary science, photoabsorption, [SDU]Sciences of the Universe [physics], temperature-dependence, carbonyl sulfide, planetary atmospheres, Astrophysics - Earth and Planetary Astrophysics
Abstract: This is an Open Access article distributed under the terms of the Creative Commons Attribution License (http://creativecommons.org/licenses/by/4.0/), which permits unrestricted reuse, distribution, and reproduction in any medium, provided the original work is properly cited., We performed a unique Venus observation campaign to measure the disk brightness of Venus over a broad range of wavelengths in 2020 August and September. The primary goal of the campaign was to investigate the absorption properties of the unknown absorber in the clouds. The secondary goal was to extract a disk mean SO2 gas abundance, whose absorption spectral feature is entangled with that of the unknown absorber at ultraviolet wavelengths. A total of three spacecraft and six ground-based telescopes participated in this campaign, covering the 52–1700 nm wavelength range. After careful evaluation of the observational data, we focused on the data sets acquired by four facilities. We accomplished our primary goal by analyzing the reflectivity spectrum of the Venus disk over the 283–800 nm wavelengths. Considerable absorption is present in the 350–450 nm range, for which we retrieved the corresponding optical depth of the unknown absorber. The result shows the consistent wavelength dependence of the relative optical depth with that at low latitudes, during the Venus flyby by MESSENGER in 2007, which was expected because the overall disk reflectivity is dominated by low latitudes. Last, we summarize the experience that we obtained during this first campaign, which should enable us to accomplish our second goal in future campaigns. © 2022. The Author(s). Published by the American Astronomical Society., This research used data collected at the Centro Astronómico Hispano-Alemán (CAHA) at Calar Alto, operated jointly by Junta de Andalucía and Consejo Superior de Investigaciones Científicas (IAA-CSIC). This research has made use of the integral field spectroscopy data reduction tool p3d, which is provided by the Leibniz-Institut für Astrophysik Potsdam (AIP). Akatsuki/UVI data are publicly available at the JAXA archive website, DARTS (http://darts.isas.jaxa.jp/), and the NASA archive website, PDS (https://pds.nasa.gov/). UVI Level 3 products (l3bx) were used in this study (Murakami et al. 2018). This study used the TSIS-1 SIM data (Version 06, doi:10.25810/y9f8-ff85). M.K. and O.E. thank the TÜBİTAK National Observatory for partial support in using the T100 telescope, with project number 20CT100-1688. R.H. and A.S.L. have been supported by the Spanish project PID2019-109467GB-I00 (MINECO/FEDER, UE) and Grupos Gobierno Vasco IT-1366-19. P.K. and M.S. acknowledge support from grant LTT-20015., With funding from the Spanish government through the Severo Ochoa Centre of Excellence accreditation SEV-2017-0709.
Published: 2022
Full Text: View/download PDF

15. BepiColombo mission confirms stagnation region of Venus and reveals its large extent

Author: M. Persson, S. Aizawa, N. André, S. Barabash, Y. Saito, Y. Harada, D. Heyner, S. Orsini, A. Fedorov, C. Mazelle, Y. Futaana, L. Z. Hadid, M. Volwerk, G. Collinson, B. Sanchez-Cano, A. Barthe, E. Penou, S. Yokota, V. Génot, J. A. Sauvaud, D. Delcourt, M. Fraenz, R. Modolo, A. Milillo, H.-U. Auster, I. Richter, J. Z. D. Mieth, P. Louarn, C. J. Owen, T. S. Horbury, K. Asamura, S. Matsuda, H. Nilsson, M. Wieser, T. Alberti, A. Varsani, V. Mangano, A. Mura, H. Lichtenegger, G. Laky, H. Jeszenszky, K. Masunaga, C. Signoles, M. Rojo, G. Murakami, 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), Swedish Institute of Space Physics [Kiruna] (IRF), Institute of Space and Astronautical Science (ISAS), Japan Aerospace Exploration Agency [Sagamihara] (JAXA), Department of Geophysics [Kyoto], Kyoto University, Institut für Geophysik und Extraterrestrische Physik [Braunschweig] (IGEP), Technische Universität Braunschweig = Technical University of Braunschweig [Braunschweig], Istituto di Astrofisica e Planetologia Spaziali - INAF (IAPS), Istituto Nazionale di Astrofisica (INAF), Laboratoire de Physique des Plasmas (LPP), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École polytechnique (X)-Sorbonne Université (SU)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), Space Research Institute of Austrian Academy of Sciences (IWF), Austrian Academy of Sciences (OeAW), NASA Goddard Space Flight Center (GSFC), School of Physics and Astronomy [Leicester], University of Leicester, Department of Earth and Space Science [Osaka], Osaka University [Osaka], Max-Planck-Institut für Sonnensystemforschung = Max Planck Institute for Solar System Research (MPS), Max-Planck-Gesellschaft, HELIOS - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), 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), Mullard Space Science Laboratory (MSSL), University College of London [London] (UCL), Imperial College London, Graduate School of the Natural Science and Technology [Kanazawa], and Kanazawa University (KU)
Subjects: Multidisciplinary, [SDU]Sciences of the Universe [physics], BepiColombo, General Physics and Astronomy, General Chemistry, magnetic fields, Venus, General Biochemistry, Genetics and Molecular Biology
Abstract: The second Venus flyby of the BepiColombo mission offer a unique opportunity to make a complete tour of one of the few gas-dynamics dominated interaction regions between the supersonic solar wind and a Solar System object. The spacecraft pass through the full Venusian magnetosheath following the plasma streamlines, and cross the subsolar stagnation region during very stable solar wind conditions as observed upstream by the neighboring Solar Orbiter mission. These rare multipoint synergistic observations and stable conditions experimentally confirm what was previously predicted for the barely-explored stagnation region close to solar minimum. Here, we show that this region has a large extend, up to an altitude of 1900 km, and the estimated low energy transfer near the subsolar point confirm that the atmosphere of Venus, despite being non-magnetized and less conductive due to lower ultraviolet flux at solar minimum, is capable of withstanding the solar wind under low dynamic pressure.
Published: 2022

16. M-type (22) Kalliope: A tiny Mercury

Author: Ferrais, Marin, Jorda, L., Vernazza, Pierre, Carry, Benoit, Broz, M., Rambaux, N., Hanus, J., Dudzinski, G., Bartczak, P., Vachier, F., Aristidi, Eric, Beck, P., Marchis, F., Marsset, M., Viikinkoski, M., Fetick, R., Drouard, A., Fusco, T., Birlan, M., Podlewska-Gaca, E., Burbine, T.H., Dyar, M.D., Bendjoya, Philippe, Benkhaldoun, Zouhair, Berthier, Jérôme, Castillo-Rogez, Julie, Cipriani, Fabrice, Colas, F., Dumas, Christophe, Ďurech, J., Fauvaud, S., Grice, J., Jehin, Emmanuël, Kaasalainen, M., Kryszczynska, A., Lamy, Philippe, Coroller, H., Marciniak, Alexandre, Michalowski, T., Michel, Patrick, Prieur, Jean-Louis, Reddy, V., Rivet, Jean‐pierre, Santana-Ros, Toni, Scardia, Marco, Tanga, Paolo, Vigan, Arthur, Witasse, Olivier, Yang, B., 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), Joseph Louis LAGRANGE (LAGRANGE), 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), Astronomical Institute of Charles University, Charles University [Prague] (CU), 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), Astronomical Observatory [Poznan], Adam Mickiewicz University in Poznań (UAM), Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Centre National d'Études Spatiales [Toulouse] (CNES)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France -Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France, SETI Institute, Department of Earth, Atmospheric and Planetary Sciences [MIT, Cambridge] (EAPS), Massachusetts Institute of Technology (MIT), University of Tampere [Finland], ONERA, Université Paris Saclay [Châtillon], ONERA-Université Paris-Saclay, Astronomical Institute of Romanian Academy, Romanian Academy, Institute of Physics [Szczecin], University of Szczecin, Department of Astronomy of the Mount Holyoke College, Mount Holyoke College, Oukaimeden Observatory, Université Cadi Ayyad [Marrakech] (UCA), Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), European Space Research and Technology Centre (ESTEC), European Space Agency (ESA), TMT International Observatory, Observatoire du Bois de Bardon, School of Physical Sciences [Milton Keynes], Faculty of Science, Technology, Engineering and Mathematics [Milton Keynes], The Open University [Milton Keynes] (OU)-The Open University [Milton Keynes] (OU), Space Sciences, Technologies and Astrophysics Research Institute (STAR), Université de Liège, HELIOS - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), 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), Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), 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)-Université Fédérale Toulouse Midi-Pyrénées-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), Lunar and Planetary Laboratory [Tucson] (LPL), University of Arizona, Departamento de Fisica, Ingenieria de Sistemas y Teoria de la Señal [Alicante] (DFESTS), Universidad de Alicante, Institut de Ciencies del Cosmos (ICCUB), Universitat de Barcelona (UB), INAF - Osservatorio Astronomico di Brera (OAB), Istituto Nazionale di Astrofisica (INAF), European Southern Observatory [Santiago] (ESO), European Southern Observatory (ESO), Universidad Diego Portales [Santiago] (UDP), DOTA, ONERA [Salon], ONERA, DOTA, ONERA, Université Paris Saclay [Palaiseau], Agence Spatiale Européenne = European Space Agency (ESA), 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), Based on observations collected at the European Organisation for Astronomical Research in the Southern Hemisphere under ESO programme 199.C-0074 (PI: P. Vernazza). P. V., A. D., M. F. and B. C. were supported by CNRS/INSU/PNP. The research of J.H. has been supported by the Czech Science Foundation through grant 20-08218S and by Charles University Research program no. UNCE/SCI/023. M.B. was supported by the Czech Science Foundation, grant 21-11058S. F.M. is supported by the National Science Foundation under grant no. 1743015. TRAPPIST is a project funded by the Belgian Fonds (National) de la Recherche Scientifique (F.R.S.-FNRS) under grant PDR T.0120.21. TRAPPIST-North is a project funded by the University of Liège, in collaboration with the Cadi Ayyad University of Marrakech (Morocco). E.J. is F.R.S.-FNRS Senior Research Associate. The work of T.S.R. was carried out through grant APOSTD/2019/046 by Generalitat Valenciana (Spain). This work was supported by the MINECO (Spanish Ministry of Economy) through grant RTI2018-095076-B-C21 (MINECO/FEDER, UE)., Universidad de Alicante. Instituto Universitario de Física Aplicada a las Ciencias y las Tecnologías, Tampere University, Computing Sciences, Centre National de la Recherche Scientifique (France), Charles University (Czech Republic), Czech Science Foundation, Fonds de La Recherche Scientifique (Belgique), National Science Foundation (US), Université Cadi Ayyad, Generalitat Valenciana, Ministerio de Economía y Competitividad (España), Agencia Estatal de Investigación (España), Ministerio de Ciencia, Innovación y Universidades (España), and European Commission
Subjects: asteroids, Astronomy and Astrophysics, Observation, (22) Kalliope, Techniques: high angular resolution, high angular resolution [Techniques], individual: (22) Kalliope [Minor planets, asteroids], Methods: observational, Space and Planetary Science, Asteroids: individual: (22) Kalliope, 111 Mathematics, minor planets, observational [Methods], [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], high angular resolution, ComputingMilieux_MISCELLANEOUS, Astronomía y Astrofísica
Abstract: M.Ferrais et al., [Context] Asteroid (22) Kalliope is the second largest M-type asteroid in the main belt and is orbited by a satellite, Linus. Whereas the mass of Kalliope is already well constrained thanks to the presence of a moon, its volume is still poorly known, leading to uncertainties on its bulk density and internal structure., [Aims] We aim to refine the shape of (22) Kalliope and thus its diameter and bulk density, as well as the orbit of its moon to better constrain its mass, hence density and internal structure., [Methods] We acquired disk-resolved observations of (22) Kalliope using the VLT/SPHERE/ZIMPOL instrument to reconstruct its three-dimensional (3D) shape using three different modeling techniques. These images were also used together with new speckle observations at the C2PU/PISCO instrument as well as archival images from other large ground-based telescopes to refine the orbit of Linus., [Results] The volume of (22) Kalliope given by the shape models, corresponding to D = 150 ± 5 km, and the mass constrained by its satellite’s orbit yield a density of ρ = 4.40 ± 0.46 g cm−3. This high density potentially makes (22) Kalliope the densest known small body in the Solar System. A macroporosity in the 10–25% range (as expected for this mass and size), implies a grain density in the 4.8–5.9 g cm−3 range. Kalliope’s high bulk density, along with its silicate-rich surface implied by its low radar albedo, implies a differentiated interior with metal contributing to most of the mass of the body., [Conclusions] Kalliope’s high metal content (40–60%) along with its metal-poor mantle makes it the smallest known Mercury-like body. A large impact at the origin of the formation of the moon Linus is likely the cause of its high metal content and density., Based on observations collected at the European Organisation for Astronomical Research in the Southern Hemisphere under ESO programme 199.C-0074 (PI: P. Vernazza). P. V., A. D., M. F. and B. C. were supported by CNRS/INSU/PNP. The research of J.H. has been supported by the Czech Science Foundation through grant 20-08218S and by Charles University Research program no. UNCE/SCI/023. M.B. was supported by the Czech Science Foundation, grant 21-11058S. F.M. is supported by the National Science Foundation under grant no. 1743015. TRAPPIST is a project funded by the Belgian Fonds (National) de la Recherche Scientifique (F.R.S.-FNRS) under grant PDR T.0120.21. TRAPPIST-North is a project funded by the University of Liège, in collaboration with the Cadi Ayyad University of Marrakech (Morocco). E.J. is F.R.S.-FNRS Senior Research Associate. The work of T.S.R. was carried out through grant APOSTD/2019/046 by Generalitat Valenciana (Spain). This work was supported by the MINECO (Spanish Ministry of Economy) through grant RTI2018-095076-B-C21 (MINECO/FEDER, UE).
Published: 2022

17. Inner southern magnetosphere observation of Mercury via SERENA ion sensors in BepiColombo mission

Author: S. Orsini, A. Milillo, H. Lichtenegger, A. Varsani, S. Barabash, S. Livi, E. De Angelis, T. Alberti, G. Laky, H. Nilsson, M. Phillips, A. Aronica, E. Kallio, P. Wurz, A. Olivieri, C. Plainaki, J. A. Slavin, I. Dandouras, J. M. Raines, J. Benkhoff, J. Zender, J.-J. Berthelier, M. Dosa, G. C. Ho, R. M. Killen, S. McKenna-Lawlor, K. Torkar, O. Vaisberg, F. Allegrini, I. A. Daglis, C. Dong, C. P. Escoubet, S. Fatemi, M. Fränz, S. Ivanovski, N. Krupp, H. Lammer, François Leblanc, V. Mangano, A. Mura, R. Rispoli, M. Sarantos, H. T. Smith, M. Wieser, F. Camozzi, A. M. Di Lellis, G. Fremuth, F. Giner, R. Gurnee, J. Hayes, H. Jeszenszky, B. Trantham, J. Balaz, W. Baumjohann, M. Cantatore, D. Delcourt, M. Delva, M. Desai, H. Fischer, A. Galli, M. Grande, M. Holmström, I. Horvath, K. C. Hsieh, R. Jarvinen, R. E. Johnson, A. Kazakov, K. Kecskemety, H. Krüger, C. Kürbisch, Frederic Leblanc, M. Leichtfried, E. Mangraviti, S. Massetti, D. Moissenko, M. Moroni, R. Noschese, F. Nuccilli, N. Paschalidis, J. Ryno, K. Seki, A. Shestakov, S. Shuvalov, R. Sordini, F. Stenbeck, J. Svensson, S. Szalai, K. Szego, D. Toublanc, N. Vertolli, R. Wallner, A. Vorburger, Istituto di Astrofisica e Planetologia Spaziali - INAF (IAPS), Istituto Nazionale di Astrofisica (INAF), Space Research Institute of Austrian Academy of Sciences (IWF), Austrian Academy of Sciences (OeAW), Swedish Institute of Space Physics [Kiruna] (IRF), Southwest Research Institute [San Antonio] (SwRI), Department of Climate and Space Sciences and Engineering (CLaSP), University of Michigan [Ann Arbor], University of Michigan System-University of Michigan System, Department of Electronics and Nanoengineering [Espoo], School of Electrical Engineering [Aalto Univ], Aalto University-Aalto University, Physics Institute [Bern], University of Bern, Italian Space Agency, Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-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 Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), European Space Research and Technology Centre (ESTEC), European Space Agency (ESA), HELIOS - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), 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), Wigner Research Centre for Physics [Budapest], Hungarian Academy of Sciences (MTA), Johns Hopkins University Applied Physics Laboratory [Laurel, MD] (APL), NASA Goddard Space Flight Center (GSFC), Space Technology Ireland Limited, Space Research Institute of the Russian Academy of Sciences (IKI), Russian Academy of Sciences [Moscow] (RAS), UTSA Department of Physics and Astronomy [San Antonio], The University of Texas at San Antonio (UTSA), National and Kapodistrian University of Athens (NKUA), Hellenic Space Center (HSC), Princeton Plasma Physics Laboratory (PPPL), Princeton University, Department of Astrophysical Sciences [Princeton], Department of Physics [Umeå], Umeå University, Max-Planck-Institut für Sonnensystemforschung (MPS), Max-Planck-Gesellschaft, INAF - Osservatorio Astronomico di Trieste (OAT), OHB-Italia SpA, AMDL srl, Laboratory for Atmospheric and Space Physics [Boulder] (LASP), University of Colorado [Boulder], Institute of Experimental Physics SAS, 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), Aberystwyth University, University of Arizona, Finnish Meteorological Institute (FMI), University of Virginia [Charlottesville], Laboratory for Plasma Physics (LPP), Ecole Royale Militaire / Koninklijke Militaire School (ERM KMS), Department of Earth and Planetary Science [Tokyo], Graduate School of Science [Tokyo], The University of Tokyo (UTokyo)-The University of Tokyo (UTokyo), National Institute for Astrophysics, Austrian Academy of Sciences, Uppsala University, Southwest Research Institute, Department of Electronics and Nanoengineering, Agenzia Spaziale Italiana, University of Michigan, Ann Arbor, Université de Toulouse, European Space Research and Technology Centre, Observatoire de Paris, Hungarian Academy of Sciences, Johns Hopkins Applied Physics Laboratory, NASA Goddard Space Flight Center, Space Technology Ireland, Ltd., Space Research Institute of the Russian Academy of Sciences, National and Kapodistrian University of Athens, European Space Research and Technology Centre (ESA/ESTEC), Max Planck Institute for Solar System Research, Osservatorio Astronomico di Trieste, UMR7095, AMDL Srl, University of Colorado Boulder, Slovak Academy of Sciences, Université d'Orléans, Johns Hopkins University, Institutet för rymdfysik, Esa Kallio Group, University of Virginia, Université Paris-Saclay, INAF - Osservatorio Astronomico di Trieste, INAF - Osservatorio Astronomico di Roma, Finnish Meteorological Institute, The University of Tokyo, Max Planck Institute for Plasma Physics, IRAP, Universität Bern - University of Bern, Aalto-yliopisto, Aalto University, Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), 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), Agence Spatiale Européenne = European Space Agency (ESA), and Max-Planck-Institut für Sonnensystemforschung = Max Planck Institute for Solar System Research (MPS)
Subjects: Fusion, plasma och rymdfysik, Multidisciplinary, Astronomi, astrofysik och kosmologi, 530 Physics, 520 Astronomy, [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], General Physics and Astronomy, Astronomy, Astrophysics and Cosmology, General Chemistry, 000 Computer science, knowledge & systems, 620 Engineering, Fusion, Plasma and Space Physics, General Biochemistry, Genetics and Molecular Biology
Abstract: Mercury’s southern inner magnetosphere is an unexplored region as it was not observed by earlier space missions. In October 2021, BepiColombo mission has passed through this region during its first Mercury flyby. Here, we describe the observations of SERENA ion sensors nearby and inside Mercury’s magnetosphere. An intermittent high-energy signal, possibly due to an interplanetary magnetic flux rope, has been observed downstream Mercury, together with low energy solar wind. Low energy ions, possibly due to satellite outgassing, were detected outside the magnetosphere. The dayside magnetopause and bow-shock crossing were much closer to the planet than expected, signature of a highly eroded magnetosphere. Different ion populations have been observed inside the magnetosphere, like low latitude boundary layer at magnetopause inbound and partial ring current at dawn close to the planet. These observations are important for understanding the weak magnetosphere behavior so close to the Sun, revealing details never reached before.
Published: 2022

18. STELLA—Potential European contributions to a NASA-led interstellar probe

Author: Robert F. Wimmer-Schweingruber, Nicolas André, Stas Barabash, Pontus C. Brandt, Timothy S. Horbury, Luciano Iess, Benoit Lavraud, Ralph L. McNutt, Jr., Elena A. Provornikova, Eric Quémerais, Robert Wicks, Martin Wieser, Peter Wurz, Institute of Experimental and Applied Physics [Kiel] (IEAP), Christian-Albrechts-Universität zu Kiel (CAU), 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), Swedish Institute of Space Physics [Kiruna] (IRF), Johns Hopkins University Applied Physics Laboratory [Laurel, MD] (APL), Imperial College London, Università degli Studi di Roma 'La Sapienza' = Sapienza University [Rome] (UNIROMA), Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), HELIOS - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), 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), University of Northumbria at Newcastle [United Kingdom], and University of Bern
Subjects: [SDU]Sciences of the Universe [physics], 520 Astronomy, Astronomy and Astrophysics, 620 Engineering
Abstract: The discovery of a myriad of exoplanets in the past decades has revolutionized the understanding of our place in the Universe. How different are exoplants and do some of them harbor life, just like Earth? To do so, their parent stars must drive a stellar wind and carve what we call astrospheres into the surrounding interstellar medium. Astrospheres are ubiquitous in our immediate neighborhood and show similar structure to our heliosphere. Voyager 1 and 2, Ulysses, Cassini, and IBEX have shown that the interaction between interstellar medium and solar wind is much more complex and involved than previously believed. This stellar-interstellar interaction is key to understand astrospheres and the shielding they provide to the planetary systems they harbor. This article summarizes a whitepaper that was submitted to NASA’s 2023/2024 decadal survey which is being conducted by the US National Academies. It is based in parts on a proposal submitted to the European Space Agency (ESA) in response to its 2021 call for medium-class mission proposals. The whitepaper and this article propose to study the interaction described above in situ at the heliospheric boundaries and to explore the very local interstellar medium beyond. Furthermore, they highlight possible European contributions to a NASA-led Interstellar Probe (ISP).
Published: 2022
Full Text: View/download PDF

19. Modeling the impact of a strong X‐class solar flare on the planetary ion composition in Mercury’s magnetosphere

Author: A. L. E. Werner, F. Leblanc, J. Y. Chaufray, R. Modolo, S. Aizawa, L. Z. Hadid, C. Baskevitch, Swedish Institute of Space Physics [Uppsala] (IRF), HELIOS - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), 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), Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique des Plasmas (LPP), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École polytechnique (X)-Sorbonne Université (SU)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), and ANR-17-CE31-0016,TEMPETE,Évolutions temporelles des environnements planétaires magnétisés pendant des tempêtes solaires(2017)
Subjects: Geophysics, Magnetosphere, [SDU]Sciences of the Universe [physics], Astrophysics::High Energy Astrophysical Phenomena, Physics::Space Physics, Ion Distribution, Solar Irradiance, General Earth and Planetary Sciences, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Mercury, Model
Abstract: International audience; We model the impact of an extreme solar flare on the Mg+, Na+, O+ and He+ ion density distribution in Mercury’s magnetosphere. The Flare Irradiance Spectral Model of the solar irradiance during the X9.3-class flare on 6 September 2017 is used as input to the time-dependent Latmos Ionized Exosphere ion density model. We find that the time-evolution of the planetary ion distribution differs with respect to energy, location and species. There exist two ion energy populations on the dayside that experience different dynamical evolution. The peak ion density in the nightside plasma sheet is delayed by ∼7 − 8 minutes compared to the dayside. The maximum Mg+ density occurs ∼ 4 minutes before He+ and O+ in the whole magnetosphere. The time delay between different species does not necessarily occur for solar flares that erupt near the apparent solar limb, where the optical depth is large.
Published: 2022

20. INSPIRE-SAT 7, a Second CubeSat to Measure the Earth's Energy Budget and to Probe the Ionosphere

Author: Mustapha Meftah, Fabrice Boust, Philippe Keckhut, Alain Sarkissian, Thomas Boutéraon, Slimane Bekki, Luc Damé, Patrick Galopeau, Alain Hauchecorne, Christophe Dufour, Adrien Finance, André-Jean Vieau, Emmanuel Bertran, Pierre Gilbert, Nicolas Caignard, Clément Dias, Jean-Luc Engler, Patrick Lacroix, Kévin Grossel, Véronique Rannou, Stéphane Saillant, Yannick Avelino, Benjamin Azoulay, Cyril Brand, Carlos Dominguez, Akos Haasz, Agne Paskeviciute, Kevin Segura, Pierre Maso, Sébastien Ancelin, Christophe Mercier, Valentin Stee, Antoine Mangin, David Bolsée, Catherine Billard, STRATO - 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), DEMR, ONERA, Université Paris Saclay [Palaiseau], ONERA-Université Paris-Saclay, 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), HELIOS - LATMOS, Analytic and Computational Research, Inc. - Earth Sciences (ACRI-ST), Observatoire de Versailles Saint-Quentin-en-Yvelines (OVSQ), Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Centre National de la Recherche Scientifique (CNRS), Sté Adrelys, OLEDCOMM, Innovative Solutions In Space [Delft] (ISIS), AMSAT-Francophone, Belgian Institute for Space Aeronomy / Institut d'Aéronomie Spatiale de Belgique (BIRA-IASB), International Centre for Research in Ecological Economics, Eco-Innovation and Tool Development for Sustainability (REEDS), Université de Versailles Saint-Quentin-en-Yvelines (UVSQ), 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), 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), Centre de recherche en épidémiologie et santé des populations (CESP), Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Assistance publique - Hôpitaux de Paris (AP-HP) (AP-HP)-Hôpital Paul Brousse-Institut National de la Santé et de la Recherche Médicale (INSERM)-Université Paris-Saclay, This research was mainly funded by Centre National de la Recherche Scientifique (CNRS,France), UVSQ (Université de Versailles Saint-Quentin-en-Yvelines, France), Agence Nationale de laRecherche (ANR, France), Office National d’Etudes et de Recherches Aérospatiales (ONERA, France),Développement économique-Saint-Quentin en Yvelines (78, France), and Département des Yvelines(78, France)., and Cardon, Catherine
Subjects: [PHYS.PHYS.PHYS-AO-PH]Physics [physics]/Physics [physics]/Atmospheric and Oceanic Physics [physics.ao-ph], 010504 meteorology & atmospheric sciences, climate observation and monitoring, Earth’s energy budget, ionosphere, nanosatellite, CubeSat constellations, Science, 7. Clean energy, 01 natural sciences, [PHYS.PHYS.PHYS-AO-PH] Physics [physics]/Physics [physics]/Atmospheric and Oceanic Physics [physics.ao-ph], [SDU.STU.CL] Sciences of the Universe [physics]/Earth Sciences/Climatology, 13. Climate action, [SDU.STU.CL]Sciences of the Universe [physics]/Earth Sciences/Climatology, 0103 physical sciences, General Earth and Planetary Sciences, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences
Abstract: INSPIRE-SAT 7 is a French 2-Unit CubeSat (11.5 × 11.5 × 22.7 cm) primarily designed for Earth and Sun observation. INSPIRE-SAT 7 is one of the missions of the International Satellite Program in Research and Education (INSPIRE). Twice the size of a 4 × 4 Rubik’s Cube and weighing about 3 kg, INSPIRE-SAT 7 will be deployed in Low Earth Orbit (LEO) in 2023 to join its sister satellite, UVSQ-SAT. INSPIRE-SAT 7 represents one of the in-orbit demonstrators needed to test how two Earth observation CubeSats in orbit can be utilized to set up a satellite constellation. This new scientific and technological pathfinder CubeSat mission (INSPIRE-SAT 7) uses a multitude of miniaturized sensors on all sides of the CubeSat to measure the Earth’s energy budget components at the top-of-the-atmosphere for climate change studies. INSPIRE-SAT 7 contains also a High-Frequency (HF) payload that will receive HF signals from a ground-based HF transmitter to probe the ionosphere for space weather studies. Finally, this CubeSat is equipped with several technological demonstrators (total solar irradiance sensors, UV sensors to measure solar spectral irradiance, a new Light Fidelity (Li-Fi) wireless communication system, a new versatile telecommunication system suitable for CubeSat). After introducing the objectives of the INSPIRE-SAT 7 mission, we present the satellite definition and the mission concept of operations. We also briefly show the observations made by the UVSQ-SAT CubeSat, and assess how two CubeSats in orbit could improve the information content of their Earth’s energy budget measurements. We conclude by reporting on the potential of future missions enabled by CubeSat constellations.
Published: 2022

21. Investigating Mercury's Environment with the Two-Spacecraft BepiColombo Mission

Author: Oleg Korablev, M. Fujimoto, Léa Griton, Cesare Grava, Masafumi Hirahara, Hirotsugu Kojima, S. Barabash, Wolfgang Baumjohann, A. Martindale, Chuanfei Dong, François Leblanc, Chris Carr, S. T. Lindsay, Yasumasa Kasaba, M. Kobayashi, Herbert Lichtenegger, Philippe-A. Bourdin, Karri Muinonen, J. S. Oliveira, Jan-Erik Wahlund, Ferdinand Plaschke, Christina Plainaki, S. M. P. McKenna-Lawlor, Dominique Delcourt, Eric Quémerais, Xianzhe Jia, Dusan Odstrcil, James A. Slavin, V. Mangano, M. G. Pelizzo, Benoit Langlais, Joe Zender, Emma J. Bunce, Ichiro Yoshikawa, Peter Wurz, Stavro Ivanovski, Stefano Massetti, George C. Ho, Y. Saito, Juhani Huovelin, Suzanne M. Imber, Sae Aizawa, Alessandro Mura, Jim M. Raines, Ayako Matsuoka, F. Sahraoui, Karl-Heinz Glassmeier, Pierre Henri, Rami Vainio, Matthew K. James, Rosemary M. Killen, Stefano Orsini, Shahab Fatemi, Tomas Karlsson, Monica Laurenza, Esa Kallio, Christoph Lhotka, Michiko Morooka, Johannes Benkhoff, David A. Rothery, Yasuhito Narita, Michel Moncuquet, Anna Milillo, Alexey A. Berezhnoy, Satoshi Yagitani, Adam Masters, F. Califano, Manuel Grande, Stefano Livi, Daniel Heyner, Emilia Kilpua, G. Murakami, Jan Deca, S. de la Fuente, R. Moissl, Bernard V. Jackson, Kanako Seki, N. André, M. Dósa, Istituto di Astrofisica e Planetologia Spaziali - INAF (IAPS), Istituto Nazionale di Astrofisica (INAF), Institute of Space and Astronautical Science (ISAS), Japan Aerospace Exploration Agency [Sagamihara] (JAXA), European Space Research and Technology Centre (ESTEC), Agence Spatiale Européenne = European Space Agency (ESA), 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), Wigner Research Centre for Physics [Budapest], Hungarian Academy of Sciences (MTA), Institut für Geophysik und Extraterrestrische Physik [Braunschweig] (IGEP), Technische Universität Braunschweig = Technical University of Braunschweig [Braunschweig], Johns Hopkins University Applied Physics Laboratory [Laurel, MD] (APL), Department of Atmospheric, Oceanic, and Space Sciences [Ann Arbor] (AOSS), University of Michigan [Ann Arbor], University of Michigan System-University of Michigan System, Space Research Centre [Leicester], University of Leicester, Department of Space and Plasma Physics [Stockholm], KTH School of Electrical Engineering, Royal Institute of Technology [Stockholm] (KTH )-Royal Institute of Technology [Stockholm] (KTH ), NASA Goddard Space Flight Center (GSFC), Space Technology Ireland Limited, Department of Climate and Space Sciences and Engineering (CLaSP), School of Physical Sciences [Milton Keynes], Faculty of Science, Technology, Engineering and Mathematics [Milton Keynes], The Open University [Milton Keynes] (OU)-The Open University [Milton Keynes] (OU), Space Research Institute of Austrian Academy of Sciences (IWF), Austrian Academy of Sciences (OeAW), Sternberg Astronomical Institute [Moscow], Lomonosov Moscow State University (MSU), University of Pisa - Università di Pisa, University of Colorado [Boulder], European Space Astronomy Centre (ESAC), Princeton Plasma Physics Laboratory (PPPL), Princeton University, Department of Astrophysical Sciences [Princeton], Southwest Research Institute [San Antonio] (SwRI), Swedish Institute of Space Physics [Kiruna] (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), INAF - Osservatorio Astronomico di Trieste (OAT), University of California [San Diego] (UC San Diego), University of California (UC), Department of Electronics and Nanoengineering [Espoo], School of Electrical Engineering [Aalto Univ], Aalto University-Aalto University, Planetary Plasma and Atmospheric Research Center [Sendai] (PPARC), Tohoku University [Sendai], Department of Physics [Helsinki], Falculty of Science [Helsinki], Helsingin yliopisto = Helsingfors universitet = University of Helsinki-Helsingin yliopisto = Helsingfors universitet = University of Helsinki, Planetary Exploration Research Center [Chiba] (PERC), Chiba Institute of Technology (CIT), 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), HELIOS - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), 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), Blackett Laboratory, Imperial College London, Swedish Institute of Space Physics [Uppsala] (IRF), Institute of Physics [Graz], Karl-Franzens-Universität Graz, Centro de Investigação da Terra e do Espaço da UC (CITEUC), Universidade de Coimbra [Coimbra], CNR Institute for Photonics and Nanotechnologies (IFN), National Research Council of Italy | Consiglio Nazionale delle Ricerche (CNR), Italian Space Agency, Laboratoire de Physique des Plasmas (LPP), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École polytechnique (X)-Sorbonne Université (SU)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), Department of Earth and Planetary Science [Tokyo], Graduate School of Science [Tokyo], The University of Tokyo (UTokyo)-The University of Tokyo (UTokyo), Space Research Laboratory [Turku] (SRL), Department of Physics and Astronomy [Turku], University of Turku-University of Turku, Physics Institute [Bern], University of Bern, Department of Physics [Imperial College London], Institute of Mathematical and Physical Sciences [Aberystwyth], University of Wales, Institute for Space-Earth Environmental Research [Nagoya] (ISEE), Nagoya University, Space Research Institute of the Russian Academy of Sciences (IKI), Russian Academy of Sciences [Moscow] (RAS), Research Institute for Sustainable Humanosphere (RISH), Kyoto University, Laboratoire d'études spatiales et d'instrumentation en astrophysique = Laboratory of Space Studies and Instrumentation in Astrophysics (LESIA), 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), Graduate School of the Natural Science and Technology [Kanazawa], Kanazawa University (KU), Department of Complexity Science and Engineering [Tokyo], The University of Tokyo (UTokyo), European Space Agency (ESA), 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), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université d'Orléans (UO)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université d'Orléans (UO)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National d’Études Spatiales [Paris] (CNES), University of California, University of Helsinki-University of Helsinki, 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), Karl-Franzens-Universität [Graz, Autriche], Consiglio Nazionale delle Ricerche [Roma] (CNR), Kyoto University [Kyoto], Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA (UMR_8109)), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), The Royal Society, Science and Technology Facilities Council, INAF National Institute for Astrophysics, JAXA Institute of Space and Astronautical Science, European Space Research and Technology Centre, IRAP, Hungarian Academy of Sciences, Technical University of Braunschweig, Johns Hopkins Applied Physics Laboratory, University of Michigan, Ann Arbor, KTH Royal Institute of Technology, NASA Goddard Space Flight Center, Space Technology Ireland, Open University Milton Keynes, Austrian Academy of Sciences, Lomonosov Moscow State University, University of Pisa, University of Colorado Boulder, European Space Astronomy Centre, Princeton Plasma Physics Laboratory, Southwest Research Institute, Uppsala University, Université d'Orléans, Osservatorio Astronomico di Trieste, University of California San Diego, Department of Electronics and Nanoengineering, Tohoku University, University of Helsinki, Chiba Institute of Technology, Université de Nantes, Sorbonne Université, University of Graz, National Research Council of Italy, Agenzia Spaziale Italiana, The University of Tokyo, University of Turku, Aberystwyth University, Space Research Institute of the Russian Academy of Sciences, Université de Versailles Saint-Quentin-en-Yvelines, Kanazawa University, Aalto-yliopisto, and Aalto University
Subjects: 010504 meteorology & atmospheric sciences, Computer science, BepiColombo, chemistry.chemical_element, FOS: Physical sciences, Astronomy & Astrophysics, 01 natural sciences, Mercury’s environment, Fusion, plasma och rymdfysik, Interplanetary dust cloud, Astronomi, astrofysik och kosmologi, 0201 Astronomical and Space Sciences, 0103 physical sciences, Astronomy, Astrophysics and Cosmology, Exosphere, Magnetosphere, Aerospace engineering, 010303 astronomy & astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), 0105 earth and related environmental sciences, Scientific instrument, Earth and Planetary Astrophysics (astro-ph.EP), Spacecraft, business.industry, 520 Astronomy, Astronomy and Astrophysics, 620 Engineering, Fusion, Plasma and Space Physics, Mercury (element), Solar wind, Planetary science, chemistry, Space and Planetary Science, [SDU]Sciences of the Universe [physics], Mercury's environment, Mercury’s environment · Magnetosphere · Exosphere · BepiColombo, Astrophysics - Instrumentation and Methods for Astrophysics, business, Astrophysics - Earth and Planetary Astrophysics
Abstract: The ESA-JAXA BepiColombo mission will provide simultaneous measurements from two spacecraft, offering an unprecedented opportunity to investigate magnetospheric and exospheric dynamics at Mercury as well as their interactions with the solar wind, radiation, and interplanetary dust. Many scientific instruments onboard the two spacecraft will be completely, or partially devoted to study the near-space environment of Mercury as well as the complex processes that govern it. Many issues remain unsolved even after the MESSENGER mission that ended in 2015. The specific orbits of the two spacecraft, MPO and Mio, and the comprehensive scientific payload allow a wider range of scientific questions to be addressed than those that could be achieved by the individual instruments acting alone, or by previous missions. These joint observations are of key importance because many phenomena in Mercury's environment are highly temporally and spatially variable. Examples of possible coordinated observations are described in this article, analysing the required geometrical conditions, pointing, resolutions and operation timing of different BepiColombo instruments sensors., Comment: 78 pages, 14 figures, published
Published: 2022
Full Text: View/download PDF

22. The Solar-Cycle Temporal Variation of the Solar Wind Charge Exchange X-ray Lines

Author: Zhijie Qu, Dimitra Koutroumpa, Joel N. Bregman, Kip D. Kuntz, Philip Kaaret, Department of Astronomy and Astrophysics [Chicago], University of Chicago, Department of Astronomy [Ann Arbor], University of Michigan [Ann Arbor], University of Michigan System-University of Michigan System, HELIOS - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), 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), Institut Pierre-Simon-Laplace (IPSL (FR_636)), École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-École polytechnique (X)-Centre National d'Études Spatiales [Toulouse] (CNES)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Department of Physics and Astronomy [Baltimore], Johns Hopkins University (JHU), NASA Goddard Space Flight Center (GSFC), Department of Physics and Astronomy [Iowa City], and University of Iowa [Iowa City]
Subjects: Circumgalactic medium, [SDU.ASTR.SR]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], Solar wind, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, Milky Way Galaxy, Space Physics (physics.space-ph), Astrophysics - Solar and Stellar Astrophysics, Physics - Space Physics, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Physics::Space Physics, Astrophysics::Solar and Stellar Astrophysics, Charge exchange ionization, Solar and Stellar Astrophysics (astro-ph.SR)
Abstract: Solar wind charge exchange (SWCX) is the primary contamination to soft X-ray emission lines from the Milky Way (MW) hot gas. We report a solar-cycle ($\approx 10$ yr) temporal variation of observed \ion{O}{7} and \ion{O}{8} emission line measurements in the {\it XMM-Newton} archive, which is tightly correlated with the solar cycle traced by the sunspot number (SSN). This temporal variation is expected to be associated with the heliospheric SWCX. Another observed correlation is that higher solar wind (SW) fluxes lead to higher O VII or O VIII fluxes, which is due to the magnetospheric SWCX. We construct an empirical model to reproduce the observed correlation between the line measurements and the solar activity (i.e., the SW flux and the SSN). With this model we discovered a lag of $0.91_{-0.22}^{+0.20}$ yr between the O VII flux and the SSN. This time lag is a combination of the SW transit time within the heliosphere, the lag of the neutral gas distribution responding to solar activity, and the intrinsic lag between the SSN and the launch of a high-energy SW (i.e., $\rm O^{7+}$ and $\rm O^{8+}$). MW O VII and O VIII fluxes have mean values of 5.4 L.U. and 1.7 L.U., which are reduced by $50\%$ and $30\%$, compared to studies where the SWCX contamination is not removed. This correction also changes the determination of the density distribution and the temperature profile of the MW hot gas., Comment: 10 pages, 5 figures. ApJ accepted
Published: 2022
Full Text: View/download PDF

23. 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

24. BepiColombo - Mission Overview and Science Goals

Author: Benkhoff, Johannes, Murakami, Go, Baumjohann, W., Besse, S., Bunce, E.J., Casale, Mauro, Cremonese, G., Glassmeier, K. H., Hayakawa, H., Heyner, Daniel, Hiesinger, H., Huovelin, Juhani, Hussmann, H., Iafolla, V., Iess, Luciano, Kasaba, Yasumasa, Kobayashi, Masanori, Milillo, Anna, Mitrofanov, Igor G., Montagnon, Elsa, Novara, M., Orsini, Stefano, Quemerais, Eric, Reininghaus, U., Saito, Yoshifumi, Santoli, Francesco, Stramaccioni, D., Sutherland, O., Thomas, N., Yoshikawa, I., Zender, Joe, Department of Physics, European Space Research and Technology Centre (ESTEC), European Space Agency (ESA), Japan Aerospace Exploration Agency [Sagamihara] (JAXA), Space Research Institute of Austrian Academy of Sciences (IWF), Austrian Academy of Sciences (OeAW), European Space Astronomy Centre (ESAC), School of Physics and Astronomy [Leicester], University of Leicester, INAF - Osservatorio Astronomico di Padova (OAPD), Istituto Nazionale di Astrofisica (INAF), Institut für Geophysik und Extraterrestrische Physik [Braunschweig] (IGEP), Technische Universität Braunschweig = Technical University of Braunschweig [Braunschweig], Institute of Space and Astronautical Science (ISAS), Institut für Planetologie [Münster], Westfälische Wilhelms-Universität Münster (WWU), Department of Physics [Helsinki], Falculty of Science [Helsinki], University of Helsinki-University of Helsinki, DLR Institut für Planetenforschung, Deutsches Zentrum für Luft- und Raumfahrt [Berlin] (DLR), Istituto di Astrofisica e Planetologia Spaziali - INAF (IAPS), Dipartimento di Ingegneria Meccanica e Aerospaziale [Roma La Sapienza] (DIMA), Università degli Studi di Roma 'La Sapienza' = Sapienza University [Rome], Planetary Plasma and Atmospheric Research Center [Sendai] (PPARC), Tohoku University [Sendai], Planetary Exploration Research Center [Chiba] (PERC), Chiba Institute of Technology (CIT), Space Research Institute of the Russian Academy of Sciences (IKI), Russian Academy of Sciences [Moscow] (RAS), European Space Operations Center (ESOC), 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), Physikalisches Institut [Bern], Universität Bern [Bern], Department of Complexity Science and Engineering [Tokyo], and The University of Tokyo (UTokyo)
Subjects: SURFACE, 010504 meteorology & atmospheric sciences, BepiColombo, Scientific Space Mission, Missions, 114 Physical sciences, 01 natural sciences, MAGNETOSPHERE, Planetary and Magnetospheric Science, 0103 physical sciences, MESSENGER OBSERVATIONS, SPECTROMETER, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, MERCURY ORBITER MISSION, Mercury exploration, 520 Astronomy, Science Goals, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy and Astrophysics, Mercury, 620 Engineering, CORNERSTONE MISSION, Surface and Interior, GAMMA-RAY, [SDU]Sciences of the Universe [physics], POLAR DEPOSITS, Space and Planetary Science, Fundamental Physics, Physics::Space Physics, Astrophysics::Earth and Planetary Astrophysics, VENUS, GENERATION
Abstract: BepiColombo is a joint mission between the European Space Agency, ESA, and the Japanese Aerospace Exploration Agency, JAXA, to perform a comprehensive exploration of Mercury. Launched on $20^{\mathrm{th}}$ 20 th October 2018 from the European spaceport in Kourou, French Guiana, the spacecraft is now en route to Mercury.Two orbiters have been sent to Mercury and will be put into dedicated, polar orbits around the planet to study the planet and its environment. One orbiter, Mio, is provided by JAXA, and one orbiter, MPO, is provided by ESA. The scientific payload of both spacecraft will provide detailed information necessary to understand the origin and evolution of the planet itself and its surrounding environment. Mercury is the planet closest to the Sun, the only terrestrial planet besides Earth with a self-sustained magnetic field, and the smallest planet in our Solar System. It is a key planet for understanding the evolutionary history of our Solar System and therefore also for the question of how the Earth and our Planetary System were formed.The scientific objectives focus on a global characterization of Mercury through the investigation of its interior, surface, exosphere, and magnetosphere. In addition, instrumentation onboard BepiColombo will be used to test Einstein’s theory of general relativity. Major effort was put into optimizing the scientific return of the mission by defining a payload such that individual measurements can be interrelated and complement each other.
Published: 2021

25. Correction to: The Vector Electric Field Investigation (VEFI) on the C/NOFS

Author: R. Pfaff, P. Uribe, R. Fourre, J. Kujawski, N. Maynard, M. Acuña, D. Rowland, H. Freudenreich, K. Bromund, S. Martin, C. Liebrecht, R. Kramer, F. Hunsaker, R. Holzworth, M. McCarthy, W. Farrell, J. Klenzing, G. Le, A. Jacobson, J. Houser, C. Steigies, J.-J. Berthelier, NASA Goddard Space Flight Center (GSFC), University of Washington [Seattle], HELIOS - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), and 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)
Subjects: 010504 meteorology & atmospheric sciences, Space and Planetary Science, 0103 physical sciences, Astronomy and Astrophysics, 010303 astronomy & astrophysics, 01 natural sciences, ComputingMilieux_MISCELLANEOUS, 0105 earth and related environmental sciences, [SDU.ASTR.IM]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM]
Abstract: International audience
Published: 2021

26. The Vector Electric Field Investigation (VEFI) on the C/NOFS Satellite

Author: Jean-Jacques Berthelier, Douglas E. Rowland, Jeffrey Klenzing, Henry Freudenreich, S. Martin, Matthew D. McCarthy, R. F. Pfaff, Mario H. Acuña, J. Houser, Abram R. Jacobson, R. Kramer, P. Uribe, C. Liebrecht, Robert H. Holzworth, R. Fourre, Guan Le, C. Steigies, William M. Farrell, J. Kujawski, Kenneth R. Bromund, F. Hunsaker, N. C. Maynard, NASA Goddard Space Flight Center (GSFC), University of Washington [Seattle], HELIOS - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), and 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)
Subjects: Spectrum analyzer, 010504 meteorology & atmospheric sciences, Meteorology, Magnetometer, Acoustics, Ionospheric satellite measurements, 01 natural sciences, Signal, law.invention, symbols.namesake, law, Electric field, 0103 physical sciences, Langmuir probe, 010303 astronomy & astrophysics, Electric field detectors, 0105 earth and related environmental sciences, Low-latitude ionosphere, Physics, Detector, Astronomy and Astrophysics, Lightning, [SDU.ASTR.IM]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], Space and Planetary Science, symbols, Satellite
Abstract: The Vector Electric Field Investigation (VEFI) on the C/NOFS satellite comprises a suite of sensors controlled by one central electronics box. The primary measurement consists of a vector DC and AC electric field detector which extends spherical sensors with embedded pre-amps at the ends of six, 9.5-m booms forming three orthogonal detectors with baselines of 20 m tip-to-tip each. The primary VEFI measurement is the DC electric field at 16 vectors/sec with an accuracy of 0.5 mV/m. The electric field receiver also measures the broad spectra of irregularities associated with equatorial spread-F and related ionospheric processes that create the scintillations responsible for the communication and navigation outages for which the C/NOFS mission is designed to understand and predict. The AC electric field measurements range from ELF to HF frequencies.VEFI includes a flux-gate magnetometer providing DC measurements at 1 vector/sec and AC-coupled measurements at 16 vector/sec, as well as a fast, fixed-bias Langmuir probe that serves as the input signal to trigger the VEFI burst memory collection of high time resolution wave data when plasma density depletions are encountered in the low latitude nighttime ionosphere. A bi-directional optical lightning detector designed by the University of Washington (UW) provides continuous average lightning counts at different irradiance levels as well as high time resolution optical lightning emissions captured in the burst memory. The VEFI central electronics box receives inputs from all of the sensors and includes a configurable burst memory with 1–8 channels at sample rates as high as 32 ks/s per channel. The VEFI instrument is thus one experiment with many sensors. All of the instruments were designed, built, and tested at the NASA/Goddard Space Flight Center with the exception of the lightning detector which was designed at UW. The entire VEFI instrument was delivered on budget in less than 2 years.VEFI included a number of technical advances and innovative features described in this article. These include: (1) Two independent sets of 3-axis, orthogonal electric field double probes; (2) Motor-driven, pre-formed cylinder booms housing signal wires that feed pre-amps within tip-mounted spherical sensors; (3) Extended shadow equalizers (2.5 times the sphere diameter) to mitigate photoelectron shadow mismatch for sun angles along the boom directions, particularly important at sunrise/sunset for a low inclination satellite; (4) DC-coupled electric field channels with “boosted” or pre-emphasized amplitude response at ELF frequencies; (5) Miniature multi-channel spectrum analyzers using hybrid technology; (6) Dual-channel optical lightning detector with on-board comparators and counters for 7 irradiance levels with high-time-resolution data capture; (7) Spherical Langmuir probe with Titanium Nitride-coated sensor element and guard; (8) Selectable data rates including 200 kbps (fast), 20 kbps (nominal), and 2 kbps (low for real-time TDRSS communication); and (9) Highly configurable burst memory with selectable channels, sample rates and number, duration, and precursor length of bursts, chosen based on best triggering algorithm “score”.This paper describes the various sensors that constitute the VEFI experiment suite and discusses their operation during the C/NOFS mission. Examples of data are included to illustrate the performance of the different sensors in space.
Published: 2021

27. Origin of the Solar Rotation Harmonics Seen in the EUV and UV Irradiance

Author: Gabriel Giono, Rangaiah Kariyappa, Joe Zender, Luc Damé, Division of Space and Plasma Physics [Stockholm] (SPP), School of Electrical Engineering [Stockholm], Royal Institute of Technology [Stockholm] (KTH )-Royal Institute of Technology [Stockholm] (KTH ), European Space Research and Technology Centre (ESTEC), European Space Agency (ESA), Indian Institute of Astrophysics (IIA), Institute for Space-Earth Environmental Research [Nagoya] (ISEE), Nagoya University, HELIOS - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), and 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)
Subjects: Rotation period, Physics, Periodicity, Photosphere, 010504 meteorology & atmospheric sciences, [SDU.ASTR.SR]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], Irradiance, Coronal hole, Astronomy and Astrophysics, Astrophysics, Solar irradiance, 01 natural sciences, Segmentation, 13. Climate action, Space and Planetary Science, Extreme ultraviolet, 0103 physical sciences, Solar rotation, EUV radiation, UV Radiation, 010303 astronomy & astrophysics, Chromosphere, 0105 earth and related environmental sciences
Abstract: Long-term periodicities in the solar irradiance are often observed with periods proportional to the solar rotational period of 27 days. These periods are linked either to some internal mechanism in the Sun or said to be higher harmonics of the rotation without further discussion of their origin. In this article, the origin of the peaks in periodicities seen in the solar extreme ultraviolet (EUV) and ultraviolet (UV) irradiance around the 7, 9, and 14 days periods is discussed. Maps of the active regions and coronal holes are produced from six images per day using the Spatial Possibilistic Clustering Algorithm (SPoCA), a segmentation algorithm. Spectral irradiance at coronal, transition-region/chromospheric, and photospheric levels are extracted for each feature as well as for the full disk by applying the maps to full-disk images (at 19.3, 30.4, and 170 nm sampling in the corona/hot flare plasma, the chromosphere/transition region, and the photosphere, respectively) from the Atmospheric Imaging Assembly (AIA) on board the Solar Dynamics Observatory (SDO) from January 2011 to December 2018. The peaks in periodicities at 7, 9, and 14 days as well as the solar rotation around 27 days can be seen in almost all of the solar irradiance time series. The segmentation also provided time series of the active regions and coronal holes visible area (i.e. in the area observed in the AIA images, not corrected for the line-of-sight effect with respect to the solar surface), which also show similar peaks in periodicities, indicating that the periodicities are due to the change in area of the features on the solar disk rather than to their absolute irradiance. A simple model was created to reproduce the power spectral density of the area covered by active regions also showing the same peaks in periodicities. Segmentation of solar images allows us to determine that the peaks in periodicities seen in solar EUV/UV irradiance from a few days to a month are due to the change in area of the solar features, in particular, active regions, as they are the main contributors to the total full-disk irradiance variability. The higher harmonics of the solar rotation are caused by the clipping of the area signal as the regions rotate behind the solar limb.
Published: 2021

28. A Possible Dust Origin for an Unusual Feature in Io’s Sodium Neutral Clouds

Author: Matthew H. Burger, V. Mangano, Cesare Grava, Hsiang-Wen Hsu, Nicholas M. Schneider, Kurt D. Retherford, François Leblanc, Timothy A. Cassidy, Jeffrey P. Morgenthaler, Cesare Barbieri, Southwest Research Institute [San Antonio] (SwRI), Laboratory for Atmospheric and Space Physics [Boulder] (LASP), University of Colorado [Boulder], Planetary Science Institute [Tucson] (PSI), 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), Istituto di Astrofisica e Planetologia Spaziali - INAF (IAPS), Istituto Nazionale di Astrofisica (INAF), Space Telescope Science Institute (STSci), Dipartimento di Fisica e Astronomia 'Galileo Galilei', and Universita degli Studi di Padova
Subjects: Physics, 010308 nuclear & particles physics, Magnetosphere, Astronomy and Astrophysics, Astrophysics, Plasma, Radius, 01 natural sciences, Jupiter, Radiation pressure, 13. Climate action, Space and Planetary Science, [SDU]Sciences of the Universe [physics], 0103 physical sciences, Atom, Astrophysics::Earth and Planetary Astrophysics, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Exosphere, Eclipse
Abstract: International audience; We report the results of model simulations performed to explain the nature of a sodium emission feature in Io Neutral Clouds. The feature was detected via high-resolution spectroscopic observations from the 3.6 m Italian telescope TNG. The emission feature is blueshifted compared to the main emission (the banana-shaped Neutral Cloud of Io) by a few tens of km s−1, and it is most prominent when Io is a few tens of degrees before eclipse behind Jupiters shadow. The feature's morphology changes with time, indicative of a geometrical effect. We constrained its direction, velocity, and column density with a model of sodium atom trajectories under the influence of Io's and Jupiter's gravity, and solar radiation pressure. The model that best explains this emission feature has the atoms injected into the exosphere from the leading/sub-Jovian hemisphere of Io (45°–68° west longitude), with velocities from 50 to 90 km s−1 relative to Io. These trajectories are consistent with those of negatively charged dust grains (radius ∼10 nm) accelerated by the corotational electric field of Jupiters magnetosphere. We propose that sputtering of sodium atoms from Na-bearing molecules (NaCl and Na2SO4) in these nanodust grains is the process responsible for our emission feature. Both modeling and observational constraints provide an order-of-magnitude estimate of the sodium production rate of ∼1026 s−1. Our work provides another method to monitor the amount of material that Io is supplying to its Neutral Clouds and plasma torus.
Published: 2021

29. Analysis of ground-based very low frequency signal recorded onboard CSES satellite

Author: Mohammed Y. Boudjada, Bruno P. Besser, Hans Eichelberger, Konrad Schwingenschuh, Patrick H. M. Galopeau, Andreas Pollinger, Xuemin Zhang, Valery V. Denisenko, Werner Magnes, Austrian Academy of Sciences (OeAW), China Earthquake Administration (CEA), Federal Research Center Krasnoyarsk Scientific Center (FRC), Siberian Branch of the Russian Academy of Sciences (SB RAS), HELIOS - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), and 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)
Subjects: Physics, Electric fields, 010504 meteorology & atmospheric sciences, [SDU.ASTR.SR]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], Transmitter, Orbits, 7. Clean energy, 01 natural sciences, Signal, Radio transmitters, Solar cycle, Time-frequency analysis, Local time, Electric field, 0103 physical sciences, Physics::Space Physics, Satellite broadcasting, Satellite, Very low frequency, Propagation, 010303 astronomy & astrophysics, Radiant intensity, Magnetic flux, 0105 earth and related environmental sciences, Remote sensing
Abstract: International audience; We report on the wave spectral intensity variations associated to very low frequency (VLF) signal observed during the minimum of solar cycle 25. The VLF signal is emitted by the ground-based NWC radio station localized in the southern hemisphere, at −21.5°S and 114°E. The variation of NWC radio signals is daily detected by the electric field experiment EFD onboard the China Seismo-Electromagnetic Satellite (CSES). This satellite has an altitude of about 507 km in a polar and circular sun-synchronous orbit with local time nodes of 02 LT and 14 LT. We study the spectral intensity variations at the frequency of 19.79 kHz in three specific regions: above the NWC station, around the magnetic equatorial plane, and at the conjugate point. We analyze the electric flux above those key regions and estimate the corresponding intensity levels.
Published: 2021

30. HaloSat Observations of Heliospheric Solar Wind Charge Exchange

Author: P. Kaaret, M. Kounkel, D. M. LaRocca, A. Zajczyk, J. Richardson, J. Bluem, K. D. Kuntz, Dimitra Koutroumpa, R. Ringuette, Keith Jahoda, ADNET Systems, Inc., NASA Goddard Space Flight Center (GSFC), 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), Department of Physics and Astronomy [Baltimore], Johns Hopkins University (JHU), Department of Physics and Astronomy [Iowa City], University of Iowa [Iowa City], Department of Astronomy and Astrophysics [PennState], Pennsylvania State University (Penn State), Penn State System-Penn State System, Department of Physics and Astronomy [Bellingham], Western Washington University (WWU), Center for Space Sciences and Technology (CSST), University of Maryland [Baltimore County] (UMBC), and University of Maryland System-University of Maryland System
Subjects: Physics, Line-of-sight, 010504 meteorology & atmospheric sciences, [SDU.ASTR.SR]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], Astrophysics::High Energy Astrophysical Phenomena, Ecliptic, Astronomy and Astrophysics, Ecliptic pole, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Latitude, Galactic halo, Solar wind, 13. Climate action, Space and Planetary Science, 0103 physical sciences, Physics::Space Physics, Emission spectrum, Astrophysics::Earth and Planetary Astrophysics, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, Line (formation)
Abstract: International audience; X-ray emission from solar wind charge exchange (SWCX) produced in interplanetary space contaminates every astrophysical observation, regardless of the line of sight. Unfortunately, the primary SWCX emission lines also happen to be important diagnostics of astrophysical plasmas. Models of SWCX emission are limited by two main uncertainties: the local solar wind fluxes along the line of sight and the charge exchange cross sections. The He cone, a localized density enhancement of helium neutrals, is the only heliospheric SWCX emission feature that is small enough and bright enough to be observationally isolated from the X-ray background and the broader SWCX emission. HaloSat, an X-ray CubeSat mission, has recently completed two series of specialized observations, near and far from the ecliptic plane, during two Earth transits of the He cone. These observations were used to test the predictions of an SWCX emission model against the emission observed at low ecliptic latitude, where the solar wind data are monitored, and at high ecliptic latitude, where the solar wind data are extrapolated. The measured SWCX emission for the set of observations near the ecliptic plane was consistent with the line intensities predicted by the model but underpredicted for the set of observations at high ecliptic latitude near the south ecliptic pole. Additionally, high-temperature Galactic halo emission components are reported for both spectral sets.
Published: 2021

31. Influence of time-variable solar wind on the response of Mercury's magnetosphere

Author: Aizawa, Sae, André, Nicolas, Modolo, Ronan, Werner, Elisabeth, Slavin, Jim, Boardsen, Scott, Leblanc, François, Chaufray, Jean-Yves, Raines, Jim, 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), Graduate School of Science [Sendai], Tohoku University [Sendai], 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), Department of Climate and Space Sciences and Engineering (CLaSP), University of Michigan [Ann Arbor], University of Michigan System-University of Michigan System, and NASA Goddard Space Flight Center (GSFC)
Subjects: [SDU]Sciences of the Universe [physics], Physics::Space Physics
Abstract: International audience; BepiColombo is going to conduct its first Mercury flyby in October 2021. During this flyby, plasma measurement will be obtained and bring new insights on the Hermean magnetosphere and its interaction with the Sun despite the limited field of view of the instruments during the cruise phase. Unlike Mariner-10 ion measurements will be obtained, and unlike MESSENGER, low energy electrons and ions will be measured simultaneously. In this study, we have revisited Mariner 10 and MESSENGER observations with the help of the global hybrid model LatHyS in order to understand the influence of time-variable solar wind and to constraint the plasma environment. We are able to reproduce the magnetic field observations of Mariner 10 along its trajectory with in particular two distinct signatures consisting of a quiet and disturbed state of the magnetosphere. In addition, the plasma spectrogram is also collected in the model and this enables us to detail the properties of the charged particles observed during the flyby. We will discuss all these signatures both in term of an interaction with a time-variable solar wind and localized processes occurring in the magnetosphere. We will then present the virtual sampling of both the magnetic field and plasma spectrogram along BepiColombo’s first Mercury flyby trajectory and discuss the possible signatures to be observed at that time.
Published: 2021

32. Ganymede's interaction with the jovian plasma from hybrid simulation

Author: Modolo, Ronan, Baskevitch, Claire, Leblanc, François, Masters, Adam, 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), Department of Physics [Imperial College London], and Imperial College London
Subjects: [SDU]Sciences of the Universe [physics], ComputingMilieux_MISCELLANEOUS
Abstract: International audience
Published: 2021

33. Segmentation of Coronal Features to Understand the Solar EUV and UV Irradiance Variability III. Inclusion and Analysis of Bright Points

Author: Rangaiah Kariyappa, Joe Zender, Gabriel Giono, Rens van der Zwaard, Luc Damé, Matthias Bergmann, European Space Research and Technology Centre (ESTEC), European Space Agency (ESA), Delft University of Technology (TU Delft), Institut für Informatik [Würzburg], Julius-Maximilians-Universität Würzburg [Wurtzbourg, Allemagne] (JMU), Indian Institute of Astrophysics (IIA), Institute for Space-Earth Environmental Research [Nagoya] (ISEE), Nagoya University, Department of Space and Plasma Physics [Stockholm], KTH School of Electrical Engineering, Royal Institute of Technology [Stockholm] (KTH )-Royal Institute of Technology [Stockholm] (KTH ), HELIOS - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), and 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)
Subjects: 010504 meteorology & atmospheric sciences, bright points, Irradiance, Coronal hole, Astrophysics, Space weather, Solar irradiance, 7. Clean energy, 01 natural sciences, UV radiation, Atmosphere, Sun: activity, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, Chromosphere, 0105 earth and related environmental sciences, Physics, Solar terrestrial relations, [SDU.ASTR.SR]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], Astronomy and Astrophysics, Corona, Atmosphere of Earth, 13. Climate action, Space and Planetary Science, Physics::Space Physics, Astrophysics::Earth and Planetary Astrophysics, corona
Abstract: The study of solar irradiance variability is of great importance in heliophysics, Earth’s climate, and space weather applications. These studies require careful identifying, tracking and monitoring of features in the solar photosphere, chromosphere, and corona. Do coronal bright points contribute to the solar irradiance or its variability as input to the Earth atmosphere? We studied the variability of solar irradiance for a period of 10 years (May 2010 – June 2020) using the Large Yield Radiometer (LYRA), the Sun Watcher using APS and image Processing (SWAP) on board PROBA2, and the Atmospheric Imaging Assembly (AIA), and applied a linear model between the segmented features identified in the EUV images and the solar irradiance measured by LYRA. Based on EUV images from AIA, a spatial possibilistic clustering algorithm (SPoCA) is applied to identify coronal holes (CHs), and a morphological feature detection algorithm is applied to identify active regions (ARs), coronal bright points (BPs), and the quiet Sun (QS). The resulting segmentation maps were then applied on SWAP images, images of all AIA wavelengths, and parameters such as the intensity, fractional area, and contribution of ARs/CHs/BPs/QS features were computed and compared with LYRA irradiance measurements as a proxy for ultraviolet irradiation incident to the Earth atmosphere. We modeled the relation between the solar disk features (ARs, CHs, BPs, and QS) applied to EUV images against the solar irradiance as measured by LYRA and the F10.7 radio flux. A straightforward linear model was used and corresponding coefficients computed using a Bayesian method, indicating a strong influence of active regions to the EUV irradiance as measured at Earth’s atmosphere. It is concluded that the long- and short-term fluctuations of the active regions drive the EUV signal as measured at Earth’s atmosphere. A significant contribution from the bright points to the LYRA irradiance could not be found.
Published: 2021

34. Io's dry body shaped by atmospheric instability

Author: Mousis, Olivier, Marcq, Emmanuel, Aguichine, Artyom, Leblanc, François, Mandt, Kathleen, Schneeberger, Antoine, Turbet, Martin, 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), PLANETO - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), 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), HELIOS - LATMOS, Johns Hopkins University Applied Physics Laboratory [Laurel, MD] (APL), Observatoire Astronomique de l'Université de Genève (ObsGE), Université de Genève = University of Geneva (UNIGE), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), 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)-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), and Université de Genève (UNIGE)
Subjects: [SDU]Sciences of the Universe [physics], ComputingMilieux_MISCELLANEOUS
Abstract: International audience; One of the outstanding questions regarding the architecture of the Galilean moons system is the nature of the processes that shaped its density gradient, which results from the fact that Ganymede and Callisto share an ice-to-rock ratio close to unity while Io and Europa are heavily depleted in volatiles. Two categories of scenarios, gathered in two distinct phases of moons formation and evolution, have been proposed to account for this density gradient in the literature: either the building blocks of the two innermost moons Io and Europa have been depleted in volatiles during their migration in the hot part of the Jovian circumplanetary disk [1-3], or they initially accreted ice-rich building blocks in a colder environment. In this case, their primitive oceans would have mostly vanished via hydrodynamic escape due to the high accretional energy [4].Figure 1.Thickness of Io's primitive atmosphere (in units of satellite radius) expressed as a function of pressure (in units of surface pressure) for several temperatures.Here, we investigate the possibility that Io also accreted from water-rich building blocks and that its hydrosphere vanished because of hydrostatic instability, i.e. when the gravity at a given height is insufficient to retain gas. Io's putative primordial atmosphere would be either situated atop of a magma mantle, or a coexisting liquid ocean, depending on the surface temperature and pressure. To do so, we use the atmosphere model elaborated by [5,6] in which the properties of a 1D spherical atmosphere of water are generated by integrating the thermodynamic profiles bottom to top. The model takes as inputs the satellite's mass and radius, as well as the thermodynamic conditions at its bottom. Figure 1 represents the atmosphere thickness as a function of surface pressure and temperature. It shows that atmospheric thicknesses higher than 10 Io's radii are reached for surface temperatures equal or higher than 1250 K, indicating that such H2O-dominated atmospheres would be gravitationally unstable at those temperatures. Such high temperatures needed at the base of the atmosphere to favor hydrostatic instabilitycould result from the combination of accretional heating and heating generated by greenhouse effect. If effective, this mechanism would naturally explain why Io is devoid in volatiles without the need of invoking pre-accretional formation scenarios. [1] Canup, R.M. & Ward, W.R. 2002, AJ, 124, 3404. doi:10.1086/344684[2] Mousis, O. & Gautier, D. 2004, PSS, 52, 361. doi:10.1016/j.pss.2003.06.004[3] Ronnet, T., Mousis, O., & Vernazza, P. 2017, ApJ, 845, 92. doi:10.3847/1538-4357/aa80e6[4] Bierson, C.J. & Nimmo, F. 2020, ApJL, 897, L43. doi:10.3847/2041-8213/aba11a[5] Marcq, E., Salvador, A., Massol, H., et al. 2017, JGR (Planets), 122, 1539. doi:10.1002/2016JE005224[6] Marcq, E. 2012, JGR (Planets), 117, E01001. doi:10.1029/2011JE003912
Published: 2021

35. The Venus Climate Database

Author: Thomas Pierron, Aymeric Spiga, Forget Francois, Antoine Martinez, Ehouarn Millour, Jean-Yves Chaufray, Fabrice Cipriani, Franck Montmessin, Sébastien Lebonnois, 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), 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), PLANETO - LATMOS, European Space Research and Technology Centre (ESTEC), and European Space Agency (ESA)
Subjects: Martian, Database, biology, Computer science, Frame (networking), Venus, Mars Exploration Program, Plan (drawing), Space (commercial competition), computer.software_genre, biology.organism_classification, [SDU]Sciences of the Universe [physics], General Circulation Model, Agency (sociology), computer
Abstract: The Venus Climate Database (VCD) is based on the outputs of our state-of-the-art Venus Global Climate Model (GCM) [1-3]. This tool, in the footsteps and spirit of its Martian equivalent, the Mars Climate Database (MCD) [4], is intended to be useful for engineers and scientists wanting to compare with their models, analyze observations or plan future missions. This project is funded by the European Space Agency, in the frame of preliminary studies for the EnVision mission to Venus. Overview of the Venus Climate Database The VCD provides mean values and statistics of the main meteorological variables (atmospheric temperature, density, pressure and winds) as well as atmospheric composition and related physical fields. It extends from the surface up to and including the thermosphere (~250km). The database contains high resolution temporal outputs (using 24 hourly bins) enabling a good representation of the diurnal evolution of quantities over a climatological Venusian day. Figure 1: Illustrative example of diurnal variations of the exospheric temperature retrieved from the VCD, compared to PV-ONMS temperature retrievals. VCD outputs In addition the main meteorological fields (atmospheric temperature, temperature, density, pressure and winds), the following outputs are available from the VCD: Altitudes with respect to the planet center, the reference sphere or above the surface Topography Astronomical quantities such as Venus Solar Longitude and distance to the Sun at any input Earth date Surface temperature (K) and pressure (Pa) Venusian hourly and day to day variability (RMS) of main meteorological fields Short Wave and Long Wave fluxes at any altitude Atmospheric scale height, mean molar mass, speed of sound, reduced gas constant, heat capacity, specific heat ratios and vicosity Volume mixing ratios and columns of CO2, CO, O2, O, H, H2, H2O, SO2, SO, OCS, O3, HCl, N2 and He An estimation of vertically integrated O2 nightglow VIRA (Venus International Reference Atmosphere) temperature, density and pressure at the same location VCD scenarios As the goal of the VCD is to provide information about the state of the Venusian atmosphere, various realistic settings have been used to run a series of baseline GCM simulations, namely: Simulations using various Extreme UltraViolet (EUV) input from the Sun, as this forcing influences significantly the thermosphere (~120km and above). In practice three cases (solar minimum, average and maximum) using fixed E10.7 forcings are provided. The user also has the possibility to obtain outputs corresponding to a chosen E10.7, which may either be specified as a set value or that corresponding to an actual Earth date. In these cases interpolation from the encompassing EUV scenarios is used to estimate the state of the system. To realistically bracket the state of the atmosphere below the thermosphere, which may vary with long-term changes (over time scales of many Venusian days) of the UV cloud albedo [5], along with the baseline case, two supplementary scenarios where that albedo is under and over-estimated are also provided. Figure 2: Illustrative example of temperature profiles retrieved from the VCD using the various EUV scenarios. VCD main features In addition to the aforementioned VCD scenarios, the following features are available: A “high resolution mode” : although the GCM simulations have been run at the resolution of a few degrees in longitude and latitude (3.75° x 1.875°), using some post-processing and a high resolution topography map (at 23 pixels/degree) to adjust the local pressure (and density). Access to the Venusian intra-hour variability (RMS) of main meteorological variables, as well as the Venusian day-to-day variability thereof, as estimated from the multiple Venus days of GCM simulations. The possibility to add perturbations to the climatological fields as: Small-scale perturbations, representative of gravity waves (which are unresolved in the GCM, but accounted for via adequate parametrizations [3]. Large-scale perturbations, representative of actual weather systems present in the GCM simulations. Figure 3: Illustrative example of wind profiles retrieved from the VCD, compared to Pioneer Venus Night probe observations Figure 4: Illustrative example of a climatological temperature profile, along with a perturbed one (using the small-scale perturbation scheme) and VIRA reference values. VCD maccess modes and availability At the time of writing this abstract, we are finalizing a prototype. We plan to release a first version of the VCD in September 2021. Based on our experience with the MCD, the VCD will be distributed as: A main Fortran subroutine that users can interface and directly call from their own software. Interfaces to call this gateway routine using other programming languages (e.g. C, Python, IDL, Matlab, …) will also be available. A web interface, based on the MCD one (at http://www-mars.lmd.jussieu.fr), for quick looks will be set up and maintained on http://www-venus.lmd.jussieu.fr Bibliography [1] S. Lebonnois et al. Wave analysis in the atmosphere of Venus below 100 km altitude, simulated by the LMD Venus GCM, Icarus, 278:38-51, 2016. [2] G. Gilli et al. Thermal structure of the upper atmosphere of Venus simulated by a ground-to-thermosphere GCM, Icarus, 281:55-72, 2017. [3] I. Garate-Lopez and S. Lebonnois. Latitudinal variation of clouds’ structure responsible for Venus’ cold collar, Icarus, 314:1-11, 2018. [4] The Mars Climate Database http://www-mars.lmd.jussieu.fr [5] Y. J. Lee et al., Long-term variations of Venus’ 365-nm albedo observed by Venus Express, Akatsuki, MESSENGER, and Hubble Space Telescope, Astron. J., 158:126, 2019.
Published: 2021

36. Pre-flight Calibration and Near-Earth Commissioning Results of the Mercury Plasma Particle Experiment (MPPE) Onboard MMO (Mio)

Author: Jean-Jacques Berthelier, Henning Fischer, Mathieu Petiot, Kazushi Asamura, Eric Le Comte, Zdenĕk Nĕmec̆ek, Andrei Fedorov, Giuseppe Consolini, Yoichi Kazama, Haruhisa Matsumoto, Yoshizumi Miyoshi, Christian Mazelle, Kanako Seki, Jean Rouzaud, Christophe Verdeil, Dominique Delcourt, Wataru Miyake, Harald Michalik, F. Leblanc, Björn Fiethe, Ulrich Bührke, Roberto Bruno, Peter Wurz, Iannis Dandouras, Alain Barthe, Henry-Claude Séran, Jean-André Sauvaud, Maria Federica Marcucci, Mats Holmström, Stas Barabash, Shoichiro Yokota, H. Andersson, Joachim Woch, Masahiro Hoshino, Iku Shinohara, Philippe Louarn, Benoit Lavraud, Dominique Fontaine, Vincent Génot, Alexandre Cadu, Yuki Harada, Christian Jacquey, Anne-Marie Frezoul, Andrew J. Coates, Bruno Katra, Yoshifumi Futaana, Emmanuel Penou, Stefan Karlsson, Jean-Marie Illiano, Markus Fraenz, Claude Aoustin, Qiugang Zong, Catherine Garat, Qiu-Mei Lee, Wing-Huen Ip, Manabu Shimoyama, Masaki N. Nishino, David Moirin, Norbert Krupp, Nicolas André, Masaki Fujimoto, Mitsuo Oka, Hiroshi Hasegawa, Martin Wieser, Guy Peyre, Jana Safrankova, Jean-Louis Médale, Kunihiro Keika, Jean-Denis Techer, Takeshi Takashima, T. Yanagimachi, Naoki Terada, Takefumi Mitani, Masafumi Hirahara, Yoshifumi Saito, Institute of Space and Astronautical Science (ISAS), Japan Aerospace Exploration Agency [Sagamihara] (JAXA), Laboratoire de Physique des Plasmas (LPP), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École polytechnique (X)-Sorbonne Université (SU)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), Institute for Space-Earth Environmental Research [Nagoya] (ISEE), Nagoya University, Swedish Institute of Space Physics [Kiruna] (IRF), 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), Osaka University [Osaka], Space Sciences Laboratory [Berkeley] (SSL), University of California [Berkeley] (UC Berkeley), University of California (UC)-University of California (UC), Kyoto University, AKKA Technologies, Institut Supérieur de l'Aéronautique et de l'Espace (ISAE-SUPAERO), Société MICROTEC, Nexeya Conseil & Formation, COMAT, Faculty of Mathematics and Physics [Charles University of Praha], Charles University [Prague] (CU), Istituto di Astrofisica e Planetologia Spaziali - INAF (IAPS), Istituto Nazionale di Astrofisica (INAF), Tokai University, The University of Tokyo (UTokyo), Mullard Space Science Laboratory (MSSL), University College of London [London] (UCL), HELIOS - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), 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), Max-Planck-Institut für Sonnensystemforschung = Max Planck Institute for Solar System Research (MPS), Max-Planck-Gesellschaft, Institute of Computer and Network Engineering [Braunschweig] (IDA), Technische Universität Braunschweig = Technical University of Braunschweig [Braunschweig], Japan Aerospace Exploration Agency [Tsukuba] (JAXA), Rikkyo University [Tokyo], Peking University [Beijing], University of Bern, Academia Sinica Institute of Astronomy and Astrophysics (ASIAA), Academia Sinica, National Central University [Taiwan] (NCU), Tohoku University [Sendai], Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), University of California [Berkeley], University of California-University of California, Kyoto University [Kyoto], 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), and Max-Planck-Institut für Sonnensystemforschung (MPS)
Subjects: Spectrum analyzer, High energy particle, 010504 meteorology & atmospheric sciences, [PHYS.ASTR.EP]Physics [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], chemistry.chemical_element, 7. Clean energy, 01 natural sciences, law.invention, Orbiter, law, 0103 physical sciences, Calibration, Aerospace engineering, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, [PHYS]Physics [physics], Energetic neutral atom, Spacecraft, business.industry, Astronomy and Astrophysics, Mercury (element), Solar wind, chemistry, 13. Climate action, Space and Planetary Science, [SDU]Sciences of the Universe [physics], Environmental science, business, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract: International audience; BepiColombo Mio (previously called MMO: Mercury Magnetospheric Orbiter) was successfully launched by Ariane 5 from Kourou, French Guiana on October 20, 2018. The Mercury Plasma/Particle Experiment (MPPE) is a comprehensive instrument package onboard Mio spacecraft used for plasma, high-energy particle and energetic neutral atom measurements. It consists of seven sensors including two Mercury Electron Analyzers (MEA1 and MEA2), Mercury Ion Analyzer (MIA), Mass Spectrum Analyzer (MSA), High Energy Particle instrument for electron (HEP-ele), High Energy Particle instrument for ion (HEP-ion), and Energetic Neutrals Analyzer (ENA). Significant efforts were made pre-flight to calibrate all of the MPPE sensors at the appropriate facilities on the ground. High voltage commissioning of MPPE analyzers was successfully performed between June and August 2019 and in February 2020 following the completion of the low voltage commissioning in November 2018. Although all of the MPPE analyzers are now ready to begin observation, the full service performance has been delayed until Mio’s arrival at Mercury. Most of the fields of view (FOVs) of the MPPE analyzers are blocked by the thermal shield surrounding the Mio spacecraft during the cruising phase. Together with other instruments on Mio including Magnetic Field Investigation (MGF) and Plasma Wave Investigation (PWI) that measure plasma field parameters, MPPE will contribute to the comprehensive understanding of the plasma environment around Mercury when BepiColombo/Mio begins observation after arriving at the planet Mercury in December 2025.
Published: 2021

37. Comparing A Heliospheric SWCX Model's Predictions To HaloSat Observations

Author: Ringuette, R., Koutroumpa, Dimitra, Kuntz, Kip D., Kaaret, P., Jahoda, K., Larocca, D., Kounkel, M., Richardson, Jacob, Zajczyk, A., Bluem, J., NASA Goddard Space Flight Center (GSFC), 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), Johns Hopkins University (JHU), Department of Physics and Astronomy [Iowa City], University of Iowa [Iowa City], Pennsylvania State University (Penn State), Penn State System, Western Washington University (WWU), and Koutroumpa, Dimitra
Subjects: [SDU] Sciences of the Universe [physics], [PHYS]Physics [physics], [SDU]Sciences of the Universe [physics], ComputingMilieux_MISCELLANEOUS, [PHYS] Physics [physics]
Abstract: International audience
Published: 2021

38. Volatiles and Refractories in Surface-Bounded Exospheres in the Inner Solar System

Author: Alexey A. Berezhnoy, Rosemary M. Killen, Jasper Halekas, B. D. Teolis, Cesare Grava, Masaki N. Nishino, Jim M. Raines, Mehdi Benna, Christina Plainaki, Audrey Vorburger, François Leblanc, Ronald J. Vervack, Menelaos Sarantos, Orenthal J. Tucker, Southwest Research Institute [San Antonio] (SwRI), NASA Goddard Space Flight Center (GSFC), University of Maryland [Baltimore], Sternberg Astronomical Institute [Moscow], Lomonosov Moscow State University (MSU), Institute of Physics [Kazan] (IoP), Kazan Federal University (KFU), Department of Physics and Astronomy [Iowa City], University of Iowa [Iowa City], 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), Institute of Space and Astronautical Science (ISAS), Japan Aerospace Exploration Agency [Sagamihara] (JAXA), Italian Space Agency, Department of Climate and Space Sciences and Engineering (CLaSP), University of Michigan [Ann Arbor], University of Michigan System-University of Michigan System, Johns Hopkins University Applied Physics Laboratory [Laurel, MD] (APL), Physikalisches Institut [Bern], Universität Bern [Bern], and Open Access funding provided by Universität Bern. Grava was supported by LRO, funded by NASA through contract NNG05EC87C. Berezhnoy was supported by RFBR grant No. 18-03-00726. Halekas was supported by SSERVI and NASA grant 80NSSC20K0311. Raines was supported by the NASA Discovery Data Analysis Program, grants NNX15AL01G and 80NSSC19K0204. Vervack was supported by NASA grant 80NSSC18K0857 (subcontract to JH-APL).
Subjects: Volatiles, Solar System, Materials science, 010504 meteorology & atmospheric sciences, Solar wind, chemistry.chemical_element, 01 natural sciences, Article, Astrobiology, Physics::Geophysics, Neon, Neutrals, 0103 physical sciences, Physics::Atomic and Molecular Clusters, Moon, 010303 astronomy & astrophysics, Helium, 0105 earth and related environmental sciences, Ions, Argon, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Refractories, Noble gas, Astronomy and Astrophysics, Mercury, Planetary science, chemistry, 13. Climate action, Space and Planetary Science, Magnetosphere, Physics::Space Physics, Astrophysics::Earth and Planetary Astrophysics, Exosphere
Abstract: Volatiles and refractories represent the two end-members in the volatility range of species in any surface-bounded exosphere. Volatiles include elements that do not interact strongly with the surface, such as neon (detected on the Moon) and helium (detected both on the Moon and at Mercury), but also argon, a noble gas (detected on the Moon) that surprisingly adsorbs at the cold lunar nighttime surface. Refractories include species such as calcium, magnesium, iron, and aluminum, all of which have very strong bonds with the lunar surface and thus need energetic processes to be ejected into the exosphere. Here we focus on the properties of species that have been detected in the exospheres of inner Solar System bodies, specifically the Moon and Mercury, and how they provide important information to understand source and loss processes of these exospheres, as well as their dependence on variations in external drivers.
Published: 2021

39. Influence of Extreme Ultraviolet Irradiance Variations on the Precipitating Ion Flux From MAVEN Observations

Author: Janet G. Luhmann, Yaxue Dong, Ludivine Leclercq, Shannon Curry, François Leblanc, Ronan Modolo, Dmitri Titov, Francis G. Eparvier, Antoine Martinez, Jasper Halekas, J. P. McFadden, Robert Lillis, Takuya Hara, Olivier Witasse, Bruce M. Jakosky, Jean-Yves Chaufray, 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), Research and Scientific Support Department, ESTEC (RSSD), European Space Research and Technology Centre (ESTEC), European Space Agency (ESA)-European Space Agency (ESA), Laboratory for Atmospheric and Space Physics [Boulder] (LASP), University of Colorado [Boulder], Space Sciences Laboratory [Berkeley] (SSL), University of California [Berkeley], University of California-University of California, Department of Physics and Astronomy [Iowa City], University of Iowa [Iowa City], Department of Materials Science and Engineering [Charlottesville] (MS), University of Virginia [Charlottesville], and European Space Agency (ESA)
Subjects: Materials science, 010504 meteorology & atmospheric sciences, Astrophysics::High Energy Astrophysical Phenomena, Extreme ultraviolet lithography, Irradiance, Atmosphere of Mars, Astrophysics, 010502 geochemistry & geophysics, 7. Clean energy, 01 natural sciences, Ion, Atmosphere, Solar wind, Geophysics, [SDU]Sciences of the Universe [physics], 13. Climate action, Sputtering, Extreme ultraviolet, Physics::Space Physics, Astrophysics::Solar and Stellar Astrophysics, General Earth and Planetary Sciences, Astrophysics::Earth and Planetary Astrophysics, Physics::Atmospheric and Oceanic Physics, 0105 earth and related environmental sciences
Abstract: International audience; We study the influence of the solar extreme ultraviolet (EUV) flux intensity on the precipitating ion fluxes as seen by the Solar Wind Ion Analyzer, an energy and angular ion spectrometer aboard the Mars Atmosphere and Volatile EvolutioN (MAVEN) spacecraft. We defined three periods with significantly different EUV flux intensity (1.6 and 3.2 times the lowest EUV intensity) and compare the precipitating ion flux measured by MAVEN/Solar Wind Ion Analyzer during each period. At low energy [30–650] eV, we find that the median (average) precipitating ion flux during the medium and low EUV periods are, respectively, 1.7 (2.1) and 3 (3.5) times more intense than the flux during the high EUV period. At high energy [650–25,000] eV, a similar trend in the intensity of the precipitating ion flux is observed but with an increase by 50% (46%) and 70% (79%), respectively. A larger EUV flux does therefore not seem to favor heavy ion precipitation into Mars's atmosphere, contrary to modeling prediction and overall expectations.
Published: 2019

40. Origin of the Extended Mars Radar Blackout of September 2017

Author: Hermann Opgenoorth, François Leblanc, Nicolas Floury, Andrea Cicchetti, Robert Lillis, Mark Lester, Roberto Orosei, Pierre-Louis Blelly, John M. C. Plane, Andrew Kopf, Philip Conroy, M. Cartacci, Beatriz Sánchez-Cano, Olivier Witasse, Raffaella Noschese, Stephen E. Milan, Radio and Space Plasma Physics Group [Leicester] (RSPP), University of Leicester, 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), European Space Research and Technology Centre (ESTEC), European Space Agency (ESA), Istituto di Astrofisica e Planetologia Spaziali - INAF (IAPS), Istituto Nazionale di Astrofisica (INAF), Istituto di Radioastronomia [Bologna] (IRA), Department of Physics [Umeå], Umeå University, Space Sciences Laboratory [Berkeley] (SSL), University of California [Berkeley], University of California-University of California, 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), School of Chemistry [Leeds], University of Leeds, Department of Physics and Astronomy [Iowa City], University of Iowa [Iowa City], ITA, USA, GBR, FRA, 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), Agence Spatiale Européenne = European Space Agency (ESA), University of California [Berkeley] (UC Berkeley), University of California (UC)-University of California (UC), and 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)
Subjects: [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010504 meteorology & atmospheric sciences, Meteorology, Solar energetic particles, MARSIS, Mars Exploration Program, Atmosphere of Mars, Space weather, Fusion, Plasma and Space Physics, 01 natural sciences, law.invention, Fusion, plasma och rymdfysik, Orbiter, Geophysics, 13. Climate action, Space and Planetary Science, law, Environmental science, Ionosphere, Radar, 0105 earth and related environmental sciences
Abstract: The Mars Advanced Radar for Subsurface and Ionosphere Sounding (MARSIS) onboard Mars Express, which operates between 0.1 and 5.5 MHz, suffered from a complete blackout for 10 days in September 2017 when observing on the nightside (a rare occurrence). Moreover, the Shallow Radar (SHARAD) onboard the Mars Reconnaissance Orbiter, which operates at 20 MHz, also suffered a blackout for three days when operating on both dayside and nightside. We propose that these blackouts are caused by solar energetic particles of few tens of keV and above associated with an extreme space weather event between 10 and 22 September 2017, as recorded by the Mars Atmosphere and Volatile EvolutioN (MAVEN) mission. Numerical simulations of energetic electron precipitation predict that a lower O-2(+) nighttime ionospheric layer of magnitude similar to 10(10) m(-3) peaking at similar to 90-km altitude is produced. Consequently, such a layer would absorb radar signals at high frequencies and explain the blackouts. The peak absorption level is found to be at 70-km altitude. Plain Language Summary Several instrument operations, as well as communication systems with rovers at the surface, depend on radio signals that propagate throughout the atmosphere of Mars. This is the case also for two radars that are currently working in Mars' orbit, sounding the ionosphere, surface, and subsurface of the planet. In mid-September 2017, a powerful solar storm hit Mars, producing a large amount of energetic particle precipitation over a 10-day period. We have found that high-energy electrons ionized the atmosphere of Mars, creating a dense layer of ions and electrons at similar to 90 km on the Martian nightside. This layer attenuated radar signals continuously for 10 days, stopping the radars to receive any signal from the planetary surface. In this work, we assess the properties of this layer in order to understand the implications of this kind of phenomenon for radar performance and communications.
Published: 2019

41. Global Distribution of the Solar Wind Flux and Velocity From SOHO/SWAN During SC‐23 and SC‐24

Author: Dimitra Koutroumpa, Eric Quémerais, Walter Schmidt, Stéphane Ferron, 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), Analytic and Computational Research, Inc. - Earth Sciences (ACRI-ST), and Finnish Meteorological Institute (FMI)
Subjects: Solar minimum, Physics, 010504 meteorology & atmospheric sciences, [SDU.ASTR.SR]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], Flux, Energy flux, 010502 geochemistry & geophysics, Atmospheric sciences, Solar maximum, 7. Clean energy, 01 natural sciences, Solar wind, Geophysics, Interplanetary scintillation, 13. Climate action, Physics::Space Physics, Astrophysics::Solar and Stellar Astrophysics, General Earth and Planetary Sciences, Astrophysics::Earth and Planetary Astrophysics, Interplanetary spaceflight, Heliosphere, 0105 earth and related environmental sciences
Abstract: International audience; We analyze SOHO/SWAN hydrogen Lyman‐α data collected between 1996 and 2018 to derive the solar wind latitudinal distribution over time. Full‐sky interplanetary Lyman‐α maps are inverted to derive the total hydrogen ionization rate latitude profiles, normalized to proton charge‐exchange and photoionization. Using Interplanetary Scintillation (IPS) velocities to calculate the velocity‐dependent charge‐exchange cross‐sections, we produce the solar wind flux latitudinal profiles. Finally, we compute solar wind velocity latitude profiles, based on the dynamic pressure and energy flux conservation (calculated from OMNI data) over latitude. SWAN reproduces the IPS velocity profiles up to at least ±60°, and also agrees with Ulysses in‐situ measurements for solar minimum periods in 1996‐1997 and 2007. During solar maximum, discrepancies are more frequent because in‐situ data reflect local solar wind conditions, while SWAN data reflect global conditions in the heliosphere.
Published: 2019

42. Variability of Precipitating Ion Fluxes During the September 2017 Event at Mars

Author: Jasper Halekas, Takuya Hara, Ronan Modolo, O. Witasse, Antoine Martinez, J. P. McFadden, Norberto Romanelli, Francis G. Eparvier, Mats Holmström, Robert Lillis, Y. J. Ma, Shannon Curry, Janet G. Luhmann, François Leblanc, Jean-Yves Chaufray, Bruce M. Jakosky, John E. P. Connerney, Davin Larson, 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), Space Sciences Laboratory [Berkeley] (SSL), University of California [Berkeley], University of California-University of California, Department of Physics and Astronomy [Iowa City], University of Iowa [Iowa City], Laboratory for Atmospheric and Space Physics [Boulder] (LASP), University of Colorado [Boulder], NASA Goddard Space Flight Center (GSFC), Imaging Sciences and Biomedical Engineering Division [London], Guy's and St Thomas' Hospital [London]-King‘s College London, Department of Earth, Planetary and Space Sciences [Los Angeles] (EPSS), University of California [Los Angeles] (UCLA), Swedish Institute of Space Physics [Uppsala] (IRF), European Space Research and Technology Centre (ESTEC), and European Space Agency (ESA)
Subjects: [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010504 meteorology & atmospheric sciences, Spectrometer, Astrophysics::High Energy Astrophysical Phenomena, Magnetosphere, Mars Exploration Program, Space weather, Atmospheric sciences, 01 natural sciences, [PHYS.PHYS.PHYS-SPACE-PH]Physics [physics]/Physics [physics]/Space Physics [physics.space-ph], Atmosphere, Solar wind, Geophysics, 13. Climate action, Space and Planetary Science, Physics::Space Physics, Coronal mass ejection, Astrophysics::Solar and Stellar Astrophysics, Environmental science, Dynamic pressure, Astrophysics::Earth and Planetary Astrophysics, Physics::Atmospheric and Oceanic Physics, 0105 earth and related environmental sciences
Abstract: International audience; In this work, we study the influence of the September 2017 solar event on the precipitating heavy ion fluxes towards Mars' atmosphere as seen by MAVEN/SWIA, an energy and angular ion spectrometer and by MAVEN/STATIC, an energy, mass and angular ion spectrometer. After a careful reconstruction of the background induced by the Solar Energetic Particle (SEP) event in the MAVEN/SWIA spectrometer, we investigate the precipitating ion flux responses to the space weather events that took place in September 2017. This period is a unique opportunity to analyze the respective role of various possible drivers of heavy ion precipitation into Mars’ atmosphere with a wide range of different space weather events occurring during the same month. This study shows an increase in the precipitation flux by more than one order of magnitude during the arrival of the September Interplanetary Coronal Mass Ejection (ICME) compared to the average flux during quiet solar conditions. We also showed that among the possible solar drivers, the solar wind dynamic pressure is the most significant during September 2017.
Published: 2019

43. A survey of water production in 61 comets from SOHO/SWAN observations of hydrogen Lyman-alpha: Twenty-one years 1996–2016

Author: T. Mäkinen, Michael R. Combi, Eric Quémerais, Stéphane Ferron, Jean-Loup Bertaux, Department of Climate and Space Sciences and Engineering (CLaSP), University of Michigan [Ann Arbor], University of Michigan System-University of Michigan System, Finnish Meteorological Institute (FMI), HELIOS - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), 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), Analytic and Computational Research, Inc. - Earth Sciences (ACRI-ST), and 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)
Subjects: 010504 meteorology & atmospheric sciences, Hydrogen, Ices, Comet, FOS: Physical sciences, chemistry.chemical_element, coma, Ultraviolet observations, 01 natural sciences, Article, Observatory, 0103 physical sciences, Comets, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, Earth and Planetary Astrophysics (astro-ph.EP), Physics, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Astronomy, Astronomy and Astrophysics, Radius, Alpha (navigation), Solar wind, Orbit, chemistry, 13. Climate action, Space and Planetary Science, Satellite, Astrophysics - Earth and Planetary Astrophysics
Abstract: The Solar Wind Anisotropies (SWAN) instrument on the SOlar and Heliospheric Observatory (SOHO) satellite has observed 44 long period and new Oort cloud comets and 36 apparitions of 17 short period comets since its launch in December 1995. Water production rates have been determined from the over 3700 images producing a consistent set of activity variations over large parts of each comet's orbit. This has enabled the calculation of exponential power-law variations with heliocentric distance of these comets both before and after perihelion, as well as the absolute values of the water production rates. These various measures of overall water activity including pre- and post-perihelion exponents, absolute water production rates at 1 AU, active surface areas and their variations have been compared with a number of dynamical quantities for each comet including dynamical class, original semi-major axis, nucleus radius (when available), and compositional taxonomic class. Evidence for evolution of cometary nuclei is seen in both long-period and short-period comets., Comment: 43 pages, 9 figures, 6 tables
Published: 2019

44. The Mass Distribution of Transit Exoplanets from the Mass–Radius Relationships: the Structurization within Planetary Systems

Author: O. Ya. Yakovlev, Inna Shashkova, Jean-Loup Bertaux, V. I. Ananyeva, A. V. Tavrov, A. E. Ivanova, Andrey Yudaev, Space Research Institute of the Russian Academy of Sciences (IKI), Russian Academy of Sciences [Moscow] (RAS), Moscow Institute of Physics and Technology [Moscow] (MIPT), HELIOS - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), and 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)
Subjects: Physics, 010504 meteorology & atmospheric sciences, Mass distribution, mass distribution, mass–radius relationship, Astronomy and Astrophysics, Radius, Astrophysics, Planetary system, 01 natural sciences, Power law, Exoplanet, Radial velocity, Spitzer Space Telescope, exoplanets, statistical analysis, Space and Planetary Science, Planet, transit method, [SDU]Sciences of the Universe [physics], 0103 physical sciences, Astrophysics::Earth and Planetary Astrophysics, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences
Abstract: International audience; Most transit exoplanets (85%) were discovered with the Kepler space telescope. However, the mass, which was measured mainly with the radial velocity method, is known only for ~15% of them. The mass of an exoplanet may be estimated by its radius from the statistical dependences based on the observational data, though no unambiguous interrelation between the mass and the radius of planets exists. Here, we calculate the earlier unknown masses of exoplanets from four statistical mass–radius relationships (Bashi et al., 2017; Chen and Kipping, 2017; Ning et al., 2018, and the averaged dependence derived) and added the results to the distribution of planets with known masses. The mass distributions of transit exoplanets obtained in this way are analyzed with taking into account the observational selection effect inherent in the transit method. The distributions are approximated by the power law ∂N/∂M ~ Mα, where the exponent (α < 0) is determined by the maximum likelihood estimation for the samplings acquired with four mass–radius relationships: α = –2.12 ± 0.03, –2.09 ± 0.03, –1.94 ± 0.03, and –2.27 ± 0.04. Moreover, for one of these distributions, we determine the parameters of the power law, the exponent of which differs on three intervals (with the boundaries at 0.025, 0.28, and 1.34 Jupiter masses): –1.99, –0.62, and –2.88. We also conclude that there is no evidence of the interrelation between the mass of an exoplanet and its average distance to the host star (the structurization within planetary systems), if this distance is smaller than 1 AU; besides, the dependence of the exponent α on the considered mass interval is analyzed. The above estimates appertain to exoplanets detected by the space telescopes: Kepler Space Telescope and Transiting Exoplanet Survey Satellite (TESS) (these exoplanets compose group 1). The masses of the other transit exoplanets, which were detected by ground-based instruments, were known (they compose group 2). For the latter group, the exponent α is estimated at –2.21 ± 0.04. In general, the results of our analysis agree with those of the earlier statistical and theoretic studies. A key idea of the present paper is to apply the model interrelations between the mass and the radius of exoplanets to the analysis of the mass distribution of exoplanets on the basis of the recent data of observations.
Published: 2021

45. Evolution of solar wind flows from the inner corona to 1 AU: constraints provided by SOHO UVCS and SWAN data

Author: Eric Quémerais, Vladislav Izmodenov, Dimitra Koutroumpa, Olga Katushkina, Alessandro Bemporad, INAF - Osservatorio Astrofisico di Torino (OATo), Istituto Nazionale di Astrofisica (INAF), Space Research Institute of the Russian Academy of Sciences (IKI), Russian Academy of Sciences [Moscow] (RAS), HELIOS - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), and 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)
Subjects: Physics, Mass flux, [PHYS]Physics [physics], Brightness, Astrophysics::High Energy Astrophysical Phenomena, Astrophysics, 7. Clean energy, Corona, law.invention, Interstellar medium, Orbiter, Solar wind, 13. Climate action, law, [SDU]Sciences of the Universe [physics], Physics::Space Physics, Solar rotation, Astrophysics::Solar and Stellar Astrophysics, Heliosphere
Abstract: The Sun modulates with the solar wind flow the shape of the whole Heliosphere interacting with the surrounding interstellar medium. Recent results from IBEX and INCA experiments, as well as recent measurements from Voyager 1 and 2, demonstrated that this interaction is much more complex and subject to temporal and heliolatitudinal variations than previously thought. These variations could be also related with the evolution of solar wind during its journey through the Heliosphere. Hence, understanding how the solar wind evolves from its acceleration region in the inner corona to the Heliospheric boundaries is very important.In this work, SWAN Lyman-α full-sky observations from SOHO are combined for the very first time with measurements acquired in the inner corona by SOHO UVCS and LASCO instruments, to trace the solar wind expansion from the Sun to 1 AU. The solar wind mass flux in the inner corona was derived over one full solar rotation period in 1997, based on LASCO polarized brightness measurements, and on the Doppler dimming technique applied to UVCS Lyman-α emission from neutral H coronal atoms due to resonant scattering of chromospheric radiation. On the other hand, the SWAN Lyman-α emission (due to back-scattering from neutral H atoms in the interstellar medium) was analyzed based on numerical models of the interstellar hydrogen distribution in the heliosphere and the radiation transfer. The SWAN full-sky Lyman-α intensity maps are used for solving of the inverse problem and deriving of the solar wind mass flux at 1 AU from the Sun as a function of heliolatitude. First results from this comparison for a chosen time period in 1997 are described here, and possible future applications for Solar Orbiter data are discussed.
Published: 2021

46. Density, Energy and Phase Space Density Distribution of Planetary Ions He+, O+ and Na+ in Mercury's Magnetosphere

Author: Jim M. Raines, François Leblanc, A. L. Elisabeth Werner, Ronan Modolo, W. Exner, Sae Aizawa, Jean-Yves Chaufray, Uwe Motschmann, 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), 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), Department of Climate and Space Sciences and Engineering (CLaSP), University of Michigan [Ann Arbor], University of Michigan System-University of Michigan System, Institut für Geophysik und Extraterrestrische Physik [Braunschweig] (IGEP), Technische Universität Braunschweig = Technical University of Braunschweig [Braunschweig], Institut für Theoretische Physik [Braunschweig], Deutsches Zentrum für Luft- und Raumfahrt [Berlin] (DLR), 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), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), and Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS)
Subjects: Physics, chemistry.chemical_element, Magnetosphere, 7. Clean energy, Ion, Mercury (element), chemistry, Density distribution, 13. Climate action, [SDU]Sciences of the Universe [physics], Phase space, Physics::Space Physics, Astrophysics::Earth and Planetary Astrophysics, Atomic physics, Energy (signal processing)
Abstract: The Mercury plasma environment is enriched in planetary ions from the tenuous neutral exosphere. We have developed a test-particle model which describes the full equation of motion for planetary ions produced from photo-ionization of the neutral exosphere. The new test-particle model is coupled to a Monte Carlo test-particle model of the neutral exosphere (Exospheric Global Model; EGM; Leblanc et al. 2017) and two hybrid-kinetic models: LatHyS (Modolo et al. 2016) and AIKEF (Müller et al. 2011). This coupling will allow us to consider the impact of non-adiabatic energization on the ion density distribution as well as the connection to seasonal asymmetries in the neutral exosphere.We compare the density, energy and phase space density distribution of He+, O+ and Na+ from our model with observations from the MErcury Surface, Space ENvironment, GEochemistry, and Ranging (MESSENGER) time-of-flight spectrometer Fast Imaging Plasma Spectrometer (FIPS; Raines et al. 2013). Our results indicate the presence of several interesting high-density structures both inside and outside FIPS observable energy range (E = 0.05 -13 keV), the properties of which are likely very sensitive to the upstream solar wind conditions. We present how these results may aid the interpretation of FIPS data and future measurements by BepiColombo.
Published: 2021

47. Response of the interplanetary hydrogen population to global changes of solar activity: a quantitative analysis based on SOHO/SWAN and SOHO/LASCO-C2 data comparison

Author: Philippe Lamy, Stéphane Ferron, Dimitra Koutroumpa, Lucile Conan, Hugo Gilardy, Eric Quémerais, 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), École Supérieure des Techniques Aéronautiques et de Construction Automobile (ESTACA), Analytic and Computational Research, Inc. - Earth Sciences (ACRI-ST), and 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)
Subjects: Physics, [PHYS]Physics [physics], Electron density, education.field_of_study, Hydrogen, Population, Phase (waves), chemistry.chemical_element, Astrophysics, 7. Clean energy, Solar wind, chemistry, 13. Climate action, [SDU]Sciences of the Universe [physics], Ionization, Physics::Space Physics, Astrophysics::Solar and Stellar Astrophysics, education, Interplanetary spaceflight, Heliosphere
Abstract: For more than two decades the SOHO/SWAN instrument has been monitoring the full-sky hydrogen backscattered Lyman-α emission, and the derived three-dimensional solar wind proton flux. We present a comparison of the time series of the latitude-integrated hydrogen ionization rates (β) derived from the inversion of the SWAN full-sky maps with the integrated coronal electron density derived from the inversion of SOHO/LASCO-C2 white light images. The analysis shows a variable time lag of the SWAN β of a few Carrington rotations, correlated with the solar cycle phase (larger delay during solar maxima compared to minima). This is a direct consequence of the variation of the size of the hydrogen ionization cavity and the time it takes for hydrogen atoms to propagate in the inner heliosphere. This effect should be taken into account in studies of the interstellar neutral populations in interplanetary space.
Published: 2021

48. The UVSQ-SAT/INSPIRESat-5 CubeSat Mission: First In-Orbit Measurements of the Earth’s Outgoing Radiation

Author: Christophe Mercier, Alain Hauchecorne, Alain Sarkissian, Philippe Keckhut, Fabrice Boust, Emmanuel Bertran, Luc Damé, Pierre Gilbert, Patrick H. M. Galopeau, André-Jean Vieau, Antoine Mangin, Michel Mahé, Adrien Finance, Xavier Arrateig, Mustapha Meftah, Christophe Dufour, Nicolas Caignard, Jean-Luc Engler, Sadok Abbaki, Jean-Paul Carta, Thomas Boutéraon, Laurent Lapauw, Odile Fanton d'Andon, Slimane Bekki, Patrick Lacroix, STRATO - 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), 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), Analytic and Computational Research, Inc. - Earth Sciences (ACRI-ST), HELIOS - LATMOS, Carta-Rouxel, DEMR, ONERA, Université Paris Saclay [Palaiseau], ONERA-Université Paris-Saclay, Radio-club de Saint-Quentin-en-Yvelines F6KRK, AMSAT-Francophone, and CNRSUVSQANRPNSTCNESCEA
Subjects: Engineering, 010504 meteorology & atmospheric sciences, Science, nanosatellite, 0211 other engineering and technologies, earth radiation budget, 02 engineering and technology, Astrophysics::Cosmology and Extragalactic Astrophysics, Radiation, 01 natural sciences, Radiation budget, Astrophysics::Solar and Stellar Astrophysics, CubeSat, Aerospace engineering, 021101 geological & geomatics engineering, 0105 earth and related environmental sciences, [PHYS.PHYS.PHYS-AO-PH]Physics [physics]/Physics [physics]/Atmospheric and Oceanic Physics [physics.ao-ph], business.industry, IPCC, climate observation and monitoring, [SDU.ASTR.IM]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], Pathfinder, [SDU.STU.CL]Sciences of the Universe [physics]/Earth Sciences/Climatology, Orbit (dynamics), General Earth and Planetary Sciences, Outgoing longwave radiation, Satellite, Launch vehicle, business
Abstract: International audience; UltraViolet & infrared Sensors at high Quantum efficiency onboard a small SATellite (UVSQ- SAT) is a small satellite at the CubeSat standard, whose development began as one of the missions in the International Satellite Program in Research and Education (INSPIRE) consortium in 2017. UVSQ- SAT is an educational, technological and scientific pathfinder CubeSat mission dedicated to the observation of the Earth and the Sun. It was imagined, designed, produced and tested by LATMOS in collaboration with its academic and industrial partners, and the French-speaking radioamateur community. About the size of a Rubik’s Cube and weighing about 2 kg, this satellite was put in orbit in January 2021 by the SpaceX Falcon 9 launch vehicle. After briefly introducing the UVSQ-SAT mission, this paper will present the importance of measuring the Earth’s radiation budget and its energy imbalance and the scientific objectives related to its various components. Finally, the first in-orbit observations will be shown (maps of the solar radiation reflected by the Earth and of the outgoing longwave radiation at the top of the atmosphere during February 2021). UVSQ-SAT is one of the few CubeSats worldwide with a scientific goal related to climate studies. It represents a research in remote sensing technologies for Climate observation and monitoring.
Published: 2021
Full Text: View/download PDF

49. The Venus Climate Database

Author: Franck Montmessin, Aymeric Spiga, Sébastien Lebonnois, Ehouarn Millour, Jean-Yves Chaufray, Antoine Martinez, Fabrice Cipriani, Thomas Pierron, 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), 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), PLANETO - LATMOS, European Space Research and Technology Centre (ESTEC), and European Space Agency (ESA)
Subjects: biology, 13. Climate action, [SDU]Sciences of the Universe [physics], Climatology, Venus, biology.organism_classification, Geology
Abstract: We have over the years developed a state of the art Venus Global Climate Model (GCM, Lebonnois et al. 2016; Gilli et al. 2017; Garate-Lopez & Lebonnois 2018). With funding from ESA in the context of the preparation of the possible upcoming EnVision mission, we have, in the footsteps of what has been done for Mars with the Mars Climate Database (), built a Venus Climate Database (VCD) based on GCM outputs.The VCD dataset and software overall enable users to:- extract atmospheric quantities (temperature, pressure, winds, density, …) from the surface to the exobase (~250km) over a climatological Venusian day.- to better bracket reality, several scenarios are provided, in order to reflect the possible range of solar activity (Extreme UV input from the Sun) which strongly affects the thermosphere (above ~150km), as well as a realistic range of UV albedo cloud top.- in addition to a baseline climatology, the VCD software provides statistics (internal short term and day-to-day variability) along with means to add perturbations to represent Venusian weather.At EGU we will present the VCD and its features, emphasizing how it can be useful for scientific users wanting to compare with their models or analyze observations, and for engineers planning future missions.
Published: 2021

50. Ray paths of VLF/LF transmitter radio signals in the seismic Adriatic regions

Author: A. Ermini, Patrick H. M. Galopeau, Konstantinos Katzis, Michael E. Contadakis, Pier Francesco Biagi, Mourad Bezzeghoud, Özer Aydogar, Konrad Schwingenschuh, Giovanni Nico, Iren Adelina Moldovan, Aleksandra Nina, Helmut Lammer, Maria Solovieva, Hans Eichelberger, Bruno P. Besser, Mohammed Y. Boudjada, Institut für Weltraumforschung [Graz] (IWF), Osterreichische Akademie der Wissenschaften (ÖAW), Department of Physics [Bari], Università degli studi di Bari Aldo Moro (UNIBA), Istituto per le Applicazioni del Calcolo [Bari] (IAC), Consiglio Nazionale delle Ricerche (CNR), Schmidt United Institute of Physics of the Earth [Moscow] (IPE), Russian Academy of Sciences [Moscow] (RAS), Dipartimento di Ingegneria Industriale [Roma], Università degli Studi di Roma Tor Vergata [Roma], National Institute for Earth Physics [Bucharest] (NIEP), Department of Geodesy and Surveying [Thessaloniki], Aristotle University of Thessaloniki, Institute of Physics [Belgrade], University of Belgrade [Belgrade], European University of Cyprus, Centre of Geophysics of Evora (CGE), Universidade de Évora, HELIOS - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), and 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)
Subjects: VLF/LF radio signals, Ray paths, Adriatic region, 13. Climate action, [SDU.STU.GP]Sciences of the Universe [physics]/Earth Sciences/Geophysics [physics.geo-ph], Settore FIS/07, Transmitter, Geology, Seismology
Abstract: We analyze the radio wave propagations of VLF/LF transmitter signals along subionospheric paths using two different reception systems localized in the Graz seismo-electromagnetic facility (15.43E,47.06N). Those systems allow the simultaneous detection of more than fifteen transmitter signals emitting in the northern (i.e. France, Germany and United Kingdom) and southern (i.e. Italy and Turkey) parts of Europe. In this work, we investigate the transmitter radio wave propagations associated with two earthquakes (EQs) which occurred, at two occasions, in nearly the same Croatian regions (Geo. Long.=16°E; Geo. Lat.=45°N). The first and second EQs happened, respectively, on March 22 and December 29, 2020, with magnitudes Mw equal to 5.4 and 6.4. The use of two complementary reception systems, i.e. INFREP (Biagi et al., Open Journal of Earthquake Research, 8, 2019) and UltraMSK (Schwingenschuh et al., Nat. Hazards Earth Syst. Sci., 11, 2011), and the proximity to the epicenters lead us to characterize the behavior of the transmitter signal amplitudes particularly above the Croatian seismic regions. We analyze the amplitude variation for a given transmitter frequency starting few weeks before the earthquakes occurrences. We discuss the observed anomalies in the transmitter signals which may be considered as precursors due to the ionospheric disturbances of the transmitter ray paths above the earthquakes preparation zones.
Published: 2021

Catalog

Books, media, physical & digital resources

See catalog results

Searchworks

Select search scope, currently: Articles Catalog books, media & more in Jio Institute collections Articles journal articles & other e-resources

Search

Search Constraints

Refine your results

Search Limiters

Topic

Publication Year Range

Language

Journal

Database

Publisher

835 results on '"HELIOS - LATMOS"'

Search Results

Catalog

Select search scope, currently: Articles

Catalog

books, media & more in Jio Institute collections

Articles

journal articles & other e-resources