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1. On the Formation of Trapped Electron Radiation Belts at Ganymede

Author

Lucas Liuzzo, Quentin Nénon, Andrew R. Poppe, Aaron Stahl, Sven Simon, and Shahab Fatemi

Subjects
Geophysics. Cosmic physics, QC801-809
Abstract

Abstract This study presents evidence of stably trapped electrons at Jupiter's moon Ganymede. We model energetic electron pitch angle distributions and compare them to observations from the Galileo Energetic Particle Detector to identify signatures of trapped particles during the G28 encounter. We trace electron trajectories to show that they enter Ganymede's mini‐magnetospheric environment, become trapped, and drift around the moon for up to 30 min, in some cases stably orbiting the moon multiple times. Conservation of the first adiabatic invariant partially contributes to energy changes throughout the electrons' orbits, with additional acceleration driven by local electric fields, before they return to Jupiter's magnetosphere or impact the surface. These trapped particles manifest as an electron population with an enhanced flux compared to elsewhere within the mini‐magnetosphere that are detectable by future spacecraft.

Published
2024
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2. Direct evidence of substorm-related impulsive injections of electrons at Mercury

Author

Sae Aizawa, Yuki Harada, Nicolas André, Yoshifumi Saito, Stas Barabash, Dominique Delcourt, Jean-André Sauvaud, Alain Barthe, Andréi Fedorov, Emmanuel Penou, Shoichiro Yokota, Wataru Miyake, Moa Persson, Quentin Nénon, Mathias Rojo, Yoshifumi Futaana, Kazushi Asamura, Manabu Shimoyama, Lina Z. Hadid, Dominique Fontaine, Bruno Katra, Markus Fraenz, Norbert Krupp, Shoya Matsuda, and Go Murakami

Subjects
Science
Abstract

Abstract Mercury’s magnetosphere is known to involve fundamental processes releasing particles and energy like at Earth due to the solar wind interaction. The resulting cycle is however much faster and involves acceleration, transport, loss, and recycling of plasma. Direct experimental evidence for the roles of electrons during this cycle is however missing. Here we show that in-situ plasma observations obtained during BepiColombo’s first Mercury flyby reveal a compressed magnetosphere hosts of quasi-periodic fluctuations, including the original observation of dynamic phenomena in the post-midnight, southern magnetosphere. The energy-time dispersed electron enhancements support the occurrence of substorm-related, multiple, impulsive injections of electrons that ultimately precipitate onto its surface and induce X-ray fluorescence. These observations reveal that electron injections and subsequent energy-dependent drift now observed throughout Solar System is a universal mechanism that generates aurorae despite the differences in structure and dynamics of the planetary magnetospheres.

Published
2023
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4. Relativistic Particle Measurements in Jupiter’s Magnetosphere with Pix.PAN

Author

Johannes Hulsman, Xin Wu, Philipp Azzarello, Benedikt Bergmann, Michael Campbell, George Clark, Franck Cadoux, Tomoya Ilzawa, Peter Kollmann, Xavier Llopart, Quentin Nénon, Mercedes Paniccia, Elias Roussos, Petr Smolyanskiy, Daniil Sukhonos, and Pierre Alexandre Thonet

Abstract

Pix.PAN is a compact cylindrical magnetic spectrometer, intended to provide excellent high energy particle measurements under high rate and hostile operating conditions in space. Its principal design is composed of 2 Halbach-array magnetic sectors and 6 Timepix4-based tracking layers; the latest hybrid silicon pixel detector readout ASIC designed. Due to Pix.PAN's compact and relatively simple design, it has the potential to be used for space missions exploring with measurements of unprecedented precision, high energy particles in radiation belts and the heliophere (solar energetic particles, anomalous and galactic cosmic rays). In this white paper, we discuss the design and expected performance of Pix.PAN for COMPASS (Comprehensive Observations of Magnetospheric Particle Acceleration, Sources, and Sinks), a mission concept submitted to NASA’s Call "B.16 Heliophysics Mission Concept Studies (HMCS)" in 2021 that targets the extreme high energy particle environment of Jupiter's inner radiation belts. We also discuss PixPAN's operational conditions and interface requirements. The conceptual design shows that is possible to achieve an energy resolution of

Published
2023
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5. Io's Effect on Energetic Charged Particles as Seen in Juno Data

Author

Dennis Haggerty, Robert Ebert, Fran Bagenal, Masafumi Imai, Chris Paranicas, Peter Kollmann, Quentin Nénon, Jamey Szalay, George Clark, Norbert Krupp, Joseph Westlake, Elias Roussos, Robert Allen, Scott Bolton, Abigail Rymer, Barry Mauk, and Ali Sulaiman

Subjects
Physics, Geophysics, General Earth and Planetary Sciences, Atomic physics, Charged particle
Published
2019
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6. Open science questions and missing measurements in the radiation belts of Jupiter

Author

Lucas Liuzzo, Drew Turner, Elias Roussos, Andrew R. Poppe, George Clark, Tom Nordheim, Insoo Jun, Barry Mauk, Quentin Nénon, Emma Woodfield, Peter Kollmann, and Yuri Shprits

Subjects
Jupiter, symbols.namesake, Open science, 010308 nuclear & particles physics, Van Allen radiation belt, 0103 physical sciences, symbols, Astronomy, 010303 astronomy & astrophysics, 01 natural sciences, Geology
Published
2021
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7. Recommendations for Addressing Priority Io Science in the Next Decade

Author

Laszlo P. Kestay, Katherine de Kleer, Ariana Echevarria, A. Trinh, Gregor Steinbrügge, Mark P. Panning, Cesare Grava, Audrey Vorburger, Constantine Tsang, Fran Bagenal, Hamish C. F. C. Hay, Gregory A. Neumann, Julie A. Rathbun, Tracy K. P. Gregg, Tanguy Bertrand, Carver J. Bierson, Christopher W. Hamilton, Imke de Pater, Rowan Huang, Krishan K. Khurana, J. I. Moses, John Noonan, James Tuttle Keane, Isamu Matsuyama, Rachel L. Klima, Lea Klaiber, Laurent G. J. Montési, Michael T. Bland, Joseph Westlake, Quentin Nénon, Elias Roussos, Laura Kerber, Rohan Sood, J. T. Keane, Christine McCarthy, Melissa A. McGrath, Sarah M. Hörst, Kandis Lea Jessup, Amanda R. Hendrix, Alfred S. McEwen, C. D. K. Harris, Marc Neveu, Tilmann Denk, Paul M. Schenk, Maurizio Pajola, Xianzhe Jia, Nicholas M. Schneider, Arielle Moullet, Lauren Jozwiak, Daniella DellaGiustina, Alice Lucchetti, Jani Radebaugh, John R. Spencer, Lori M. Feaga, Catherine Elder, Ashley Davies, Patricio Becerra, Rosaly M. C. Lopes, Doris Breuer, Amy C. Barr Mlinar, Michelle R. Kirchoff, Dan C. Spencer, Corbin L. Kling, Andréa C. G. Hughes, Kurt D. Retherford, Francis Nimmo, J. Schools, David A. Williams, Ryan S. Park, Walter S. Kiefer, Walter M. Harris, Edwin S. Kite, Ali Sulaiman, Lynnae C. Quick, Ross A. Beyer, Anne Pommier, James H. Roberts, Sarah S. Sutton, Janet Vertesi, Patricia M. Gregg, Ko Basu, Valery Lainey, Alexandra A. Ahern, and Kathleen Mandt

Subjects
spacecraft, decadal survey, Io, White paper, Galilean satellites
Published
2021
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8. Jupiter's ion radiation belts inward of Europa's orbit

Author

George Clark, Angélica Sicard, Abigail Rymer, Barry Mauk, Henry B. Garrett, Quentin Nénon, Chris Paranicas, Elias Roussos, Peter Kollmann, and Dennis Haggerty

Subjects
Physics, 010504 meteorology & atmospheric sciences, Astronomy, Radiation, 01 natural sciences, Ion, Jupiter, symbols.namesake, Geophysics, Space and Planetary Science, Van Allen radiation belt, Physics::Space Physics, symbols, Astrophysics::Earth and Planetary Astrophysics, Orbit (control theory), 0105 earth and related environmental sciences
Abstract

Jupiter is surrounded by intense and energetic radiation belts, yet most of the available in-situ data, in volume and quality, were taken outside of Europa's orbit, where radiation conditions are n...

Published
2020
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9. Measuring the Earth's Synchrotron Emission from Radiation Belts with a Lunar Near Side Radio Array

Author

J. C. Kasper, Robert J. MacDowall, Alexander M. Hegedus, Daniel N. Baker, Baptiste Cecconi, Angélica Sicard, Antoine Brunet, Quentin Nénon, University of Michigan [Ann Arbor], University of Michigan System, Space Sciences Laboratory [Berkeley] (SSL), University of California [Berkeley], University of California-University of California, ONERA / DPHY, Université de Toulouse [Toulouse], ONERA-PRES Université de Toulouse, Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA (UMR_8109)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), NASA Goddard Space Flight Center (GSFC), Laboratory for Atmospheric and Space Physics [Boulder] (LASP), University of Colorado [Boulder], and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP)

Subjects
Synthetic aperture radar, Brightness, Electron density, 010504 meteorology & atmospheric sciences, FOS: Physical sciences, 02 engineering and technology, Noon, 7. Clean energy, 01 natural sciences, law.invention, Physics::Geophysics, symbols.namesake, Orbiter, [SPI]Engineering Sciences [physics], Optics, Physics - Space Physics, RADIATION BELT, law, 0202 electrical engineering, electronic engineering, information engineering, Electrical and Electronic Engineering, Instrumentation and Methods for Astrophysics (astro-ph.IM), 0105 earth and related environmental sciences, Physics, [PHYS]Physics [physics], business.industry, SYNCHROTRON, 020206 networking & telecommunications, CEINTURES DE RADIATION, Condensed Matter Physics, Synchrotron, Space Physics (physics.space-ph), 13. Climate action, Van Allen radiation belt, Physics::Space Physics, symbols, General Earth and Planetary Sciences, Astrophysics::Earth and Planetary Astrophysics, business, Astrophysics - Instrumentation and Methods for Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Noise (radio)
Abstract

The high kinetic energy electrons that populate the Earth's radiation belts emit synchrotron emissions because of their interaction with the planetary magnetic field. A lunar near side array would be uniquely positioned to image this emission and provide a near real time measure of how the Earth's radiation belts are responding to the current solar input. The Salammbo code is a physical model of the dynamics of the three-dimensional phase-space electron densities in the radiation belts, allowing the prediction of 1 keV to 100 MeV electron distributions trapped in the belts. This information is put into a synchrotron emission simulator which provides the brightness distribution of the emission up to 1 MHz from a given observation point. Using Digital Elevation Models from Lunar Reconnaissance Orbiter (LRO) Lunar Orbiter Laser Altimeter (LOLA) data, we select a set of locations near the Lunar sub-Earth point with minimum elevation variation over various sized patches where we simulate radio receivers to create a synthetic aperture. We consider all realistic noise sources in the low frequency regime. We then use a custom CASA code to image and process the data from our defined array, using SPICE to align the lunar coordinates with the Earth. We find that for a moderate lunar surface electron density of 250/cm^3, the radiation belts may be detected every 12-24 hours with a 16384 element array over a 10 km diameter circle. Changing electron density can make measurements 10x faster at lunar night, and 10x slower at lunar noon., Comment: 23 pages plus references. 3 Tables, 6 Figures

Published
2020
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10. Priority Questions for Jupiter System Science in the 2020s and Opportunities for Europa Clipper

Author

Maryame El Moutamid, Emma Dahl, Alfred S. McEwen, P. Molyneux, Julianne I. Moses, Michael H. Wong, Kandis Jussep, Imke de Pater, Tracy M. Becker, Shawn Brueshaber, Shawn Brooks, Cindy L. Young, Luke Moore, Glenn S. Orton, Leigh N. Fletcher, Quentin Nénon, Matthew S. Tiscareno, Chris Paranicas, Kunio M. Sayanagi, Mark R. Showalter, Joseph Westlake, Robert Ebert, and Linda Spilker

Subjects
Earth and Planetary Astrophysics (astro-ph.EP), Engineering, business.industry, Jupiter system, FOS: Physical sciences, ComputerApplications_COMPUTERSINOTHERSYSTEMS, Astrophysics - Instrumentation and Methods for Astrophysics, business, Clipper (electronics), Instrumentation and Methods for Astrophysics (astro-ph.IM), Astrophysics - Earth and Planetary Astrophysics, Astrobiology
Abstract

This whitepaper identifies important science questions that can be answered through exploration of the Jupiter System, with emphasis on the questions that can be addressed by the Europa Clipper Mission. We advocate for adding Jupiter System Science to the mission after launch when expanding the scientific scope will not affect the development cost., Comment: White Paper submitted to the Astrobiology and Planetary Science Decadal Survey

Published
2020
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11. THE IN-SITU EXPLORATION OF JUPITER'S RADIATION BELTS

Author

Xin Wu, Norbert Krupp, Christina Plainaki, Iannis Dandouras, Go Murakami, Elias Roussos, Ali Sulaiman, K. Dialynas, Tom Nordheim, R. T. Desai, Nicolas André, Jonathan Rae, B. Bertucci, Geraint H. Jones, Matina Gkioulidou, Yoshifumi Futaana, Benjamin Palmaerts, Peter Kollmann, Quentin Nénon, Yuri Shprits, Theodore E. Sarris, Emma Woodfield, George Clark, Graziella Branduardi-Raymont, Oliver Allanson, Elena A. Kronberg, Daniel Santos-Costa, Zonghua Yao, Anna Kotova, Max Planck Institute for Solar System Research (MPS), Max-Planck-Gesellschaft, 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), Mullard Space Science Laboratory (MSSL), University College of London [London] (UCL), Swedish Institute of Space Physics [Kiruna] (IRF), Bullard Laboratories, University of Cambridge, Madingley Road, Cambridge CB3 0EZ, UK (BULLARD LABORATORIES,UNIVERSITY OF CAMBRIDGE), University of Cambridge [UK] (CAM), Institute of Space and Astronautical Science (ISAS), Japan Aerospace Exploration Agency [Sagamihara] (JAXA), ONERA / DPHY, Université de Toulouse [Toulouse], PRES Université de Toulouse-ONERA, National and Kapodistrian University of Athens (NKUA), Department of Physics and Astronomy [Iowa City], University of Iowa [Iowa City], British Antarctic Survey (BAS), Natural Environment Research Council (NERC), Max-Planck-Institut für Sonnensystemforschung = Max Planck Institute for Solar System Research (MPS), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Max-Planck-Institut für Sonnensystemforschung (MPS), and ONERA-PRES Université de Toulouse

Subjects
Solar System, 010504 meteorology & atmospheric sciences, Computer science, [PHYS.ASTR.EP]Physics [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], F300, Magnetosphere, F500, 7. Clean energy, 01 natural sciences, Space missions, Space exploration, Astrobiology, Jupiter, symbols.namesake, Exploration of Jupiter, Planet, 0103 physical sciences, Particle radiation, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Voyage-2050, Astronomy and Astrophysics, Radiation belts, 13. Climate action, Space and Planetary Science, Van Allen radiation belt, Physics::Space Physics, symbols, Astrophysics::Earth and Planetary Astrophysics
Abstract

Jupiter has the most complex and energetic radiation belts in our Solar System and one of the most challenging space environments to measure and characterize in-depth. Their hazardous environment is also a reason why so many spacecraft avoid flying directly through their most intense regions, thus explaining how Jupiter’s radiation belts have kept many of their secrets so well hidden, despite having been studied for decades. In this paper we argue why these secrets are worth unveiling. Jupiter’s radiation belts and the vast magnetosphere that encloses them constitute an unprecedented physical laboratory, suitable for interdisciplinary and novel scientific investigations: from studying fundamental high energy plasma physics processes which operate throughout the Universe, such as adiabatic charged particle acceleration and nonlinear wave-particle interactions, to exploiting the astrobiological consequences of energetic particle radiation. The in-situ exploration of the uninviting environment of Jupiter’s radiation belts presents us with many challenges in mission design, science planning, instrumentation, and technology. We address these challenges by reviewing the different options that exist for direct and indirect observations of this unique system. We stress the need for new instruments, the value of synergistic Earth and Jupiter-based remote sensing and in-situ investigations, and the vital importance of multi-spacecraft in-situ measurements. While simultaneous, multi-point in-situ observations have long become the standard for exploring electromagnetic interactions in the inner Solar System, they have never taken place at Jupiter or any strongly magnetized planet besides Earth. We conclude that a dedicated multi-spacecraft mission to Jupiter is an essential and obvious way forward for exploring the planet’s radiation belts. Besides guaranteeing numerous discoveries and huge leaps in our understanding of radiation belt systems, such a mission would also enable us to view Jupiter, its extended magnetosphere, moons, and rings under new light, with great benefits for space, planetary, and astrophysical sciences. For all these reasons, in-situ investigations of Jupiter’s radiation belts deserve to be given a high priority in the future exploration of our Solar System. This article is based on a White Paper submitted in response to the European Space Agency’s call for science themes for its Voyage 2050 programme.

Published
2019
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12. Evidence of Europa Neutral Gas Torii From Energetic Sulfur Ion Measurements

Author

Quentin Nénon, N. André, Institut de recherche en astrophysique et planétologie (IRAP), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), and Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS)

Subjects
Physics, 010504 meteorology & atmospheric sciences, Inorganic chemistry, [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], chemistry.chemical_element, 01 natural sciences, Sulfur, Ion, Geophysics, chemistry, 0103 physical sciences, General Earth and Planetary Sciences, 010303 astronomy & astrophysics, ComputingMilieux_MISCELLANEOUS, 0105 earth and related environmental sciences
Abstract

International audience

Published
2019
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13. Bombardment of Lunar Polar Crater Interiors by Out-of-ecliptic Ions: ARTEMIS Observations

Author

Quentin Nénon and Andrew R. Poppe

Subjects
Astrophysics::High Energy Astrophysical Phenomena, Ecliptic, Astronomy and Astrophysics, Physics::Geophysics, Ion, Astrobiology, Solar wind, Geophysics, Impact crater, Physics::Plasma Physics, Space and Planetary Science, Physics::Space Physics, Earth and Planetary Sciences (miscellaneous), Polar, Astrophysics::Earth and Planetary Astrophysics, Geology
Abstract

Permanently shadowed regions (PSRs) inside lunar polar craters likely harbor volatiles which are of great interest for both science and resource utilization. The origin and evolution of this resource is in part driven by external space weathering, including the bombardment by space plasma ions. Previous work has investigated the flux of horizontal solar wind ions that are deflected into lunar polar craters by plasma wake electrostatic fields. Here, we constrain the flux of ions that travel northward or southward in the natural environment encountered by the Moon along its orbit. Using 9 years of in situ ion measurements gathered by the ARTEMIS mission, we find that all locations inside lunar craters are altered by a flux of out-of-ecliptic ions of 10−3 times the solar wind flux. In particular, the central floor of Shackleton’s crater is weathered by a non-null ion flux. The origin of northward and southward ions impacting the Moon is identified as (i) shocked thermalized solar wind ions in the terrestrial magnetosheath and (ii) the isotropic component of ion distributions in the terrestrial magnetotail. The energy spectrum of out-of-ecliptic ions is found to be flatter than the solar wind spectrum. Thus, sputtering of pure water ice irradiated by out-of-ecliptic ions would be created for more than 30% by >3 keV protons, unlike equatorial locations that are mostly sputtered by 1 keV protons. Future work may investigate the influence of the low, but nonzero flux of out-of-ecliptic ions reported here on the budget of volatiles in lunar PSRs.

Published
2021
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14. On the Long-term Weathering of Airless Body Surfaces by the Heavy Minor Ions of the Solar Wind: Inputs from Ion Observations and SRIM Simulations

Author

Quentin Nénon and Andrew R. Poppe

Subjects
Materials science, Dwarf planet, Astronomy and Astrophysics, Weathering, Astrobiology, Term (time), Ion, Solar wind, Geophysics, Space and Planetary Science, Physics::Space Physics, Earth and Planetary Sciences (miscellaneous), Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics
Abstract

The importance of solar wind minor ions heavier than alpha particles in weathering airless body surfaces is an open debate. The fundamental question at stake is whether the variety of different minor ion species, their high masses, and their high charge states may overcome their low densities in the solar wind to enable them to significantly contribute to ion weathering processes. Here, long-term effects that develop on geological timescales are investigated. To do so, the long-term averaged energy spectrum of thermal and suprathermal solar wind ions is estimated by compiling and contrasting ion measurements gathered by the Advanced Composition Explorer (ACE), Wind, Solar TErrestrial RElations Observatory (STEREO), ARTEMIS, and Mars Atmosphere and Volatile Evolution (MAVEN) missions. The long-term ion environment is then convolved with Stopping and Range of Ions in Matter simulations. Combining these data and models, we find that solar wind minor ions significantly alter airless body surfaces, as they contribute to 8%–14% of the total sputtering and create 20%–50% of atomic displacements at depths greater than 100 nm. The new approach presented in this article therefore confirms that solar wind minor ions play an important role in the ion weathering of airless surfaces throughout the solar system.

Published
2020
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15. The Rings of Jupiter as Seen by the Electron and Proton Radiation Belt Model Salammbô

Author

Quentin Nénon, Angélica Sicard, P. Caron, ONERA / DPHY, Université de Toulouse [Toulouse], ONERA-PRES Université de Toulouse, and PRES Université de Toulouse-ONERA

Subjects
010504 meteorology & atmospheric sciences, Galileo Probe, Electron, 01 natural sciences, Jovian, Jupiter, symbols.namesake, RADIATION BELT, 0103 physical sciences, ANNEAUX DE JUPITER, CEINTURES DE RADIATIONS, 010303 astronomy & astrophysics, Optical depth, 0105 earth and related environmental sciences, Physics, JUPITER RING, MODELE SALAMMBO, Radius, [PHYS.PHYS.PHYS-SPACE-PH]Physics [physics]/Physics [physics]/Space Physics [physics.space-ph], Magnetic field, Geophysics, SALAMMBO MODEL, [SDU]Sciences of the Universe [physics], Van Allen radiation belt, Physics::Space Physics, symbols, General Earth and Planetary Sciences, Astrophysics::Earth and Planetary Astrophysics, Atomic physics
Abstract

International audience; A modeling of the effect of the rings of Jupiter on trapped >3‐MeV electrons and protons is proposed. The effect is then added to the physical model Salammbô and discussed against in situ measurements obtained by the Pioneer 11 and Galileo Probe missions. It is first shown that there is no evidence of an effect of the rings on the Jovian radiation belts, thanks to the new internal magnetic field model proposed by the Juno mission. Two grain populations are then studied: small grains, with a radius lower than 100 μm, are shown to not affect observable >3‐MeV trapped particles. The normal optical depth of grains with a radius larger than 2 cm, which may exist in the main ring, is constrained to be lower than 10−7 by the Salammbô model.

Published
2018
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16. A Physical Model of the Proton Radiation Belts of Jupiter inside Europa's Orbit

Author

Stephan P. A. Sauer, Henry B. Garrett, Angélica Sicard, Quentin Nénon, Peter Kollmann, Chris Paranicas, ONERA / DPHY, Université de Toulouse [Toulouse], ONERA-PRES Université de Toulouse, Johns Hopkins University Applied Physics Laboratory [Laurel, MD] (APL), Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), Department of Chemistry [Copenhagen], Faculty of Science [Copenhagen], University of Copenhagen = Københavns Universitet (KU)-University of Copenhagen = Københavns Universitet (KU), and PRES Université de Toulouse-ONERA

Subjects
Physics, 010504 meteorology & atmospheric sciences, Astronomy, EUROPA’S ORBIT, 7. Clean energy, 01 natural sciences, [PHYS.PHYS.PHYS-SPACE-PH]Physics [physics]/Physics [physics]/Space Physics [physics.space-ph], Proton (rocket family), Jupiter, PROTON RADIATION BELTS OF JUPITER, symbols.namesake, Geophysics, Proton radiation, SALAMMBO MODEL, Space and Planetary Science, [SDU]Sciences of the Universe [physics], Van Allen radiation belt, 0103 physical sciences, Physics::Space Physics, symbols, Astrophysics::Earth and Planetary Astrophysics, Orbit (control theory), Nuclear Experiment, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences
Abstract

International audience; A physical model of the Jovian trapped protons with kinetic energies higher than 1 MeV inward of the orbit of the icy moon Europa is presented. The model, named Salammbô, takes into account the radial diffusion process, the absorption effect of the Jovian moons, and the Coulomb collisions and charge exchanges with the cold plasma and neutral populations of the inner Jovian magnetosphere. Preliminary modeling of the wave‐particle interaction with electromagnetic ion cyclotron waves near the moon Io is also performed. Salammbô is validated against in situ proton measurements of Pioneer 10, Pioneer 11, Voyager 1, Galileo Probe, and Galileo Orbiter. A prominent feature of the MeV proton intensity distribution in the modeled area is the 2 orders of magnitude flux depletion observed in MeV measurements near the orbit of Io. Our simulations reveal that this is not due to direct interactions with the moon or its neutral environment but results from scattering of the protons by electromagnetic ion cyclotron waves.

Published
2018
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17. NOIRE study report: Towards a low frequency radio interferometer in space

Author

Albert-Jan Boonstra, Mickael Bruno, Mark J. Bentum, Patrick Gélard, Alain Lamy, Julien N. Girard, Baptiste Cecconi, Quentin Nénon, Michel Delpech, Jean-Mathias Grießmeier, Moustapha Dekkali, Carine Briand, David Valat, Boris Segret, Martin Bucher, Andre Laurens, Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), CEA Sorbonne Paris Cité, Centre National d'Études Spatiales [Toulouse] (CNES), AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, ONERA / DPHY, Université de Toulouse [Toulouse], ONERA-PRES Université de Toulouse, 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), Unité Scientifique de la Station de Nançay (USN), Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS), Netherlands Institute for Radio Astronomy (ASTRON), Eindhoven Technical University, Université Paris Diderot, Sorbonne Paris Cité, Paris, France, Université Paris Diderot - Paris 7 (UPD7), PRES Université de Toulouse-ONERA, 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), Centre National de la Recherche Scientifique (CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire des Sciences de l'Univers en région Centre (OSUC), Université Paris sciences et lettres (PSL)-Université d'Orléans (UO), Electromagnetics, Center for Wireless Technology Eindhoven, EM for Radio Science Lab, 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), 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), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), and Technische Universiteit Eindhoven (TU/e)

Subjects
[PHYS.ASTR.IM]Physics [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], Computer science, business.industry, Electrical engineering, Electromagnetic compatibility, FOS: Physical sciences, Magnetosphere, Lagrangian point, Ranging, Orbit of the Moon, 7. Clean energy, 01 natural sciences, Clock synchronization, Interferometry, Observatory, [SDU]Sciences of the Universe [physics], 0103 physical sciences, Astronomical interferometer, 010306 general physics, business, Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), 010303 astronomy & astrophysics
Abstract

Ground based low frequency radio interferometers have been developed in the last decade and are providing the scientific community with high quality observations. Conversely, current radioastronomy instruments in space have a poor angular resolution with single point observation systems. Improving the observation capabilities of the low frequency range (a few kHz to 100 MHz) requires to go to space and to set up a space based network of antenna that can be used as an interferometer. We present the outcome of the NOIRE (Nanosatellites pour un Observatoire Interf\'erom\'etrique Radio dans l'Espace / Nanosatellites for a Radio Interferometer Observatory in Space) study which assessed, with help of CNES PASO (Architecture Platform for Orbital Systems is CNES' cross-disciplinary team in charge of early mission and concept studies), the feasibility of a swarm of nanosatellites dedicated to a low frequency radio observatory. With such a platform, space system engineering and instrument development must be studied as a whole: each node is a sensor and all sensors must be used together to obtain a measurement. The study was conducted on the following topics: system principle and concept (swarm, node homogeneity); Space and time management (ranging, clock synchronization); Orbitography (Moon orbit, Lagrange point options); Telecommunication (between nodes and with ground) and networking; Measurements and processing; Propulsion; Power; Electromagnetic compatibility. No strong show-stopper was identified during the preliminary study, although the concept is not yet ready. Several further studies and milestones are identified. The NOIRE team will collaborate with international teams to try and build this next generation of space systems., Comment: Submitted to IEEEAeroconf 2018 proceedings

Published
2018
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18. Imaging Jupiter's radiation belts down to 127 MHz with LOFAR

Author

Gianni Bernardi, Jörg R. Hörandel, A. G. Polatidis, Ashish Asgekar, A. Nelles, Angélica Sicard, H. Munk, R. J. van Weeren, Jason W. T. Hessels, D. McKay-Bukowski, I. de Pater, Matthias Hoeft, Oleg Smirnov, A. W. Gunst, Frank Breitling, Arthur Corstanje, Sebastien Hess, Quentin Nénon, Mark J. Bentum, J. van Leeuwen, R. C. Vermeulen, M. Loose, P. Zarka, H. J. A. Röttgering, P. Maat, M. J. Norden, M. Tagger, J. Moldón, F. de Gasperin, S. Bourdarie, Rene P. Breton, Annalisa Bonafede, John D. Swinbank, I. van Bemmel, Stephane Corbel, Martin Bell, V. I. Kondratiev, M. Pandey-Pommier, M. Iacobelli, James M. Anderson, Roberto Pizzo, Marcus Brüggen, Satyendra Thoudam, M. C. Toribio, Gerard H. Kuper, Antonia Rowlinson, Jochen Eislöffel, S. Duscha, Rebecca McFadden, M. A. Garrett, Daniel Santos-Costa, Julien N. Girard, Matthias Steinmetz, B. Ciardi, O. Wucknitz, J.-M. Grießmeier, M. Kuniyoshi, Ralph A. M. J. Wijers, Wilfred Frieswijk, Heino Falcke, C. Tasse, W. N. Brouw, S. Markov, Emanuela Orrú, H. Paas, Adam Deller, W. Reich, Dominik J. Schwarz, J. W. Broderick, E. Juette, G. Mann, Philip Best, C. Vocks, E. de Geus, Girard, J.N., Zarka, P., Tasse, C., Hess, S., De Pater, I., Santos-Costa, D., Nenon, Q., Sicard, A., Bourdarie, S., Anderson, J., Asgekar, A., Bell, M.E., Van Bemmel, I., Bentum, M.J., Bernardi, G., Best, P., Bonafede, A., Breitling, F., Breton, R.P., Broderick, J.W., Brouw, W.N., Brüggen, M., Ciardi, B., Corbel, S., Corstanje, A., De Gasperin, F., De Geus, E., Deller, A., Duscha, S., Eislöffel, J., Falcke, H., Frieswijk, W., Garrett, M.A., Grießmeier, J., Gunst, A.W., Hessels, J.W.T., Hoeft, M., Hörandel, J., Iacobelli, M., Juette, E., Kondratiev, V.I., Kuniyoshi, M., Kuper, G., Van Leeuwen, J., Loose, M., Maat, P., Mann, G., Markoff, S., McFadden, R., McKay-Bukowski, D., Moldon, J., Munk, H., Nelles, A., Norden, M.J., Orru, E., Paas, H., Pandey-Pommier, M., Pizzo, R., Polatidis, A.G., Reich, W., Röttgering, H., Rowlinson, A., Schwarz, D., Smirnov, O., Steinmetz, M., Swinbank, J., Tagger, M., Thoudam, S., Toribio, M.C., Vermeulen, R., Vocks, C., Van Weeren, R.J., Wijers, R.A.M.J., Wucknitz, O., Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Galaxies, Etoiles, Physique, Instrumentation (GEPI), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, ONERA - The French Aerospace Lab [Toulouse], ONERA, Netherlands Institute for Radio Astronomy (ASTRON), University of Southampton, Laboratoire de Physique Nucléaire et de Hautes Énergies (LPNHE (UMR_7585)), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Royal Observatory Edinburgh (ROE), University of Edinburgh, Jacobs University [Bremen], Leibniz-Institut für Astrophysik Potsdam (AIP), Jodrell Bank Centre for Astrophysics (JBCA), University of Manchester [Manchester], Max Planck Institute for Astrophysics, Max-Planck-Gesellschaft, Radboud University [Nijmegen], Hamburger Sternwarte/Hamburg Observatory, Universität Hamburg (UHH), Thüringer Landessternwarte Tautenburg (TLS), Leiden Observatory [Leiden], Universiteit Leiden, Unité Scientifique de la Station de Nançay (USN), Observatoire des Sciences de l'Univers en région Centre (OSUC), 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 d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique et Chimie de l'Environnement et de l'Espace (LPC2E), 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), Astronomical Institute Anton Pannekoek (AI PANNEKOEK), University of Amsterdam [Amsterdam] (UvA), Department of Pure Mathematics and Mathematical Statistics (DPMMS), Faculty of mathematics Centre for Mathematical Sciences [Cambridge] (CMS), University of Cambridge [UK] (CAM)-University of Cambridge [UK] (CAM), Ruhr-Universität Bochum [Bochum], Max-Planck-Institut für Radioastronomie (MPIFR), University of Oulu, University of Groningen [Groningen], Centre de Recherche Astrophysique de Lyon (CRAL), École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), CSIRO Astronomy and Space Science, Commonwealth Scientific and Industrial Research Organisation [Canberra] (CSIRO), Universität Bielefeld, Rhodes University, Grahamstown, Leibniz-Institut DSMZ-Deutsche Sammlung von Mikroorganismen und Zellkulturen GmbH / Leibniz Institute DSMZ-German Collection of Microorganisms and Cell Cultures (DSMZ), Harvard-Smithsonian Center for Astrophysics (CfA), Harvard University-Smithsonian Institution, ANR-11-IDEX-0005,USPC,Université Sorbonne Paris Cité(2011), European Project: 228261,EC:FP7:ERC,ERC-2008-AdG,SPARSEASTRO(2009), ITA, GBR, FRA, DEU, NLD, Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Radboud university [Nijmegen], Universiteit Leiden [Leiden], Centre National de la Recherche Scientifique (CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire des Sciences de l'Univers en région Centre (OSUC), Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Université d'Orléans (UO), École normale supérieure - Lyon (ENS Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), Harvard University [Cambridge]-Smithsonian Institution, Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), PSL Research University (PSL)-PSL Research University (PSL)-Centre National de la Recherche Scientifique (CNRS), Jodrell Bank Centre for Astrophysics, Université d'Orléans (UO)-Observatoire des Sciences de l'Univers en région Centre (OSUC), PSL Research University (PSL)-PSL Research University (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, PSL Research University (PSL)-Centre National de la Recherche Scientifique (CNRS), PSL Research University (PSL)-PSL Research University (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), DPMMS/CMS, University of Cambridge [UK] (CAM), ANR-11-IDEX-0005-02/10-LABX-0023,UnivEarthS,Earth - Planets - Universe: observation, modeling, transfer(2011), Astronomy, High Energy Astrophys. & Astropart. Phys (API, FNWI), and Faculty of Science

Subjects
radio continuum: planetary systems, Brightness, 010504 meteorology & atmospheric sciences, radio continuum: planetary, EWI-27447, Astronomy, Astrophysics::High Energy Astrophysical Phenomena, Magnetosphere, FOS: Physical sciences, Astrophysics, Electron, METIS-321662, 7. Clean energy, 01 natural sciences, Jupiter, symbols.namesake, 0103 physical sciences, Emission spectrum, IR-103183, 010303 astronomy & astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), 0105 earth and related environmental sciences, Physics, Earth and Planetary Astrophysics (astro-ph.EP), [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Radio continuum: planetary system, Planets and satellites: magnetic field, Astronomy and Astrophysics, LOFAR, Astronomy and Astrophysic, planets and satellites: magnetic fields, Spectral flux density, 13. Climate action, Space and Planetary Science, Van Allen radiation belt, Techniques: interferometric, symbols, ComputingMethodologies_DOCUMENTANDTEXTPROCESSING, systems, Astrophysics::Earth and Planetary Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Earth and Planetary Astrophysics
Abstract

Context. Observing Jupiter's synchrotron emission from the Earth remains today the sole method to scrutinize the distribution and dynamical behavior of the ultra energetic electrons magnetically trapped around the planet (because in-situ particle data are limited in the inner magnetosphere). Aims. We perform the first resolved and low-frequency imaging of the synchrotron emission with LOFAR at 127 MHz. The radiation comes from low energy electrons (~1-30 MeV) which map a broad region of Jupiter's inner magnetosphere. Methods (see article for complete abstract) Results. The first resolved images of Jupiter's radiation belts at 127-172 MHz are obtained along with total integrated flux densities. They are compared with previous observations at higher frequencies and show a larger extent of the synchrotron emission source (>=4 $R_J$). The asymmetry and the dynamic of east-west emission peaks are measured and the presence of a hot spot at lambda_III=230 {\deg} $\pm$ 25 {\deg}. Spectral flux density measurements are on the low side of previous (unresolved) ones, suggesting a low-frequency turnover and/or time variations of the emission spectrum. Conclusions. LOFAR is a powerful and flexible planetary imager. The observations at 127 MHz depict an extended emission up to ~4-5 planetary radii. The similarities with high frequency results reinforce the conclusion that: i) the magnetic field morphology primarily shapes the brightness distribution of the emission and ii) the radiating electrons are likely radially and latitudinally distributed inside about 2 $R_J$. Nonetheless, the larger extent of the brightness combined with the overall lower flux density, yields new information on Jupiter's electron distribution, that may shed light on the origin and mode of transport of these particles., Comment: 10 pages, 12 figures, accepted for publication in A&A (27/11/2015) - abstract edited because of limited characters

Published
2015
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