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1. Thin current sheet behind the dipolarization front

Author

Nakamura, Baumjohann, M., T. K., Panov, Schmid, Varsani, Apatenkov, S., Sergeev, V. A., Birn, J., Nagai, T., Gabrielse, C., Andre, M., Burch, J. L., Carr, C., Dandouras, I. S, Escoubet, C. P., A, Fazakerley, N., Giles, B. L., Contel, O. Le, Russell, C. T., Torbert, R. B., Space Research Institute of Austrian Academy of Sciences (IWF), Austrian Academy of Sciences (OeAW), Saint Petersburg State University (SPBU), Swedish Institute of Space Physics [Uppsala] (IRF), Uppsala University, 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), 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), 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 Agence Spatiale Européenne = European Space Agency (ESA)

Subjects
010504 meteorology & atmospheric sciences, [SDU.STU.GP]Sciences of the Universe [physics]/Earth Sciences/Geophysics [physics.geo-ph], Flow (psychology), Mesoscale meteorology, [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], FOS: Physical sciences, 01 natural sciences, Wedge (geometry), Current sheet, Physics - Space Physics, 0103 physical sciences, Substorm, Perpendicular, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, Physics, Earth and Planetary Astrophysics (astro-ph.EP), Front (oceanography), [PHYS.PHYS.PHYS-SPACE-PH]Physics [physics]/Physics [physics]/Space Physics [physics.space-ph], Space Physics (physics.space-ph), Computational physics, Geophysics, Space and Planetary Science, Physics::Space Physics, Current (fluid), Astrophysics - Earth and Planetary Astrophysics
Abstract

International audience; We report a unique conjugate observation of fast flows and associated current sheet disturbances in the near-Earth magnetotail by MMS (Magnetospheric Multiscale) and Cluster preceding a positive bay onset of a small substorm at ∼14:10 UT, September 8, 2018. MMS and Cluster were located both at X ∼ −14 RE. A dipolarization front (DF) of a localized fast flow was detected by Cluster and MMS, separated in the dawn-dusk direction by ∼4 RE, almost simultaneously. Adiabatic electron acceleration signatures revealed from the comparison of the energy spectra confirm that both spacecraft encounter the same DF. We analyzed the change in the current sheet structure based on multi-scale multi-point data analysis. The current sheet thickened during the passage of DF, yet, temporally thinned subsequently associated with another flow enhancement centered more on the dawnward side of the initial flow. MMS and Cluster observed intense perpendicular and parallel current in the off-equatorial region mainly during this interval of the current sheet thinning. Maximum field-aligned currents both at MMS and Cluster are directed tailward. Detailed analysis of MMS data showed that the intense field-aligned currents consisted of multiple small-scale intense current layers accompanied by enhanced Hall-currents in the dawn-dusk flow-shear region. We suggest that the current sheet thinning is related to the flow bouncing process and/or to the expansion/activation of reconnection. Based on these mesoscale and small-scale multipoint observations, 3D evolution of the flow and current-sheet disturbances was inferred preceding the development of a substorm current wedge.

Published
2022
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2. High-energy particle enhancements in the solar wind upstream Mercury during the first BepiColombo flyby: SERENA/PICAM and MPO-MAG observations

Author

Alberti, T., Sun, W., Varsani, A., Heyner, D., Orsini, S., Milillo, A., Slavin, J. A., Raines, J. M., Aronica, A., Auster, H.-U., Barabash, S., De Angelis, E., Dandouras, I., Jarvinen, R., Jeszenszky, H., Kallio, E., Kazakov, A., Laky, G., Livi, S., Mangano, V., Massetti, S., Moroni, M., Mura, A., Noschese, R., Plainaki, C., Plaschke, F., Richter, I., Rispoli, R., Sordini, R., Wurz, P., National Institute for Astrophysics, Austrian Academy of Sciences, Technical University of Braunschweig, University of Michigan, Ann Arbor, Uppsala University, Université de Toulouse, Esa Kallio Group, Department of Electronics and Nanoengineering, Southwest Research Institute, INAF - Osservatorio Astronomico di Roma, Agenzia Spaziale Italiana, University of Bern, Aalto-yliopisto, and Aalto University

Subjects
530 Physics, Space and Planetary Science, 520 Astronomy, Astronomy and Astrophysics, 620 Engineering
Abstract

Context. The first BepiColombo Mercury flyby offered the unique opportunity to simultaneously characterize the plasma and the magnetic field properties of the solar wind in the vicinity of the innermost planet of the Solar System (0.4 AU). Aims. In this study, we use plasma observations by SERENA/PICAM and magnetic field measurements by MPO-MAG to characterize the source with intermittent features (with a timescale of a few minutes) at ion energies above 1 keV observed in the solar wind upstream of Mercury. Methods. The solar wind properties have been investigated by means of low-resolution magnetic field (1 s) and plasma (64 s) data. The minimum variance analysis and the Lundquist force-free model have been used. Results. The combined analyses demonstrate that the intermittent ion features observed by PICAM at energies above 1 keV can be associated with the passage of an interplanetary magnetic flux rope. We also validate our findings by means of Solar Orbiter observations at a larger distance (0.6 AU). Conclusions. The core of an interplanetary magnetic flux rope, hitting BepiColombo during its first Mercury flyby, produced high-energy (> -pagination1 keV) intermittent-like particle acceleration clearly distinct from the background solar wind, while at the edges of this interplanetary structure compressional low-energy fluctuations have also been observed.

Published
2023
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4. Theory for planetary exospheres: III. Radiation pressure effect on the Circular Restricted Three Body Problem and its implication on planetary atmospheres

Author

Beth, A., Garnier, P., Toublanc, D., Dandouras, I., Mazelle, C., 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), 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
Earth and Planetary Astrophysics (astro-ph.EP), Atmosphere, FOS: Physical sciences, Astronomy and Astrophysics, dynamics, Extra-solar planets, [SDU]Sciences of the Universe [physics], Space and Planetary Science, Atmosphere, dynamics, Celestial mechanics, Physics::Space Physics, Solar radiation, Astrophysics::Earth and Planetary Astrophysics, Astrophysics - Earth and Planetary Astrophysics
Abstract

International audience; The planetary exospheres are poorly known in their outer parts, since the neutral densities are low compared with the instruments detection capabilities. The exospheric models are thus often the main source of information at such high altitudes. We present a new way to take into account analytically the additional effect of the stellar radiation pressure on planetary exospheres. In a series of papers, we present with a Hamiltonian approach the effect of the radiation pressure on dynamical trajectories, density profiles and escaping thermal flux. Our work is a generalization of the study by Bishop and Chamberlain [1989] Icarus, 81, 145-163. In this third paper, we investigate the effect of the stellar radiation pressure on the Circular Restricted Three Body Problem (CR3BP), called also the photogravitational CR3BP, and its implication on the escape and the stability of planetary exospheres, especially for hot Jupiters. In particular, we describe the transformation of the equipotentials and the location of the Lagrange points, and we provide a modified equation for the Hill sphere radius that includes the influence of the radiation pressure. Finally, an application to the hot Jupiter HD 209458b and hot Neptune GJ 436b reveals the existence of a blow-off escape regime induced by the stellar radiation pressure.

Published
2015
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13. Near-simultaneous magnetotail flux rope observations with Cluster and Double Star

Author

Andrew Walsh, Fazakerley, A. N., Wilson, R. J., Alexeev, I. V., Henderson, P. D., Owen, C. J., Lucek, E., Carr, C., Dandouras, I., Mullard Space Science Laboratory (MSSL), University College of London [London] (UCL), Los Alamos National Laboratory (LANL), Space and Atmospheric Physics Group [London], Blackett Laboratory, Imperial College London-Imperial College London, Centre d'étude spatiale des rayonnements (CESR), Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées, Mullard Space Science Laboratory ( MSSL ), University College of London [London] ( UCL ), Los Alamos National Laboratory ( LANL ), Centre d'étude spatiale des rayonnements ( CESR ), Université Paul Sabatier - Toulouse 3 ( UPS ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Observatoire Midi-Pyrénées ( OMP ) -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
[ SDU.OCEAN ] Sciences of the Universe [physics]/Ocean, Atmosphere, [SDU.OCEAN]Sciences of the Universe [physics]/Ocean, Atmosphere, lcsh:Geophysics. Cosmic physics, Physics::Space Physics, lcsh:QC801-809, [SDU.STU]Sciences of the Universe [physics]/Earth Sciences, [ SDU.STU ] Sciences of the Universe [physics]/Earth Sciences, lcsh:Q, lcsh:Science, lcsh:Physics, lcsh:QC1-999
Abstract

We present observations of three magnetic flux ropes in the tail of the Earth's magnetosphere on 7 August 2004 by the Cluster and Double Star TC-1 spacecraft. The first two flux rope signatures were observed, near-simultaneously, by Cluster and TC-1, which were located at (–16.3, –8.7, 0.10) RE GSM and (–10.3, –7.11, 0.81) RE GSM, respectively, a separation of 6.3 RE. A third signature was observed some four minutes later by two of the four Cluster spacecraft, while the other two spacecraft observed a feature resembling a Travelling Compression Region (TCR). These observations are interpreted as three individual flux ropes existing in the magnetotail, the first two, at least, simultaneously. The formation mechanism of the flux ropes and the consequences of their presence for the structure of the magnetotail on this day are discussed in the context of multiple X-point reconnection.

14. Solar wind turbulence at kinetic scales: Cluster observations

Author

Alexandrova, O., Perrone, D., Sonny LION, Lacombe, C., Matteini, L., Maksimovic, M., Rossi, C., Sorriso-Valvo, L., Nicole Cornilleau-Wehrlin, Dandouras, I., Mangeney, A., 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), Laboratoire de Physique des Plasmas (LPP), Université Paris-Saclay-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris-Sud - Paris 11 (UP11)-École polytechnique (X)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), Université Paris-Sud - Paris 11 (UP11)-Observatoire de Paris, and 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)

Subjects
[PHYS.PHYS.PHYS-PLASM-PH]Physics [physics]/Physics [physics]/Plasma Physics [physics.plasm-ph], [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], ComputingMilieux_MISCELLANEOUS
Abstract

International audience

15. The Solar Orbiter Solar Wind Analyser (SWA) suite

Author

Owen, C. J., Bruno, R., Livi, S., Louarn, P., Al Janabi, K., Allegrini, F., Amoros, C., Baruah, R., Barthe, A., Berthomier, M., Bordon, S., Brockley-Blatt, C., Brysbaert, C., Capuano, G., Collier, M., DeMarco, R., Fedorov, A., Ford, J., Fortunato, V., Fratter, I., Galvin, A. B., Hancock, B., Heirtzler, D., Kataria, D., Kistler, L., Lepri, S. T., Lewis, G., Loeffler, C., Marty, W., Mathon, R., Mayall, A., Mele, G., Ogasawara, K., Orlandi, M., Pacros, A., Penou, E., Persyn, S., Petiot, M., Phillips, M., Přech, L., Raines, J. M., Reden, M., Rouillard, A. P., Rousseau, A., Rubiella, J., Seran, H., Spencer, A., Thomas, J. W., Trevino, J., Verscharen, D., Wurz, P., Alapide, A., Amoruso, L., André, N., Anekallu, C., Arciuli, V., Arnett, K. L., Ascolese, R., Bancroft, C., Bland, P., Brysch, M., Calvanese, R., Castronuovo, M., Čermák, I., Chornay, D., Clemens, S., Coker, J., Collinson, G., D’Amicis, R., Dandouras, I., Darnley, R., Davies, D., Davison, G., De Los Santos, A., Devoto, P., Dirks, G., Edlund, E., Fazakerley, A., Ferris, M., Frost, C., Fruit, G., Garat, C., Génot, V., Gibson, W., Gilbert, J. A., de Giosa, V., Gradone, S., Hailey, M., Horbury, T. S., Hunt, T., Jacquey, C., Johnson, M., Lavraud, B., Lawrenson, A., Leblanc, F., Lockhart, W., Maksimovic, M., Malpus, A., Marcucci, F., Mazelle, C., Monti, F., Myers, S., Nguyen, T., Rodriguez-Pacheco, J., Phillips, I., Popecki, M., Rees, K., Rogacki, S. A., Ruane, K., Rust, D., Salatti, M., Sauvaud, J. A., Stakhiv, M. O., Stange, J., Stubbs, T., Taylor, T., Techer, J.-D., Terrier, G., Thibodeaux, R., Urdiales, C., Varsani, A., Walsh, A. P., Watson, G., Wheeler, P., Willis, G., Wimmer-Schweingruber, R. F., Winter, B., Yardley, J., and Zouganelis, I.

Subjects
520 Astronomy, Physics::Space Physics, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, 620 Engineering, 7. Clean energy
Abstract

The Solar Orbiter mission seeks to make connections between the physical processes occurring at the Sun or in the solar corona and the nature of the solar wind created by those processes which is subsequently observed at the spacecraft. The mission also targets physical processes occurring in the solar wind itself during its journey from its source to the spacecraft. To meet the specific mission science goals, Solar Orbiter will be equipped with both remote-sensing and in-situ instruments which will make unprecedented measurements of the solar atmosphere and the inner heliosphere. A crucial set of measurements will be provided by the Solar Wind Analyser (SWA) suite of instruments. This suite consists of an Electron Analyser System (SWA-EAS), a Proton and Alpha particle Sensor (SWA-PAS), and a Heavy Ion Sensor (SWA-HIS) which are jointly served by a central control and data processing unit (SWA-DPU). Together these sensors will measure and categorise the vast majority of thermal and suprathermal ions and electrons in the solar wind and determine the abundances and charge states of the heavy ion populations. The three sensors in the SWA suite are each based on the top hat electrostatic analyser concept, which has been deployed on numerous space plasma missions. The SWA-EAS uses two such heads, each of which have 360◦ azimuth acceptance angles and ±45◦ aperture deflection plates. Together these two sensors, which are mounted on the end of the boom, will cover a full sky field-of-view (FoV) (except for blockages by the spacecraft and its appendages) and measure the full 3D velocity distribution function (VDF) of solar wind electrons in the energy range of a few eV to ∼5 keV. The SWA-PAS instrument also uses an electrostatic analyser with a more confined FoV (−24◦ to +42◦ × ±22.5◦ around the expected solar wind arrival direction), which nevertheless is capable of measuring the full 3D VDF of the protons and alpha particles arriving at the instrument in the energy range from 200 eV/q to 20 keV/e. Finally, SWA-HIS measures the composition and 3D VDFs of heavy ions in the bulk solar wind as well as those of the major constituents in the suprathermal energy range and those of pick-up ions. The sensor resolves the full 3D VDFs of the prominent heavy ions at a resolution of 5 min in normal mode and 30 s in burst mode. Additionally, SWA-HIS measures 3D VDFs of alpha particles at a 4 s resolution in burst mode. Measurements are over a FoV of −33◦ to +66◦ × ±20◦ around the expected solar wind arrival direction and at energies up to 80 keV/e. The mass resolution (m/∆m) is >5. This paper describes how the three SWA scientific sensors, as delivered to the spacecraft, meet or exceed the performance requirements originally set out to achieve the mission’s science goals. We describe the motivation and specific requirements for each of the three sensors within the SWA suite, their expected science results, their main characteristics, and their operation through the central SWA-DPU. We describe the combined data products that we expect to return from the suite and provide to the Solar Orbiter Archive for use in scientific analyses by members of the wider solar and heliospheric communities. These unique data products will help reveal the nature of the solar wind as a function of both heliocentric distance and solar latitude. Indeed, SWA-HIS measurements of solar wind composition will be the first such measurements made in the inner heliosphere. The SWA data are crucial to efforts to link the in situ measurements of the solar wind made at the spacecraft with remote observations of candidate source regions. This is a novel aspect of the mission which will lead to significant advances in our understanding of the mechanisms accelerating and heating the solar wind, driving eruptions and other transient phenomena on the Sun, and controlling the injection, acceleration, and transport of the energetic particles in the heliosphere.

19. Solar orbiter neutral solar-wind detector

Author

Hilchenbach, M., Orsini, S., Hseih, K. C., Antonucci, E., Barabash, S., Bamert, K., Bruno, R., Collier, M. R., Czechowski, A., D Amicis, R., Angelis, E., Dandouras, I., Di Lellis, A. M., Esser, R., Giacalone, J., Gruntman, M., Habbal, S. R., Jokipii, J. R., Kallio, E., Kota, J., Kucharek, H., Leonl, R., Livi, S., Mann, I., Marsch, E., Massetti, S., Milillo, A., Möbius, E., Alessandro Mura, Sheldon, R. B., Schmidt, W., Selci, S., Szego, K., Woch, J., Wurz, P., Zanza, V., and Zurbuchen, T. H.

Subjects
Solar equipment, Astrophysics::High Energy Astrophysical Phenomena, Physics::Space Physics, Magnetic field effects, Astrophysics::Solar and Stellar Astrophysics, Dust, Astrophysics::Earth and Planetary Astrophysics, Velocity distribution, Hydrogen
Abstract

Neutral hydrogen atoms, which give rise to the prominent solar Ly-? corona, are closely coupled to the emerging solar-wind plasma. The density ratio of neutral hydrogen to protons is minute, ?10-6; therefore, the neutral atoms are tracers in the solar wind. In-situ observations of the neutral atoms, their flight paths (imaging), density, and velocity distributions are a new tool to the understanding of the Ly-? corona, i.e. setting limits on the plasma velocity distribution along the solar magnetic field lines. The other goal of the neutral solar-wind instrumentation is the in-situ observation of the interactions between solar wind plasma and dust grains near the Sun. We will discuss the science objectives and the potential "zero charge" solar-wind instrument envelope onboard Solar Orbiter.

20. SERENA: Particle Instrument Suite for Determining the Sun-Mercury Interaction from BepiColombo

Author

Orsini, S., Livi, S. A., Lichtenegger, H., Barabash, S., Milillo, A., De Angelis, E., Phillips, M., Laky, G., Wieser, M., Olivieri, A., Plainaki, C., Ho, G., Killen, R. M., Slavin, J. A., Wurz, Peter, Berthelier, J.-J., Dandouras, I., Kallio, E., McKenna-Lawlor, S., Szalai, S., Torkar, K., Vaisberg, O., Allegrini, F., Daglis, I. A., Dong, C., Escoubet, C. P., Fatemi, S., Fränz, M., Ivanovski, S., Krupp, N., Lammer, H., Leblanc, François, Mangano, V., Mura, A., Nilsson, H., Raines, J. M., Rispoli, R., Sarantos, M., Smith, H. T., Szego, K., Aronica, A., Camozzi, F., Di Lellis, A. M., Fremuth, G., Giner, F., Gurnee, R., Hayes, J., Jeszenszky, H., Tominetti, F., Trantham, B., Balaz, J., Baumjohann, W., Brienza, D., Bührke, U., Bush, M. D., Cantatore, M., Cibella, S., Colasanti, L., Cremonese, G., Cremonesi, L., D’Alessandro, M., Delcourt, D., Delva, M., Desai, M., Fama, M., Ferris, M., Fischer, H., Gaggero, A., Gamborino, Diana, Garnier, P., Gibson, W. C., Goldstein, R., Grande, M., Grishin, V., Haggerty, D., Holmström, M., Horvath, I., Hsieh, K.-C., Jacques, A., Johnson, R. E., Kazakov, A., Kecskemety, K., Krüger, H., Kürbisch, C., Lazzarotto, F., Leblanc, Frederic, Leichtfried, M., Leoni, R., Loose, A., Maschietti, D., Massetti, S., Mattioli, F., Miller, G., Moissenko, D., Morbidini, A., Noschese, R., Nuccilli, F., Nunez, C., Paschalidis, N., Persyn, S., Piazza, Daniele, Oja, M., Ryno, J., Schmidt, W., Scheer, J. A., Shestakov, A., Shuvalov, S., Seki, K., Selci, S., Smith, K., Sordini, R., Svensson, J., Szalai, L., Toublanc, D., Urdiales, C., Varsani, A., Vertolli, N., Wallner, R., Wahlstroem, P., Wilson, P., and Zampieri, S.

Subjects
520 Astronomy, Physics::Space Physics, Astrophysics::Earth and Planetary Astrophysics, 620 Engineering, 7. Clean energy
Abstract

The ESA-JAXA BepiColombo mission to Mercury will provide simultaneous measurements from two spacecraft, offering an unprecedented opportunity to investigate magnetospheric and exospheric particle dynamics at Mercury as well as their interactions with solar wind, solar radiation, and interplanetary dust. The particle instrument suite SERENA (Search for Exospheric Refilling and Emitted Natural Abundances) is flying in space on-board the BepiColombo Mercury Planetary Orbiter (MPO) and is the only instrument for ion and neutral particle detection aboard the MPO. It comprises four independent sensors: ELENA for neutral particle flow detection, Strofio for neutral gas detection, PICAM for planetary ions observations, and MIPA, mostly for solar wind ion measurements. SERENA is managed by a System Control Unit located inside the ELENA box. In the present paper the scientific goals of this suite are described, and then the four units are detailed, as well as their major features and calibration results. Finally, the SERENA operational activities are shown during the orbital path around Mercury, with also some reference to the activities planned during the long cruise phase.

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