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1. Mercury’s plasma environment after BepiColombo’s third flyby

Author

Hadid, Lina Z., Delcourt, Dominique, Harada, Yuki, Rojo, Mathias, Aizawa, Sae, Saito, Yoshifumi, André, Nicolas, Glass, Austin N., Raines, Jim M., Yokota, Shoichiro, Fränz, Markus, Katra, Bruno, Verdeil, Christophe, Fiethe, Björn, Leblanc, Francois, Modolo, Ronan, Fontaine, Dominique, Krupp, Norbert, Krüger, Harald, Leblanc, Frédéric, Fischer, Henning, Berthelier, Jean-Jacques, Sauvaud, Jean-André, Murakami, Go, and Matsuda, Shoya

Published
2024
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2. Maps of solar wind plasma precipitation onto Mercury's surface: a geographical perspective

Author

Lavorenti, Federico, Jensen, Elizabeth A., Aizawa, Sae, Califano, Francesco, D'Amore, Mario, Domingue, Deborah, Henri, Pierre, Lindsay, Simon, Raines, Jim M., and Savin, Daniel Wolf

Subjects
Physics - Space Physics, Astrophysics - Earth and Planetary Astrophysics
Abstract

Mercury is the closest planet to the Sun, possesses a weak intrinsic magnetic field and has only a very tenuous atmosphere (exosphere). These three conditions result in a direct coupling between the plasma emitted from the Sun (namely the solar wind) and Mercury's surface. The planet's magnetic field leads to a non-trivial pattern of plasma precipitation onto the surface, that is expected to contribute to the alteration of the regolith over geological time scales. The goal of this work is to study the solar wind plasma precipitation onto the surface of Mercury from a geographical perspective, as opposed to the local-time-of-day approach of previous precipitation modeling studies. We employ solar wind precipitation maps for protons and electrons from two fully-kinetic numerical simulations of Mercury's plasma environment. These maps are then integrated over two full Mercury orbits (176 Earth days). We found that the plasma precipitation pattern at the surface is most strongly affected by the upstream solar wind conditions, particularly by the interplanetary magnetic field direction, and less by Mercury's 3:2 spin-orbit resonance. We also found that Mercury's magnetic field is able to shield the surface from roughly 90% of the incoming solar wind flux. At the surface, protons have a broad energy distribution from below 500 eV to more than 1.5 keV; while electrons are mostly found in the range 0.1-4 keV. These results will help to better constrain space weathering and exosphere source processes at Mercury, as well as to interpret observations by the ongoing ESA/JAXA BepiColombo mission., Comment: Submitted to PSJ on focus issue "Mercury's Surface Response to the Interplanetary Environment: Identifying Needed Studies in Laboratory Astrophysics"

Published
2023

3. Solar-wind electron precipitation on weakly magnetized bodies: the planet Mercury

Author

Lavorenti, Federico, Henri, Pierre, Califano, Francesco, Deca, Jan, Lindsay, Simon, Aizawa, Sae, and Benkhoff, Johannes

Subjects
Physics - Space Physics
Abstract

Mercury is the archetype of a weakly magnetized, airless, telluric body immersed in the solar wind. Due to the lack of any substantial atmosphere, the solar wind directly precipitates on Mercury's surface. Using a 3D fully-kinetic self-consistent plasma model, we show for the first time that solar-wind electron precipitation drives (i) efficient ionization of multiple species (H, He, O and Mn) in Mercury's neutral exosphere and (ii) emission of X-rays from the planet's surface. This is the first, independent evidence of X-ray auroras on Mercury using a numerical approach., Comment: Submitted to Physical Review Letters

Published
2022
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4. Electron dynamics in small magnetospheres: insights from global fully-kinetic plasma simulations of planet Mercury

Author

Lavorenti, Federico, Henri, Pierre, Califano, Francesco, Deca, Jan, Aizawa, Sae, André, Nicolas, and Benkhoff, Johannes

Subjects
Physics - Space Physics, Physics - Plasma Physics
Abstract

The planet Mercury possesses a small but highly dynamic magnetosphere in which the role and dynamics of electrons are still largely unknown. We aim at modeling 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. 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. Numerical simulations are carried out using two different solar wind conditions: purely northward or purely southward interplanetary magnetic field direction. We find a high plasma current (of the order of few $\mu$A/m2) 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., Comment: Article submitted to "Astronomy and Astrophysics"

Published
2022
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5. Review of Mercury's Dynamic Magnetosphere: Post-MESSENGER Era and Comparative Magnetospheres

Author

Sun, Weijie, Dewey, Ryan M., Aizawa, Sae, Huang, Jia, Slavin, James A., Fu, Suiyan, Wei, Yong, and Bowers, Charles F.

Subjects
Physics - Space Physics, Astrophysics - Earth and Planetary Astrophysics, Physics - Plasma Physics
Abstract

This review summarizes the research of Mercury's magnetosphere in the Post-MESSENGER era and compares its dynamics to those in other planetary magnetospheres, especially to those in Earth's magnetosphere. This review starts by introducing the planet Mercury, including its interplanetary environment, magnetosphere, exosphere, and conducting core. The frequent and intense magnetic reconnection on the dayside magnetopause, which is represented by the flux transfer event "shower", is reviewed on how they depend on magnetosheath plasma beta and magnetic shear angle across the magnetopause, following by how they contribute to the flux circulation and magnetosphere-surface-exosphere coupling. In the next, the progress of Mercury's magnetosphere under extreme solar events, including the core induction and the reconnection erosion on the dayside magnetosphere, the responses of the nightside magnetosphere, are reviewed. Then, the dawn-dusk properties of the plasma sheet, including the features of the ions, the structure of the current sheet, and the dynamics of magnetic reconnection, are summarized. The last topic reviews the particle energization in Mercury's magnetosphere, which includes the energization of the Kelvin-Helmholtz waves on the magnetopause boundaries, reconnection-generated magnetic structures, and the cross-tail electric field. In each chapter, the last section discusses the open questions related with each topic, which can be considered by the simulations and the future spacecraft mission. We close by summarizing the future BepiColombo opportunities, which is a joint mission between ESA and JAXA, and is en route to Mercury., Comment: 50 pages, 28 figures, 4 tables, Published by Science China Earth Sciences

Published
2021
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6. Direct evidence of substorm-related impulsive injections of electrons at Mercury

Author

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

Published
2023
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7. Forecasting Heliospheric CME Solar-Wind Parameters Using the UCSD Time-Dependent Tomography and ISEE Interplanetary Scintillation Data: The 10 March 2022 CME

Author

Jackson, Bernard V., Tokumaru, Munetoshi, Iwai, Kazumasa, Bracamontes, Matthew T., Buffington, Andrew, Fujiki, Ken’ichi, Murakami, Go, Heyner, Daniel, Sanchez-Cano, Beatriz, Rojo, Mathias, Aizawa, Sae, Andre, Nicolas, Barthe, Alain, Penou, Emmanuel, Fedorov, Andrei, Sauvaud, Jean-Andre, Yokota, Shoichiro, and Saito, Yoshifumi

Published
2023
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9. Deep Entry of Low-Energy Ions Into Mercury's Magnetosphere: BepiColombo Mio’s Third Flyby Observations

Author

90823386, Harada, Yuki, Saito, Yoshifumi, Hadid, Lina Z., Delcourt, Dominique, Aizawa, Sae, Rojo, Mathias, André, Nicolas, Persson, Moa, Fraenz, Markus, Yokota, Shoichiro, Fedorov, Andréi, Miyake, Wataru, Penou, Emmanuel, Barthe, Alain, Sauvaud, Jean‐André, Katra, Bruno, Matsuda, Shoya, Murakami, Go, 90823386, Harada, Yuki, Saito, Yoshifumi, Hadid, Lina Z., Delcourt, Dominique, Aizawa, Sae, Rojo, Mathias, André, Nicolas, Persson, Moa, Fraenz, Markus, Yokota, Shoichiro, Fedorov, Andréi, Miyake, Wataru, Penou, Emmanuel, Barthe, Alain, Sauvaud, Jean‐André, Katra, Bruno, Matsuda, Shoya, and Murakami, Go

Abstract

Although solar wind-driven convection is expected to dominate magnetospheric circulation at Mercury, its exact pattern remains poorly characterized by observations. Here we present BepiColombo Mio observations during the third Mercury flyby indicative of convection-driven transport of low-energy dense ions into the deep magnetosphere. During the flyby, Mio observed an energy-dispersed ion population from the duskside magnetopause to the deep region of the midnight magnetosphere. A comparison of the observations with backward test particle simulations suggests that the observed energy dispersion structure can be explained in terms of energy-selective transport by convection from the duskside tail magnetopause. We also discuss the properties and origins of more energetic ions observed in the more dipole-like field regions of the magnetosphere in comparison to previously reported populations of the plasma sheet horn and ring current ions. Additionally, forward test particle simulations predict that most of the observed ions on the nightside will precipitate onto relatively low-latitude regions of the nightside surface of Mercury for a typical convection case. The presented observations and simulation results reveal the critical role of magnetospheric convection in determining the structure of Mercury's magnetospheric plasma. The upstream driver dependence of magnetospheric convection and its effects on other magnetospheric processes and plasma-surface interactions should be further investigated by in-orbit BepiColombo observations.

Published
2024

10. Deep Entry of Low-Energy Ions Into Mercury's Magnetosphere : BepiColombo Mio's Third Flyby Observations

Author

Harada, Yuki, Saito, Yoshifumi, Hadid, Lina Z., Delcourt, Dominique, Aizawa, Sae, Rojo, Mathias, Andre, Nicolas, Persson, Moa, Fraenz, Markus, Yokota, Shoichiro, Fedorov, Andrei, Miyake, Wataru, Penou, Emmanuel, Barthe, Alain, Sauvaud, Jean-Andre, Katra, Bruno, Matsuda, Shoya, Murakami, Go, Harada, Yuki, Saito, Yoshifumi, Hadid, Lina Z., Delcourt, Dominique, Aizawa, Sae, Rojo, Mathias, Andre, Nicolas, Persson, Moa, Fraenz, Markus, Yokota, Shoichiro, Fedorov, Andrei, Miyake, Wataru, Penou, Emmanuel, Barthe, Alain, Sauvaud, Jean-Andre, Katra, Bruno, Matsuda, Shoya, and Murakami, Go

Abstract

Although solar wind-driven convection is expected to dominate magnetospheric circulation at Mercury, its exact pattern remains poorly characterized by observations. Here we present BepiColombo Mio observations during the third Mercury flyby indicative of convection-driven transport of low-energy dense ions into the deep magnetosphere. During the flyby, Mio observed an energy-dispersed ion population from the duskside magnetopause to the deep region of the midnight magnetosphere. A comparison of the observations with backward test particle simulations suggests that the observed energy dispersion structure can be explained in terms of energy-selective transport by convection from the duskside tail magnetopause. We also discuss the properties and origins of more energetic ions observed in the more dipole-like field regions of the magnetosphere in comparison to previously reported populations of the plasma sheet horn and ring current ions. Additionally, forward test particle simulations predict that most of the observed ions on the nightside will precipitate onto relatively low-latitude regions of the nightside surface of Mercury for a typical convection case. The presented observations and simulation results reveal the critical role of magnetospheric convection in determining the structure of Mercury's magnetospheric plasma. The upstream driver dependence of magnetospheric convection and its effects on other magnetospheric processes and plasma-surface interactions should be further investigated by in-orbit BepiColombo observations. BepiColombo Mio observed low-energy dense ions deep within Mercury's magnetosphere during the third Mercury flyby Backward test particle simulations suggest that low-energy ions are transported by convection from the duskside tail magnetopause Forward test particle simulations imply convection-driven ion precipitation onto the nightside low-latitude surface of Mercury

Published
2024
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11. Overview of the LAPYUTA mission (Life-environmentology, Astronomy, and PlanetarY Ultraviolet Telescope Assembly)

Author

den Herder, Jan-Willem A., Nikzad, Shouleh, Nakazawa, Kazuhiro, Tsuchiya, Fuminori, Murakami, Go, Yamazaki, Atsushi, Kameda, Shingo, Kimura, Tomoki, Koga, Ryoichi, Masunaga, Kei, Sakai, Shotaro, Ikoma, Masahiro, Nakayama, Akifumi, Ouchi, Masami, Tanaka, Masaomi, Toriumi, Shin, Kagitani, Masato, Yoshioka, Kazuo, Tao, Chihiro, Kita, Hajime, Yajima, Hidenobu, Sagawa, Hideo, Nakagawa, Hiromu, Hamori, Hitoshi, Kimura, Jun, Enya, Keigo, Namekata, Kosuke, Yamada, Manabu, Kuwabara, Masaki, Terada, Naoki, Ozaki, Naoya, Narita, Norio, Aizawa, Sae, Takagi, Seiko, Sakai, Shinitiro, Aoki, Shohei, Matsuda, Shoya, Tan, Shuya, Sumi, Takahiro, Kodama, Takanori, Moriya, Takashi, Shibuya, Takatoshi, Satoh, Takehiko, Kawano, Taro, Tominaga, Nozomu, Shimizu, Toshifumi, Kasaba, Yasumasa, Yatsu, Yoichi, Ono, Yoshiaki, Suzuki, Yudai, Matsuda, Yuichi, Harada, Yuki, and Notsu, Yuta

Published
2024
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12. BepiColombo Science Investigations During Cruise and Flybys at the Earth, Venus and Mercury

Author

Mangano, Valeria, Dósa, Melinda, Fränz, Markus, Milillo, Anna, Oliveira, Joana S., Lee, Yeon Joo, McKenna-Lawlor, Susan, Grassi, Davide, Heyner, Daniel, Kozyrev, Alexander S., Peron, Roberto, Helbert, Jörn, Besse, Sebastien, de la Fuente, Sara, Montagnon, Elsa, Zender, Joe, Volwerk, Martin, Chaufray, Jean-Yves, Slavin, James A., Krüger, Harald, Maturilli, Alessandro, Cornet, Thomas, Iwai, Kazumasa, Miyoshi, Yoshizumi, Lucente, Marco, Massetti, Stefano, Schmidt, Carl A., Dong, Chuanfei, Quarati, Francesco, Hirai, Takayuki, Varsani, Ali, Belyaev, Denis, Zhong, Jun, Kilpua, Emilia K. J., Jackson, Bernard V., Odstrcil, Dusan, Plaschke, Ferdinand, Vainio, Rami, Jarvinen, Riku, Ivanovski, Stavro Lambrov, Madár, Ákos, Erdős, Géza, Plainaki, Christina, Alberti, Tommaso, Aizawa, Sae, Benkhoff, Johannes, Murakami, Go, Quemerais, Eric, Hiesinger, Harald, Mitrofanov, Igor G., Iess, Luciano, Santoli, Francesco, Orsini, Stefano, Lichtenegger, Herbert, Laky, Gunther, Barabash, Stas, Moissl, Richard, Huovelin, Juhani, Kasaba, Yasumasa, Saito, Yoshifumi, Kobayashi, Masanori, and Baumjohann, Wolfgang

Published
2021
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13. Spacecraft outgassing observed by the BepiColombo ion spectrometers

Author

Fraenz, Markus, primary, Rojo, Mathias, additional, Cornet, Thomas, additional, HADID, Lina, additional, Saito, Yoshifumi, additional, André, Nicolas, additional, Varsani, Ali, additional, Schmid, Daniel, additional, Krueger, Harald, additional, Krupp, Norbert, additional, Delcourt, Dominique, additional, Katra, Bruno, additional, Harada, Yuki, additional, Yokota, Shoichiro, additional, Verdeil, Christophe, additional, Aizawa, Sae, additional, Milillo, Anna, additional, Orsini, Stefano, additional, Mangano, Valeria, additional, Fiethe, Björn, additional, Benkhoff, Johannes, additional, and Murakami, Go, additional

Published
2023
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22. BepiColombo Mio Observations of Low‐Energy Ions During the First Mercury Flyby: Initial Results

Author

Harada, Yuki, primary, Aizawa, Sae, additional, Saito, Yoshifumi, additional, André, Nicolas, additional, Persson, Moa, additional, Delcourt, Dominique, additional, Hadid, Lina Z., additional, Fraenz, Markus, additional, Yokota, Shoichiro, additional, Fedorov, Andréi, additional, Miyake, Wataru, additional, Penou, Emmanuel, additional, Barthe, Alain, additional, Sauvaud, Jean‐André, additional, Katra, Bruno, additional, Matsuda, Shoya, additional, and Murakami, Go, additional

Published
2022
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23. Electron dynamics in small magnetospheres

Author

Lavorenti, Federico, primary, Henri, Pierre, additional, Califano, Francesco, additional, Deca, Jan, additional, Aizawa, Sae, additional, André, Nicolas, additional, and Benkhoff, Johannes, additional

Published
2022
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24. Dayside magnetopause reconnection and flux transfer events under radial interplanetary magnetic field (IMF): BepiColombo Earth-flyby observations

Author

Sun, Weijie, primary, Slavin, James A., additional, Nakamura, Rumi, additional, Heyner, Daniel, additional, Trattner, Karlheinz J., additional, Mieth, Johannes Z. D., additional, Zhao, Jiutong, additional, Zong, Qiu-Gang, additional, Aizawa, Sae, additional, Andre, Nicolas, additional, and Saito, Yoshifumi, additional

Published
2022
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25. Modeling the impact of a strong X-class solar flare on the planetary ion composition in Mercury's magnestosphere

Author

Werner, Elisabeth, Leblanc, François, Chaufray, Jean-Yves, Modolo, Ronan, Aizawa, Sae, Hadid, L. Z., Baskevitch, Claire, and Cardon, Catherine

Subjects
[SDU] Sciences of the Universe [physics], magnetosphere, dynamics, Mercury, Exosphere
Abstract

Solar flares could potentially give rise to sudden changes in the planetary ion composition in Mercury's magnetosphere. We model the time-dependent evolution of the Mg + , Na +, O + and He+ ion density distribution during the extreme X9.3-class solar flare event on 6 September 2017 with the Latmos Ionized Exosphere (LIZE) model. We find that the peak ion density in the nightside plasma sheet is delayed by ∼7−8 min compared to the dayside, and that the maximum Mg + density occurs ∼4 min before He + and O + in the whole magnetosphere. We also find that there exist two ion energy populations on the dayside which experience different dynamical evolution during the event.

Published
2022

26. LatHyS hybrid simulation of the August, 10 2021 BepiColombo Venus flyby

Author

Aizawa, Sae, primary, Persson, Moa, additional, Menez, Thibault, additional, Andre, Nicolas, additional, Modolo, Ronan, additional, Barthe, Alain, additional, Penou, Emmanuel, additional, Fedorov, Andrei, additional, Sauvaud, Jean-Andre, additional, Leblanc, Francois, additional, Chaufray, Jean-Yves, additional, Saito, Yoshifumi, additional, Yokota, Shoichiro, additional, Murakami, Go, additional, Genot, Vincent, additional, Sanchez-Cano, Beatriz, additional, Heyner, Daniel, additional, Horbury, Tim, additional, Louarn, Philippe, additional, and Owen, Christopher, additional

Published
2022
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29. 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
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33. Supplementary material to "Dayside magnetopause reconnection and flux transfer events: BepiColombo earth-Flyby observations"

Author

Sun, Weijie, primary, Slavin, James A., additional, Nakamura, Rumi, additional, Heyner, Daniel, additional, Trattner, Karlheinz J., additional, Mieth, Johannes Z. D., additional, Zhao, Jiutong, additional, Zong, Qiu-Gang, additional, Aizawa, Sae, additional, Andre, Nicolas, additional, and Saito, Yoshifumi, additional

Published
2021
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34. Electron acceleration driven by the lower-hybrid-drift instability: An extended quasilinear model

Author

Lavorenti, Federico, Henri, Pierre, Califano, Francesco, Aizawa, Sae, André, Nicolas, Joseph Louis LAGRANGE (LAGRANGE), Université Côte d'Azur (UCA)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), 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), Dipartimento di Fisica 'E. Fermi', University of Pisa - Università di Pisa, 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 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), 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
numerical, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], plasmas, numerical, instabilities, waves, observational, instabilities, waves, observational, methods: observational, plasmas, [PHYS.PHYS.PHYS-SPACE-PH]Physics [physics]/Physics [physics]/Space Physics [physics.space-ph], methods: numerical
Abstract

International audience; Context. Density inhomogeneities are ubiquitous in space and astrophysical plasmas, particularly at contact boundaries between different media. They often correspond to regions that exhibit strong dynamics across a wide range of spatial and temporal scales. Indeed, density inhomogeneities are a source of free energy that can drive various instabilities such as the lower-hybrid-drift instability, which, in turn, transfers energy to the particles through wave-particle interactions and eventually heats the plasma.Aims. Our study is aimed at quantifying the efficiency of the lower-hybrid-drift instability to accelerate or heat electrons parallel to the ambient magnetic field.Methods. We combine two complementary methods: full-kinetic and quasilinear models.Results. We report self-consistent evidence of electron acceleration driven by the development of the lower-hybrid-drift instability using 3D-3V full-kinetic numerical simulations. The efficiency of the observed acceleration cannot be explained by standard quasilinear theory. For this reason, we have developed an extended quasilinear model that is able to quantitatively predict the interaction between lower-hybrid fluctuations and electrons on long time scales, which is now in agreement with full-kinetic simulations results. Finally, we apply this new, extended quasilinear model to a specific inhomogeneous space plasma boundary, namely, the magnetopause of Mercury. Furthermore, we discuss our quantitative predictions of electron acceleration to support future BepiColombo observations.

Published
2021
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35. Venus's induced magnetosphere during active solar wind conditions at BepiColombo's Venus 1 flyby

Author

Volwerk, Martin, primary, Sánchez-Cano, Beatriz, additional, Heyner, Daniel, additional, Aizawa, Sae, additional, André, Nicolas, additional, Varsani, Ali, additional, Mieth, Johannes, additional, Orsini, Stefano, additional, Baumjohann, Wolfgang, additional, Fischer, David, additional, Futaana, Yoshifumi, additional, Harrison, Richard, additional, Jeszenszky, Harald, additional, Kazumasa, Iwai, additional, Laky, Gunter, additional, Lichtenegger, Herbert, additional, Milillo, Anna, additional, Miyoshi, Yoshizumi, additional, Nakamura, Rumi, additional, Plaschke, Ferdinand, additional, Richter, Ingo, additional, Rojas Mata, Sebastián, additional, Saito, Yoshifumi, additional, Schmid, Daniel, additional, Shiota, Daikou, additional, and Simon Wedlund, Cyril, additional

Published
2021
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38. MESSENGER observations of planetary ion characteristics within Kelvin- Helmholtz vortices at Mercury

Author

Aizawa, Sae, Raines, Jim, Delcourt, Dominique, Terada, Naoki, André, Nicolas, Institut de recherche en astrophysique et planétologie (IRAP), Centre National de la Recherche Scientifique (CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS)-Université Fédérale Toulouse Midi-Pyrénées-Centre National d'Études Spatiales [Toulouse] (CNES)-Météo France-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS)-Université Fédérale Toulouse Midi-Pyrénées-Centre National d'Études Spatiales [Toulouse] (CNES)-Météo France-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS), Tohoku University [Sendai], Department of Climate and Space Sciences and Engineering, University of Michigan, Laboratoire de Physique et Chimie de l'Environnement et de l'Espace (LPC2E), Observatoire des Sciences de l'Univers en région Centre (OSUC), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), and Graduate School of Information Sciences [Sendai]

Subjects
[PHYS]Physics [physics], [PHYS.ASTR.EP]Physics [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], Physics::Space Physics, Astrophysics::Earth and Planetary Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract

The MErcury Surface, Space ENvironment, Geochemistry, and Ranging (MESSENGER) spacecraft regularly observed the magnetospheric flanks of Mercury during its orbital phase. Data from the Magnetometer (MAG) and the Fast Imaging Plasma Spectrometer (FIPS) allow us to investigate the statistical properties of planetary ions (Na+) in the presence of Kelvin-Helmholtz (KH) waves at the duskside magnetopause. We collect the data from orbits with clear signatures of KH waves under northward interplanetary magnetic field, as well as adjacent orbits that do not have KH signatures, and we compare the energy characteristics between the KH and non-KH events. Although low planetary counts in FIPS data make the comparison of these characteristics difficult, we find that in the presence of KH waves: (1) large counts of planetary ions are observed, (2) differences in Na+ energy spectra are only seen inside the magnetosphere, where they show a decelerating signature for ions with energies above 2.0 keV/e. These results suggest that planetary ions can stagnate within KH vortices and that electric field structures related to KH waves can decelerate planetary ions originating from the magnetotail region.

Published
2020

40. Solar Orbiter observations of magnetic Kelvin-Helmholtz waves in the solar wind

Author

Kieokaew, Rungployphan, primary, Lavraud, Benoit, additional, Ruffolo, David, additional, Matthaeus, William, additional, Yang, Yan, additional, Stawarz, Julia, additional, Aizawa, Sae, additional, Louarn, Philippe, additional, Rouillard, Alexis, additional, Génot, Vincent, additional, Fedorov, Andrey, additional, Pinto, Rui, additional, Foullon, Claire, additional, Owen, Christopher, additional, and Horbury, Timothy, additional

Published
2021
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45. Statistical study of non-adiabatic energization and transport in Kelvin-Helmholtz vortices 2 at Mercury Key words: Mercury's magnetosphere, Kelvin-Helmholtz instability, particle

Author

Aizawa, Sae, Delcourt, Dominique, Terada, Naoki, André, Nicolas, 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), Tohoku University [Sendai], 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), Graduate School of Information Sciences [Sendai], 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
Mercury's magnetosphere, Kelvin-Helmholtz instability, Planetary ion, Particle accelerationTransport, [PHYS.ASTR.EP]Physics [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], [SDU]Sciences of the Universe [physics], Astrophysics::High Energy Astrophysical Phenomena, Physics::Space Physics, Astrophysics::Earth and Planetary Astrophysics
Abstract

International audience; Non-adiabatic energization and transport of planetary ions in the vicinity of Kelvin-Helmholtz (KH) vortices at Mercury are statistically investigated using a magnetohydrodynamic model combined with a test particle tracing technique. The measurements from the MErcury Surface, Space ENvironment, GEochemistry, and Ranging spacecraft show the signature of KH waves in the magnetospheric flanks, especially on the duskside. We examine here the energization and transport of heavy ions of planetary origin such as associated with the growth of the KH instability on both the dawn and dusk sides Na+ of the magnetosphere, and for both northward and southward interplanetary magnetic field configurations. We find that in all cases picked up planetary ions in the magnetosphere can be accelerated non-adiabatically with a level of acceleration larger on the dawnside. The transport of ions is controlled by the convection electric field in the magnetosheath. The planetary ions picked up in the duskside magnetosphere stagnate inside the magnetosphere where the KH waves have been mainly observed at Mercury and, hence, are not expected to escape. The present study indicates that these energized ions may likely stay inside the magnetosphere and sputter the planetary surface on the duskside preferentially, being the source of secondary neutrals from the planetary surface.

Published
2020
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46. MESSENGER observations of planetary ion characteristics within Kelvin-Helmholtz vortices

Author

Aizawa, Sae, Raines, Jim, Terada, Naoki, Delcourt, Dominique, Andre, Nicolas, 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 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), Laboratoire de Physique des Plasmas (LPP), 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
[SDU]Sciences of the Universe [physics], Physics::Space Physics, Astrophysics::Earth and Planetary Astrophysics
Abstract

International audience; The MErcury Surface, Space ENvironment, GEochemistry, and Ranging (MESSENGER) spacecraft regularly observed the magnetospheric flanks of Mercury during its orbital phase, 2011-2015. Data from the magnetometer (MAG) and Fast Imaging Plasma Spectrometer (FIPS) allow us to investigate the statistical properties of planetary ions in the presence of Kelvin-Helmholtz (KH) vortices near the duskside magnetopause. We collect data from orbits with clear signatures of KH waves, as well as consecutive orbits that do not have KH signatures, and we compare energy characteristics between KH and non-KH events. Although low planetary counts in FIPS data make the comparison of these characteristics difficult, we find that : (1) large counts of planetary ions are observed in the presence of KH waves, (2) differences in Na+ energy spectra are only seen inside the magnetosphere, where they show a decelerating signature for KH events for ions with energies above 2.0 keV/e. These results suggest that planetary ions can stagnate within KH vortices and that electric field structures related to KH waves can decelerate planetary ions originating from the magnetotail region. In this study, I analyzed the whole data by myself and compared with my previous numerical studies.

Published
2019

47. Review of Mercury's dynamic magnetosphere: Post-MESSENGER era and comparative magnetospheres.

Author

Sun, Weijie, Dewey, Ryan M., Aizawa, Sae, Huang, Jia, Slavin, James A., Fu, Suiyan, Wei, Yong, and Bowers, Charles F.

Subjects
MAGNETOSPHERE, MAGNETIC reconnection, INTERPLANETARY medium, MERCURY (Planet), MERCURY (Element)
Abstract

This review paper summarizes the research of Mercury's magnetosphere in the Post-MESSENGER era and compares its dynamics to those in other planetary magnetospheres, especially to those in Earth's magnetosphere. This review starts by introducing the planet Mercury, including its interplanetary environment, magnetosphere, exosphere, and conducting core. The frequent and intense magnetic reconnection on the dayside magnetopause, which is represented by the flux transfer event "shower", is reviewed on how they depend on magnetosheath plasma β and magnetic shear angle across the magnetopause, following by how it contributes to the flux circulation and magnetosphere-surface-exosphere coupling. In the next, Mercury's magnetosphere under extreme solar events, including the core induction and the reconnection erosion on the dayside magnetosphere, the responses of the nightside magnetosphere, are reviewed. Then, the dawn-dusk properties of the plasma sheet, including the features of the ions, the structure of the current sheet, and the dynamics of magnetic reconnection, are summarized. The last topic is devoted to the particle energization in Mercury's magnetosphere, which includes the energization of the Kelvin-Helmholtz waves on the magnetopause boundaries, reconnection-generated magnetic structures, and the cross-tail electric field. In each chapter, the last section discusses the open questions related to each topic, which can be considered by the simulations and the future spacecraft mission. We end this paper by summarizing the future BepiColombo opportunities, which is a joint mission of ESA and JAXA and is en route to Mercury. [ABSTRACT FROM AUTHOR]

Published
2022
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48. A 3D MHD‐Particle Tracing Model of Na+ Energization on Mercury's Dayside.

Author

Glass, Austin N., Raines, Jim M., Jia, Xianzhe, Tenishev, Valeriy, Shou, Yinsi, Aizawa, Sae, and Slavin, James A.

Subjects
PHOTOIONIZATION, SPECTROMETERS, MAGNETOHYDRODYNAMICS, EXOSPHERE, COMPUTER simulation
Abstract

Data collected by the Fast Imaging Plasma Spectrometer (FIPS) aboard the MErcury Surface, Space ENvironment, GEochemistry, and Ranging (MESSENGER) spacecraft showed singly charged Na+‐group ions at energies of between 1 and 13 keV in Mercury's northern planetary cusp. Most of these ions are likely formed by either photoionization or charge exchange of exospheric Na atoms, with initial energies of approximately 1 eV or less. FIPS observations did not establish which acceleration mechanism most reasonably accounts for this energy gain. Using the Adaptive Mesh Particle Simulator (AMPS) model, we undertake kinetic simulations of 1 eV Na+ test particles through the electric and magnetic fields output from the Block Adaptive Tree Solar wind Roe‐type Upwind Scheme (BATSRUS) global magnetohydrodynamic (MHD) model of Mercury's magnetosphere, in search of plausible explanations for the source of this energization. We find that Na+ with initial energy of 1 eV are readily picked up by the Dungey cycle return flow in the dayside magnetosphere. In some cases, this flow provides the energy for the ions to escape into the magnetosheath, and in other cases it energizes the ions to hundreds of eV before they pass immediately into the cusp. Those that escape can be rapidly picked up into the magnetosheath flow, where they are accelerated by pickup again up to tens of keV. These one‐ and two‐stage pickup processes on Mercury's dayside can account for the energies of many of the Na+ ions observed in Mercury's northern magnetospheric cusp by MESSENGER. Plain Language Summary: Data collected in orbit at Mercury showed sodium ions in the northern planetary cusp at high energies. The processes that likely create these ions are only responsible for 0.01%–0.1% of that high energy, and no mechanism previously known to operate at Mercury can account for the difference. We model the Mercury system, and the paths of ions through that system, in search of such a mechanism. We find two mechanisms, both involving energization into proton flows, that explain the data observations. Key Points: Sodium ions (Na+) with initial energy of 1 eV are energized by Dungey cycle return flow in the dayside dipolar regionNa+ are not trapped within the dayside dipolar region of MercuryOne‐ and two‐stage pickup processes can energize Na+ up to tens of keV entirely on the dayside [ABSTRACT FROM AUTHOR]

Published
2021
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