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320 results on '"Benoit Lavraud"'

1. Capsule Electron Distributions Near the Diffusion Region of Magnetic Reconnection

Author

Yong Ren, Lei Dai, Chi Wang, Benoit Lavraud, C. Philippe Escoubet, and James L. Burch

Subjects
magnetic reonnection, electron distribution, whistler waves, non‐Maxwellian distribution, electron heating, Geophysics. Cosmic physics, QC801-809
Abstract

Abstract Understanding electron kinetic processes is crucial for elucidating the energy conversion mechanisms in magnetic reconnection. Non‐Maxwellian electron distributions are strong indicators of kinetic‐scale processes near the electron diffusion region, yet they remain incompletely understood. Using in‐situ spacecraft data from 29 magnetopause reconnection events, we unambiguously identify a non‐Maxwellian capsule electron distribution near the electron diffusion region. This distribution comprises an elongated component parallel with the magnetic field at lower energies and a butterfly component (with peaks at pitch angles near 45° and 135°) at higher energies. We provide evidence that these distributions are partly linked to electron trapping and preferential heating along the direction of magnetic fields. The parallel electric potentials needed for the parallel heating may be linked to kinetic Alfvén waves. These capsule‐like electron distributions are also found to generate whistler emissions. Our results suggest that these kinetic processes are prevalent in magnetic reconnection.

Published
2024
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2. Editorial: The future of space physics 2022

Author

Joseph E. Borovsky, Gian Luca Delzanno, Philip J. Erickson, Alexa Jean Halford, Benoit Lavraud, and Sabrina Savage

Subjects
space physics, ionosphere, magnetosphere, solar wind, solar physics, heliosphere, Astronomy, QB1-991, Geophysics. Cosmic physics, QC801-809
Published
2024
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3. Connecting Solar Wind Velocity Spikes Measured by Solar Orbiter and Coronal Brightenings Observed by SDO

Author

Chuanpeng Hou, Alexis P. Rouillard, Jiansen He, Bahaeddine Gannouni, Victor Réville, Philippe Louarn, Andrey Fedorov, Lubomír Přech, Christopher J. Owen, Daniel Verscharen, Raffaella D’Amicis, Luca Sorriso-Valvo, Naïs Fargette, Jesse Coburn, Vincent Génot, Jim M. Raines, Roberto Bruno, Stefano Livi, Benoit Lavraud, Nicolas André, Gabriel Fruit, Rungployphan Kieokaew, Illya Plotnikov, Emmanuel Penou, Alain Barthe, Dhiren Kataria, Matthieu Berthomier, Frederic Allegrini, Vito Fortunato, Gennaro Mele, and Timothy Horbury

Subjects
Interplanetary magnetic fields, Solar wind, Solar coronal transients, Supergranulation, Astrophysics, QB460-466
Abstract

The Parker Solar Probe's discovery that magnetic switchbacks and velocity spikes in the young solar wind are abundant has prompted intensive research into their origin(s) and formation mechanism(s) in the solar atmosphere. Recent studies, based on in situ measurements and numerical simulations, argue that velocity spikes are produced through interchange magnetic reconnection. Our work studies the relationship between interplanetary velocity spikes and coronal brightenings induced by changes in the photospheric magnetic field. Our analysis focuses on the characteristic periodicities of velocity spikes detected by the Proton Alpha Sensor on the Solar Orbiter during its fifth perihelion pass. Throughout the time period analyzed here, we estimate their origin along the boundary of a coronal hole. Around the boundary region, we identify periodic variations in coronal brightening activity observed by the Atmospheric Imaging Assembly onboard the Solar Dynamics Observatory. The spectral characteristics of the time series of in situ velocity spikes, remote coronal brightenings, and remote photospheric magnetic flux exhibit correspondence in their periodicities. Therefore, we suggest that the localized small-scale magnetic flux within coronal holes fuels a magnetic reconnection process that can be observed as slight brightness augmentations and outward fluctuations or jets. These dynamic elements may act as mediators, bonding magnetic reconnection with the genesis of velocity spikes and magnetic switchbacks.

Published
2024
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4. Asymmetric deformation of the Earth’s magnetosphere under low Alfvén Mach number solar wind: Observations and MHD simulation

Author

Masaki N. Nishino, Hiroshi Hasegawa, Yoshifumi Saito, Benoit Lavraud, Yukinaga Miyashita, Motoharu Nowada, Satoshi Kasahara, and Tsugunobu Nagai

Subjects
Low density solar wind, Earth’s magnetosphere, Alfvén Mach number, Solar wind–magnetosphere interaction, Geography. Anthropology. Recreation, Geodesy, QB275-343, Geology, QE1-996.5
Abstract

Abstract The density of the solar wind plasma near the Earth’s magnetosphere sometimes decreases to only several per cent of the usual value, and such density extrema result in a significant reduction of the dynamic pressure and Alfvén Mach number ( $$M_A$$ M A ) of the solar wind flow. While a symmetric expansion of the Earth’s magnetosphere by the low dynamic pressure was assumed in previous studies, a global magnetohydrodynamic (MHD) simulation study predicted a remarkable dawn-dusk asymmetry of the magnetospheric shape under low-density solar wind and Parker-spiral interplanetary magnetic field (IMF) configuration. Here, we present observations consistent with the asymmetric deformation of the magnetosphere under low- $$M_A$$ M A solar wind and Parker-spiral IMF conditions, focusing on the significant expansion of the dawn-flank magnetosphere detected by the Geotail spacecraft. A global MHD simulation reproduced the dawnward expansion of the near-Earth magnetosphere, which was consistent with the observation by Geotail. The solar wind flow had a non-negligible dusk-to-dawn component and partly affected the dawnward expansion of the magnetosphere. Local, roughly Alfvénic sunward acceleration of magnetosheath ions at the dawn flank magnetopause suggests magnetosheath plasma entry into the magnetosphere through open field lines generated by magnetic reconnection at the dayside magnetopause. At the same time, Cluster 1 and 3, located near the southern polar cusp, also detected continuous antisunward ion jets and occasional sunward jets, which are consistent with the occurrence of magnetic reconnection near the southern cusp. These observations suggest that enhanced plasma acceleration at the dayside magnetopause operates under the low- $$M_A$$ M A solar wind and Parker spiral IMF conditions and that plasma influx across the dawnside magnetopause is at work under such a low- $$M_A$$ M A condition. These results can be helpful in understanding interactions between low- $$M_A$$ M A solar/stellar winds and celestial objects, such as inner planets and exoplanets. Graphic Abstract

Published
2022
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5. Evidence of a Thick Heliopause Boundary Layer Resulting from Active Magnetic Reconnection with the Interstellar Medium

Author

Drew L. Turner, Adam Michael, Elena Provornikova, Marc Kornbleuth, Merav Opher, Stefan Eriksson, Benoit Lavraud, Parisa Mostafavi, Matthew E. Hill, Pontus Brandt, Ian J. Cohen, Joseph Westlake, John D. Richardson, Nathan A. Schwadron, and David J. McComas

Subjects
Heliopause, Stellar-interstellar interactions, Heliosheath, Heliosphere, Astrospheres, Interstellar medium, Astrophysics, QB460-466
Abstract

Voyager 1 and 2 data from the vicinity of the heliopause and very local interstellar medium are reexamined to better understand the confounding lack of rotation in the magnetic field ( B -field) across the heliopause observed by both Voyagers, despite their very large spatial separations (>100 au). Using three estimates for the orientation of the B -field in the pristine interstellar medium and four models of the heliosphere, we calculate draped interstellar B -field orientations along the model heliopauses and compare those estimates to the Voyager observations. At both Voyagers, expected draped B -fields are inconsistent with the observed B -field orientations after the boundary crossings. Furthermore, we show how the longer-term trends of the observed B -fields at both Voyagers after the crossings actually rotated away from both the expected draped B -field and the pristine interstellar B -field directions. We develop evidence, including an illustrative and analogous set of observations from Magnetospheric Multiscale spacecraft along Earth’s magnetopause, in support of a hypothesis that both Voyagers transited a thick boundary layer of reconnected magnetic flux along the heliopause surface. We estimate that Voyager 1 has not yet fully transited this boundary layer, the radial thickness of which at the Voyager 1 crossing location may be >18 au and likely much thicker. Meanwhile, at Voyager 2's crossing location, the boundary layer is likely much thinner, and for Voyager 2, we present evidence that Voyager 2 might already have transited the boundary layer and entered a region of fields and plasma that were never connected to the Sun—the very local interstellar medium.

Published
2024
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6. On the importance of investigating CME complexity evolution during interplanetary propagation

Author

Réka M. Winslow, Camilla Scolini, Lan K. Jian, Teresa Nieves-Chinchilla, Manuela Temmer, Fernando Carcaboso, Brigitte Schmieder, Stefaan Poedts, Benjamin J. Lynch, Brian E. Wood, Erika Palmerio, Noé Lugaz, Charles J. Farrugia, Christina O. Lee, Emma E. Davies, Florian Regnault, Tarik M. Salman, Tibor Török, Nada Al-Haddad, Angelos Vourlidas, Ward B. Manchester, Meng Jin, Benoit Lavraud, and Antoinette B. Galvin

Subjects
CME, heliosphere, magnetic ejecta, flux rope, Sun, Astronomy, QB1-991, Geophysics. Cosmic physics, QC801-809
Abstract

This perspective paper brings to light the need for comprehensive studies on the evolution of interplanetary coronal mass ejection (ICME) complexity during propagation. To date, few studies of ICME complexity exist. Here, we define ICME complexity and associated changes in complexity, describe recent works and their limitations, and outline key science questions that need to be tackled. Fundamental research on ICME complexity changes from the solar corona to 1 AU and beyond is critical to our physical understanding of the evolution and interaction of transients in the inner heliosphere. Furthermore, a comprehensive understanding of such changes is required to understand the space weather impact of ICMEs at different heliospheric locations and to improve on predictive space weather models.

Published
2022
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7. STELLA—Potential European contributions to a NASA-led interstellar probe

Author

Robert F. Wimmer-Schweingruber, Nicolas André, Stanislav Barabash, Pontus C. Brandt, Timothy S. Horbury, Luciano Iess, Benoit Lavraud, Ralph L. McNutt, Elena A. Provornikova, Eric Quémerais, Robert Wicks, Martin Wieser, and Peter Wurz

Subjects
mission proposal, interstellar probe, space science, solar system, very local interstellar medium, fundamental physics, Astronomy, QB1-991, Geophysics. Cosmic physics, QC801-809
Abstract

The discovery of a myriad of exoplanets in the past decades has revolutionized the understanding of our place in the Universe. How different are exoplants and do some of them harbor life, just like Earth? To do so, their parent stars must drive a stellar wind and carve what we call astrospheres into the surrounding interstellar medium. Astrospheres are ubiquitous in our immediate neighborhood and show similar structure to our heliosphere. Voyager 1 and 2, Ulysses, Cassini, and IBEX have shown that the interaction between interstellar medium and solar wind is much more complex and involved than previously believed. This stellar-interstellar interaction is key to understand astrospheres and the shielding they provide to the planetary systems they harbor. This article summarizes a whitepaper that was submitted to NASA’s 2023/2024 decadal survey which is being conducted by the US National Academies. It is based in parts on a proposal submitted to the European Space Agency (ESA) in response to its 2021 call for medium-class mission proposals. The whitepaper and this article propose to study the interaction described above in situ at the heliospheric boundaries and to explore the very local interstellar medium beyond. Furthermore, they highlight possible European contributions to a NASA-led Interstellar Probe (ISP).

Published
2022
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8. Geoeffectiveness of Interplanetary Alfvén Waves. I. Magnetopause Magnetic Reconnection and Directly Driven Substorms

Author

Lei Dai, Yimin Han, Chi Wang, Shuo Yao, Walter Gonzalez, Suping Duan, Benoit Lavraud, Yong Ren, and Zhenyuan Guo

Subjects
Solar-terrestrial interactions, Solar-planetary interactions, Planetary magnetospheres, Solar magnetic reconnection, Astrophysics, QB460-466
Abstract

In particular during the descending phase of the solar cycle, Alfvén waves in the high-speed solar wind streams are a major form of interplanetary disturbances. The fluctuating southward interplanetary magnetic field (IMF) of Alfvén waves has been suggested to induce geomagnetic activities through intermittent magnetic reconnection at the magnetopause. In this study, we provide in situ observational evidence for dayside magnetopause reconnection induced by such interplanetary Alfvén waves. Using multipoint conjunction observations, we show that the IMF B _z from interplanetary Alfvén waves is transmitted through and amplified by the Earth’s bow shock. Associated with the intensified southward B _z to the magnetopause, in situ signatures of magnetic reconnection are detected. Repetitively, interplanetary Alfvén waves transmit the intensified B _z to the magnetosheath, leading to intervals of large magnetic shear angles across the magnetopause and magnetopause reconnection. Such intervals are promptly followed by hundreds of nanoTesla (nT) increases in the auroral electrojet indices (AE and AU) within 10–20 minutes. These observations are confirmed in multiple events in corotating interaction region-driven geomagnetic storms. To put the observations into context, we propose a phenomenological model of a strongly driven substorm. The substorm electrojet is linked to the enhanced magnetopause reconnection in the short timescale of re-establishing the ionosphere electric field and the two-cell convection. These results provide insights on the temporal patterns of solar wind magnetosphere–ionosphere coupling, especially during the descending phase of the solar cycle.

Published
2023
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9. Geoeffectiveness of Interplanetary Alfvén Waves. II. Spectral Characteristics and Geomagnetic Responses

Author

Yimin Han, Lei Dai, Shuo Yao, Chi Wang, Walter Gonzalez, Suping Duan, Benoit Lavraud, Yong Ren, and Zhenyuan Guo

Subjects
Planetary magnetospheres, Solar-terrestrial interactions, Solar-planetary interactions, Astrophysics, QB460-466
Abstract

Using multipoint observations over 10 yr near 1 au, we investigate the spectra (5 minutes to 2 hr) of interplanetary Alfvén waves and the responses in the geomagnetic activities. We compute the two-point correlations of the wave magnetic field between the ACE and the THEMIS spacecraft, which are separated by ∼200 Earth radius ( R _E ) in the solar wind. Alfvén waves associated with high two-point correlations exhibit steep spectra (spectra index ∼−1.63). Such Alfvén waves occur mostly in slow-speed streams. By contrast, Alfvén waves with low two-point correlations exhibit flatter spectra (spectra index ∼−1.51) with a relative enhancement of power above 2 × 10 ^−4 Hz. The occurrence of Alfvén waves with low two-point correlations is more equally distributed between high-speed and low-speed streams. In general, interplanetary Alfvén waves show correlations with moderate geomagnetic responses in symmetric ring-current intensity, SuperMAG electrojet (SME), and Kp indices. Statistical analyses indicate that the Alfvén waves with flat spectra correspond to stronger responses in the geomagnetic indices than those with steep spectra, suggesting the importance of the tens of minutes (30–90 minutes) Alfvénic power spectra in the generation of SME/Auroral Electrojets. These observations may shed light on the response of the magnetosphere to fluctuating interplanetary magnetic field B _z .

Published
2023
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11. Wave-particle energy exchange directly observed in a kinetic Alfvén-branch wave

Author

Daniel J. Gershman, Adolfo F-Viñas, John C. Dorelli, Scott A. Boardsen, Levon A. Avanov, Paul M. Bellan, Steven J. Schwartz, Benoit Lavraud, Victoria N. Coffey, Michael O. Chandler, Yoshifumi Saito, William R. Paterson, Stephen A. Fuselier, Robert E. Ergun, Robert J. Strangeway, Christopher T. Russell, Barbara L. Giles, Craig J. Pollock, Roy B. Torbert, and James L. Burch

Subjects
Science
Abstract

Alfvén waves are fundamental plasma modes that provide a mechanism for the transfer of energy between particles and fields. Here the authors confirm experimentally the conservative energy exchange between Alfvén wave fields and plasma particles via high-resolution MMS observations of Earth’s magnetosphere.

Published
2017
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12. Cluster and MMS Simultaneous Observations of Magnetosheath High Speed Jets and Their Impact on the Magnetopause

Author

C. Philippe Escoubet, K.-J. Hwang, S. Toledo-Redondo, L. Turc, S. E. Haaland, N. Aunai, J. Dargent, Jonathan P. Eastwood, R. C. Fear, H. Fu, K. J. Genestreti, Daniel B. Graham, Yu V. Khotyaintsev, G. Lapenta, Benoit Lavraud, C. Norgren, D. G. Sibeck, A. Varsani, J. Berchem, A. P. Dimmock, G. Paschmann, M. Dunlop, Y. V. Bogdanova, Owen Roberts, H. Laakso, Arnaud Masson, M. G. G. T. Taylor, P. Kajdič, C. Carr, I. Dandouras, A. Fazakerley, R. Nakamura, Jim L. Burch, B. L. Giles, C. Pollock, C. T. Russell, and R. B. Torbert

Subjects
magnetosheath, magnetopause, high-speed jet, multi-scale, turbulence, Astronomy, QB1-991, Geophysics. Cosmic physics, QC801-809
Abstract

When the supersonic solar wind encounters the Earth's magnetosphere a shock, called bow shock, is formed and the plasma is decelerated and thermalized in the magnetosheath downstream from the shock. Sometimes, however, due to discontinuities in the solar wind, bow shock ripples or ionized dust clouds carried by the solar wind, high speed jets (HSJs) are observed in the magnetosheath. These HSJs have typically a Vx component larger than 200 km s−1 and their dynamic pressure can be a few times the solar wind dynamic pressure. They are typically observed downstream from the quasi-parallel bow shock and have a typical size around one Earth radius (RE) in XGSE. We use a conjunction of Cluster and MMS, crossing simultaneously the magnetopause, to study the characteristics of these HSJs and their impact on the magnetopause. Over 1 h 15 min interval in the magnetosheath, Cluster observed 21 HSJs. During the same period, MMS observed 12 HSJs and entered the magnetosphere several times. A jet was observed simultaneously by both MMS and Cluster and it is very likely that they were two distinct HSJs. This shows that HSJs are not localized into small regions but could span a region larger than 10 RE, especially when the quasi-parallel shock is covering the entire dayside magnetosphere under radial IMF. During this period, two and six magnetopause crossings were observed, respectively, on Cluster and MMS with a significant angle between the observation and the expected normal deduced from models. The angles observed range between from 11° up to 114°. One inbound magnetopause crossing observed by Cluster (magnetopause moving out at 142 km s−1) was observed simultaneous to an outbound magnetopause crossing observed by MMS (magnetopause moving in at −83 km s−1), showing that the magnetopause can have multiple local indentation places, most likely independent from each other. Under the continuous impacts of HSJs, the magnetopause is deformed significantly and can even move in opposite directions at different places. It can therefore not be considered as a smooth surface anymore but more as surface full of local indents. Four dust impacts were observed on MMS, although not at the time when HSJs are observed, showing that dust clouds would have been present during the observations. No dust cloud in the form of Interplanetary Field Enhancements was however observed in the solar wind which may exclude large clouds of dust as a cause of HSJs. Radial IMF and Alfvén Mach number above 10 would fulfill the criteria for the creation of bow shock ripples and the subsequent crossing of HSJs in the magnetosheath.

Published
2020
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13. The need for reference-able and peer reviewed position papers

Author

Alexa Jean Halford, Benoit Lavraud, Sabrina Savage, Joseph E Borovsky, and Gina Luca Delzanno

Subjects
Space Sciences (General)
Abstract

Space Physics community members are putting substantial efforts and ideas into position papers, in preparation for the U.S. Heliophysics Decadal Survey process; an analysis of the current state of the field and where future research, mission programs, and funding should focus. Furthermore, Space Physics community members in Europe and the U.S. have recently put substantial efforts and ideas into position papers for Vision 2050 and Heliophysics 2050. There are also other ideas in the community about the needs and focus of future Space Physics research efforts, whether they were submitted to other road mapping activities, or have yet to find the appropriate home. With this in mind, we have created a Frontiers in Astronomy and Space Sciences Research Topic ’The Future of Space Physics 2022’, to provide a format for a reference-able, peer reviewed, archived, accessible collection of these ideas from around the world. We wish to make these ideas available to the national academies decadal survey committees, the broader research community and a wider audience, by developing this collection. The collection will publish high-quality papers on key topics across the field of Space Physics, aiming to highlight recent advances in the field, whilst emphasizing important directions and new possibilities for future inquiries.

Published
2022

14. A Case for Electron-Astrophysics

Author

Daniel Verscharen, Robert T. Wicks, Olga Alexandrova, Roberto Bruno, David Burgess, Christopher H. K. Chen, Raffaella D’Amicis, Johan De Keyser, Thierry Dudok de Wit, Luca Franci, Jiansen He, Pierre Henri, Satoshi Kasahara, Yuri Khotyaintsev, Kristopher G. Klein, Benoit Lavraud, Bennett A. Maruca, Milan Maksimovic, Ferdinand Plaschke, Stefaan Poedts, Christopher S. Reynolds, Owen Roberts, Fouad Sahraoui, Shinji Saito, Chadi S. Salem, Joachim Saur, Sergio Servidio, Julia E. Stawarz, Štěpán Štverák, and Daniel Told

Published
2021
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16. Characteristic Scales of Magnetic Switchback Patches Near the Sun and Their Possible Association With Solar Supergranulation and Granulation

Author

Naïs Fargette, Benoit Lavraud, Alexis P. Rouillard, Victor Réville, Thierry Dudok De Wit, Clara Froment, Jasper S. Halekas, Tai D. Phan, David M. Malaspina, Stuart D. Bale, Justin C. Kasper, Philippe Louarn, Anthony W. Case, Kelly E. Korreck, Davin E. Larson, Marc Pulupa, Michael L. Stevens, Phyllis L. Whittlesey, and Matthieu Berthomier

Published
2021
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17. Source and Propagation of a Streamer Blowout Coronal Mass Ejection Observed by the Parker Solar Probe

Author

Kelly Elizabeth Korreck, Adam Szabo, Teresa Nieves-Chinchilla, Benoit Lavraud, Janet Luhmann, Tatiana Niembro, Aleida Higginson, Nathalia Alzate, Samantha Wallace, Kristoff Paulson, Alexis Rouillard, Athanasios Kouloumvakos, Nicolas Poirier, Justin C Kasper, A W Case, Michael L Stevens, Stuart D Bale, Marc Pulupa, Phyllis Whittlesey, Roberto Livi, Keith Goetz, David Larson, David M Malaspina, Huw Morgan, Ayris A Narock, Nathan A Schwadron, John Bonnell, Peter Harvey, and John Wygant

Subjects
Astrophysics
Abstract

In the first orbit of the Parker Solar Probe (PSP), in situ thermal plasma and magnetic field measurements were collected as close as 35RSun from the Sun, an environment that had not been previously explored. During the first orbit of PSP, the spacecraft flew through a streamer blowout coronal mass ejection (SBO-CME) on 2018 November 11 at 23:50 UT as it exited the science encounter. The SBO-CME on November 11 was directed away from the Earth and was not visible by L1 or Earth-based telescopes due to this geometric configuration. However, PSP and the STEREO-A spacecraft were able to make observations of this slow (v ≈ 380 kms−1) SBO-CME. Using the PSP data, STEREO-A images, and Wang–Sheeley–Arge model, the source region of the CME is found to be a helmet streamer formed between the northern polar coronal hole and a mid-latitude coronal hole. Using the YGUAZU-A model, the propagation of the CME is traced from the source at the Sun to PSP. This model predicts the travel time of the flux rope to the PSP spacecraft as 30 hr, which is within 0.33 hr of the actual measured arrival time. The in situ Solar Wind Electrons Alphas and Protons data were examined to determine that no shock was associated with this SBO-CME. Modeling of the SBO-CME shows that no shock was present at PSP; however, at other positions along the SBO-CME front, a shock could have formed. The geometry of the event requires in situ and remote sensing observations to characterize the SBO-CME and further understand its role in space weather.

Published
2020
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18. 90° PA ojačitve supertermičnih elektronov v bližini medplanetarnih udarnih valov

Author

Primož Kajdič, Benoit Lavraud, Xóchitl Blanco-Cano, Jean-Andre Sauvaud, Arnaud Zaslavsky Arnaud Zaslavsky, Andrea Opitz, Lan K. Jian, Christopher T. Russell, Janet G. Luhmann, and Milan Maksimovic

Abstract

V tem pismu poročamo o prvi sistematični študiji tipa populacije supertermičnih elektronov v sončevem vetru, imenovane ojačitve pri 90° PA (ang. pitch angle). Ta populacija je bila najdena v bližini medplanetarnih udarnih valov, pri čemer smo analizirali dvourne časovne intervale centrirane na udarnih valovih. Ojačitve pri 90° PA smo našli pri 114 od 232 (49 %) dogodkov, kar pomeni, da je ta tip populacije dokaj pogost v sončevem vetru. Statistična analiza lastnosti medplanetarnih udarnih valov je pokazala, da ni bistvenih razlik v lastnostih med udarnimi valovi ob katerih so bile ojačitve prosotne in tistimi kjer jih ni bilo. Preliminarna analiza fluktuacij električnega polja pa je pokazala, da je njihova aktivnost intenzivnejša v bližini udarnih valov, ob katerih smo našli ojačitve pri 90° PA.

Published
2022
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19. Solar Orbiter reveals that reconnection jets cluster in the solar wind

Author

Naïs Fargette, Benoit Lavraud, Alexis Rouillard, Pierre Houdayer, Tai Phan, Marit Oieroset, Jonathan Eastwood, Andrei Fedorov, Philippe Louarn, Christopher Owen, and Tim Horbury

Abstract

Magnetic reconnection is a fundamental process in astrophysical plasma, as it enables the dissipation of energy at kinetic scales. Detecting it in-situ is therefore key to further our understanding of energy conversion in space plasma. However, ion reconnection jets usually scale from seconds to minutes in-situ, and as such they can be quite tedious to find in the months or years of data provided by Wind, ACE, Helios, PSP and Solar Orbiter.In this work, we use a new approach to identify automatically reconnection exhausts in-situ. The method strongly relies on the Walén relation and uses Bayesian inference as well as physical considerations to detect reconnection jets in-situ. Applying the detection algorithm to one month of Solar Orbiter data at 0.7 ~AU, we find an occurrence rate of 6.4~jets/day, which is significantly higher than in previous studies performed at 1~AU. We repeat the analysis over the Solar Orbiter perihelion at 0.3 AU and show that the occurrence rate of magnetic reconnection tends to increase with radial distance.We show that magnetic reconnection exhausts clearly cluster in the solar wind. We perform a statistical analysis, distinguishing between the exhausts associated with the heliospheric current sheet and turbulent reconnection. We find that the source and the degree of Alfvénicity of the solar wind might have an impact on magnetic reconnection occurrence.

Published
2023
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20. Global environmental constraints on magnetic reconnection at the magnetopause from in situ measurements

Author

Bayane Michotte de Welle, Nicolas Aunai, Benoit Lavraud, Vincent Génot, and Roch Smets

Abstract

The location of magnetic reconnection at the Earth's magnetopause is a longstanding question in the field of magnetospheric physics. Various models (Alexeev et al. 1998, Borovsky 2013, Trattner et al. 2007, etc) predicting the position of the X-line have been proposed. These models often rely on quantities whose global spatial distributions at the magnetopause are typically obtained through numerical simulations. In this study, we attempt to reconstruct these global distributions using only in-situ measurements. To do this, we have used statistical learning to automatically select in-situ data from four missions (Cluster, Doublestar, THEMIS, MMS). The 3D reconstruction of the magnetic field draping in the dayside magnetosheath (Michotte de Welle et al. 2022) reveals significant differences with the model of Kobel et Fluckiger 1994 for a certain range of IMF orientations. As this magnetostatic model is frequently used to predict magnetic shear at the magnetopause, we will examine the implications of these differences on the X-lines maximizing this quantity (Trattner et al. 2007). We will also extend this discussion to other relevant quantities such as current density and the Cassak-Shay reconnection rate, which can also be accessed using in-situ measurements.

Published
2023
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21. From research to the operation of solar wind forecasting with SafeSpace Helio1D: lessons learned and ways forward

Author

Rungployphan Kieokaew, Rui Pinto, Mikel Indurain, Evangelia Samara, Benoit Lavraud, Antoine Brunet, Stefaan Poedts, Vincent Génot, Alexis Rouillard, Sébastien Bourdarie, and Ioannis Daglis

Abstract

Our current capability of space weather prediction in the Earth's radiation belts is limited to only an hour in advance using solar wind monitoring at the Lagrangian L1 point. To mitigate the impacts of space weather on telecommunication satellites, advancing the lead time of the prediction is a critical task. We develop a prototype pipeline called "Helio1D" to forecast ambient solar wind conditions (speed, density, temperature, tangential magnetic field) at L1 with a lead time of 4 days. This pipeline predicts Corotating Interaction Regions (CIRs) in which their compressed stream interfaces and high-speed streams can increase high-energy fluxes in the radiation belts. The Helio1D pipeline connects the Multi-VP model, which provides real-time solar wind emergence at 0.14 AU, and the 1D MHD model. Using the long-term data from Multi-VP, we benchmark the Helio1D pipeline for solar wind speed against the observation data in 2004 - 2013 and 2017 - 2018. We developed a framework based on the Fast Dynamic Time Warping technique that allows us to continuously compare time-series outputs containing CIRs to observations to measure the pipeline's performance. In particular, we use this framework to calibrate and improve the pipeline's performance for operational forecasting. Since the 1D MHD model is computationally inexpensive, we provide daily ensemble forecasting of 21 members, including several targets around the Earth to account for the uncertainties. This pipeline can be used to feed real-time, daily solar wind forecasting to predict the dynamics of the inner magnetosphere and the radiation belts. In this presentation, we will share the lessons from this research-to-operation project and discuss ways to effectively implement operational space weather pipelines.

Published
2023
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22. Energy Conversion Associated with Flux Transfer Events at Earth’s Magnetopause

Author

Souhail Dahani, Benoit Lavraud, Vincent Génot, Sergio Toledo-Redondo, Rungployphan Kieokaew, Naïs Fargette, Daniel Gershman, Barbara Giles, Roy Torbert, and Jim Burch

Abstract

Flux Transfer Events (FTEs) are transient phenomena generated at the dayside magnetopause as a result of magnetic reconnection. FTEs have a significant role in the transfer of momentum and energy into the magnetosphere. We study here, in a multifluid framework, how the energy is converted within FTEs and their surrounding plasma. In particular we investigate how the plasma gains or loses kinetic energy through electric and/or pressure gradient terms. We also investigate the terms that control how the internal energy of the plasma is gained or dissipated through the pressure work term. Using observations from Magnetospheric MultiScale (MMS), we perform a statistical study based on an existing FTE catalog (Fargette et al., 2020). We analyze FTEs with or without internal current sheets. We discuss the contribution of the different terms in the energy conversion process separately for ions and electrons and as a function of location within the FTE. We analyze and compare the results found for FTEs’ intervals with magnetosheath intervals (Wang et al. 2021), taking into account their locations, using probability distribution functions of the various energy terms measured in each interval. This work contributes to a better understanding of energy conversion processes associated with FTEs at the magnetopause.

Published
2023
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23. Estimation of the error on the calculation of the pressure-strain term: application in the terrestrial magnetosphere

Author

Owen Wyn Roberts, Zoltán Voros, Klaus Torkar, Julia E. Stawarz, Riddhi Bandyopadhyay, Daniel J Gershman, Yasuhito Narita, Rungployphan Kieokaew, Benoit Lavraud, Kristopher Gregory Klein, Yan Yang, Rumi Nakamura, Alexandros Chasapis, and William H. Matthaeus

Abstract

Calculating the pressure-strain terms has recently been performed to quantify energy conversion between the bulk flow energy and the internal energy of plasmas. It has been applied to numerical simulations and satellite data from the Magnetospheric MultiScale Mission. The method requires spatial gradients of the velocity and the use of the full pressure tensor. Here we present a derivation of the errors associated with calculating the pressure-strain terms from multi-spacecraft measurements and apply it to previously studied examples of magnetic reconnection at the magnetopause and the magnetotail. The errors are small in a dense magnetosheath event but much larger in the more tenuous magnetotail. This is likely due to larger counting statistics in the dense plasma at the magnetopause than in the magnetotail. The propagated errors analyzed in this work are important to understand uncertainties of energy conversion measurements in space plasmas and have applications to current and future multi-spacecraft missions.

Published
2023
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28. Ion Kinetics in a Hot Flow Anomaly: MMS Observations

Author

Steven J Schwartz, Levon Avanov, Drew Turner, Hui Zhang, Imogen Gingell, Jonathan P Eastwood, Daniel J Gershman, Andreas Johlander, Christopher T Russell, James L Burch, John C Dorelli, Stefan Eriksson, Robert E Ergun, Stephen A Fuselier, Barbara L Giles, Katherine A Goodrich, Yuri V Khotyaintsev, Benoit Lavraud, Per‐Arne Lindqvist, Mitsuo Oka, Tai‐Duc Phan, Robert J Strangeway, Karlheinz J Trattner, Roy B Torbert, Andris Vaivads, Hanying Wei, and Frederick Wilder

Published
2018
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29. Whistler Waves Associated With Electron Beams in Magnetopause Reconnection Diffusion Regions

Author

Shan Wang, Naoki Bessho, Daniel B. Graham, Olivier Le Contel, Frederick D. Wilder, Yuri V. Khotyaintsev, Kevin J. Genestreti, Benoit Lavraud, Seung Choi, James L. Burch, Swedish Institute of Space Physics [Uppsala] (IRF), 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), 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), and Southwest Research Institute [San Antonio] (SwRI)

Subjects
Fusion, plasma och rymdfysik, Geophysics, Astronomi, astrofysik och kosmologi, Space and Planetary Science, [PHYS.ASTR.EP]Physics [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], Astronomy, Astrophysics and Cosmology, Fusion, Plasma and Space Physics
Abstract

Whistler waves are often observed in magnetopause reconnection associated with electron beams. We analyze seven MMS crossings surrounding the electron diffusion region (EDR) to study the role of electron beams in whistler excitation. Waves have two major types: (a) Narrow-band waves with high ellipticities and (b) broad-band waves that are more electrostatic with significant variations in ellipticities and wave normal angles. While both types of waves are associated with electron beams, the key difference is the anisotropy of the background population, with perpendicular and parallel anisotropies, respectively. The linear instability analysis suggests that the first type of wave is mainly due to the background anisotropy, with the beam contributing additional cyclotron resonance to enhance the wave growth. The second type of broadband waves are excited via Landau resonance, and as seen in one event, the beam anisotropy induces an additional cyclotron mode. The results are supported by particle-in-cell simulations. We infer that the first type occurs downstream of the central EDR, where background electrons experience Betatron acceleration to form the perpendicular anisotropy; the second type occurs in the central EDR of guide field reconnection. A parametric study is conducted with linear instability analysis. A beam anisotropy alone of above similar to 3 likely excites the cyclotron mode waves. Large beam drifts cause Doppler shifts and may lead to left-hand polarizations in the ion frame. Future studies are needed to determine whether the observation covers a broader parameter regime and to understand the competition between whistler and other instabilities.

Published
2022
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31. Global three-dimensional draping of magnetic field lines in Earth's magnetosheath from in-situ spacecraft measurements

Author

Bayane Michotte de Welle, Nicolas Aunai, Gautier Nguyen, Benoit Lavraud, Vincent Génot, Alexis Jeandet, Roch Smets, 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), Délégation générale de l'armement (DGA), Ministère de la Défense, Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), 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
[PHYS.ASTR.EP]Physics [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP]
Abstract

Magnetic field draping occurs when the magnetic field lines frozen in a plasma flow wrap around a body or plasma environment. The draping of the interplanetary magnetic field (IMF) around the Earth's magnetosphere has been confirmed in the early days of space exploration. However, its global and three-dimensional structure is known from modeling only, mostly numerical. Here, this structure in the dayside of the Earth's magnetosheath is determined as a function of the upstream IMF orientation purely from in-situ spacecraft observations. We show the draping structure can be organized in three distinct regimes depending on how radial the upstream IMF is. Quantitative analysis demonstrates how the draping pattern results from the frozen-in condition with the magnetosheath flow, deflected around the magnetopause.

Published
2022
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32. Global three-dimensional draping of magnetic field in Earth's magnetosheath from in-situ measurements

Author

Bayane Michotte de Welle, Nicolas Aunai, Gautier Nguyen, Benoit Lavraud, Vincent Genot, Roch Smets, and Alexis Jeandet

Abstract

Understanding where the magnetic reconnection occurs at the Earth’s magnetopause is one of the important remaining questions about this phenomena. Since the last decades various models predicting the position of the X-line have been made. These models largely depend on the orientation of the magnetic field in the magnetosheath close to the magnetopause, such as the Maximum Magnetic Shear model (Trattner et al 2007). Therefore understanding how it is structured as a function of the solar wind and interplanetary magnetic field is of pivotal importance. Machine learning was used to collect around 45 million measurements in the magnetosheath at 5s resolution in all available Cluster, MMS, Double Star, THEMIS dataset, and to build detailed maps of the field structure in that region as a function of the IMF orientation. It allowed us to reconstruct for the first time the three dimensional magnetic field draping in the dayside magnetosheath from in-situ data only. Our results reveal how the frozen-in condition constrains the draping around the magnetopause. A comparison of the draping obtained with in-situ data with the one from a widely used magnetostatic model (Kobel et al 1994) was made. Differences of up to 180° were found for cone angle between 12.5° and 45°, for which the consequences regarding the position of the X-line will be discussed.

Published
2022
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33. Characterization of Jason-3 Spacecraft Surface Charging in LEO Polar Regions From AMBER Observations

Author

Florine Enengl, Mika K. G. Holmberg, Fabrice Cipriani, Jean-Andre Sauvaud, Denis Payan, Jean-Charles Mateo-Velez, Angelica Sicard, Benoit Lavraud, Agence Spatiale Européenne = European Space Agency (ESA), Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Centre National d'Études Spatiales [Toulouse] (CNES), ONERA / DPHY, Université de Toulouse [Toulouse], and ONERA-PRES Université de Toulouse

Subjects
spacecraft charging, Nuclear and High Energy Physics, ELECTRIQUE, Condensed Matter Physics, plasma spectrometer, Electron, [PHYS.PHYS.PHYS-SPACE-PH]Physics [physics]/Physics [physics]/Space Physics [physics.space-ph], Electric potential, Satellite, [PHYS.PHYS.PHYS-PLASM-PH]Physics [physics]/Physics [physics]/Plasma Physics [physics.plasm-ph], ION, AUTOMOBILE, POTENTIEL, Automotive industry
Abstract

International audience; We have characterized spacecraft charging events in low Earth orbit (LEO) polar regions with the Active Monitor Box of Electrostatic Risk (AMBER) instrument onboard the Joint Altimetry Satellite Oceanography Network-3 (Jason-3) ocean topography mission for the first time for this spacecraft. AMBER data, taken at an altitude of 1336 km, over the period January 2017-March 2020, with measurements recorded close to the current solar minimum have been analyzed, using systematic filtering of ions spectrograms with selected threshold energies and time windows to detect negative spacecraft charging events; 109 spacecraft charging events were found. The events are examined visually and characterized by their spatial and temporal location, duration, and intensity (e.g., spacecraft potential). At the Jason-3 altitude (1336 km), the ion signature predominately lasts under 30 s in conjunction with auroral inverted V crossings, while intense fluxes of electrons corresponding to the encounter of the discrete auroral region last between 30 s and 1 min. Most of the detected spacecraft charging events show charging levels between −30 and −1000 V. The spacecraft charging events are located in the magnetic local time (MLT) sector 17h-05h, predominately before midnight. The distribution is equal between the northern and southern hemispheres. We found a high correlation between the charging time profile and that of the auroral electron average energy and energy flux along the satellite path. Overall statistics over three years as well as different event morphologies, electron spectra, and comparisons to worst case electron flux spectral distributions are presented and discussed.

Published
2022
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34. The preferential orientation of magnetic switchbacks, implications for solar magnetic flux transport

Author

Naïs Fargette, Benoit Lavraud, Alexis P. Rouillard, Victor Réville, Stuart D. Bale, Justin Kasper, 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 d'Astrophysique de Bordeaux [Pessac] (LAB), and Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)

Subjects
methods: statistical, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Sun: corona, Sun: photosphere, FOS: Physical sciences, Astronomy and Astrophysics, methods: data analysis, Space Physics (physics.space-ph), solar wind, Astrophysics - Solar and Stellar Astrophysics, Physics - Space Physics, Space and Planetary Science, [SDU]Sciences of the Universe [physics], Physics::Space Physics, Astrophysics::Solar and Stellar Astrophysics, Sun: magnetic fields, Solar and Stellar Astrophysics (astro-ph.SR)
Abstract

We investigate the orientation of the magnetic field deflections in switchbacks (SB) to determine if they are characterised by a possible preferential orientation. We compute the deflection angles of the magnetic field relative to the Parker spiral direction for encounters 1 to 9 of the PSP mission. We first characterize the distribution of these deflection angles for calm solar wind intervals, and assess the precision of the Parker model as a function of distance to the Sun. We then assume that the solar wind is composed of two populations, the background calm solar wind and the population of SB, characterized by larger fluctuations. We model the total distribution of deflection angles we observe in the solar wind as a weighed sum of two distinct normal distributions, each corresponding to one of the populations. We fit the observed data with our model using a MCMC algorithm and retrieve the most probable mean vector and covariance matrix coefficients of the two Gaussian functions, as well as the population proportion. We first observe that the accuracy of the spiral direction in the ecliptic is a function of radial distance, in a manner that is consistent with PSP being near the solar wind acceleration region. We then find that the fitted switchback population presents a systematic bias in its deflections compared to the calm solar wind population. This result holds for all encounters but E6, and regardless of the magnetic field main polarity. This implies a marked preferential orientation of SB in the clockwise direction in the ecliptic plane, and we discuss this result and its implications in the context of the existing switchback formation theories. Finally, we report the observation of a 12-hour patch of SB that systematically deflect in the same direction, so that the magnetic field vector tip within the patch deflects and returns to the Parker spiral within a given plane., Comment: 12 pages, 10 figures, 4 pages of appendix

Published
2022
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35. A Case for Electron-Astrophysics

Author

Satoshi Kasahara, Julia E. Stawarz, Thierry Dudok de Wit, Daniel Told, Yuri V. Khotyaintsev, Christopher S. Reynolds, Stepan Stverak, Bennett A. Maruca, David Burgess, Milan Maksimovic, Jiansen He, Owen Roberts, Joachim Saur, Robert T. Wicks, Benoit Lavraud, Shinji Saito, Olga Alexandrova, Luca Franci, Sergio Servidio, Ferdinand Plaschke, Katja Klein, Raffaella D'Amicis, Pierre Henri, Chadi S. Salem, Christopher H. K. Chen, Johan De Keyser, Daniel Verscharen, Fouad Sahraoui, Roberto Bruno, Stefaan Poedts, Observatoire de Paris - Site de Paris (OP), Centre National de la Recherche Scientifique (CNRS)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Institut national des sciences de l'Univers (INSU - 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)-Centre National de la Recherche Scientifique (CNRS)-Université d'Orléans (UO)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université d'Orléans (UO)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Centre National d’Études Spatiales [Paris] (CNES), Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique des Plasmas (LPP), Université Paris-Sud - Paris 11 (UP11)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-École polytechnique (X)-Sorbonne Universités-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), Mullard Space Science Laboratory (MSSL), University College of London [London] (UCL), University of New Hampshire (UNH), University of Northumbria at Newcastle [United Kingdom], Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA (UMR_8109)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Istituto di Astrofisica e Planetologia Spaziali - INAF (IAPS), Istituto Nazionale di Astrofisica (INAF), Queen Mary University of London (QMUL), Belgian Institute for Space Aeronomy / Institut d'Aéronomie Spatiale de Belgique (BIRA-IASB), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), INAF - Osservatorio Astrofisico di Arcetri (OAA), School of Earth and Space Sciences [Beijing], Peking University [Beijing], Joseph Louis LAGRANGE (LAGRANGE), Université Nice Sophia Antipolis (... - 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, Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), The University of Tokyo (UTokyo), Institutet för Rymdfysik, University of Arizona, Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), 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), Bartol Research Institute, University of Delaware [Newark], Space Research Institute of Austrian Academy of Sciences (IWF), Austrian Academy of Sciences (OeAW), Centre for Mathematical Plasma-Astrophysics [Leuven] (CmPA), Catholic University of Leuven - Katholieke Universiteit Leuven (KU Leuven), Maria Curie-Sklodowska University (UMCS), Institute of Astronomy, University of Cambridge, 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), National Institute of Information and Communications Technology [Tokyo, Japan] (NICT), University of California [Berkeley], University of California, Institut für Geophysik und Meteorologie [Köln], Universität zu Köln, Università della Calabria [Arcavacata di Rende] (Unical), Department of Physics [Imperial College London], Imperial College London, Czech Academy of Sciences [Prague] (CAS), Max Planck Institute for Plasma physics (IPP-MPG), Max-Planck-Gesellschaft, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS), 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), Verscharen, Daniel [0000-0002-0497-1096], and Apollo - University of Cambridge Repository

Subjects
Field (physics), F300, FOS: Physical sciences, Electrons, F500, Electron, 7. Clean energy, 01 natural sciences, F900, Physics - Space Physics, Voyage 2050, Physics::Plasma Physics, 0103 physical sciences, Thermal, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], 010306 general physics, Instrumentation and Methods for Astrophysics (astro-ph.IM), 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), High Energy Astrophysical Phenomena (astro-ph.HE), Physics, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Astronomy and Astrophysics, Plasma, space missions, Dissipation, plasma astrophysics, Physics - Plasma Physics, Space Physics (physics.space-ph), [PHYS.PHYS.PHYS-GEN-PH]Physics [physics]/Physics [physics]/General Physics [physics.gen-ph], Computational physics, Magnetic field, Plasma Physics (physics.plasm-ph), space plasma, Solar wind, Astrophysics - Solar and Stellar Astrophysics, solar wind, Space and Planetary Science, Physics::Space Physics, Astrophysical plasma, Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Instrumentation and Methods for Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract

A grand-challenge problem at the forefront of physics is to understand how energy is transported and transformed in plasmas. This fundamental research priority encapsulates the conversion of plasma-flow and electromagnetic energies into particle energy, either as heat or some other form of energisation. The smallest characteristic scales, at which electron dynamics determines the plasma behaviour, are the next frontier in space and astrophysical plasma research. The analysis of astrophysical processes at these scales lies at the heart of the field of electron-astrophysics. Electron scales are the ultimate bottleneck for dissipation of plasma turbulence, which is a fundamental process not understood in the electron-kinetic regime. Since electrons are the most numerous and most mobile plasma species in fully ionised plasmas and are strongly guided by the magnetic field, their thermal properties couple very efficiently to global plasma dynamics and thermodynamics., Comment: White Paper for the Voyage 2050 Long-Term Plan in the ESA Science Programme; 27 pages

Published
2022
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38. Massive multi-mission statistical study and analytical modeling of the Earth's magnetopause: 1 - A gradient boosting based automatic detection of near-Earth regions

Author

Benoit Lavraud, Bayane Michotte de Welle, Dominique Fontaine, N. Aunai, Gautier Nguyen, Alexis Jeandet, and Direction générale de l'Armement (DGA)

Subjects
Spacecraft, business.industry, [PHYS.ASTR.EP]Physics [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], Astrophysics::High Energy Astrophysical Phenomena, Magnetosphere, Geophysics, 7. Clean energy, Solar wind, Magnetosheath, 13. Climate action, [PHYS.PHYS.PHYS-PLASM-PH]Physics [physics]/Physics [physics]/Plasma Physics [physics.plasm-ph], Physics::Space Physics, Astrophysics::Solar and Stellar Astrophysics, Classification methods, Magnetopause, Astrophysics::Earth and Planetary Astrophysics, Gradient boosting, business, Earth (classical element), Geology
Abstract

We present an automatic classification method of the three near-Earth regions, the magnetosphere, the magnetosheath and the solar wind from their in-situ data measurement by multiple spacecraft. Ba...

Published
2021

39. Parker Solar Probe observations of solar wind energetic proton beams produced by magnetic reconnection in the near-Sun heliospheric current sheet

Author

Tai-Duc Phan, J. L. Verniero, Davin E. Larson, Benoit Lavraud, Jonathan P. Eastwood, Marit Øieroset, James F. Drake, Stuart d Bale, Roberto Livi, Jasper S. Halekas, Phyllis L Whittlesey, Ali Rahmati, Marc Pulupa, Robert John MacDowall, Adam Szabo, Andriy Koval, Mihir Desai, Stephen A. Fuselier, Marco Velli, Michael Hesse, Prayash Sharma Pyakurel, Kush Maheshwari, Justin C. Kasper, Mike Stevens, Anthony William Case, and Nour-Eddine Raouafi

Published
2021
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40. Solar Wind—Magnetosphere Coupling During Radial Interplanetary Magnetic Field Conditions: Simultaneous Multi‐Point Observations

Author

J. Dargent, Robert Fear, C. P. Escoubet, Cecilia Norgren, K. J. Hwang, Huimin Fu, Benoit Lavraud, Jesús Fornieles, N. Aunai, S. A. Fuselier, T. D. Phan, Wangping Li, Yu. V. Khotyaintsev, Sergio Toledo-Redondo, Kevin Genestreti, Department of Electromagnetism and Electronics [Murcia], Universidad de Murcia, 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), Southwest Research Institute [San Antonio] (SwRI), European Space Research and Technology Centre (ESTEC), European Space Agency (ESA), Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Department of Electromagnetism and Matter Physics [Granada] (EFM), University of Granada [Granada], 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), School of Physics and Astronomy [Southampton], University of Southampton, Institut für Theoretische Physik IV [Bochum] (ITP4), Ruhr-Universität Bochum [Bochum], School of Space and Environment [Beijing], Beihang University (BUAA), UTSA Department of Physics and Astronomy [San Antonio], The University of Texas at San Antonio (UTSA), Swedish Institute of Space Physics [Uppsala] (IRF), National Space Science Center [Beijing] (NSSC), Chinese Academy of Sciences [Beijing] (CAS), University of Bergen (UiB), Space Sciences Laboratory [Berkeley] (SSL), University of California [Berkeley], University of California-University of California, Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Agence Spatiale Européenne = European Space Agency (ESA), Universidad de Granada = University of Granada (UGR), University of California [Berkeley] (UC Berkeley), and University of California (UC)-University of California (UC)

Subjects
010504 meteorology & atmospheric sciences, [SDU.STU.GP]Sciences of the Universe [physics]/Earth Sciences/Geophysics [physics.geo-ph], Solar wind, Magnetosphere, 01 natural sciences, 7. Clean energy, magnetopause (MP), Fusion, plasma och rymdfysik, Astronomi, astrofysik och kosmologi, 0103 physical sciences, Astronomy, Astrophysics and Cosmology, Interplanetary magnetic field, 010303 astronomy & astrophysics, Multi point, 0105 earth and related environmental sciences, Physics, Magnetic reconnection, Magnetopause (MP), Fusion, Plasma and Space Physics, [PHYS.PHYS.PHYS-SPACE-PH]Physics [physics]/Physics [physics]/Space Physics [physics.space-ph], Computational physics, Coupling (physics), Geophysics, solar wind, 13. Climate action, Space and Planetary Science, magnetic reconnection, Physics::Space Physics, magnetosphere, Magnetopause
Abstract

S. Toledo-Redondo and J. Fornieles acknowledge support of the Ministry of Economy and Competitiveness (MINECO) of Spain (grant FIS2017-90102-R) and of Ministry of Science and Innovation (grant PID2020-112805GA-I00). Research at IRAP was supported by CNRS, CNES, and the University of Toulouse. We acknowledge support of the ISSI teams MMS and Cluster observations of magnetic reconnection and Cold plasma of ionospheric in the Earth's magnetosphere, and of the ESAC Science faculty., In-situ spacecraft missions are powerful assets to study processes that occur in space plasmas. One of their main limitations, however, is extrapolating such local measurements to the global scales of the system. To overcome this problem at least partially, multi-point measurements can be used. There are several multi-spacecraft missions currently operating in the Earth's magnetosphere, and the simultaneous use of the data collected by them provides new insights into the large-scale properties and evolution of magnetospheric plasma processes. In this work, we focus on studying the Earth's magnetopause (MP) using a conjunction between the Magnetospheric Multiscale and Cluster fleets, when both missions skimmed the MP for several hours at distant locations during radial interplanetary magnetic field (IMF) conditions. The observed MP positions as a function of the evolving solar wind conditions are compared to model predictions of the MP. We observe an inflation of the magnetosphere (similar to 0.7 R-E), consistent with magnetosheath pressure decrease during radial IMF conditions, which is less pronounced on the flank (, Ministry of Economy and Competitiveness (MINECO) of Spain FIS2017-90102-R, Spanish Government PID2020-112805GA-I00, Centre National de la Recherche Scientifique (CNRS), European Commission, Centre National D'etudes Spatiales, University of Toulouse, ESAC Science faculty

Published
2021
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41. Characteristic Scales of Magnetic Switchback Patches Near the Sun and Their Possible Association With Solar Supergranulation and Granulation

Author

Victor Réville, Matthieu Berthomier, Kelly E. Korreck, Phyllis Whittlesey, Jasper Halekas, Justin C. Kasper, Davin Larson, N. Fargette, Clara Froment, Stuart D. Bale, Philippe Louarn, Benoit Lavraud, Thierry Dudok de Wit, David M. Malaspina, Tai Phan, Anthony W. Case, Marc Pulupa, Alexis P. Rouillard, Michael L. Stevens, 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)-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, and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National d’Études Spatiales [Paris] (CNES)

Subjects
Physics, [PHYS.ASTR.IM]Physics [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], 010504 meteorology & atmospheric sciences, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Solar physics, [PHYS.ASTR.SR]Physics [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], 01 natural sciences, [PHYS.PHYS.PHYS-SPACE-PH]Physics [physics]/Physics [physics]/Space Physics [physics.space-ph], Solar wind, Granulation, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, [PHYS.PHYS.PHYS-PLASM-PH]Physics [physics]/Physics [physics]/Plasma Physics [physics.plasm-ph], 0103 physical sciences, Physics::Space Physics, Astrophysics::Solar and Stellar Astrophysics, Supergranulation, Astrophysics::Earth and Planetary Astrophysics, 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), [PHYS.PHYS.PHYS-DATA-AN]Physics [physics]/Physics [physics]/Data Analysis, Statistics and Probability [physics.data-an], 0105 earth and related environmental sciences
Abstract

Parker Solar Probe (PSP) data recorded within a heliocentric radial distance of 0.3 AU have revealed a magnetic field dominated by Alfv\'enic structures that undergo large local variations or even reversals of the radial magnetic field. They are called magnetic switchbacks, they are consistent with folds in magnetic field lines within a same magnetic sector, and are associated with velocity spikes during an otherwise calmer background. They are thought to originate either in the low solar atmosphere through magnetic reconnection processes, or result from the evolution of turbulence or velocity shears in the expanding solar wind. In this work, we investigate the temporal and spatial characteristic scales of magnetic switchback patches. We define switchbacks as a deviation from the nominal Parker spiral direction and detect them automatically for PSP encounters 1, 2, 4 and 5. We focus in particular on a 5.1-day interval dominated by switchbacks during E5. We perform a wavelet transform of the solid angle between the magnetic field and the Parker spiral and find periodic spatial modulations with two distinct wavelengths, respectively consistent with solar granulation and supergranulation scales. In addition we find that switchback occurrence and spectral properties seem to depend on the source region of the solar wind rather than on the radial distance of PSP. These results suggest that switchbacks are formed in the low corona and modulated by the solar surface convection pattern., Comment: 12 pages, 7 figures

Published
2021
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42. Solar wind rotation rate and shear at coronal hole boundaries

Author

R. Kieokaew, Léa Griton, N. Fargette, A. P. Rouillard, Rui Pinto, Nicolas Poirier, A. S. Brun, A. Kouloumvakos, Benoit Lavraud, 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 de Paris (UP), 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), Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), We acknowledge support from the French space agency (Centre National des Études Spatiales, CNES, STORMS, ERC SLOW_SOURCE project DLV-819189. ERC synergy grant Whole Sun #810218., 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 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
010504 meteorology & atmospheric sciences, Astrophysics::High Energy Astrophysical Phenomena, Flux, Coronal hole, FOS: Physical sciences, Context (language use), Astrophysics, Rotation, 01 natural sciences, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), Sun: rotation, 0105 earth and related environmental sciences, Physics, Sun: corona, Astronomy and Astrophysics, Geophysics, Corona, Magnetic field, Solar wind, Astrophysics - Solar and Stellar Astrophysics, solar wind, 13. Climate action, Space and Planetary Science, Physics::Space Physics, Solar rotation, Astrophysics::Earth and Planetary Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract

In-situ measurements by several spacecraft have revealed that the solar wind is frequently perturbed by transient structures (magnetic folds, jets, waves, flux-ropes) that propagate rapidly away from the Sun over large distances. Parker Solar Probe has detected frequent rotations of the magnetic field vector at small heliocentric distances, accompanied by surprisingly large solar wind rotation rates. The physical origin of such magnetic field bends, the conditions for their survival across the interplanetary space, and their relation to solar wind rotation are yet to be clearly understood. We traced measured solar wind flows from the spacecraft position down to the surface of the Sun to identify their potential source regions and used a global MHD model of the corona and solar wind to relate them to the rotational state of the low solar corona. We identified regions of the solar corona for which solar wind speed and rotational shear are important and long-lived, that can be favourable to the development of magnetic deflections and to their propagation across extended heights in the solar wind. We show that coronal rotation is highly structured and that enhanced flow shear develops near the boundaries between coronal holes and streamers, around and above pseudo-streamers, even when such boundaries are aligned with the direction of solar rotation. A large fraction of the switchbacks identified by PSP map back to these regions, both in terms of instantaneous magnetic field connectivity and of the trajectories of wind streams that reach the spacecraft. These regions of strong shears are likely to leave an imprint on the solar wind over large distances and to increase the transverse speed variability in the slow solar wind. The simulations and connectivity analysis suggest they can be a source of the switchbacks and spikes observed by Parker Solar Probe., Comment: Accepted for publication in Astronomy & Astrophysics

Published
2021
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43. Upper‐Hybrid Waves Driven by Meandering Electrons Around Magnetic Reconnection X Line

Author

Daniel J. Gershman, Cunguo Wang, Wangping Li, Binbin Tang, Benoit Lavraud, Christopher T. Russell, James L. Burch, Cecilia Norgren, Daniel B. Graham, P. A. Lindqvist, Ari Le, Yu. V. Khotyaintsev, Andris Vaivads, Roy B. Torbert, Quanming Lu, Stephen A. Fuselier, Kyunghwan Dokgo, Jan Egedal, Mats André, Jin He, Xiaocheng Guo, Robert E. Ergun, Ferdinand Plaschke, Keizo Fujimoto, Barbara L. Giles, O. Le Contel, State Key Laboratory of Space Weather [Beijing] (SKSW), National Space Science Center [Beijing] (NSSC), Chinese Academy of Sciences [Beijing] (CAS)-Chinese Academy of Sciences [Beijing] (CAS), Swedish Institute of Space Physics [Uppsala] (IRF), Department of Physics and Technology [Bergen] (UiB), University of Bergen (UiB), Royal Institute of Technology [Stockholm] (KTH ), Los Alamos National Laboratory (LANL), Department of Physics, University of Wisconsin—Milwaukee, P.O. Box 413, Milwaukee, Wisconsin 53201, Southwest Research Institute [San Antonio] (SwRI), School of Space and Environment [Beijing], Beihang University (BUAA), School of Earth and Space Sciences [Beijing], Peking University [Beijing], Laboratory for Atmospheric and Space Physics [Boulder] (LASP), University of Colorado [Boulder], University of New Hampshire (UNH), 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), NASA Goddard Space Flight Center (GSFC), 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), Institut für Weltraumforschung = Space Research institute [Graz] (IWF), Osterreichische Akademie der Wissenschaften (ÖAW), Department of Earth, Planetary and Space Sciences [Los Angeles] (EPSS), University of California [Los Angeles] (UCLA), University of California (UC)-University of California (UC), CAS Key Laboratory of Geospace Environment, University of Science and Technology of China [Hefei] (USTC), State Key Laboratory for Space Weather [Beijing] (SKSW), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Institut für Weltraumforschung [Graz] (IWF), and University of California-University of California

Subjects
Physics, 010504 meteorology & atmospheric sciences, [PHYS.ASTR.EP]Physics [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], Magnetic reconnection, Electron, 01 natural sciences, Computational physics, Geophysics, 0103 physical sciences, General Earth and Planetary Sciences, 010303 astronomy & astrophysics, ComputingMilieux_MISCELLANEOUS, 0105 earth and related environmental sciences, Line (formation)
Abstract

International audience

Published
2021
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44. Pre-flight Calibration and Near-Earth Commissioning Results of the Mercury Plasma Particle Experiment (MPPE) Onboard MMO (Mio)

Author

Jean-Jacques Berthelier, Henning Fischer, Mathieu Petiot, Kazushi Asamura, Eric Le Comte, Zdenĕk Nĕmec̆ek, Andrei Fedorov, Giuseppe Consolini, Yoichi Kazama, Haruhisa Matsumoto, Yoshizumi Miyoshi, Christian Mazelle, Kanako Seki, Jean Rouzaud, Christophe Verdeil, Dominique Delcourt, Wataru Miyake, Harald Michalik, F. Leblanc, Björn Fiethe, Ulrich Bührke, Roberto Bruno, Peter Wurz, Iannis Dandouras, Alain Barthe, Henry-Claude Séran, Jean-André Sauvaud, Maria Federica Marcucci, Mats Holmström, Stas Barabash, Shoichiro Yokota, H. Andersson, Joachim Woch, Masahiro Hoshino, Iku Shinohara, Philippe Louarn, Benoit Lavraud, Dominique Fontaine, Vincent Génot, Alexandre Cadu, Yuki Harada, Christian Jacquey, Anne-Marie Frezoul, Andrew J. Coates, Bruno Katra, Yoshifumi Futaana, Emmanuel Penou, Stefan Karlsson, Jean-Marie Illiano, Markus Fraenz, Claude Aoustin, Qiugang Zong, Catherine Garat, Qiu-Mei Lee, Wing-Huen Ip, Manabu Shimoyama, Masaki N. Nishino, David Moirin, Norbert Krupp, Nicolas André, Masaki Fujimoto, Mitsuo Oka, Hiroshi Hasegawa, Martin Wieser, Guy Peyre, Jana Safrankova, Jean-Louis Médale, Kunihiro Keika, Jean-Denis Techer, Takeshi Takashima, T. Yanagimachi, Naoki Terada, Takefumi Mitani, Masafumi Hirahara, Yoshifumi Saito, Institute of Space and Astronautical Science (ISAS), Japan Aerospace Exploration Agency [Sagamihara] (JAXA), Laboratoire de Physique des Plasmas (LPP), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École polytechnique (X)-Sorbonne Université (SU)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), Institute for Space-Earth Environmental Research [Nagoya] (ISEE), Nagoya University, Swedish Institute of Space Physics [Kiruna] (IRF), Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Osaka University [Osaka], Space Sciences Laboratory [Berkeley] (SSL), University of California [Berkeley] (UC Berkeley), University of California (UC)-University of California (UC), Kyoto University, AKKA Technologies, Institut Supérieur de l'Aéronautique et de l'Espace (ISAE-SUPAERO), Société MICROTEC, Nexeya Conseil & Formation, COMAT, Faculty of Mathematics and Physics [Charles University of Praha], Charles University [Prague] (CU), Istituto di Astrofisica e Planetologia Spaziali - INAF (IAPS), Istituto Nazionale di Astrofisica (INAF), Tokai University, The University of Tokyo (UTokyo), Mullard Space Science Laboratory (MSSL), University College of London [London] (UCL), HELIOS - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Max-Planck-Institut für Sonnensystemforschung = Max Planck Institute for Solar System Research (MPS), Max-Planck-Gesellschaft, Institute of Computer and Network Engineering [Braunschweig] (IDA), Technische Universität Braunschweig = Technical University of Braunschweig [Braunschweig], Japan Aerospace Exploration Agency [Tsukuba] (JAXA), Rikkyo University [Tokyo], Peking University [Beijing], University of Bern, Academia Sinica Institute of Astronomy and Astrophysics (ASIAA), Academia Sinica, National Central University [Taiwan] (NCU), Tohoku University [Sendai], Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), University of California [Berkeley], University of California-University of California, Kyoto University [Kyoto], Sorbonne Université (SU)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), and Max-Planck-Institut für Sonnensystemforschung (MPS)

Subjects
Spectrum analyzer, High energy particle, 010504 meteorology & atmospheric sciences, [PHYS.ASTR.EP]Physics [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], chemistry.chemical_element, 7. Clean energy, 01 natural sciences, law.invention, Orbiter, law, 0103 physical sciences, Calibration, Aerospace engineering, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, [PHYS]Physics [physics], Energetic neutral atom, Spacecraft, business.industry, Astronomy and Astrophysics, Mercury (element), Solar wind, chemistry, 13. Climate action, Space and Planetary Science, [SDU]Sciences of the Universe [physics], Environmental science, business, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract

International audience; BepiColombo Mio (previously called MMO: Mercury Magnetospheric Orbiter) was successfully launched by Ariane 5 from Kourou, French Guiana on October 20, 2018. The Mercury Plasma/Particle Experiment (MPPE) is a comprehensive instrument package onboard Mio spacecraft used for plasma, high-energy particle and energetic neutral atom measurements. It consists of seven sensors including two Mercury Electron Analyzers (MEA1 and MEA2), Mercury Ion Analyzer (MIA), Mass Spectrum Analyzer (MSA), High Energy Particle instrument for electron (HEP-ele), High Energy Particle instrument for ion (HEP-ion), and Energetic Neutrals Analyzer (ENA). Significant efforts were made pre-flight to calibrate all of the MPPE sensors at the appropriate facilities on the ground. High voltage commissioning of MPPE analyzers was successfully performed between June and August 2019 and in February 2020 following the completion of the low voltage commissioning in November 2018. Although all of the MPPE analyzers are now ready to begin observation, the full service performance has been delayed until Mio’s arrival at Mercury. Most of the fields of view (FOVs) of the MPPE analyzers are blocked by the thermal shield surrounding the Mio spacecraft during the cruising phase. Together with other instruments on Mio including Magnetic Field Investigation (MGF) and Plasma Wave Investigation (PWI) that measure plasma field parameters, MPPE will contribute to the comprehensive understanding of the plasma environment around Mercury when BepiColombo/Mio begins observation after arriving at the planet Mercury in December 2025.

Published
2021
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45. Dust, Field and Plasma instrument onboard ESA’s Comet Interceptor mission

Author

Hanna Rothkaehl, Nicolas Andre, Uli Auster, vincenzo Della Corte, Niklas Edberg, Marina Galand, Pierre Henri, Johan De Keyser, Ivana Kolmasova, Marek Morawski, Hans Nilsson, Lubomir Prech, Martin Volwerk, Charlotte Goetz, Herbert Gunell, Benoit Lavraud, Alessandra Rotundi, and Jan Soucek

Abstract

The main goal of ESA’s F-1 class Comet Interceptor mission is to characterise, for the first time, a long period comet; preferably a dynamically-new or an interstellar object. The main spacecraft, will have its trajectory outside of the inner coma, whereas two sub-spacecrafts will be targeted inside the inner coma, closer to the nucleus. The flyby of such a comet will offer unique multipoint measurement opportunity to study the comet's dusty and ionised environment in ways exceeding that of the previous cometary missions, including Rosetta. The Dust Field and Plasma (DFP) instruments located on both the main spacecraft A and on the sub-spacecraft B2, is a combined experiment dedicated to the in situ, multi-point study of the multi-phased ionized and dusty environment in the coma of the target and its interaction with the surrounding space environment and the Sun. The DFP instruments will be present in different configurations on the Comet Interceptor spacecraft A and B2. To enable the measurements on spacecraft A, the DFP is composed of 5 sensors; Fluxgate magnetometer DFP-FGM-A, Plasma instrument with nanodust and E-field measurements capabilities DFP-COMPLIMENT, Electron spectrometer DFP-LEES, Ion and energetic neutrals spectrometer DFP-SCIENA and Dust detector DFP-DISC. On board of spacecraft B2 the DFP is composed of 2 sensors: Fluxgate magnetometer DFP-FGM-B2 and Cometary dust detector DFP-DISC. The DFP instrument will measure magnetic field, the electric field, plasma parameters (density, temperature, speed), the distribution functions of electrons, ions and energetic neutrals, spacecraft potential, mass, number and spatial density of cometary dust particles and the dust impacts. The full set of DFP sensors will allow to model the comet plasma environment and its interaction with the solar wind. It will also allow to describe the complex physical processes including wave particle interaction in dusty cometary plasma.

Published
2021
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46. Massive multi-mission statistical study and analytical modeling of the Earth's magnetopause: 4- On the near-cusp magnetopause indentation

Author

Gautier Nguyen, Nicolas Aunai, Bayane Michotte de Welle, Alexis Jeandet, Benoit Lavraud, Dominique Fontaine, Direction Générale de l'Armement, and Direction Generale de l'Armement

Subjects
[PHYS.PHYS.PHYS-PLASM-PH]Physics [physics]/Physics [physics]/Plasma Physics [physics.plasm-ph], [PHYS.ASTR.EP]Physics [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP]
Published
2021
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47. Massive multi-missions statistical study and analytical modeling of the Earth magnetopause: 3- An asymmetric non indented magnetopause analytical model

Author

Gautier Nguyen, Nicolas Aunai, Bayane Michotte de Welle, Alexis Jeandet, Benoit Lavraud, Dominique Fontaine, Direction Générale de l'Armement, and Direction Generale de l'Armement

Subjects
[PHYS.PHYS.PHYS-PLASM-PH]Physics [physics]/Physics [physics]/Plasma Physics [physics.plasm-ph], [PHYS.ASTR.EP]Physics [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP]
Published
2021
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49. Kinetic Interaction of Cold and Hot Protons With an Oblique EMIC Wave Near the Dayside Reconnecting Magnetopause

Author

Thomas E. Moore, Richard E. Denton, Barbara L. Giles, Huimin Fu, Adolfo F. Viñas, Justin H. Lee, Mats André, N. Kitamura, Daniel B. Graham, Benoit Lavraud, Stephen A. Fuselier, O. Le Contel, James L. Burch, Alfonso Salinas, D. J. Gershman, Yu. V. Khotyaintsev, Enrique A. Navarro, Sarah K. Vines, Jorge A. Portí, Robert Allen, Wangping Li, Sergio Toledo-Redondo, Drew Turner, Scott A. Boardsen, Department of Electromagnetism and Electronics [Murcia], Universidad de Murcia, The Aerospace Corporation, Johns Hopkins University Applied Physics Laboratory [Laurel, MD] (APL), Swedish Institute of Space Physics [Uppsala] (IRF), NASA Goddard Space Flight Center (GSFC), Southwest Research Institute [San Antonio] (SwRI), Department of Physics and Astronomy [Hanover], Dartmouth College [Hanover], School of Space and Environment [Beijing], Beihang University (BUAA), Department of Earth and Planetary Sciences [TITECH Tokyo], Tokyo Institute of Technology [Tokyo] (TITECH), Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique des Plasmas (LPP), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École polytechnique (X)-Sorbonne Université (SU)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), National Space Science Center [Beijing] (NSSC), Chinese Academy of Sciences [Beijing] (CAS), University of Valencia, Universidad de Granada = University of Granada (UGR), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Department of Applied Physics, School of Science, University of Granada, 18071 Granada, Spain, University of Granada, and University of Granada [Granada]

Subjects
Ones, 010504 meteorology & atmospheric sciences, [PHYS.ASTR.EP]Physics [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], oblique propagation, Magnetosphere, wave-particle interaction, Plasma (Gasos ionitzats), 010502 geochemistry & geophysics, Kinetic energy, 01 natural sciences, 7. Clean energy, Computer Science::Digital Libraries, Fusion, plasma och rymdfysik, Physics::Plasma Physics, Nuclear Experiment, ComputingMilieux_MISCELLANEOUS, 0105 earth and related environmental sciences, Physics, electromagnetic ion cyclotron, Geofysik, magnetopause, Astronomy, Oblique case, Geofísica, Fusion, Plasma and Space Physics, Geophysics, 13. Climate action, [SDU]Sciences of the Universe [physics], Physics::Space Physics, General Earth and Planetary Sciences, Emic and etic, Magnetopause, cold ions, Christian ministry, Astrophysics::Earth and Planetary Astrophysics, Ionosphere, multi-ion plasma
Abstract

STR acknowledges support from the ISSI international team Cold plasma of ionospheric origin in the Earth's magnetosphere and of the Ministry of Economy and Competitiveness (MINECO) of Spain (grant FIS2017-90102-R). Research at IRAP was supported by CNRS, CNES and the University of Toulouse. JHL and DLT acknowledge support from NASA Grant 80NSSC18K1378. RED was supported by NASA grants 80NSSC19K070 and 80NSSC19K0254. MA was supported by SNSA Grant 56/18. SKV and RCA acknowledge support from NASA Grant 80NSSC19K0270. Work performed by MMS team members is supported by NASA contract NNG04EB99C., We report observations of the ion dynamics inside an Alfvén branch wave that propagates near the reconnecting dayside magnetopause. The measured frequency, wave normal angle and polarization are consistent with the predictions of a dispersion solver. The magnetospheric plasma contains hot protons (keV), cold protons (eV), plus some heavy ions. While the cold protons follow the magnetic field fluctuations and remain frozen-in, the hot protons are at the limit of magnetization. The cold protons exchange energy back and forth, adiabatically, with the wave fields. The cold proton velocity fluctuations contribute to balance the Hall term fluctuations in Ohm's law, and the wave E field has small ellipticity and right-handed polarization. The dispersion solver indicates that increasing the cold proton density facilitates propagation and amplification of these waves at oblique angles, as for the observed wave., ISSI international team Cold plasma of ionospheric origin in the Earth's magnetosphere, Ministry of Economy and Competitiveness (MINECO) of Spain FIS2017-90102-R, Centre National de la Recherche Scientifique (CNRS), European Commission, Centre National D'etudes Spatiales, University of Toulouse, National Aeronautics & Space Administration (NASA) 80NSSC18K1378 80NSSC19K070 80NSSC19K0254 80NSSC19K0270 NNG04EB99C, SNSA 56/18

Published
2021
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50. The Solar Wind

Author

Alexis P., Rouillard, Nicholeen, Viall, Viviane, Pierrard, Christian, Vocks, Lorenzo, Matteini, Olga, Alexandrova, Aleida K., Higginson, Benoit, Lavraud, Michael, Lavarra, Yihong, Wu, Rui, Pinto, Alessandro, Bemporad, Eduardo, Sanchez-Diaz, 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), Belgian Institute for Space Aeronomy / Institut d'Aéronomie Spatiale de Belgique (BIRA-IASB), Imperial College London, Laboratoire d'études spatiales et d'instrumentation en astrophysique = Laboratory of Space Studies and Instrumentation in Astrophysics (LESIA), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Faculty of Engineering of the University of Porto, INAF - Osservatorio Astrofisico di Torino (OATo), Istituto Nazionale di Astrofisica (INAF), Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), and 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)

Subjects
[PHYS]Physics [physics], Solar System, [SDU.ASTR.SR]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], Astronomical unit, Plasma, Space exploration, Astrobiology, Solar wind, Physics::Space Physics, Astrophysics::Solar and Stellar Astrophysics, Environmental science, Outflow, Astrophysics::Earth and Planetary Astrophysics, Interplanetary spaceflight
Abstract

The solar corona produces a continuous outflow of plasma influencing the entire solar system and beyond to over a hundred of astronomical units. Due to the Sun's proximity the source regions of that wind can be observed remotely with great precision and the escaping plasma can be measured directly in situ. Space missions launched over the past six decades have exploited this fantastic plasma laboratory to reveal the very rich physical processes at play as the solar wind forms and expands into space. This chapter provides a brief synthesis of these observational discoveries. It covers a broad range of topics, from the large‐scale imaging and detailed spectroscopic observations of the wind source regions to the dynamical evolution of interplanetary plasma down to kinetic scales. Despite the great advances accomplished in solar wind research over the past decades, many mysteries remain concerning the origins of the solar winds. These mysteries are currently being addressed with a new fleet of extraordinary missions en route to our star.

Published
2021
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