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1. Solar Orbiter's encounter with the tail of comet C/2019 Y4 (ATLAS): Magnetic field draping and cometary pick-up ion waves

Author

L. Matteini, R. Laker, T. Horbury, L. Woodham, S. D. Bale, J. E. Stawarz, T. Woolley, K. Steinvall, G. H. Jones, S. R. Grant, Q. Afghan, M. Galand, H. O’Brien, V. Evans, V. Angelini, M. Maksimovic, T. Chust, Y. Khotyaintsev, V. Krasnoselskikh, M. Kretzschmar, E. Lorfèvre, D. Plettemeier, J. Souček, M. Steller, Š. Štverák, P. Trávníček, A. Vaivads, A. Vecchio, R. F. Wimmer-Schweingruber, G. C. Ho, R. Gómez-Herrero, J. Rodríguez-Pacheco, P. Louarn, A. Fedorov, C. J. Owen, R. Bruno, S. Livi, I. Zouganelis, D. Müller, 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), 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), Laboratoire de Physique et Chimie de l'Environnement et de l'Espace (LPC2E), Observatoire des Sciences de l'Univers en région Centre (OSUC), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Centre National d'Études Spatiales [Toulouse] (CNES), Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), 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
Astronomy, Comet, Astrophysics, Astronomy & Astrophysics, Ion, law.invention, GIACOBINI-ZINNER, PHYSICS, Orbiter, FILAMENTATION, law, Atlas (anatomy), 0201 Astronomical and Space Sciences, medicine, PROTON CYCLOTRON FREQUENCY, comets: individual: C/2019 Y4 ATLAS, waves, Physics, Science & Technology, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], [SDU.ASTR.SR]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], Astronomy and Astrophysics, plasmas, Magnetic field, medicine.anatomical_structure, solar wind, instabilities, Space and Planetary Science, Physical Sciences, Physics::Space Physics, TURBULENCE, Astrophysics::Earth and Planetary Astrophysics, ELECTROMAGNETIC-WAVES
Abstract

Context. Solar Orbiter is expected to have flown close to the tail of comet C/2019 Y4 (ATLAS) during the spacecraft’s first perihelion in June 2020. Models predict a possible crossing of the comet tails by the spacecraft at a distance from the Sun of approximately 0.5 AU. Aims. This study is aimed at identifying possible signatures of the interaction of the solar wind plasma with material released by comet ATLAS, including the detection of draped magnetic field as well as the presence of cometary pick-up ions and of ion-scale waves excited by associated instabilities. This encounter provides us with the first opportunity of addressing such dynamics in the inner Heliosphere and improving our understanding of the plasma interaction between comets and the solar wind. Methods. We analysed data from all in situ instruments on board Solar Orbiter and compared their independent measurements in order to identify and characterize the nature of structures and waves observed in the plasma when the encounter was predicted. Results. We identified a magnetic field structure observed at the start of 4 June, associated with a full magnetic reversal, a local deceleration of the flow and large plasma density, and enhanced dust and energetic ions events. The cross-comparison of all these observations support a possible cometary origin for this structure and suggests the presence of magnetic field draping around some low-field and high-density object. Inside and around this large scale structure, several ion-scale wave-forms are detected that are consistent with small-scale waves and structures generated by cometary pick-up ion instabilities. Conclusions. Solar Orbiter measurements are consistent with the crossing through a magnetic and plasma structure of cometary origin embedded in the ambient solar wind. We suggest that this corresponds to the magnetotail of one of the fragments of comet ATLAS or to a portion of the tail that was previously disconnected and advected past the spacecraft by the solar wind.

Published
2021
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2. Millisecond observations of nonlinear wave–electron interaction in electron phase space holes

Author

C. Norgren, D. B. Graham, M. R. Argall, K. Steinvall, M. Hesse, Yu. V. Khotyaintsev, A. Vaivads, P. Tenfjord, D. J. Gershman, P.-A. Lindqvist, J. L. Burch, and F. Plaschke

Subjects
Fusion, plasma och rymdfysik, Astrophysics::High Energy Astrophysical Phenomena, Physics::Space Physics, Condensed Matter Physics, Fusion, Plasma and Space Physics
Abstract

Electron phase space holes (EHs) associated with electron trapping are commonly observed as bipolar electric field signatures in both space and laboratory plasma. Until recently, it has not been possible to resolve EHs in electron measurements. We report observations of EHs in the plasma sheet boundary layer, here identified as the separatrix region of magnetic reconnection in the magnetotail. The intense EHs are observed together with an electron beam moving toward the X line, showing signs of thermalization. Using the electron drift instrument onboard the satellites of the Magnetospheric Multiscale mission, we make direct millisecond measurements of the electron particle flux associated with individual electron phase space holes. The electron flux is measured at a millisecond cadence in a narrow parallel speed range within that of the trapped electrons. The flux modulations are of order unity and are direct evidence of the strong nonlinear wave-electron interaction that may effectively thermalize beams and contribute to transforming directed drift energy to thermal energy. (C) 2022 Author(s). All article content, except where otherwise noted, is licensed under a Creative Commons Attribution (CC BY) license (http://creativecommons.org/licenses/by/4.0/).

Published
2022

3. Cross-scale Dynamics Driven by Plasma Jet Braking in Space

Author

C. M. Liu, A. Vaivads, Y. V. Khotyaintsev, H. S. Fu, D. B. Graham, K. Steinvall, Y. Y. Liu, and J. L. Burch

Subjects
Fusion, plasma och rymdfysik, Space and Planetary Science, Astrophysics::High Energy Astrophysical Phenomena, Physics::Space Physics, Astronomy and Astrophysics, Fusion, Plasma and Space Physics
Abstract

Plasma jets are ubiquitous in space. In geospace, jets can be generated by magnetic reconnection. These reconnection jets, typically at fluid scale, brake in the near-Earth region, dissipate their energies, and drive plasma dynamics at kinetic scales, generating field-aligned currents that are crucial to magnetospheric dynamics. Understanding of the cross-scale dynamics is fundamentally important, but observation of coupling among phenomena at various scales is highly challenging. Here we report, using unprecedentedly high-cadence data from NASA's Magnetospheric Multiscale Mission, the first observation of cross-scale dynamics driven by jet braking in geospace. We find that jet braking causes MHD-scale distortion of magnetic field lines and development of an ion-scale jet front that hosts strong Hall electric fields. Parallel electric fields arising from the ion-scale Hall potential generate intense electron-scale field-aligned currents, which drive strong Debye-scale turbulence. Debye-scale waves conversely limit intensity of the field-aligned currents, thereby coupling back to the large-scale dynamics. Our study can help in understanding how energy deposited in large-scale structures is transferred into small-scale structures in space.

Published
2022

4. The first widespread solar energetic particle event observed by Solar Orbiter on 2020 November 29

Author

A. Kollhoff, A. Kouloumvakos, D. Lario, N. Dresing, R. Gómez-Herrero, L. Rodríguez-García, O. E. Malandraki, I. G. Richardson, A. Posner, K.-L. Klein, D. Pacheco, A. Klassen, B. Heber, C. M. S. Cohen, T. Laitinen, I. Cernuda, S. Dalla, F. Espinosa Lara, R. Vainio, M. Köberle, R. Kühl, Z. G. Xu, L. Berger, S. Eldrum, M. Brüdern, M. Laurenza, E. J. Kilpua, A. Aran, A. P. Rouillard, R. Bučík, N. Wijsen, J. Pomoell, R. F. Wimmer-Schweingruber, C. Martin, S. I. Böttcher, J. L. Freiherr von Forstner, J.-C. Terasa, S. Boden, S. R. Kulkarni, A. Ravanbakhsh, M. Yedla, N. Janitzek, J. Rodríguez-Pacheco, M. Prieto Mateo, S. Sánchez Prieto, P. Parra Espada, O. Rodríguez Polo, A. Martínez Hellín, F. Carcaboso, G. M. Mason, G. C. Ho, R. C. Allen, G. Bruce Andrews, C. E. Schlemm, H. Seifert, K. Tyagi, W. J. Lees, J. Hayes, S. D. Bale, V. Krupar, T. S. Horbury, V. Angelini, V. Evans, H. O’Brien, M. Maksimovic, Yu. V. Khotyaintsev, A. Vecchio, K. Steinvall, E. Asvestari, German Research Foundation, National Aeronautics and Space Administration (US), Academy of Finland, Ministerio de Ciencia, Innovación y Universidades (España), Swedish National Space Agency, 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'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), ANR-17-CE31-0006,COROSHOCK,EVALUER LE ROLE DU CHOC COMME ACCELERATEUR DE PARTICULES SOLAIRES(2017), Space Physics Research Group, Doctoral Programme in Particle Physics and Universe Sciences, Department of Physics, University of Helsinki, and Particle Physics and Astrophysics

Subjects
Astronomy, particle emission [Sun], PROPAGATION, Astrophysics, PROTON, 7. Clean energy, Astronomi, astrofysik och kosmologi, Coronal mass ejection, Astronomy, Astrophysics and Cosmology, Astrophysics::Solar and Stellar Astrophysics, Physics, heliosphere [Sun], [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], PLASMA, Astrophysics::Instrumentation and Methods for Astrophysics, F530, Fusion, Plasma and Space Physics, Solar cycle, Particle acceleration, Solar wind, Physical Sciences, Physics::Space Physics, ELECTRON, Astrophysics::Earth and Planetary Astrophysics, interplanetary medium, Sun: flares, MULTI-SPACECRAFT OBSERVATIONS, Sun: coronal mass ejections (CMEs), Interplanetary medium, Astronomy & Astrophysics, Computer Science::Digital Libraries, Fusion, plasma och rymdfysik, Sun: particle emission, Pitch angle, Sun: heliosphere, RELEASE, Science & Technology, RADIO, Astronomy and Astrophysics, WIND, 115 Astronomy, Space science, Physics::History of Physics, coronal mass ejections (CMEs) [Sun], TRANSPORT, flares [Sun], [SDU]Sciences of the Universe [physics], Space and Planetary Science, STEREO, Event (particle physics), Heliosphere
Abstract

Kollhoff, A., et al., Context. On 2020 November 29, the first widespread solar energetic particle (SEP) event of solar cycle 25 was observed at four widely separated locations in the inner (≲ 1 AU) heliosphere. Relativistic electrons as well as protons with energies > 50 MeV were observed by Solar Orbiter (SolO), Parker Solar Probe, the Solar Terrestrial Relations Observatory (STEREO)-A and multiple near-Earth spacecraft. The SEP event was associated with an M4.4 class X-ray flare and accompanied by a coronal mass ejection and an extreme ultraviolet (EUV) wave as well as a type II radio burst and multiple type III radio bursts. Aims. We present multi-spacecraft particle observations and place them in context with source observations from remote sensing instruments and discuss how such observations may further our understanding of particle acceleration and transport in this widespread event. Methods. Velocity dispersion analysis (VDA) and time shift analysis (TSA) were used to infer the particle release times at the Sun. Solar wind plasma and magnetic field measurements were examined to identify structures that influence the properties of the energetic particles such as their intensity. Pitch angle distributions and first-order anisotropies were analyzed in order to characterize the particle propagation in the interplanetary medium. Results. We find that during the 2020 November 29 SEP event, particles spread over more than 230° in longitude close to 1 AU. The particle onset delays observed at the different spacecraft are larger as the flare-footpoint angle increases and are consistent with those from previous STEREO observations. Comparing the timing when the EUV wave intersects the estimated magnetic footpoints of each spacecraft with particle release times from TSA and VDA, we conclude that a simple scenario where the particle release is only determined by the EUV wave propagation is unlikely for this event. Observations of anisotropic particle distributions at SolO, Wind, and STEREO-A do not rule out that particles are injected over a wide longitudinal range close to the Sun. However, the low values of the first-order anisotropy observed by near-Earth spacecraft suggest that diffusive propagation processes are likely involved., The CAU Kiel team acknowledges support from the German Federal Ministry for Economic Affairs and Energy, the German Space Agency (Deutsches Zentrum für Luft- und Raumfahrt e.V., DLR) under grants 50OT0901, 50OT1202, 50OT1702, and 50OT2002. A.K. acknowledges financial support from the ANR COROSHOCK project (ANR-17-CE31-0006-01). D.L. acknowledges support from NASA-HGI grant NNX16AF73G and the NASA Program NNH17ZDA001N-LWS. This study has received funding from the European Union’s Horizon 2020 research and innovation programme under grant agreement No. 101004159 (SERPENTINE). The U. Turku team acknowledges funding by the Academy of Finland (Grant No. 336809). The UAH team acknowledges financial support by the Spanish Ministerio de Ciencia, Innovación y Universidades FEDER/MCIU/AEI Projects ESP2017-88436-R and PID2019-104863RB-I00/AEI/10.13039/501100011033. [...] The Swedish National Space Agency, ESA-PRODEX and all the participating institutes. I.G.R. acknowledges support from NASA programs NNH19ZDA001N-HSR and NNH19ZDA001N-LWS, and the STEREO mission. IRFU team acknowledges support from the Swedish National Space Agency grant 20/136. A.A. acknowledges the support of the Spanish Ministerio de Ciencia e Innovación (MICINN) under grant PID2019- 105510GB-C31 and through the ‘Center of Excellence María de Maeztu 2020-2023’ award to the ICCUB (CEX2019-000918- M). F.C. acknowledges the financial support by the Spanish MINECO-FPI-2016 predoctoral grant with FSE. E.A. would like to acknowledge the financial support by the Academy of Finland (Postdoctoral Grant No 322455). V.K. acknowledges the support by NASA under grants 18-2HSWO218_2-0010 and 19-HSR-19_2-0143. Solar Orbiter magnetometer operations are funded by the UK Space Agency (grant ST/T001062/1). T.S.H. is supported by STFC grant ST/S000364/1. T.L. and S.D. acknowledge support from the UK Science and Technology Facilities Council (STFC; grant ST/R000425/1).

Published
2021
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5. Study of two interacting interplanetary coronal mass ejections encountered by Solar Orbiter during its first perihelion passage. Observations and modeling

Author

D. Telloni, C. Scolini, C. Möstl, G. P. Zank, L.-L. Zhao, A. J. Weiss, M. A. Reiss, R. Laker, D. Perrone, Y. Khotyaintsev, K. Steinvall, L. Sorriso-Valvo, T. S. Horbury, R. F. Wimmer-Schweingruber, R. Bruno, R. D’Amicis, R. De Marco, V. K. Jagarlamudi, F. Carbone, R. Marino, M. Stangalini, M. Nakanotani, L. Adhikari, H. Liang, L. D. Woodham, E. E. Davies, H. Hietala, S. Perri, R. Gómez-Herrero, J. Rodríguez-Pacheco, E. Antonucci, M. Romoli, S. Fineschi, M. Maksimovic, J. Souček, T. Chust, M. Kretzschmar, A. Vecchio, D. Müller, I. Zouganelis, R. M. Winslow, S. Giordano, S. Mancuso, R. Susino, S. L. Ivanovski, M. Messerotti, H. O’Brien, V. Evans, V. Angelini, École Centrale de Lyon (ECL), Université de Lyon, Centre National de la Recherche Scientifique (CNRS), and Commission of the European Communities

Subjects
010504 meteorology & atmospheric sciences, Sun: coronal mass ejections (CMEs), Astronomy, Astrophysics, Astronomy & Astrophysics, ACCELERATION, 7. Clean energy, 01 natural sciences, magnetohydrodynamics (MHD), law.invention, Orbiter, [SPI]Engineering Sciences [physics], MAGNETIC CLOUD EROSION, law, 0103 physical sciences, 0201 Astronomical and Space Sciences, Coronal mass ejection, Astrophysics::Solar and Stellar Astrophysics, COMPLEX EJECTA, Sun: heliosphere, 010303 astronomy & astrophysics, ComputingMilieux_MISCELLANEOUS, 0105 earth and related environmental sciences, Physics, [PHYS]Physics [physics], Science & Technology, Astronomy and Astrophysics, WIND, solar-terrestrial relations, ARRIVAL-TIME, EVOLUTION, Sun: evolution, solar wind, Space and Planetary Science, [SDU]Sciences of the Universe [physics], Physical Sciences, solar wind solar-terrestrial relations, Physics::Space Physics, SHOCK, TURBULENCE, Astrophysics::Earth and Planetary Astrophysics, Interplanetary spaceflight, FLUX ROPES, IN-SITU OBSERVATIONS
Abstract

Context. Solar Orbiter, the new-generation mission dedicated to solar and heliospheric exploration, was successfully launched on February 10, 2020, 04:03 UTC from Cape Canaveral. During its first perihelion passage in June 2020, two successive interplanetary coronal mass ejections (ICMEs), propagating along the heliospheric current sheet (HCS), impacted the spacecraft. Aims. This paper addresses the investigation of the ICMEs encountered by Solar Orbiter on June 7−8, 2020, from both an observational and a modeling perspective. The aim is to provide a full description of those events, their mutual interaction, and their coupling with the ambient solar wind and the HCS. Methods. Data acquired by the MAG magnetometer, the Energetic Particle Detector suite, and the Radio and Plasma Waves instrument are used to provide information on the ICMEs’ magnetic topology configuration, their magnetic connectivity to the Sun, and insights into the heliospheric plasma environment where they travel, respectively. On the modeling side, the Heliospheric Upwind eXtrapolation model, the 3D COronal Rope Ejection technique, and the EUropean Heliospheric FORecasting Information Asset (EUHFORIA) tool are used to complement Solar Orbiter observations of the ambient solar wind and ICMEs, and to simulate the evolution and interaction of the ejecta in the inner heliosphere, respectively. Results. Both data analysis and numerical simulations indicate that the passage of two distinct, dynamically and magnetically interacting (via magnetic reconnection processes) ICMEs at Solar Orbiter is a possible scenario, supported by the numerous similarities between EUHFORIA time series at Solar Orbiter and Solar Orbiter data. Conclusions. The combination of in situ measurements and numerical simulations (together with remote sensing observations of the corona and inner heliosphere) will significantly lead to a deeper understanding of the physical processes occurring during the CME-CME interaction.

Published
2021
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6. First observations and performance of the RPW instrument on board the Solar Orbiter mission

Author

M. Maksimovic, J. Souček, T. Chust, Y. Khotyaintsev, M. Kretzschmar, X. Bonnin, A. Vecchio, O. Alexandrova, S. D. Bale, D. Bérard, J.-Y. Brochot, N. J. T. Edberg, A. Eriksson, L. Z. Hadid, E. P. G. Johansson, T. Karlsson, B. Katra, V. Krasnoselskikh, V. Krupař, S. Lion, E. Lorfèvre, L. Matteini, Q. N. Nguyen, D. Píša, R. Piberne, D. Plettemeier, H. O. Rucker, O. Santolík, K. Steinvall, M. Steller, Š. Štverák, P. Trávníček, A. Vaivads, A. Zaslavsky, S. Chaintreuil, M. Dekkali, P.-A. Astier, G. Barbary, K. Boughedada, B. Cecconi, F. Chapron, C. Collin, D. Dias, L. Guéguen, L. Lamy, V. Leray, L. R. Malac-Allain, F. Pantellini, J. Parisot, P. Plasson, S. Thijs, I. Fratter, E. Bellouard, P. Danto, S. Julien, E. Guilhem, C. Fiachetti, J. Sanisidro, C. Laffaye, F. Gonzalez, B. Pontet, N. Quéruel, G. Jannet, P. Fergeau, T. Dudok de Wit, T. Vincent, C. Agrapart, J. Pragout, M. Bergerard-Timofeeva, G. T. Delory, P. Turin, A. Jeandet, P. Leroy, J.-C. Pellion, V. Bouzid, W. Recart, I. Kolmašová, O. Krupařová, L. Uhlíř, R. Lán, J. Baše, M. André, L. Bylander, V. Cripps, C. Cully, S.-E. Jansson, W. Puccio, J. Břínek, H. Ottacher, V. Angelini, M. Berthomier, V. Evans, K. Goetz, P. Hellinger, T. S. Horbury, K. Issautier, E. Kontar, O. Le Contel, P. Louarn, M. Martinović, D. Müller, H. O’Brien, C. J. Owen, A. Retino, J. Rodríguez-Pacheco, F. Sahraoui, L. Sanchez, A. P. Walsh, R. F. Wimmer-Schweingruber, I. Zouganelis, 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), 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), Swedish Institute of Space Physics [Uppsala] (IRF), Laboratoire de Physique et Chimie de l'Environnement et de l'Espace (LPC2E), Observatoire des Sciences de l'Univers en région Centre (OSUC), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Space Sciences Laboratory [Berkeley] (SSL), University of California [Berkeley] (UC Berkeley), University of California (UC)-University of California (UC), Centre National d'Études Spatiales [Toulouse] (CNES), Innovations for High Performance Microelectronics (IHP), Institut für Weltraumforschung = Space Research institute [Graz] (IWF), Osterreichische Akademie der Wissenschaften (ÖAW), Centre Hospitalier Régional Universitaire de Tours (CHRU Tours), Laboratoire de Biométrie et Biologie Evolutive - UMR 5558 (LBBE), Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut National de Recherche en Informatique et en Automatique (Inria)-VetAgro Sup - Institut national d'enseignement supérieur et de recherche en alimentation, santé animale, sciences agronomiques et de l'environnement (VAS)-Centre National de la Recherche Scientifique (CNRS), Centre Hospitalier Lyon Sud [CHU - HCL] (CHLS), Hospices Civils de Lyon (HCL), ALTRAN (FRANCE), GeNeuro Innovation [Lyon], Hôpital Saint Eloi (CHRU Montpellier), Centre Hospitalier Régional Universitaire [Montpellier] (CHRU Montpellier), Institut des Neurosciences de Montpellier (INM), Institut National de la Santé et de la Recherche Médicale (INSERM)-Université de Montpellier (UM), Centre National de la Recherche Scientifique (CNRS), Université de Rennes (UR), Nexeya Conseil & Formation, Institute of Atmospheric Physics [Prague] (IAP), Czech Academy of Sciences [Prague] (CAS), Microbes, Intestin, Inflammation et Susceptibilité de l'Hôte (M2iSH), Institut National de la Santé et de la Recherche Médicale (INSERM)-Centre de Recherche en Nutrition Humaine d'Auvergne (CRNH d'Auvergne)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Clermont Auvergne (UCA), Service de Médecine Interne [CHU Clermont-Ferrand], CHU Gabriel Montpied [Clermont-Ferrand], CHU Clermont-Ferrand-CHU Clermont-Ferrand, Royal Institute of Technology [Stockholm] (KTH ), Department of Physics and Astronomy [Calgary], University of Calgary, Space Research Institute of Austrian Academy of Sciences (IWF), Austrian Academy of Sciences (OeAW), NOAA National Marine Fisheries Service (NMFS), National Oceanic and Atmospheric Administration (NOAA), National Institute of Water and Atmospheric Research [Wellington] (NIWA), Department of Physics [Imperial College London], Imperial College London, Université Paris sciences et lettres (PSL), 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), Lunar and Planetary Laboratory [Tucson] (LPL), University of Arizona, University of Belgrade [Belgrade], Laboratoire des sciences de l'ingénieur, de l'informatique et de l'imagerie (ICube), École Nationale du Génie de l'Eau et de l'Environnement de Strasbourg (ENGEES)-Université de Strasbourg (UNISTRA)-Institut National des Sciences Appliquées - Strasbourg (INSA Strasbourg), Institut National des Sciences Appliquées (INSA)-Institut National des Sciences Appliquées (INSA)-Institut National de Recherche en Informatique et en Automatique (Inria)-Les Hôpitaux Universitaires de Strasbourg (HUS)-Centre National de la Recherche Scientifique (CNRS)-Matériaux et Nanosciences Grand-Est (MNGE), Université de Strasbourg (UNISTRA)-Université de Haute-Alsace (UHA) Mulhouse - Colmar (Université de Haute-Alsace (UHA))-Institut National de la Santé et de la Recherche Médicale (INSERM)-Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS)-Université de Strasbourg (UNISTRA)-Université de Haute-Alsace (UHA) Mulhouse - Colmar (Université de Haute-Alsace (UHA))-Institut National de la Santé et de la Recherche Médicale (INSERM)-Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS)-Réseau nanophotonique et optique, Université de Strasbourg (UNISTRA)-Université de Haute-Alsace (UHA) Mulhouse - Colmar (Université de Haute-Alsace (UHA))-Centre National de la Recherche Scientifique (CNRS)-Université de Strasbourg (UNISTRA)-Centre National de la Recherche Scientifique (CNRS), Sorbonne Université (SU), International Centre for Radio Astronomy Research - Curtin University, Curtin University [Perth], Planning and Transport Research Centre (PATREC)-Planning and Transport Research Centre (PATREC), European Space Astronomy Centre (ESAC), Agence Spatiale Européenne = European Space Agency (ESA), Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA (UMR_8109)), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), University of California [Berkeley], University of California-University of California, Institut für Weltraumforschung [Graz] (IWF), CHU Saint-Eloi, Institut des Neurosciences de Montpellier - Déficits sensoriels et moteurs (INM), Université de Montpellier (UM)-Institut National de la Santé et de la Recherche Médicale (INSERM), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Institut National des Sciences Appliquées - Strasbourg (INSA Strasbourg), Institut National des Sciences Appliquées (INSA)-Institut National des Sciences Appliquées (INSA)-Université de Strasbourg (UNISTRA)-Centre National de la Recherche Scientifique (CNRS)-École Nationale du Génie de l'Eau et de l'Environnement de Strasbourg (ENGEES)-Réseau nanophotonique et optique, Centre National de la Recherche Scientifique (CNRS)-Université de Strasbourg (UNISTRA)-Université de Haute-Alsace (UHA) Mulhouse - Colmar (Université de Haute-Alsace (UHA))-Centre National de la Recherche Scientifique (CNRS)-Université de Strasbourg (UNISTRA)-Université de Haute-Alsace (UHA) Mulhouse - Colmar (Université de Haute-Alsace (UHA))-Matériaux et nanosciences d'Alsace (FMNGE), Institut de Chimie du CNRS (INC)-Université de Strasbourg (UNISTRA)-Université de Haute-Alsace (UHA) Mulhouse - Colmar (Université de Haute-Alsace (UHA))-Institut National de la Santé et de la Recherche Médicale (INSERM)-Centre National de la Recherche Scientifique (CNRS)-Institut de Chimie du CNRS (INC)-Université de Strasbourg (UNISTRA)-Institut National de la Santé et de la Recherche Médicale (INSERM)-Centre National de la Recherche Scientifique (CNRS), European Space Agency (ESA), and Centre Hospitalier Régional Universitaire de Tours (CHRU TOURS)

Subjects
Sun: general, 010504 meteorology & atmospheric sciences, Astronomy, Astrophysics, 01 natural sciences, 7. Clean energy, law.invention, Orbiter, Astronomi, astrofysik och kosmologi, law, 0103 physical sciences, Astronomy, Astrophysics and Cosmology, Aerospace engineering, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, Physics, Sun: radio radiation, business.industry, Astrophysics::Instrumentation and Methods for Astrophysics, Sun, Astronomy and Astrophysics, solar wind, Space and Planetary Science, general, radio radiation, Physics::Space Physics, Astrophysics::Earth and Planetary Astrophysics, business, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract

International audience; The Radio and Plasma Waves (RPW) instrument on the ESA Solar Orbiter mission is designed to measure in situ magnetic and electric fields and waves from the continuum up to several hundred kHz. The RPW also observes solar and heliospheric radio emissions up to 16 MHz. It was switched on and its antennae were successfully deployed two days after the launch of Solar Orbiter on February 10, 2020. Since then, the instrument has acquired enough data to make it possible to assess its performance and the electromagnetic disturbances it experiences. In this article, we assess its scientific performance and present the first RPW observations. In particular, we focus on a statistical analysis of the first observations of interplanetary dust by the instrument’s Thermal Noise Receiver. We also review the electro-magnetic disturbances that RPW suffers, especially those which potential users of the instrument data should be aware of before starting their research work.

Published
2021
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7. Density fluctuations associated with turbulence and waves First observations by Solar Orbiter

Author

Yu. V. Khotyaintsev, D. B. Graham, A. Vaivads, K. Steinvall, N. J. T. Edberg, A. I. Eriksson, E. P. G. Johansson, L. Sorriso-Valvo, M. Maksimovic, S. D. Bale, T. Chust, V. Krasnoselskikh, M. Kretzschmar, E. Lorfèvre, D. Plettemeier, J. Souček, M. Steller, Š. Štverák, P. Trávníček, A. Vecchio, T. S. Horbury, H. O’Brien, V. Evans, and V. Angelini

Subjects
Physics, Turbulence, Computer Science::Information Retrieval, Astronomy, turbulence, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Fusion, Plasma and Space Physics, Physics - Plasma Physics, Space Physics (physics.space-ph), law.invention, Plasma Physics (physics.plasm-ph), Orbiter, Fusion, plasma och rymdfysik, Physics - Space Physics, Astrophysics - Solar and Stellar Astrophysics, solar wind, Astronomi, astrofysik och kosmologi, Space and Planetary Science, law, Physics::Space Physics, Astronomy, Astrophysics and Cosmology, waves, Solar and Stellar Astrophysics (astro-ph.SR)
Abstract

We use the plasma density based on measurements of the probe-to-spacecraft potential in combination with magnetic field measurements by MAG to study fields and density fluctuations in the solar wind observed by Solar Orbiter during the first perihelion encounter ($\sim$0.5~AU away from the Sun). In particular we use the polarization of the wave magnetic field, the phase between the compressible magnetic field and density fluctuations and the compressibility ratio (the ratio of the normalized density fluctuations to the normalized compressible fluctuations of B) to characterize the observed waves and turbulence. We find that the density fluctuations are out-of-phase with the compressible component of magnetic fluctuations for intervals of turbulence, while they are in phase for the circular-polarized waves around the proton cyclotron frequency. We analyze in detail two specific events with simultaneous presence of left- and right-handed waves at different frequencies. We compare observed wave properties to a prediction of the three-fluid (electrons, protons and alphas) model. We find a limit on the observed wavenumbers, $10^{-6} < k < 7 \times 10^{-6}$~m$^{-1}$, which corresponds to wavelength $7 \times 10^6 >\lambda > 10^6$~m. We conclude that most likely both the left- and right-handed waves correspond to the low-wavenumber part (close to the cut-off at $\Omega_{c\mathrm{He}++}$) proton-band electromagnetic ion cyclotron (left-handed wave in the plasma frame confined to the frequency range $\Omega_{c\mathrm{He}++} < \omega < \Omega_{c\mathrm{H}+}$) waves propagating in the outwards and inwards directions respectively. The fact that both wave polarizations are observed at the same time and the identified wave mode has a low group velocity suggests that the double-banded events occur in the source regions of the waves., Comment: 13 pages, 9 figures

Published
2021
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8. Solar wind current sheets and deHoffmann-Teller analysis. First results from Solar Orbiter's DC electric field measurements

Author

K. Steinvall, Yu. V. Khotyaintsev, G. Cozzani, A. Vaivads, E. Yordanova, A. I. Eriksson, N. J. T. Edberg, M. Maksimovic, S. D. Bale, T. Chust, V. Krasnoselskikh, M. Kretzschmar, E. Lorfèvre, D. Plettemeier, J. Souček, M. Steller, Š. Štverák, A. Vecchio, T. S. Horbury, H. O’Brien, V. Evans, A. Fedorov, P. Louarn, V. Génot, N. André, B. Lavraud, A. P. Rouillard, C. J. Owen, 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), 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), Laboratoire de Physique et Chimie de l'Environnement et de l'Espace (LPC2E), Observatoire des Sciences de l'Univers en région Centre (OSUC), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Université d'Orléans (UO), Centre National d'Études Spatiales [Toulouse] (CNES), Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Laboratoire 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), and Science and Technology Facilities Council (STFC)

Subjects
astro-ph.SR, Astronomy, data analysis, MAGNETOPAUSE, Astrophysics, Astronomy & Astrophysics, law.invention, methods, Orbiter, Physics - Space Physics, law, Electric field, physics.plasm-ph, RECONNECTION, 0201 Astronomical and Space Sciences, Astrophysics::Solar and Stellar Astrophysics, Aerospace engineering, Physics, Science & Technology, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], business.industry, MAGNETIC-FIELD, Astronomy and Astrophysics, plasmas, methods: data analysis, Physics - Plasma Physics, Solar wind, solar wind, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, physics.space-ph, magnetic reconnection, Physical Sciences, Physics::Space Physics, SWITCHBACKS, Astrophysics::Earth and Planetary Astrophysics, Current (fluid), business
Abstract

Context.Solar Orbiter was launched on 10 February 2020 with the purpose of investigating solar and heliospheric physics using a payload of instruments designed for both remote and in situ studies. Similar to the recently launched Parker Solar Probe, and unlike earlier missions, Solar Orbiter carries instruments designed to measure low-frequency DC electric fields.Aims.In this paper, we assess the quality of the low-frequency DC electric field measured by the Radio and Plasma Waves instrument (RPW) on Solar Orbiter. In particular, we investigate the possibility of using Solar Orbiter’s DC electric and magnetic field data to estimate the solar wind speed.Methods.We used a deHoffmann-Teller (HT) analysis, based on measurements of the electric and magnetic fields, to find the velocity of solar wind current sheets, which minimises a single component of the electric field. By comparing the HT velocity to the proton velocity measured by the Proton and Alpha particle Sensor (PAS), we have developed a simple model for the effective antenna length,Leffof the E-field probes. We then used the HT method to estimate the speed of the solar wind.Results.Using the HT method, we find that the observed variations inEyare often in excellent agreement with the variations in the magnetic field. The magnitude ofEy, however, is uncertain due to the fact that theLeffdepends on the plasma environment. Here, we derive an empirical model relatingLeffto the Debye length, which we can use to improve the estimate ofEyand, consequently, the estimated solar wind speed.Conclusions.The low-frequency electric field provided by RPW is of high quality. Using the deHoffmann-Teller analysis, Solar Orbiter’s magnetic and electric field measurements can be used to estimate the solar wind speed when plasma data are unavailable.

Published
2021
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9. Evidence for local particle acceleration in the first recurrent galactic cosmic ray depression observed by Solar Orbiter The ion event on 19 June 2020

Author

A. Aran, D. Pacheco, M. Laurenza, N. Wijsen, D. Lario, S. Benella, I. G. Richardson, E. Samara, J. L. Freiherr von Forstner, B. Sanahuja, L. Rodriguez, L. Balmaceda, F. Espinosa Lara, R. Gómez-Herrero, K. Steinvall, A. Vecchio, V. Krupar, S. Poedts, R. C. Allen, G. B. Andrews, V. Angelini, L. Berger, D. Berghmans, S. Boden, S. I. Böttcher, F. Carcaboso, I. Cernuda, R. De Marco, S. Eldrum, V. Evans, A. Fedorov, J. Hayes, G. C. Ho, T. S. Horbury, N. P. Janitzek, Yu. V. Khotyaintsev, A. Kollhoff, P. Kühl, S. R. Kulkarni, W. J. Lees, P. Louarn, J. Magdalenic, M. Maksimovic, O. Malandraki, A. Martínez, G. M. Mason, C. Martín, H. O’Brien, C. Owen, P. Parra, M. Prieto Mateo, A. Ravanbakhsh, J. Rodriguez-Pacheco, O. Rodriguez Polo, S. Sánchez Prieto, C. E. Schlemm, H. Seifert, J. C. Terasa, K. Tyagi, C. Verbeeck, R. F. Wimmer-Schweingruber, Z. G. Xu, M. K. Yedla, A. N. Zhukov, Ministerio de Ciencia, Innovación y Universidades (España), European Space Agency, German Research Foundation, National Aeronautics and Space Administration (US), 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), 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
Physics, Acceleration of particles, heliosphere [Sun], [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Solar wind, Astrophysics::High Energy Astrophysical Phenomena, Astronomy, Astronomy and Astrophysics, Cosmic ray, Astrophysics, Ion, law.invention, Particle acceleration, Orbiter, Space and Planetary Science, law, [SDU]Sciences of the Universe [physics], Physics::Space Physics, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Sun: heliosphere, Event (particle physics)
Abstract

Aran, A., et al., [Context] In mid-June 2020, the Solar Orbiter (SolO) mission reached its first perihelion at 0.51 au and started its cruise phase, with most of the in situ instruments operating continuously. [Aims] We present the in situ particle measurements of the first proton event observed after the first perihelion obtained by the Energetic Particle Detector (EPD) suite on board SolO. The potential solar and interplanetary (IP) sources of these particles are investigated. Methods. Ion observations from ∼20 keV to ∼1 MeV are combined with available solar wind data from the Radio and Plasma Waves (RPW) instrument and magnetic field data from the magnetometer on board SolO to evaluate the energetic particle transport conditions and infer the possible acceleration mechanisms through which particles gain energy. We compare > 17-20 MeV ion count rate measurements for two solar rotations, along with the solar wind plasma data available from the Solar Wind Analyser (SWA) and RPW instruments, in order to infer the origin of the observed galactic cosmic ray (GCR) depressions. [Results] The lack of an observed electron event and of velocity dispersion at various low-energy ion channels and the observed IP structure indicate a local IP source for the low-energy particles. From the analysis of the anisotropy of particle intensities, we conclude that the low-energy ions were most likely accelerated via a local second-order Fermi process. The observed GCR decrease on 19 June, together with the 51.8-1034.0 keV nuc-1 ion enhancement, was due to a solar wind stream interaction region (SIR). The observation of a similar GCR decrease in the next solar rotation favours this interpretation and constitutes the first observation of a recurrent GCR decrease by SolO. The analysis of the recurrence times of this SIR suggests that it is the same SIR responsible for the He events previously measured in April and May. Finally, we point out that an IP structure more complex than a common SIR cannot be discarded, mainly due to the lack of solar wind temperature measurements and the lack of a higher cadence of solar wind velocity observations., EPD was built with funding from Ministerio de Ciencia e Innovación (Spain), Deutsches Zentrum für Luft- und Raumfahrt (Germany), and the European Space Agency (ESA); operations are funded by FEDER/MCI/AEI Projects ESP2017-88436-R and PID2019-104863RBI00/AEI/10.13039/501100011033 (Spain), 50OT 2002 (DLR, Germany), and NASA contract 80MSFC19F0002. The UB team acknowledges the support by the Spanish Ministerio de Ciencia e Innovación (MICINN) under grant PID2019-105510GB-C31 and through the “Center of Excellence María de Maeztu 2020-2023” award to the ICCUB (CEX2019-000918-M). The CAU Kiel team acknowledges support by the German Federal Ministry for Economic Affairs and Energy, the German Space Agency (Deutsches Zentrum für Luft- und Raumfahrt e.V., DLR) under grants 50OT0901, 50OT1202, 50OT1702, 50OT2002, and 50OC1702. The Solar Orbiter magnetometer was funded by the UK Space Agency (grant ST/T001062/1). M.L. and S.B. acknowledge financial support by the Italian MIUR-PRIN grant 2017APKP7T on Circumterrestrial Environment: Impact of Sun-Earth Interaction. N.W. acknowledges funding from the Research Foundation – Flanders (FWO – Vlaanderen, fellowship no. 1184319N). D.L. acknowledges the support from the NASA-HGI grant NNX16AF73G and the NASA Programs NNH17ZDA001N-LWS. I.G.R. and D.L. acknowledge support from NASA program NNH19ZDA001N-LWS. E.S. was supported by a PhD grant awarded by the Royal Observatory of Belgium. V.K. acknowledges the support by NASA under grants 18-2HSWO218_2-0010 and 19-HSR-19_2-0143. S.P. is supported by the projects C14/19/089 (C1 project Internal Funds KU Leuven), G.0D07.19N (FWO-Vlaanderen), SIDEX (ESA Prodex-12), and EUHFORIA 2.0 (funding from the European Union’s Horizon 2020 research and innovation programme under grant agreement No 870405). IRFU team acknowledges support from the Swedish National Space Agency grant 20/136. F.C. acknowledges the financial support by the Spanish MINECO-FPI-2016 predoctoral grant with FSE. The JHU/APL team is supported under NASA contract NNN06AA01C and thanks NASA headquarters and the NASA/GSFC Solar Orbiter project office for their continuing support. Solar Orbiter Solar Wind Analyser (SWA) data are derived from scientific sensors which have been designed and created, and are operated under funding provided in numerous contracts from the UK Space Agency (UKSA, most recently grant ST/T001356/1), the UK Science and Technology Facilities Council (STFC), the Agenzia Spaziale Italiana (ASI), the Centre National d’Etudes Spatiales (CNES, France), the Centre National de la Recherche Scientifique (CNRS, France), the Czech contribution to the ESA PRODEX programme and NASA.

Published
2021
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10. Whistler waves observed by Solar Orbiter/RPW between 0.5 AU and 1 AU

Author

M. Kretzschmar, T. Chust, V. Krasnoselskikh, D. Graham, L. Colomban, M. Maksimovic, Yu. V. Khotyaintsev, J. Soucek, K. Steinvall, O. Santolík, G. Jannet, J.-Y. Brochot, O. Le Contel, A. Vecchio, X. Bonnin, S. D. Bale, C. Froment, A. Larosa, M. Bergerard-Timofeeva, P. Fergeau, E. Lorfevre, D. Plettemeier, M. Steller, Š. Štverák, P. Trávníček, A. Vaivads, T. S. Horbury, H. O’Brien, V. Evans, V. Angelini, C. J. Owen, P. Louarn, Space Sciences Laboratory [Berkeley] (SSL), University of California [Berkeley], University of California-University of California, Laboratoire de Physique et Chimie de l'Environnement et de l'Espace (LPC2E), Observatoire des Sciences de l'Univers en région Centre (OSUC), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Centre National d'Études Spatiales [Toulouse] (CNES), 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 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), Swedish Institute of Space Physics [Uppsala] (IRF), Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA (UMR_8109)), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Institute of Atmospheric Physics [Prague] (IAP), Czech Academy of Sciences [Prague] (CAS), Technische Universität Dresden = Dresden University of Technology (TU Dresden), Institut für Weltraumforschung [Graz] (IWF), Osterreichische Akademie der Wissenschaften (ÖAW), Astronomical Institute of the Czech Academy of Sciences (ASU / CAS), Department of Physics [Imperial College London], Imperial College London, Mullard Space Science Laboratory (MSSL), University College of London [London] (UCL), Laboratoire d'études spatiales et d'instrumentation en astrophysique = Laboratory of Space Studies and Instrumentation in Astrophysics (LESIA), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), University of California [Berkeley] (UC Berkeley), University of California (UC)-University of California (UC), Institut für Weltraumforschung = Space Research institute [Graz] (IWF), 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 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
010504 meteorology & atmospheric sciences, Whistler, Astronomy, data analysis, [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], FOS: Physical sciences, Astrophysics, 01 natural sciences, law.invention, methods, Orbiter, Fusion, plasma och rymdfysik, Physics - Space Physics, Astronomi, astrofysik och kosmologi, law, 0103 physical sciences, Astronomy, Astrophysics and Cosmology, waves, Sun: heliosphere, 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), 0105 earth and related environmental sciences, Physics, Computer Science::Information Retrieval, Sun, heliosphere, Astronomy and Astrophysics, Fusion, Plasma and Space Physics, methods: data analysis, Space Physics (physics.space-ph), Astrophysics - Solar and Stellar Astrophysics, solar wind, Space and Planetary Science, Physics::Space Physics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract

The goal of our study is to detect and characterize the electromagnetic waves that can modify the electron distribution functions, with a special attention to whistler waves. We analyse in details the electric and magnetic field fluctuations observed by the Solar Orbiter spacecraft during its first orbit around the Sun between 0.5 and 1 AU. Using data of the Search Coil Magnetometer and electric antenna, both parts of the Radio and Plasma Waves (RPW) instrumental suite, we detect the electromagnetic waves with frequencies above 3 Hz and determine the statistical distribution of their amplitudes, frequencies, polarization and k-vector as a function of distance. We also discuss relevant instrumental issues regarding the phase between the electric and magnetic measurements and the effective length of the electric antenna. An overwhelming majority of the observed waves are right hand circularly polarized in the solar wind frame and identified as outward propagating and quasi parallel whistler waves. Their occurrence rate increases by a least a factor two from 1 AU to 0.5 AU. These results are consistent with the regulation of the heat flux by the whistler heat flux instability. Near 0.5 AU, whistler waves are found to be more field-aligned and to have smaller normalized frequency ($f/f_{ce}$), larger amplitude, and larger bandwidth than at 1 AU., accepted in A&A

Published
2021
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11. Electron Acceleration and Thermalization at Magnetotail Separatrices

Author

C. Norgren, M. Hesse, D. B. Graham, Yu. V. Khotyaintsev, P. Tenfjord, A. Vaivads, K. Steinvall, Y. Xu, D. J. Gershman, P.‐A. Lindqvist, F. Plaschke, and J. L. Burch

Subjects
010504 meteorology & atmospheric sciences, FOS: Physical sciences, Electron, 01 natural sciences, Fusion, plasma och rymdfysik, Physics - Space Physics, Astronomi, astrofysik och kosmologi, Astronomy, Astrophysics and Cosmology, 0105 earth and related environmental sciences, Line (formation), Physics, business.industry, Magnetic reconnection, Fusion, Plasma and Space Physics, Space Physics (physics.space-ph), Geophysics, Thermalisation, Amplitude, Space and Planetary Science, Physics::Space Physics, Cathode ray, Physics::Accelerator Physics, Atomic physics, business, Thermal energy, Beam (structure)
Abstract

In this study we use the Magnetospheric Multiscale mission to investigate the electron acceleration and thermalization occurring along the magnetic reconnection separatrices in the magnetotail. We find that initially cold electron lobe populations are accelerated toward the X line forming beams with energies up to a few kiloelectron volts, corresponding to a substantial fraction of the electron thermal energy inside the exhaust. The accelerated electron populations are unstable to the formation of electrostatic waves which develop into nonlinear electrostatic solitary waves. The waves' amplitudes are large enough to interact efficiently with a large part of the electron population, including the electron beam. The wave-particle interaction gradually thermalizes the beam, transforming directed drift energy to thermal energy. publishedVersion

Published
2020

12. Statistical study of electron density turbulence and ion-cyclotron waves in the inner heliosphere: Solar Orbiter observations

Author

F. Carbone, L. Sorriso-Valvo, Yu. V. Khotyaintsev, K. Steinvall, A. Vecchio, D. Telloni, E. Yordanova, D. B. Graham, N. J. T. Edberg, A. I. Eriksson, E. P. G. Johansson, C. L. Vásconez, M. Maksimovic, R. Bruno, R. D’Amicis, S. D. Bale, T. Chust, V. Krasnoselskikh, M. Kretzschmar, E. Lorfèvre, D. Plettemeier, J. Souček, M. Steller, Š. Štverák, P. Trávníček, A. Vaivads, T. S. Horbury, H. O’Brien, V. Angelini, and V. Evans

Subjects
Electron density, Astronomy, Cyclotron, FOS: Physical sciences, Astrophysics, 01 natural sciences, Ion, law.invention, Orbiter, Physics - Space Physics, law, 0103 physical sciences, waves, 010303 astronomy & astrophysics, Physics, 010308 nuclear & particles physics, Turbulence, turbulence, Astronomy and Astrophysics, plasmas, Space Physics (physics.space-ph), Physics - Plasma Physics, Computational physics, Plasma Physics (physics.plasm-ph), solar wind, Space and Planetary Science, Physics::Space Physics, Heliosphere
Abstract

Context. The recently released spacecraft potential measured by the RPW instrument on board Solar Orbiter has been used to estimate the solar wind electron density in the inner heliosphere. Aims. The measurement of the solar wind’s electron density, taken in June 2020, has been analysed to obtain a thorough characterization of the turbulence and intermittency properties of the fluctuations. Magnetic field data have been used to describe the presence of ion-scale waves. Methods. To study and quantify the properties of turbulence, we extracted selected intervals. We used empirical mode decomposition to obtain the generalized marginal Hilbert spectrum, equivalent to the structure functions analysis, which additionally reduced issues typical of non-stationary, short time series. The presence of waves was quantitatively determined by introducing a parameter describing the time-dependent, frequency-filtered wave power. Results. A well-defined inertial range with power-law scalng was found almost everywhere in the sample studied. However, the Kolmogorov scaling and the typical intermittency effects are only present in fraction of the samples. Other intervals have shallower spectra and more irregular intermittency, which are not described by models of turbulence. These are observed predominantly during intervals of enhanced ion frequency wave activity. Comparisons with compressible magnetic field intermittency (from the MAG instrument) and with an estimate of the solar wind velocity (using electric and magnetic field) are also provided to give general context and help determine the cause of these anomalous fluctuations.

Published
2021
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13. Active and passive imaging NIR/SWIR performance for slant paths close to ground

Author

Ove K. Steinvall

Subjects
Passive imaging, Optics, Geography, business.industry, Turbulence, Attenuation coefficient, Attenuation, Diffuse sky radiation, Atmospheric turbulence, Visibility, business, Near infrared radiation, Remote sensing
Abstract

Imaging active and passive EO-sensors are gaining an increasing interest in military and security applications. However the performance is often hampered by atmospheric effects such as attenuation and/or turbulence. This paper will investigate the performance for slant paths close to ground and show that a substantial improvement in imaging performance can be obtained by elevating the sensor, sometimes even by a small amount.

Published
2013
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14. Electron Heating by Debye-Scale Turbulence in Guide-Field Reconnection.

Author

Khotyaintsev YV, Graham DB, Steinvall K, Alm L, Vaivads A, Johlander A, Norgren C, Li W, Divin A, Fu HS, Hwang KJ, Burch JL, Ahmadi N, Le Contel O, Gershman DJ, Russell CT, and Torbert RB

Abstract

We report electrostatic Debye-scale turbulence developing within the diffusion region of asymmetric magnetopause reconnection with a moderate guide field using observations by the Magnetospheric Multiscale mission. We show that Buneman waves and beam modes cause efficient and fast thermalization of the reconnection electron jet by irreversible phase mixing, during which the jet kinetic energy is transferred into thermal energy. Our results show that the reconnection diffusion region in the presence of a moderate guide field is highly turbulent, and that electrostatic turbulence plays an important role in electron heating.

Published
2020
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15. Observations of Electromagnetic Electron Holes and Evidence of Cherenkov Whistler Emission.

Author

Steinvall K, Khotyaintsev YV, Graham DB, Vaivads A, Le Contel O, and Russell CT

Abstract

We report observations of electromagnetic electron holes (EHs). We use multispacecraft analysis to quantify the magnetic field contributions of three mechanisms: the Lorentz transform, electron drift within the EH, and Cherenkov emission of whistler waves. The first two mechanisms account for the observed magnetic fields for slower EHs, while for EHs with speeds approaching half the electron Alfvén speed, whistler waves excited via the Cherenkov mechanism dominate the perpendicular magnetic field. The excited whistler waves are kinetically damped and typically confined within the EHs.

Published
2019
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16. Balancing a changed life situation: the lived experience from next of kin to persons with inoperable lung cancer.

Author

Steinvall K, Johansson H, and Berterö C

Subjects
Aged, Female, Humans, Interpersonal Relations, Male, Middle Aged, Palliative Care, Sweden, Uncertainty, Family psychology, Lung Neoplasms diagnosis, Quality of Life psychology
Abstract

The purpose of this study was to identify and describe the experiences of quality of life/life situation among those who were next of kin to persons with inoperable lung cancer. Data were collected in qualitative interviews, where 11 next of kin articulated their lived experiences, and were interpreted through interpretive phenomenology. Four themes were identified: changed life situation, experiences of uncertainty due to awareness of the ill person's changed health status, interpersonal relationships, and false hopes due to health care professionals' treatment. These four themes gave a structure presenting the essence: balancing a changed life situation. The findings of the study point out the importance of promoting support for the next of kin, because they are significantly affected by the changed life situation. There is a need to identify their needs and to support them.

Published
2011
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