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1. Electron Bernstein waves driven by electron crescents near the electron diffusion region.

Author

Li, WY, Graham, DB, Khotyaintsev, Yu V, Vaivads, A, André, M, Min, K, Liu, K, Tang, BB, Wang, C, Fujimoto, K, Norgren, C, Toledo-Redondo, S, Lindqvist, P-A, Ergun, RE, Torbert, RB, Rager, AC, Dorelli, JC, Gershman, DJ, Giles, BL, Lavraud, B, Plaschke, F, Magnes, W, Le Contel, O, Russell, CT, and Burch, JL

Abstract

The Magnetospheric Multiscale (MMS) spacecraft encounter an electron diffusion region (EDR) of asymmetric magnetic reconnection at Earth's magnetopause. The EDR is characterized by agyrotropic electron velocity distributions on both sides of the neutral line. Various types of plasma waves are produced by the magnetic reconnection in and near the EDR. Here we report large-amplitude electron Bernstein waves (EBWs) at the electron-scale boundary of the Hall current reversal. The finite gyroradius effect of the outflow electrons generates the crescent-shaped agyrotropic electron distributions, which drive the EBWs. The EBWs propagate toward the central EDR. The amplitude of the EBWs is sufficiently large to thermalize and diffuse electrons around the EDR. The EBWs contribute to the cross-field diffusion of the electron-scale boundary of the Hall current reversal near the EDR.

Published
2020

2. The Space Physics Environment Data Analysis System (SPEDAS).

Author

Angelopoulos, V, Cruce, P, Drozdov, A, Grimes, EW, Hatzigeorgiu, N, King, DA, Larson, D, Lewis, JW, McTiernan, JM, Roberts, DA, Russell, CL, Hori, T, Kasahara, Y, Kumamoto, A, Matsuoka, A, Miyashita, Y, Miyoshi, Y, Shinohara, I, Teramoto, M, Faden, JB, Halford, AJ, McCarthy, M, Millan, RM, Sample, JG, Smith, DM, Woodger, LA, Masson, A, Narock, AA, Asamura, K, Chang, TF, Chiang, C-Y, Kazama, Y, Keika, K, Matsuda, S, Segawa, T, Seki, K, Shoji, M, Tam, SWY, Umemura, N, Wang, B-J, Wang, S-Y, Redmon, R, Rodriguez, JV, Singer, HJ, Vandegriff, J, Abe, S, Nose, M, Shinbori, A, Tanaka, Y-M, UeNo, S, Andersson, L, Dunn, P, Fowler, C, Halekas, JS, Hara, T, Harada, Y, Lee, CO, Lillis, R, Mitchell, DL, Argall, MR, Bromund, K, Burch, JL, Cohen, IJ, Galloy, M, Giles, B, Jaynes, AN, Le Contel, O, Oka, M, Phan, TD, Walsh, BM, Westlake, J, Wilder, FD, Bale, SD, Livi, R, Pulupa, M, Whittlesey, P, DeWolfe, A, Harter, B, Lucas, E, Auster, U, Bonnell, JW, Cully, CM, Donovan, E, Ergun, RE, Frey, HU, Jackel, B, Keiling, A, Korth, H, McFadden, JP, Nishimura, Y, Plaschke, F, Robert, P, Turner, DL, Weygand, JM, Candey, RM, Johnson, RC, Kovalick, T, Liu, MH, McGuire, RE, and Breneman, A

Subjects
Geospace science, Ionospheric physics, Magnetospheric physics, Planetary magnetospheres, Solar wind, Space plasmas, Solarwind, Astronomical and Space Sciences, Astronomy & Astrophysics
Abstract

With the advent of the Heliophysics/Geospace System Observatory (H/GSO), a complement of multi-spacecraft missions and ground-based observatories to study the space environment, data retrieval, analysis, and visualization of space physics data can be daunting. The Space Physics Environment Data Analysis System (SPEDAS), a grass-roots software development platform (www.spedas.org), is now officially supported by NASA Heliophysics as part of its data environment infrastructure. It serves more than a dozen space missions and ground observatories and can integrate the full complement of past and upcoming space physics missions with minimal resources, following clear, simple, and well-proven guidelines. Free, modular and configurable to the needs of individual missions, it works in both command-line (ideal for experienced users) and Graphical User Interface (GUI) mode (reducing the learning curve for first-time users). Both options have "crib-sheets," user-command sequences in ASCII format that can facilitate record-and-repeat actions, especially for complex operations and plotting. Crib-sheets enhance scientific interactions, as users can move rapidly and accurately from exchanges of technical information on data processing to efficient discussions regarding data interpretation and science. SPEDAS can readily query and ingest all International Solar Terrestrial Physics (ISTP)-compatible products from the Space Physics Data Facility (SPDF), enabling access to a vast collection of historic and current mission data. The planned incorporation of Heliophysics Application Programmer's Interface (HAPI) standards will facilitate data ingestion from distributed datasets that adhere to these standards. Although SPEDAS is currently Interactive Data Language (IDL)-based (and interfaces to Java-based tools such as Autoplot), efforts are under-way to expand it further to work with python (first as an interface tool and potentially even receiving an under-the-hood replacement). We review the SPEDAS development history, goals, and current implementation. We explain its "modes of use" with examples geared for users and outline its technical implementation and requirements with software developers in mind. We also describe SPEDAS personnel and software management, interfaces with other organizations, resources and support structure available to the community, and future development plans.Electronic supplementary materialThe online version of this article (10.1007/s11214-018-0576-4) contains supplementary material, which is available to authorized users.

Published
2019

3. Direct observations of energy transfer from resonant electrons to whistler-mode waves in magnetosheath of Earth

Author

Kitamura, N., Amano, T., Omura, Y., Boardsen, S. A., Gershman, D. J., Miyoshi, Y., Kitahara, M., Katoh, Y., Kojima, H., Nakamura, S., Shoji, M., Saito, Y., Yokota, S., Giles, B. L., Paterson, W. R., Pollock, C. J., Barrie, A. C., Skeberdis, D. G., Kreisler, S., Le Contel, O., Russell, C. T., Strangeway, R. J., Lindqvist, P.-A., Ergun, R. E., Torbert, R. B., and Burch, J. L.

Published
2022
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5. Global Compression of the Plasma Sheet and Magnetotail During Intense Storms From THEMIS Observations.

Author

Alqeeq, S. W., Fontaine, D., Le Contel, O., Akhavan Tafti, M., Cazzola, E., Atilaw, T., Angelopoulos, V., and Auster, H. U.

Subjects
CORONAL mass ejections, STORMS, SPACE environment, MAGNETIC storms, DYNAMIC pressure, SOLAR wind
Abstract

We estimate the global impact of storms on the global structure and dynamics of the night side plasma sheet from observations by the NASA mission Time History of Events and Macroscale Interactions during Substorms (THEMIS). We focus on an intense storm occurring in December 2015 triggered by interplanetary coronal mass ejections (ICMEs). It starts with a storm sudden commencement (SSC) phase (SYM‐H ∼ ${\sim} $ +50 nT) followed by a growth phase (SYM‐H ∼ ${\sim} $ −188 nT at the minimum) and then a long recovery phase lasting several days. We investigate THEMIS observations when the spacecraft were located in the midnight sector of the plasma sheet at distances typically between 8 and 13 Earth's radii. It is found that the plasma sheet has been globally compressed up to a value of about ∼> ${\sim} > $4 nPa during the SSC and main phases, that is, 8 times larger than its value during the quiet phase before the event. This compression occurs during periods of high dynamic pressure in the ICME (20 nPa) about one order of magnitude larger than its value in the pristine solar wind. We infer a global increase of the lobe magnetic field from 30 to 100 nT, confirmed by THEMIS data just outside the plasma sheet. During the SSC and main phases, the plasma sheet is found thinner by a factor of 2 relative to its thickness at quiet times, while the Tsyganenko T96 magnetic field model shows very stretched magnetic field lines from inner magnetospheric regions toward the night side. During the recovery phase, whereas the interplanetary pressure has dropped off, the plasma sheet tends to gradually recover its quiet phase characteristics (pressure, thickness, magnetic configuration, etc.) during a long recovery phase of several days. Key Points: The global plasma sheet's structure and dynamics are quantified during storms triggered by interplanetary coronal mass ejections using Time History of Events and Macroscale Interactions during Substorms observationsDuring the storm sudden commencement (SSC) and main phases, the magnetotail and plasma sheet have been compressed by a factor of 8 relative to the preceding quiet phaseUsing the T96 model, the plasma sheet is highly stretched during the storm SSC and main phases, gradually returning to the quiet phase [ABSTRACT FROM AUTHOR]

Published
2024
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6. Wave Phenomena and Beam-Plasma Interactions at the Magnetopause Reconnection Region.

Author

Burch, JL, Webster, JM, Genestreti, KJ, Torbert, RB, Giles, BL, Fuselier, SA, Dorelli, JC, Rager, AC, Phan, TD, Allen, RC, Chen, L-J, Wang, S, Le Contel, O, Russell, CT, Strangeway, RJ, Ergun, RE, Jaynes, AN, Lindqvist, P-A, Graham, DB, Wilder, FD, Hwang, K-J, and Goldstein, J

Subjects
magnetopause, reconnection, Astronomical and Space Sciences, Atmospheric Sciences
Abstract

This paper reports on Magnetospheric Multiscale observations of whistler mode chorus and higher-frequency electrostatic waves near and within a reconnection diffusion region on 23 November 2016. The diffusion region is bounded by crescent-shaped electron distributions and associated dissipation just upstream of the X-line and by magnetic field-aligned currents and electric fields leading to dissipation near the electron stagnation point. Measurements were made southward of the X-line as determined by southward directed ion and electron jets. We show that electrostatic wave generation is due to magnetosheath electron beams formed by the electron jets as they interact with a cold background plasma and more energetic population of magnetospheric electrons. On the magnetosphere side of the X-line the electron beams are accompanied by a strong perpendicular electron temperature anisotropy, which is shown to be the source of an observed rising-tone whistler mode chorus event. We show that the apex of the chorus event and the onset of electrostatic waves coincide with the opening of magnetic field lines at the electron stagnation point.

Published
2018

8. Reconnection Inside a Dipolarization Front of a Diverging Earthward Fast Flow

Author

Hosner, M., primary, Nakamura, R., additional, Schmid, D., additional, Nakamura, T. K. M., additional, Panov, E. V., additional, Volwerk, M., additional, Vörös, Z., additional, Roberts, O. W., additional, Blasl, K. A., additional, Settino, A., additional, Korovinskiy, D., additional, Marshall, A. T., additional, Denton, R. E., additional, Burch, J. L., additional, Giles, B. L., additional, Torbert, R. B., additional, Le Contel, O., additional, Escoubet, C. P., additional, Dandouras, I. S., additional, Carr, C., additional, and Fazakerley, A. N., additional

Published
2024
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9. Electron-scale dynamics of the diffusion region during symmetric magnetic reconnection in space

Author

Torbert, R. B., Burch, J. L., Phan, T. D., Hesse, M., Argall, M. R., Shuster, J., Ergun, R. E., Alm, L., Nakamura, R., Genestreti, K. J., Gershman, D. J., Paterson, W. R., Turner, D. L., Cohen, I., Giles, B. L., Pollock, C. J., Wang, S., Chen, L.-J., Stawarz, J. E., Eastwood, J. P., Hwang, K. J., Farrugia, C., Dors, I., Vaith, H., Mouikis, C., Ardakani, A., Mauk, B. H., Fuselier, S. A., Russell, C. T., Strangeway, R. J., Moore, T. E., Drake, J. F., Shay, M. A., Khotyaintsev, Yuri V., Lindqvist, P.-A., Baumjohann, W., Wilder, F. D., Ahmadi, N., Dorelli, J. C., Avanov, L. A., Oka, M., Baker, D. N., Fennell, J. F., Blake, J. B., Jaynes, A. N., Le Contel, O., Petrinec, S. M., Lavraud, B., and Saito, Y.

Published
2018

10. Chorus intensity modulation driven by time‐varying field‐aligned low‐energy plasma

Author

Nishimura, Y, Bortnik, J, Li, W, Liang, J, Thorne, RM, Angelopoulos, V, Le Contel, O, Auster, U, and Bonnell, JW

Subjects
Affordable and Clean Energy, whistler mode chorus waves, pulsating aurora, low-energy electrons and ions, Astronomical and Space Sciences, Atmospheric Sciences
Abstract

©2015. American Geophysical Union. Recent studies have shown that chorus waves are responsible for scattering and precipitating the energetic electrons that drive the pulsating aurora. While some of the chorus intensity modulation events are correlated with

Published
2015

11. Magnetospheric Time‐History in Storm‐Time Magnetic Flux Dynamics: A Global Simulation Campaign.

Author

Atilaw, T. Y., Akhavan‐Tafti, M., Al Shidi, Q., Pulkkinen, T. I., Fontaine, D., Le Contel, O., Slavin, J. A., Le, G., Chen, L.‐J., Reiff, P. H., and Alqeeq, S. W.

Subjects
MAGNETIC flux, MAGNETIC flux density, SOLAR photosphere, STORMS, SPACE environment
Abstract

This paper aims to quantify the magnetospheric magnetic flux contents under moderate to intense space weather conditions using global simulations. This study is a companion to Akhavan‐Tafti, Atilaw, et al. (2023, https://doi.org/10.1029/2023JA031832) where magnetic flux evolution is presented for a catalog of storm events, using Heliophysics System Observatory (HSO) observations. For this study, we used the Space Weather Modeling Framework (SWMF) in Geospace configuration to study magnetic flux dynamics for a subset of their storm events (15 events). Simulations reliably resolve the storm‐time magnetic flux Bz and current density |J| asymmetries across the different storm phases. It is revealed that: relative to the quiet period, flux content is enhanced during the storm sudden commencement (SSC) phase in the dayside by ΔBz/Bz, quiet = +17%, and reduced in the nightside magnetosphere (r[RE] < −6 RE) by −15%. At the same time, the cross‐tail current is found to enhance (|J| = 2 nA/m2), which suggests the storm impact in the nightside magnetosphere is much earlier in the storm cycle than previously shown. Concurring with previous studies, a significant depletion of magnetic flux by up to −40%, with day‐night and dawn‐dusk asymmetries, can be seen during the main and recovery phases. This corresponds to the enhanced current density (|J| = 5–8 nA/m2) at ∼6 RE further confirming the role of ring current in driving magnetospheric dynamics during the main and recovery phases. This is in contrast with the SSC phase wherein the Chapman‐Ferraro and cross‐tail currents are the dominant current systems. Key Points: The nightside magnetospheric flux is impacted by the storm event earlier in the storm cycle than expected, (i.e., the SSC phase)Decrease in flux content of up to −40% within the inner magnetosphere for the main and recovery phases is associated with the enhanced ring currentStorm‐time asymmetries in magnetic flux and current density are well‐resolved throughout the storm phases [ABSTRACT FROM AUTHOR]

Published
2024
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12. Two Classes of Equatorial Magnetotail Dipolarization Fronts Observed by Magnetospheric Multiscale Mission: A Statistical Overview

Author

Alqeeq, S. W., primary, Le Contel, O., additional, Canu, P., additional, Retinò, A., additional, Chust, T., additional, Mirioni, L., additional, Chuvatin, A., additional, Nakamura, R., additional, Ahmadi, N., additional, Wilder, F. D., additional, Gershman, D. J., additional, Khotyaintsev, Yu. V., additional, Lindqvist, P.‐A., additional, Ergun, R. E., additional, Burch, J. L., additional, Torbert, R. B., additional, Fuselier, S. A., additional, Russell, C. T., additional, Wei, H. Y., additional, Strangeway, R. J., additional, Bromund, K. R., additional, Fischer, D., additional, Giles, B. L., additional, and Saito, Y., additional

Published
2023
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13. Electron magnetic reconnection without ion coupling in Earth’s turbulent magnetosheath

Author

Phan, T. D., Eastwood, J. P., Shay, M. A., Drake, J. F., Sonnerup, B. U. Ö., Fujimoto, M., Cassak, P. A., Øieroset, M., Burch, J. L., Torbert, R. B., Rager, A. C., Dorelli, J. C., Gershman, D. J., Pollock, C., Pyakurel, P. S., Haggerty, C. C., Khotyaintsev, Y., Lavraud, B., Saito, Y., Oka, M., Ergun, R. E., Retino, A., Le Contel, O., Argall, M. R., Giles, B. L., Moore, T. E., Wilder, F. D., Strangeway, R. J., Russell, C. T., Lindqvist, P. A., and Magnes, W.

Published
2018
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14. Two Classes of Equatorial Magnetotail Dipolarization Fronts Observed by Magnetospheric Multiscale Mission : A Statistical Overview

Author

Alqeeq, S. W., Le Contel, O., Canu, P., Retino, A., Chust, T., Mirioni, L., Chuvatin, A., Nakamura, R., Ahmadi, N., Wilder, F. D., Gershman, D. J., Khotyaintsev, Yuri V., Lindqvist, P. -A, Ergun, R. E., Burch, J. L., Torbert, R. B., Fuselier, S. A., Russell, C. T., Wei, H. Y., Strangeway, R. J., Bromund, K. R., Fischer, D., Giles, B. L., Saito, Y., Alqeeq, S. W., Le Contel, O., Canu, P., Retino, A., Chust, T., Mirioni, L., Chuvatin, A., Nakamura, R., Ahmadi, N., Wilder, F. D., Gershman, D. J., Khotyaintsev, Yuri V., Lindqvist, P. -A, Ergun, R. E., Burch, J. L., Torbert, R. B., Fuselier, S. A., Russell, C. T., Wei, H. Y., Strangeway, R. J., Bromund, K. R., Fischer, D., Giles, B. L., and Saito, Y.

Abstract

We carried out a statistical study of equatorial dipolarization fronts (DFs) detected by the Magnetospheric Multiscale mission during the full 2017 Earth's magnetotail season. We found that two DF classes are distinguished: class I (74.4%) corresponds to the standard DF properties and energy dissipation and a new class II (25.6%). This new class includes the six DF discussed in Alqeeq et al. (2022, ) and corresponds to a bump of the magnetic field associated with a minimum in the ion and electron pressures and a reversal of the energy conversion process. The possible origin of this second class is discussed. Both DF classes show that the energy conversion process in the spacecraft frame is driven by the diamagnetic current dominated by the ion pressure gradient. In the fluid frame, it is driven by the electron pressure gradient. In addition, we have shown that the energy conversion processes are not homogeneous at the electron scale mostly due to the variations of the electric fields for both DF classes.

Published
2023
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15. Magnetospheric Time History in Storm‐Time Magnetic Flux Dynamics.

Author

Akhavan‐Tafti, M., Atilaw, T. Y., Fontaine, D., Le Contel, O., Slavin, J. A., and Pulkkinen, T.

Subjects
MAGNETIC flux, EXTREME weather, CORONAL mass ejections, WEATHER forecasting, SPACE environment
Abstract

Magnetospheric magnetic flux dynamics is quantified in 29 geomagnetic storms between 2015 and 2019, using near‐equatorial Van Allen Probe, GOES, and Magnetospheric Multiscale satellites. For the first time, concurrent, multi‐probe observations are utilized to preserve magnetospheric time history, defined as the state of the magnetosphere leading up to an observation. It is revealed that, relative to pre‐storm conditions, (a) during the storm sudden commencement (SSC), magnetic flux uniformly increases ΔΨ = +15% throughout the magnetosphere, except in the nightside inner magnetosphere where ΔΨ = −30%, and (b) during storm main and recovery phases, ΔΨ = −30% and −15%, respectively, in the nightside magnetosphere, at radial distances 5 ≤ r [RE] < 8. It is found that a symmetric ring current is likely formed in the nightside, early in the storm process (localized during SSC), which then broadens during the main phase, before weakening during the recovery phase. The current system on the dayside shows a distinct dawn‐dusk asymmetry. Plain Language Summary: The Earth's magnetosphere serves as a shield against extreme space weather conditions, including interplanetary coronal mass ejections. Understanding the magnetospheric dynamics during geomagnetic storms is critical for a reliable and accurate space weather prediction capability. This study provides a novel statistical analysis technique for investigating the magnetospheric closed magnetic flux content during different storm phases, using magnetic field data from a multitude of satellite missions. The technique considers critical information, such as the state of the magnetosphere before a geomagnetic storm. This multi‐mission analysis technique, though challenging due to orbital differences, provides a comprehensive view of the storm‐time magnetosphere. Our analysis suggests that the magnetosphere is non‐uniformly impacted by different geomagnetic storm phases, paving the path for more reliable storm prediction models. Key Points: Concurrent, multi‐probe observations help preserve magnetospheric time history for a more reliable space weather prediction capabilityMagnetic flux is substantially reduced in the nightside inner magnetosphere during all storm phases, relative to the quiet periodMagnetic flux changes between different storm phases are most significant in the nightside inner magnetosphere, asymmetric on the dayside [ABSTRACT FROM AUTHOR]

Published
2023
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16. Electron Diffusion Regions in Magnetotail Reconnection Under Varying Guide Fields

Author

Chen, L.‐J, Wang, S, Hesse, M, Ergun, R. E, Moore, T, Giles, B, Bessho, N, Russell, C, Burch, J, Torbert, R. B, Genestreti, K. J, Paterson, W, Pollock, C, Lavraud, B, Le Contel, O, Strangeway, R, Khotyaintsev, Yu V, and Lindqvist, P.‐A

Subjects
Geophysics
Abstract

Kinetic structures of electron diffusion regions (EDRs) under finite guide fields in magnetotail reconnection are reported. The EDRs with guide fields 0.14–0.5 (in unit of the reconnecting component) are detected by the Magnetospheric Multiscale spacecraft. The key new features include the following: (1) cold inflowing electrons accelerated along the guide field and demagnetized at the magnetic field minimum while remaining a coherent population with a low perpendicular temperature, (2) wave fluctuations generating strong perpendicular electron flows followed by alternating parallel flows inside the reconnecting current sheet under an intermediate guide field, and (3) gyrophase bunched electrons with high parallel speeds leaving the X‐line region. The normalized reconnection rates for the three EDRs range from 0.05 to 0.3. The measurements reveal that finite guide fields introduce new mechanisms to break the electron frozen‐in condition.

Published
2019
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18. The THEMIS Magnetic Cleanliness Program

Author

Ludlam, M., Angelopoulos, V., Taylor, E., Snare, R. C., Means, J. D., Ge, Y. S., Narvaez, P., Auster, H. U., Le Contel, O., Larson, D., Moreau, T., Burch, J. L., editor, and Angelopoulos, V., editor

Published
2009
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19. First Results of the THEMIS Search Coil Magnetometers

Author

Le Contel, O., Roux, A., Robert, P., Coillot, C., Bouabdellah, A., de la Porte, B., Alison, D., Ruocco, S., Angelopoulos, V., Bromund, K., Chaston, C. C., Cully, C., Auster, H. U., Glassmeier, K. H., Baumjohann, W., Carlson, C. W., McFadden, J. P., Larson, D., Burch, J. L., editor, and Angelopoulos, V., editor

Published
2009
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21. The Search-Coil Magnetometer for MMS

Author

Le Contel, O., primary, Leroy, P., additional, Roux, A., additional, Coillot, C., additional, Alison, D., additional, Bouabdellah, A., additional, Mirioni, L., additional, Meslier, L., additional, Galic, A., additional, Vassal, M. C., additional, Torbert, R. B., additional, Needell, J., additional, Rau, D., additional, Dors, I., additional, Ergun, R. E., additional, Westfall, J., additional, Summers, D., additional, Wallace, J., additional, Magnes, W., additional, Valavanoglou, A., additional, Olsson, G., additional, Chutter, M., additional, Macri, J., additional, Myers, S., additional, Turco, S., additional, Nolin, J., additional, Bodet, D., additional, Rowe, K., additional, Tanguy, M., additional, and de la Porte, B., additional

Published
2016
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22. Electron Bulk Acceleration and Thermalization at Earth's Quasiperpendicular Bow Shock

Author

Chen, L.-J, Wang, S, Wilson, L. B., III, Schwartz, S, Bessho, Naoki, Moore, T, Gershman, D, Giles, B, Wilder, F. D, Ergun, R. E, Hesse, M, Lai, H, Russell, C, Strangeway, R, Torbert, R. B, F.-Vinas, A, Burch, J, Lee, S, Pollock, C, Dorelli, J, Paterson, W, Ahmadi, N, Goodrich, K, Lavraud, B, Le Contel, O, Khotyaintsev, Yu V, Lindqvist, P.-A, Boardsen, S, Wei, h, Le, A, and Avanov, L

Subjects
Solar Physics
Abstract

Electron heating at Earth's quasiperpendicular bow shock has been surmised to be due to the combined effects of a quasistatic electric potential and scattering through wave-particle interaction. Here we report the observation of electron distribution functions indicating a new electron heating process occurring at the leading edge of the shock front. Incident solar wind electrons are accelerated parallel to the magnetic field toward downstream, reaching an electron-ion relative drift speed exceeding the electron thermal speed. The bulk acceleration is associated with an electric field pulse embedded in a whistler-mode wave. The high electron-ion relative drift is relaxed primarily through a nonlinear current-driven instability. The relaxed distributions contain a beam traveling toward the shock as a remnant of the accelerated electrons. Similar distribution functions prevail throughout the shock transition layer, suggesting that the observedacceleration and thermalization is essential to the cross-shock electron heating.

Published
2018
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23. The Search-Coil Magnetometer for MMS

Author

Le Contel, O., Leroy, P., Roux, A., Coillot, C., Alison, D., Bouabdellah, A., Mirioni, L., Meslier, L., Galic, A., Vassal, M. C., Torbert, R. B., Needell, J., Rau, D., Dors, I., Ergun, R. E., Westfall, J., Summers, D., Wallace, J., Magnes, W., Valavanoglou, A., Olsson, G., Chutter, M., Macri, J., Myers, S., Turco, S., Nolin, J., Bodet, D., Rowe, K., Tanguy, M., and de la Porte, B.

Published
2016
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24. Evidence for Whistler Waves Propagating Into the Electron Diffusion Region of Collisionless Magnetic Reconnection

Author

Zhong, Z. H., Zhou, M., Graham, Daniel B., Khotyaintsev, Yuri V., Wu, Y. F., Le Contel, O., Li, H. M., Tao, X., Tang, R. X., Deng, X. H., Zhong, Z. H., Zhou, M., Graham, Daniel B., Khotyaintsev, Yuri V., Wu, Y. F., Le Contel, O., Li, H. M., Tao, X., Tang, R. X., and Deng, X. H.

Abstract

Despite a growing number of observations of whistler waves in/around the reconnection diffusion region, the origin of the whistler waves in the diffusion region and their role in reconnection remain elusive. This paper investigates the whistler-mode waves within an electron-scale reconnecting current sheet observed by the Magnetospheric Multiscale mission on 23 December 2016. These whistlers were observed in both the electron diffusion region (EDR) and the immediate inflow region of the electron-scale magnetic reconnection site. The dispersion relation of these whistlers is measured and compared to predictions from linear theory for the first time in these regions. The comparison shows that the field-aligned drifting electron component critically modifies the dispersion relation of whistlers in the EDR due to the Doppler-shift effects. We demonstrate that these whistlers propagated into the EDR from outside rather than locally excited, however, they did not provide sufficiently large anomalous dissipation in this EDR.

Published
2022
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25. Investigation of the homogeneity of energy conversion processes at dipolarization fronts from MMS measurements

Author

Alqeeq, S. W., Le Contel, O., Canu, P., Retino, A., Chust, T., Mirioni, L., Richard, Louis, Ait-Si-Ahmed, Y., Alexandrova, A., Chuvatin, A., Ahmadi, N., Baraka, S. M., Nakamura, R., Wilder, F. D., Gershman, D. J., Lindqvist, P. A., Khotyaintsev, Yuri V., Ergun, R. E., Burch, J. L., Torbert, R. B., Russell, C. T., Magnes, W., Strangeway, R. J., Bromund, K. R., Wei, H., Plaschke, F., Anderson, B. J., Giles, B. L., Fuselier, S. A., Saito, Y., Lavraud, B., Alqeeq, S. W., Le Contel, O., Canu, P., Retino, A., Chust, T., Mirioni, L., Richard, Louis, Ait-Si-Ahmed, Y., Alexandrova, A., Chuvatin, A., Ahmadi, N., Baraka, S. M., Nakamura, R., Wilder, F. D., Gershman, D. J., Lindqvist, P. A., Khotyaintsev, Yuri V., Ergun, R. E., Burch, J. L., Torbert, R. B., Russell, C. T., Magnes, W., Strangeway, R. J., Bromund, K. R., Wei, H., Plaschke, F., Anderson, B. J., Giles, B. L., Fuselier, S. A., Saito, Y., and Lavraud, B.

Abstract

We report on six dipolarization fronts (DFs) embedded in fast earthward flows detected by the Magnetospheric Multiscale mission during a substorm event on 23 July 2017. We analyzed Ohm's law for each event and found that ions are mostly decoupled from the magnetic field by Hall fields. However, the electron pressure gradient term is also contributing to the ion decoupling and likely responsible for an electron decoupling at DF. We also analyzed the energy conversion process and found that the energy in the spacecraft frame is transferred from the electromagnetic field to the plasma (J & BULL; E > 0) ahead or at the DF, whereas it is the opposite (J & BULL; E < 0) behind the front. This reversal is mainly due to a local reversal of the cross-tail current indicating a substructure of the DF. In the fluid frame, we found that the energy is mostly transferred from the plasma to the electromagnetic field (J & BULL; E & PRIME; < 0) and should contribute to the deceleration of the fast flow. However, we show that the energy conversion process is not homogeneous at the electron scales due to electric field fluctuations likely related to lower-hybrid drift waves. Our results suggest that the role of DF in the global energy cycle of the magnetosphere still deserves more investigation. In particular, statistical studies on DF are required to be carried out with caution due to these electron scale substructures.

Published
2022
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26. Publisher Correction: Electron magnetic reconnection without ion coupling in Earth’s turbulent magnetosheath

Author

Phan, T. D., Eastwood, J. P., Shay, M. A., Drake, J. F., Sonnerup, B. U. Ö., Fujimoto, M., Cassak, P. A., Øieroset, M., Burch, J. L., Torbert, R. B., Rager, A. C., Dorelli, J. C., Gershman, D. J., Pollock, C., Pyakurel, P. S., Haggerty, C. C., Khotyaintsev, Y., Lavraud, B., Saito, Y., Oka, M., Ergun, R. E., Retino, A., Le Contel, O., Argall, M. R., Giles, B. L., Moore, T. E., Wilder, F. D., Strangeway, R. J., Russell, C. T., Lindqvist, P. A., and Magnes, W.

Published
2019
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27. Electron Scattering by High-Frequency Whistler Waves at Earth's Bow Shock

Author

Oka, M, Wilson, L. B., III, Phan, T. D, Hull, A. J, Amano, T, Hoshino, M, Argall, M. R, Le Contel, O, Agapitov, O, Gersham, D. J, Khotyaintsev, Y. V, Burch, J. L, Torbert, R. B, Pollock, C, Dorelli, J. C, Giles, B. L, Moore, T. E, Saito, Y, Avanov, L. A, Paterson, W, Ergun, R. E, Strangeway, R. J, Russell, C. T, and Lindqvist, P. A

Subjects
Plasma Physics
Abstract

Electrons are accelerated to non-thermal energies at shocks in space and astrophysical environments. While different mechanisms of electron acceleration have been proposed, it remains unclear how non-thermal electrons are produced out of the thermal plasma pool. Here, we report in situ evidence of pitch-angle scattering of non-thermal electrons by whistler waves at Earths bow shock. On 2015 November 4, the Magnetospheric Multiscale (MMS) mission crossed the bow shock with an Alfvn Mach number is approximately 11 and a shock angle of approximately 84deg. In the ramp and overshoot regions, MMS revealed bursty enhancements of non-thermal (0.52 keV) electron flux, correlated with high-frequency (0.2 - 0.4 Omega(sub ce), where Omega(sub ce) is the cyclotron frequency) parallel-propagating whistler waves. The electron velocity distribution (measured at 30 ms cadence) showed an enhanced gradient of phase-space density at and around the region where the electron velocity component parallel to the magnetic field matched the resonant energy inferred from the wave frequency range. The flux of 0.5 keV electrons (measured at 1ms cadence) showed fluctuations with the same frequency. These features indicate that non-thermal electrons were pitch-angle scattered by cyclotron resonance with the high-frequency whistler waves. However, the precise role of the pitch-angle scattering by the higher-frequency whistler waves and possible nonlinear effects in the electron acceleration process remains unclear.

Published
2017
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29. Identifying the Driver of Pulsating Aurora

Author

Nishimura, Y., Bortnik, J., Li, W., Thorne, R. M., Lyons, L. R., Angelopoulos, V., Mende, S. B., Bonnell, J. W., Le Contel, O., Cully, C., Ergun, R., and Auster, U.

Published
2010

31. Investigation of the homogeneity of energy conversion processes at dipolarization fronts from MMS measurements

Author

Alqeeq, S. W., primary, Le Contel, O., additional, Canu, P., additional, Retinò, A., additional, Chust, T., additional, Mirioni, L., additional, Richard, L., additional, Aït-Si-Ahmed, Y., additional, Alexandrova, A., additional, Chuvatin, A., additional, Ahmadi, N., additional, Baraka, S. M., additional, Nakamura, R., additional, Wilder, F. D., additional, Gershman, D. J., additional, Lindqvist, P. A., additional, Khotyaintsev, Yu. V., additional, Ergun, R. E., additional, Burch, J. L., additional, Torbert, R. B., additional, Russell, C. T., additional, Magnes, W., additional, Strangeway, R. J., additional, Bromund, K. R., additional, Wei, H., additional, Plaschke, F., additional, Anderson, B. J., additional, Giles, B. L., additional, Fuselier, S. A., additional, Saito, Y., additional, and Lavraud, B., additional

Published
2022
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33. Low-frequency Whistler Waves Modulate Electrons and Generate Higher-frequency Whistler Waves in the Solar Wind

Author

Yao, S. T., primary, Shi, Q. Q., additional, Zong, Q. G., additional, Degeling, A. W., additional, Guo, R. L., additional, Li, L., additional, Li, J. X., additional, Tian, A. M., additional, Zhang, H., additional, Yao, Z. H., additional, Fu, H. S., additional, Liu, C. M., additional, Sun, W. J., additional, Niu, Z., additional, Li, W. Y., additional, Liu, Z. Y., additional, Le Contel, O., additional, Zhang, S., additional, Xiao, C., additional, Shang, W. S., additional, Torbert, R. B., additional, Ergun, R. E., additional, Lindqvist, P.-A., additional, and Pollock, C. J., additional

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

Author

Kretzschmar, M., primary, Chust, T., additional, Krasnoselskikh, V., additional, Graham, D., additional, Colomban, L., additional, Maksimovic, M., additional, Khotyaintsev, Yu. V., additional, Soucek, J., additional, Steinvall, K., additional, Santolík, O., additional, Jannet, G., additional, Brochot, J.-Y., additional, Le Contel, O., additional, Vecchio, A., additional, Bonnin, X., additional, Bale, S. D., additional, Froment, C., additional, Larosa, A., additional, Bergerard-Timofeeva, M., additional, Fergeau, P., additional, Lorfevre, E., additional, Plettemeier, D., additional, Steller, M., additional, Štverák, Š., additional, Trávníček, P., additional, Vaivads, A., additional, Horbury, T. S., additional, O’Brien, H., additional, Evans, V., additional, Angelini, V., additional, Owen, C. J., additional, and Louarn, P., additional

Published
2021
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35. Observations of whistler mode waves by Solar Orbiter’s RPW Low Frequency Receiver (LFR): In-flight performance and first results

Author

Chust, T., primary, Kretzschmar, M., additional, Graham, D. B., additional, Le Contel, O., additional, Retinò, A., additional, Alexandrova, A., additional, Berthomier, M., additional, Hadid, L. Z., additional, Sahraoui, F., additional, Jeandet, A., additional, Leroy, P., additional, Pellion, J.-C., additional, Bouzid, V., additional, Katra, B., additional, Piberne, R., additional, Khotyaintsev, Yu. V., additional, Vaivads, A., additional, Krasnoselskikh, V., additional, Souček, J., additional, Santolík, O., additional, Lorfèvre, E., additional, Plettemeier, D., additional, Steller, M., additional, Štverák, Š., additional, Trávníček, P., additional, Vecchio, A., additional, Maksimovic, M., additional, Bale, S. D., additional, Horbury, T. S., additional, O’Brien, H., additional, Evans, V., additional, and Angelini, V., additional

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

Author

Maksimovic, M., primary, Souček, J., additional, Chust, T., additional, Khotyaintsev, Y., additional, Kretzschmar, M., additional, Bonnin, X., additional, Vecchio, A., additional, Alexandrova, O., additional, Bale, S. D., additional, Bérard, D., additional, Brochot, J.-Y., additional, Edberg, N. J. T., additional, Eriksson, A., additional, Hadid, L. Z., additional, Johansson, E. P. G., additional, Karlsson, T., additional, Katra, B., additional, Krasnoselskikh, V., additional, Krupař, V., additional, Lion, S., additional, Lorfèvre, E., additional, Matteini, L., additional, Nguyen, Q. N., additional, Píša, D., additional, Piberne, R., additional, Plettemeier, D., additional, Rucker, H. O., additional, Santolík, O., additional, Steinvall, K., additional, Steller, M., additional, Štverák, Š., additional, Trávníček, P., additional, Vaivads, A., additional, Zaslavsky, A., additional, Chaintreuil, S., additional, Dekkali, M., additional, Astier, P.-A., additional, Barbary, G., additional, Boughedada, K., additional, Cecconi, B., additional, Chapron, F., additional, Collin, C., additional, Dias, D., additional, Guéguen, L., additional, Lamy, L., additional, Leray, V., additional, Malac-Allain, L. R., additional, Pantellini, F., additional, Parisot, J., additional, Plasson, P., additional, Thijs, S., additional, Fratter, I., additional, Bellouard, E., additional, Danto, P., additional, Julien, S., additional, Guilhem, E., additional, Fiachetti, C., additional, Sanisidro, J., additional, Laffaye, C., additional, Gonzalez, F., additional, Pontet, B., additional, Quéruel, N., additional, Jannet, G., additional, Fergeau, P., additional, Dudok de Wit, T., additional, Vincent, T., additional, Agrapart, C., additional, Pragout, J., additional, Bergerard-Timofeeva, M., additional, Delory, G. T., additional, Turin, P., additional, Jeandet, A., additional, Leroy, P., additional, Pellion, J.-C., additional, Bouzid, V., additional, Recart, W., additional, Kolmašová, I., additional, Krupařová, O., additional, Uhlíř, L., additional, Lán, R., additional, Baše, J., additional, André, M., additional, Bylander, L., additional, Cripps, V., additional, Cully, C., additional, Jansson, S.-E., additional, Puccio, W., additional, Břínek, J., additional, Ottacher, H., additional, Angelini, V., additional, Berthomier, M., additional, Evans, V., additional, Goetz, K., additional, Hellinger, P., additional, Horbury, T. S., additional, Issautier, K., additional, Kontar, E., additional, Le Contel, O., additional, Louarn, P., additional, Martinović, M., additional, Müller, D., additional, O’Brien, H., additional, Owen, C. J., additional, Retino, A., additional, Rodríguez-Pacheco, J., additional, Sahraoui, F., additional, Sanchez, L., additional, Walsh, A. P., additional, Wimmer-Schweingruber, R. F., additional, and Zouganelis, I., additional

Published
2021
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37. Solar Orbiter’s first Venus flyby: Observations from the Radio and Plasma Wave instrument

Author

Hadid, L. Z., primary, Edberg, N. J. T., additional, Chust, T., additional, Píša, D., additional, Dimmock, A. P., additional, Morooka, M. W., additional, Maksimovic, M., additional, Khotyaintsev, Yu. V., additional, Souček, J., additional, Kretzschmar, M., additional, Vecchio, A., additional, Le Contel, O., additional, Retino, A., additional, Allen, R. C., additional, Volwerk, M., additional, Fowler, C. M., additional, Sorriso-Valvo, L., additional, Karlsson, T., additional, Santolík, O., additional, Kolmašová, I., additional, Sahraoui, F., additional, Stergiopoulou, K., additional, Moussas, X., additional, Issautier, K., additional, Dewey, R. M., additional, Klein Wolt, M., additional, Malandraki, O. E., additional, Kontar, E. P., additional, Howes, G. G., additional, Bale, S. D., additional, Horbury, T. S., additional, Martinović, M., additional, Vaivads, A., additional, Krasnoselskikh, V., additional, Lorfèvre, E., additional, Plettemeier, D., additional, Steller, M., additional, Štverák, Š., additional, Trávníček, P., additional, O’Brien, H., additional, Evans, V., additional, Angelini, V., additional, Velli, M. C., additional, and Zouganelis, I., additional

Published
2021
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38. Observations of Turbulence in a Kelvin-Helmholtz Event on 8 September 2015 by the Magnetospheric Multiscale Mission

Author

Stawarz, J. E, Eriksson, S, Wilder, F. D, Ergun, R. E, Schwartz, S. J, Pouquet, A, Burch, J. L, Giles, B. L, Khotyaintsev, Y, Le Contel, O, Lindqvist, P.-A, Magnes, W, Pollock, C. J, Russell, C.T, Strangeway, R. J, Torbert, R. B, Avanov, L. A, Dorelli, J. C, Eastwood, J. P, Gershman, D. J, Goodrich, K. A, Malaspina, D. M, Marklund, G. T, Mirioni, L, and Sturner, A. P

Subjects
Solar Physics, Plasma Physics
Abstract

Spatial and high-time-resolution properties of the velocities, magnetic field, and 3-D electric field within plasma turbulence are examined observationally using data from the Magnetospheric Multiscale mission. Observations from a Kelvin-Helmholtz instability (KHI) on the Earth's magnetopause are examined, which both provides a series of repeatable intervals to analyze, giving better statistics, and provides a first look at the properties of turbulence in the KHI. For the first time direct observations of both the high-frequency ion and electron velocity spectra are examined, showing differing ion and electron behavior at kinetic scales. Temporal spectra exhibit power law behavior with changes in slope near the ion gyrofrequency and lower hybrid frequency. The work provides the first observational evidence for turbulent intermittency and anisotropy consistent with quasi two-dimensional turbulence in association with the KHI. The behavior of kinetic-scale intermittency is found to have differences from previous studies of solar wind turbulence, leading to novel insights on the turbulent dynamics in the KHI.

Published
2016
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41. Thin Current Sheet Behind the Dipolarization Front

Author

Nakamura, R., primary, Baumjohann, W., additional, Nakamura, T. K. M., additional, Panov, E. V., additional, Schmid, D., additional, Varsani, A., additional, Apatenkov, S., additional, Sergeev, V. A., additional, Birn, J., additional, Nagai, T., additional, Gabrielse, C., additional, André, M., additional, Burch, J. L., additional, Carr, C., additional, Dandouras, I. S., additional, Escoubet, C. P., additional, Fazakerley, A. N., additional, Giles, B. L., additional, Le Contel, O., additional, Russell, C. T., additional, and Torbert, R. B., additional

Published
2021
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42. The Solar Orbiter Radio and Plasma Waves (RPW) instrument (Corrigendum)

Author

Maksimovic, M., primary, Bale, S. D., additional, Chust, T., additional, Khotyaintsev, Y., additional, Krasnoselskikh, V., additional, Kretzschmar, M., additional, Plettemeier, D., additional, Rucker, H. O., additional, Souček, J., additional, Steller, M., additional, Štverák, Š., additional, Trávníček, P., additional, Vaivads, A., additional, Chaintreuil, S., additional, Dekkali, M., additional, Alexandrova, O., additional, Astier, P.-A., additional, Barbary, G., additional, Bérard, D., additional, Bonnin, X., additional, Boughedada, K., additional, Cecconi, B., additional, Chapron, F., additional, Chariet, M., additional, Collin, C., additional, de Conchy, Y., additional, Dias, D., additional, Guéguen, L., additional, Lamy, L., additional, Leray, V., additional, Lion, S., additional, Malac-Allain, L. R., additional, Matteini, L., additional, Nguyen, Q. N., additional, Pantellini, F., additional, Parisot, J., additional, Plasson, P., additional, Thijs, S., additional, Vecchio, A., additional, Fratter, I., additional, Bellouard, E., additional, Lorfèvre, E., additional, Danto, P., additional, Julien, S., additional, Guilhem, E., additional, Fiachetti, C., additional, Sanisidro, J., additional, Laffaye, C., additional, Gonzalez, F., additional, Pontet, B., additional, Quéruel, N., additional, Jannet, G., additional, Fergeau, P., additional, Brochot, J.-Y., additional, Cassam-Chenai, G., additional, Dudok de Wit, T., additional, Timofeeva, M., additional, Vincent, T., additional, Agrapart, C., additional, Delory, G. T., additional, Turin, P., additional, Jeandet, A., additional, Leroy, P., additional, Pellion, J.-C., additional, Bouzid, V., additional, Katra, B., additional, Piberne, R., additional, Recart, W., additional, Santolík, O., additional, Kolmašová, I., additional, Krupař, V., additional, Krupařová, O., additional, Píša, D., additional, Uhlíř, L., additional, Lán, R., additional, Baše, J., additional, Ahlèn, L., additional, André, M., additional, Bylander, L., additional, Cripps, V., additional, Cully, C., additional, Eriksson, A., additional, Jansson, S.-E., additional, Johansson, E. P. G., additional, Karlsson, T., additional, Puccio, W., additional, Břínek, J., additional, Öttacher, H., additional, Panchenko, M., additional, Berthomier, M., additional, Goetz, K., additional, Hellinger, P., additional, Horbury, T. S., additional, Issautier, K., additional, Kontar, E., additional, Krucker, S., additional, Le Contel, O., additional, Louarn, P., additional, Martinović, M., additional, Owen, C. J., additional, Retino, A., additional, Rodríguez-Pacheco, J., additional, Sahraoui, F., additional, Wimmer-Schweingruber, R. F., additional, Zaslavsky, A., additional, and Zouganelis, I., additional

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

Author

Li, W.‐Y., primary, Khotyaintsev, Yu V., additional, Tang, B.‐B., additional, Graham, D. B., additional, Norgren, C., additional, Vaivads, A., additional, André, M., additional, Le, A., additional, Egedal, J., additional, Dokgo, K., additional, Fujimoto, K., additional, He, J.‐S., additional, Burch, J. L., additional, Lindqvist, P.‐A., additional, Ergun, R. E., additional, Torbert, R. B., additional, Le Contel, O., additional, Gershman, D. J., additional, Giles, B. L., additional, Lavraud, B., additional, Fuselier, S., additional, Plaschke, F., additional, Russell, C. T., additional, Guo, X.‐C., additional, Lu, Q.‐M., additional, and Wang, C., additional

Published
2021
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46. Solar Orbiter's first Venus flyby: Observations from the Radio and Plasma Wave instrument

Author

Hadid, L. Z. Edberg, N. J. T. Chust, T. Pisa, D. and Dimmock, A. P. Morooka, M. W. Maksimovic, M. Khotyaintsev, V, Yu Soucek, J. Kretzschmar, M. Vecchio, A. Le Contel, O. Retino, A. Allen, R. C. Volwerk, M. Fowler, C. M. and Sorriso-Valvo, L. Karlsson, T. Santolik, O. Kolmasova, I and Sahraoui, F. Stergiopoulou, K. Moussas, X. Issautier, K. and Dewey, R. M. Wolt, M. Klein Malandraki, O. E. Kontar, E. P. and Howes, G. G. Bale, S. D. Horbury, T. S. Martinovic, M. and Vaivads, A. Krasnoselskikh, V Lorfevre, E. Plettemeier, D. Steller, M. Stverak, S. Travnicek, P. O'Brien, H. and Evans, V Angelini, V Velli, M. C. Zouganelis, I

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

Context. On December 27, 2020, Solar Orbiter completed its first gravity assist manoeuvre of Venus (VGAM1). While this flyby was performed to provide the spacecraft with sufficient velocity to get closer to the Sun and observe its poles from progressively higher inclinations, the Radio and Plasma Wave (RPW) consortium, along with other operational in situ instruments, had the opportunity to perform high cadence measurements and study the plasma properties in the induced magnetosphere of Venus. Aims. In this paper, we review the main observations of the RPW instrument during VGAM1. They include the identification of a number of magnetospheric plasma wave modes, measurements of the electron number densities computed using the quasi-thermal noise spectroscopy technique and inferred from the probe-to-spacecraft potential, the observation of dust impact signatures, kinetic solitary structures, and localized structures at the bow shock, in addition to the validation of the wave normal analysis on-board from the Low Frequency Receiver. Methods. We used the data products provided by the different subsystems of RPW to study Venus' induced magnetosphere. Results. The results include the observations of various electromagnetic and electrostatic wave modes in the induced magnetosphere of Venus: strong emissions of similar to 100 Hz whistler waves are observed in addition to electrostatic ion acoustic waves, solitary structures and Langmuir waves in the magnetosheath of Venus. Moreover, based on the different levels of the wave amplitudes and the large-scale variations of the electron number densities, we could identify different regions and boundary layers at Venus. Conclusions. The RPW instrument provided unprecedented AC magnetic and electric field measurements in Venus' induced magnetosphere for continuous frequency ranges and with high time resolution. These data allow for the conclusive identification of various plasma waves at higher frequencies than previously observed and a detailed investigation regarding the structure of the induced magnetosphere of Venus. Furthermore, noting that prior studies were mainly focused on the magnetosheath region and could only reach 10-12 Venus radii (R-V) down the tail, the particular orbit geometry of Solar Orbiter's VGAM1, allowed the first investigation of the nature of the plasma waves continuously from the bow shock to the magnetosheath, extending to similar to 70R(V) in the far distant tail region.

Published
2021

47. Whistler waves observed by Solar Orbiter/RPW between 0.5 AU and 1 AU

Author

Kretzschmar, M., Chust, T., Krasnoselskikh, V, Graham, Daniel B., Colomban, L., Maksimovic, M., Khotyaintsev, Yuri V., Soucek, J., Steinvall, Konrad, Santolik, O., Jannet, G., Brochot, J-Y, Le Contel, O., Vecchio, A., Bonnin, X., Bale, S. D., Froment, C., Larosa, A., Bergerard-Timofeeva, M., Fergeau, P., Lorfevre, E., Plettemeier, D., Steller, M., Stverak, S., Travnicek, P., Vaivads, Andris, Horbury, T. S., O'Brien, H., Evans, V, Angelini, V, Owen, C. J., Louarn, P., Kretzschmar, M., Chust, T., Krasnoselskikh, V, Graham, Daniel B., Colomban, L., Maksimovic, M., Khotyaintsev, Yuri V., Soucek, J., Steinvall, Konrad, Santolik, O., Jannet, G., Brochot, J-Y, Le Contel, O., Vecchio, A., Bonnin, X., Bale, S. D., Froment, C., Larosa, A., Bergerard-Timofeeva, M., Fergeau, P., Lorfevre, E., Plettemeier, D., Steller, M., Stverak, S., Travnicek, P., Vaivads, Andris, Horbury, T. S., O'Brien, H., Evans, V, Angelini, V, Owen, C. J., and Louarn, P.

Abstract

Context. Solar wind evolution differs from a simple radial expansion, while wave-particle interactions are assumed to be the major cause for the observed dynamics of the electron distribution function. In particular, whistler waves are thought to inhibit the electron heat flux and ensure the diffusion of the field-aligned energetic electrons (Strahl electrons) to replenish the halo population. Aims. The goal of our study is to detect and characterize the electromagnetic waves that have the capacity to modify the electron distribution functions, with a special focus on whistler waves. Methods. We carried out a detailed analysis of 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 from the Search Coil Magnetometer and electric antenna, both part of the Radio and Plasma Waves (RPW) instrumental suite, we detected the electromagnetic waves with frequencies above 3 Hz and determined the statistical distribution of their amplitudes, frequencies, polarization, and k-vector as a function of distance. Here, we also discuss the relevant instrumental issues regarding the phase between the electric and magnetic measurements as well as the effective length of the electric antenna. Results. An overwhelming majority of the observed waves are right-handed circularly polarized in the solar wind frame and identified as outwardly propagating quasi-parallel whistler waves. Their occurrence rate increases by a least a factor of 2 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 a smaller normalized frequency (f/f(ce)), larger amplitude, and greater bandwidth than at 1 AU.

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

Author

Maksimovic, M., Soucek, J., Chust, T., Khotyaintsev, Yuri V., Kretzschmar, M., Bonnin, X., Vecchio, A., Alexandrova, O., Bale, S. D., Berard, D., Brochot, J-Y, Edberg, Niklas J. T., Eriksson, Anders, Hadid, L. Z., Johansson, Erik P. G., Karlsson, T., Katra, B., Krasnoselskikh, V, Krupar, V, Lion, S., Lorfevre, E., Matteini, L., Nguyen, Q. N., Pisa, D., Piberne, R., Plettemeier, D., Rucker, H. O., Santolik, O., Steinvall, Konrad, Steller, M., Stverak, S., Travnicek, P., Vaivads, Andris, Zaslavsky, A., Chaintreuil, S., Dekkali, M., Astier, P-A, Barbary, G., Boughedada, K., Cecconi, B., Chapron, F., Collin, C., Dias, D., Gueguen, L., Lamy, L., Leray, V, Malac-Allain, L. R., Pantellini, F., Parisot, J., Plasson, P., Thijs, S., Fratter, I, Bellouard, E., Danto, P., Julien, S., Guilhem, E., Fiachetti, C., Sanisidro, J., Laffaye, C., Gonzalez, F., Pontet, B., Queruel, N., Jannet, G., Fergeau, P., de Wit, T. Dudok, Vincent, T., Agrapart, C., Pragout, J., Bergerard-Timofeeva, M., Delory, G. T., Turin, P., Jeandet, A., Leroy, P., Pellion, J-C, Bouzid, V, Recart, W., Kolmasova, I, Kruparova, O., Uhlir, L., Lan, R., Base, J., André, Mats, Bylander, L., Cripps, Victoria, Cully, C., Jansson, S-E, Puccio, Walter, Brinek, J., Ottacher, H., Angelini, V, Berthomier, M., Evans, V, Goetz, K., Hellinger, P., Horbury, T. S., Issautier, K., Kontar, E., Le Contel, O., Louarn, P., Martinovic, M., Mueller, D., O'Brien, H., Owen, C. J., Retino, A., Rodriguez-Pacheco, J., Sahraoui, F., Sanchez, L., Walsh, A. P., Wimmer-Schweingruber, R. F., Zouganelis, I, Maksimovic, M., Soucek, J., Chust, T., Khotyaintsev, Yuri V., Kretzschmar, M., Bonnin, X., Vecchio, A., Alexandrova, O., Bale, S. D., Berard, D., Brochot, J-Y, Edberg, Niklas J. T., Eriksson, Anders, Hadid, L. Z., Johansson, Erik P. G., Karlsson, T., Katra, B., Krasnoselskikh, V, Krupar, V, Lion, S., Lorfevre, E., Matteini, L., Nguyen, Q. N., Pisa, D., Piberne, R., Plettemeier, D., Rucker, H. O., Santolik, O., Steinvall, Konrad, Steller, M., Stverak, S., Travnicek, P., Vaivads, Andris, Zaslavsky, A., Chaintreuil, S., Dekkali, M., Astier, P-A, Barbary, G., Boughedada, K., Cecconi, B., Chapron, F., Collin, C., Dias, D., Gueguen, L., Lamy, L., Leray, V, Malac-Allain, L. R., Pantellini, F., Parisot, J., Plasson, P., Thijs, S., Fratter, I, Bellouard, E., Danto, P., Julien, S., Guilhem, E., Fiachetti, C., Sanisidro, J., Laffaye, C., Gonzalez, F., Pontet, B., Queruel, N., Jannet, G., Fergeau, P., de Wit, T. Dudok, Vincent, T., Agrapart, C., Pragout, J., Bergerard-Timofeeva, M., Delory, G. T., Turin, P., Jeandet, A., Leroy, P., Pellion, J-C, Bouzid, V, Recart, W., Kolmasova, I, Kruparova, O., Uhlir, L., Lan, R., Base, J., André, Mats, Bylander, L., Cripps, Victoria, Cully, C., Jansson, S-E, Puccio, Walter, Brinek, J., Ottacher, H., Angelini, V, Berthomier, M., Evans, V, Goetz, K., Hellinger, P., Horbury, T. S., Issautier, K., Kontar, E., Le Contel, O., Louarn, P., Martinovic, M., Mueller, D., O'Brien, H., Owen, C. J., Retino, A., Rodriguez-Pacheco, J., Sahraoui, F., Sanchez, L., Walsh, A. P., Wimmer-Schweingruber, R. F., and Zouganelis, I

Abstract

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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49. Observations of whistler mode waves by Solar Orbiter's RPW Low Frequency Receiver (LFR) : In-flight performance and first results

Author

Chust, T., Kretzschmar, M., Graham, Daniel B., Le Contel, O., Retino, A., Alexandrova, A., Berthomier, M., Hadid, L. Z., Sahraoui, F., Jeandet, A., Leroy, P., Pellion, J-C, Bouzid, V, Katra, B., Piberne, R., Khotyaintsev, Yuri V., Vaivads, Andris, Krasnoselskikh, V, Soucek, J., Santolik, O., Lorfevre, E., Plettemeier, D., Steller, M., Stverak, S., Vecchio, A., Maksimovic, M., Bale, S. D., Horbury, T. S., O'Brien, H., Evans, V, Angelini, V, Chust, T., Kretzschmar, M., Graham, Daniel B., Le Contel, O., Retino, A., Alexandrova, A., Berthomier, M., Hadid, L. Z., Sahraoui, F., Jeandet, A., Leroy, P., Pellion, J-C, Bouzid, V, Katra, B., Piberne, R., Khotyaintsev, Yuri V., Vaivads, Andris, Krasnoselskikh, V, Soucek, J., Santolik, O., Lorfevre, E., Plettemeier, D., Steller, M., Stverak, S., Vecchio, A., Maksimovic, M., Bale, S. D., Horbury, T. S., O'Brien, H., Evans, V, and Angelini, V

Abstract

Context. The Radio and Plasma Waves (RPW) instrument is one of the four in situ instruments of the ESA/NASA Solar Orbiter mission, which was successfully launched on February 10, 2020. The Low Frequency Receiver (LFR) is one of its subsystems, designed to characterize the low frequency electric (quasi-DC - 10 kHz) and magnetic (similar to 1 Hz-10 kHz) fields that develop, propagate, interact, and dissipate in the solar wind plasma. Combined with observations of the particles and the DC magnetic field, LFR measurements will help to improve the understanding of the heating and acceleration processes at work during solar wind expansion. Aims. The capability of LFR to observe and analyze a variety of low frequency plasma waves can be demontrated by taking advantage of whistler mode wave observations made just after the near-Earth commissioning phase of Solar Orbiter. In particular, this is related to its capability of measuring the wave normal vector, the phase velocity, and the Poynting vector for determining the propagation characteristics of the waves. Methods. Several case studies of whistler mode waves are presented, using all possible LFR onboard digital processing products, waveforms, spectral matrices, and basic wave parameters. Results. Here, we show that whistler mode waves can be very properly identified and characterized, along with their Doppler-shifted frequency, based on the waveform capture as well as on the LFR onboard spectral analysis. Conclusions. Despite the fact that calibrations of the electric and magnetic data still require some improvement, these first whistler observations show a good overall consistency between the RPW LFR data, indicating that many science results on these waves, as well as on other plasma waves, can be obtained by Solar Orbiter in the solar wind.

Published
2021
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50. Solar Orbiter's first Venus flyby : Observations from the Radio and Plasma Wave instrument

Author

Hadid, L. Z., Edberg, Niklas J. T., Chust, T., Pisa, D., Dimmock, Andrew P., Morooka, Michiko, Maksimovic, M., Khotyaintsev, Yuri V., Soucek, J., Kretzschmar, M., Vecchio, A., Le Contel, O., Retino, A., Allen, R. C., Volwerk, M., Fowler, C. M., Sorriso-Valvo, Luca, Karlsson, T., Santolik, O., Kolmasova, I, Sahraoui, F., Stergiopoulou, Katerina, Moussas, X., Issautier, K., Dewey, R. M., Wolt, M. Klein, Malandraki, O. E., Kontar, E. P., Howes, G. G., Bale, S. D., Horbury, T. S., Martinovic, M., Vaivads, Andris, Krasnoselskikh, V, Lorfevre, E., Plettemeier, D., Steller, M., Stverak, S., Travnicek, P., O'Brien, H., Evans, V, Angelini, V, Velli, M. C., Zouganelis, I, Hadid, L. Z., Edberg, Niklas J. T., Chust, T., Pisa, D., Dimmock, Andrew P., Morooka, Michiko, Maksimovic, M., Khotyaintsev, Yuri V., Soucek, J., Kretzschmar, M., Vecchio, A., Le Contel, O., Retino, A., Allen, R. C., Volwerk, M., Fowler, C. M., Sorriso-Valvo, Luca, Karlsson, T., Santolik, O., Kolmasova, I, Sahraoui, F., Stergiopoulou, Katerina, Moussas, X., Issautier, K., Dewey, R. M., Wolt, M. Klein, Malandraki, O. E., Kontar, E. P., Howes, G. G., Bale, S. D., Horbury, T. S., Martinovic, M., Vaivads, Andris, Krasnoselskikh, V, Lorfevre, E., Plettemeier, D., Steller, M., Stverak, S., Travnicek, P., O'Brien, H., Evans, V, Angelini, V, Velli, M. C., and Zouganelis, I

Abstract

Context. On December 27, 2020, Solar Orbiter completed its first gravity assist manoeuvre of Venus (VGAM1). While this flyby was performed to provide the spacecraft with sufficient velocity to get closer to the Sun and observe its poles from progressively higher inclinations, the Radio and Plasma Wave (RPW) consortium, along with other operational in situ instruments, had the opportunity to perform high cadence measurements and study the plasma properties in the induced magnetosphere of Venus. Aims. In this paper, we review the main observations of the RPW instrument during VGAM1. They include the identification of a number of magnetospheric plasma wave modes, measurements of the electron number densities computed using the quasi-thermal noise spectroscopy technique and inferred from the probe-to-spacecraft potential, the observation of dust impact signatures, kinetic solitary structures, and localized structures at the bow shock, in addition to the validation of the wave normal analysis on-board from the Low Frequency Receiver. Methods. We used the data products provided by the different subsystems of RPW to study Venus' induced magnetosphere. Results. The results include the observations of various electromagnetic and electrostatic wave modes in the induced magnetosphere of Venus: strong emissions of similar to 100 Hz whistler waves are observed in addition to electrostatic ion acoustic waves, solitary structures and Langmuir waves in the magnetosheath of Venus. Moreover, based on the different levels of the wave amplitudes and the large-scale variations of the electron number densities, we could identify different regions and boundary layers at Venus. Conclusions. The RPW instrument provided unprecedented AC magnetic and electric field measurements in Venus' induced magnetosphere for continuous frequency ranges and with high time resolution. These data allow for the conclusive identification of various plasma waves at higher frequencies than previously observed a

Published
2021
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