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Whistler wave occurrence and the interaction with strahl electrons during the first encounter of Parker Solar Probe

Aims. We studied the properties and occurrence of narrowband whistler waves and their interaction with strahl electrons observed between 0.17 and 0.26 au during the first encounter of Parker Solar Probe. Methods. We used Digital Fields Board band-pass filtered (BPF) data from FIELDS to detect the si...

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Published in:Astronomy and astrophysics (Berlin) 2021-06, Vol.650, p.A9
Main Authors: Jagarlamudi, V. K., Dudok de Wit, T., Froment, C., Krasnoselskikh, V., Larosa, A., Bercic, L., Agapitov, O., Halekas, J. S., Kretzschmar, M., Malaspina, D., Moncuquet, M., Bale, S. D., Case, A. W., Kasper, J. C., Korreck, K. E., Larson, D. E., Pulupa, M., Stevens, M. L., Whittlesey, P.
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cited_by cdi_FETCH-LOGICAL-c356t-e37886a91814b45d4b7d546ce0ec3aed1c774e04536bca1e466491c324031dc33
cites cdi_FETCH-LOGICAL-c356t-e37886a91814b45d4b7d546ce0ec3aed1c774e04536bca1e466491c324031dc33
container_end_page
container_issue
container_start_page A9
container_title Astronomy and astrophysics (Berlin)
container_volume 650
creator Jagarlamudi, V. K.
Dudok de Wit, T.
Froment, C.
Krasnoselskikh, V.
Larosa, A.
Bercic, L.
Agapitov, O.
Halekas, J. S.
Kretzschmar, M.
Malaspina, D.
Moncuquet, M.
Bale, S. D.
Case, A. W.
Kasper, J. C.
Korreck, K. E.
Larson, D. E.
Pulupa, M.
Stevens, M. L.
Whittlesey, P.
description Aims. We studied the properties and occurrence of narrowband whistler waves and their interaction with strahl electrons observed between 0.17 and 0.26 au during the first encounter of Parker Solar Probe. Methods. We used Digital Fields Board band-pass filtered (BPF) data from FIELDS to detect the signatures of whistler waves. Additionally parameters derived from the particle distribution functions measured by the Solar Wind Electrons Alphas and Protons (SWEAP) instrument suite were used to investigate the plasma properties, and FIELDS suite measurements were used to investigate the electromagnetic (EM) fields properties corresponding to the observed whistler signatures. Results. We observe that the occurrence of whistler waves is low, nearly ~1.5% and less than 0.5% in the analyzed peak and average BPF data, respectively. Whistlers occur highly intermittently and 80% of the whistlers appear continuously for less than 3 s. The spacecraft frequencies of the analyzed waves are less than 0.2 electron cyclotron frequency ( f ce ). The occurrence rate of whistler waves was found to be anticorrelated with the solar wind bulk velocity. The study of the duration of the whistler intervals revealed an anticorrelation between the duration and the solar wind velocity, as well as between the duration and the normalized amplitude of magnetic field variations. The pitch-angle widths (PAWs) of the field-aligned electron population referred to as the strahl are broader by at least 12 degrees during the presence of large amplitude narrowband whistler waves. This observation points toward an EM wave electron interaction, resulting in pitch-angle scattering. PAWs of strahl electrons corresponding to the short duration whistlers are higher compared to the long duration whistlers, indicating short duration whistlers scatter the strahl electrons better than the long duration ones. Parallel cuts through the strahl electron velocity distribution function (VDF) observed during the whistler intervals appear to depart from the Maxwellian shape typically found in the near-Sun strahl VDFs. The relative decrease in the parallel electron temperature and the increase in PAW for the electrons in the strahl energy range suggests that the interaction with whistler waves results in a transfer of electron momentum from the parallel to the perpendicular direction.
doi_str_mv 10.1051/0004-6361/202039808
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Additionally parameters derived from the particle distribution functions measured by the Solar Wind Electrons Alphas and Protons (SWEAP) instrument suite were used to investigate the plasma properties, and FIELDS suite measurements were used to investigate the electromagnetic (EM) fields properties corresponding to the observed whistler signatures. Results. We observe that the occurrence of whistler waves is low, nearly ~1.5% and less than 0.5% in the analyzed peak and average BPF data, respectively. Whistlers occur highly intermittently and 80% of the whistlers appear continuously for less than 3 s. The spacecraft frequencies of the analyzed waves are less than 0.2 electron cyclotron frequency ( f ce ). The occurrence rate of whistler waves was found to be anticorrelated with the solar wind bulk velocity. 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L.</creatorcontrib><creatorcontrib>Whittlesey, P.</creatorcontrib><title>Whistler wave occurrence and the interaction with strahl electrons during the first encounter of Parker Solar Probe</title><title>Astronomy and astrophysics (Berlin)</title><description>Aims. We studied the properties and occurrence of narrowband whistler waves and their interaction with strahl electrons observed between 0.17 and 0.26 au during the first encounter of Parker Solar Probe. Methods. We used Digital Fields Board band-pass filtered (BPF) data from FIELDS to detect the signatures of whistler waves. Additionally parameters derived from the particle distribution functions measured by the Solar Wind Electrons Alphas and Protons (SWEAP) instrument suite were used to investigate the plasma properties, and FIELDS suite measurements were used to investigate the electromagnetic (EM) fields properties corresponding to the observed whistler signatures. Results. 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Additionally parameters derived from the particle distribution functions measured by the Solar Wind Electrons Alphas and Protons (SWEAP) instrument suite were used to investigate the plasma properties, and FIELDS suite measurements were used to investigate the electromagnetic (EM) fields properties corresponding to the observed whistler signatures. Results. We observe that the occurrence of whistler waves is low, nearly ~1.5% and less than 0.5% in the analyzed peak and average BPF data, respectively. Whistlers occur highly intermittently and 80% of the whistlers appear continuously for less than 3 s. The spacecraft frequencies of the analyzed waves are less than 0.2 electron cyclotron frequency ( f ce ). The occurrence rate of whistler waves was found to be anticorrelated with the solar wind bulk velocity. The study of the duration of the whistler intervals revealed an anticorrelation between the duration and the solar wind velocity, as well as between the duration and the normalized amplitude of magnetic field variations. The pitch-angle widths (PAWs) of the field-aligned electron population referred to as the strahl are broader by at least 12 degrees during the presence of large amplitude narrowband whistler waves. This observation points toward an EM wave electron interaction, resulting in pitch-angle scattering. PAWs of strahl electrons corresponding to the short duration whistlers are higher compared to the long duration whistlers, indicating short duration whistlers scatter the strahl electrons better than the long duration ones. Parallel cuts through the strahl electron velocity distribution function (VDF) observed during the whistler intervals appear to depart from the Maxwellian shape typically found in the near-Sun strahl VDFs. 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identifier ISSN: 0004-6361
ispartof Astronomy and astrophysics (Berlin), 2021-06, Vol.650, p.A9
issn 0004-6361
1432-0746
1432-0756
language eng
recordid cdi_hal_primary_oai_HAL_hal_03265977v1
source EZB Electronic Journals Library
subjects Amplitudes
Astrophysics
Cyclotron frequency
Cyclotrons
Distribution functions
Electron energy
Electron velocity distribution
Intervals
Narrowband
Physics
Pitch
Pitch (inclination)
Sciences of the Universe
Signatures
Solar probes
Solar wind
Solar wind velocity
Space Physics
Whistlers
Wind speed
title Whistler wave occurrence and the interaction with strahl electrons during the first encounter of Parker Solar Probe
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