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Proton Temperature Anisotropies in the Plasma Environment of Venus
Swedish Inst Space Phys, Kiruna, Sweden;Lulea Tekniska Univ, Kiruna, Sweden;Univ Lancaster, Phys, Lancaster, England.
Swedish Inst Space Phys, Kiruna, Sweden.
Uppsala University, Disciplinary Domain of Science and Technology, Physics, Swedish Institute of Space Physics, Uppsala Division.ORCID iD: 0000-0003-3725-4920
Swedish Inst Space Phys, Kiruna, Sweden.
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2019 (English)In: Journal of Geophysical Research - Space Physics, ISSN 2169-9380, E-ISSN 2169-9402, Vol. 124, no 5, p. 3312-3330Article in journal (Refereed) Published
Abstract [en]

Velocity distribution functions (VDFs) are a key to understanding the interplay between particles and waves in a plasma. Any deviation from an isotropic Maxwellian distribution may be unstable and result in wave generation. Using data from the ion mass spectrometer IMA (Ion Mass Analyzer) and the magnetometer (MAG) onboard Venus Express, we study proton distributions in the plasma environment of Venus. We focus on the temperature anisotropy, that is, the ratio between the proton temperature perpendicular (T-perpendicular to) and parallel (T-parallel to) to the background magnetic field. We calculate average values of T-perpendicular to and T-parallel to for different spatial areas around Venus. In addition we present spatial maps of the average of the two temperatures and of their average ratio. Our results show that the proton distributions in the solar wind are quite isotropic, while at the bow shock stronger perpendicular than parallel heating makes the downstream VDFs slightly anisotropic (T-perpendicular to/T-parallel to > 1) and possibly unstable to generation of proton cyclotron waves or mirror mode waves. Both wave modes have previously been observed in Venus's magnetosheath. The perpendicular heating is strongest in the near-subsolar magnetosheath (T-perpendicular to/ T-parallel to approximate to 3/2), which is also where mirror mode waves are most frequently observed. We believe that the mirror mode waves observed here are indeed generated by the anisotropy. In the magnetotail we observe planetary protons with largely isotropic VDFs, originating from Venus's ionosphere.

Place, publisher, year, edition, pages
American Geophysical Union (AGU), 2019. Vol. 124, no 5, p. 3312-3330
National Category
Geophysics
Identifiers
URN: urn:nbn:se:uu:diva-389832DOI: 10.1029/2019JA026619ISI: 000471601500011OAI: oai:DiVA.org:uu-389832DiVA, id: diva2:1339348
Funder
Swedish National Space Board, 96/15Available from: 2019-07-29 Created: 2019-07-29 Last updated: 2019-07-29Bibliographically approved

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