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Spatial distribution of plasma density and magnetic field amplitude in the dayside magnetosheath as a function of the IMF orientation

hal.structure.identifierLaboratoire de Physique des Plasmas [LPP]
dc.contributor.authorMICHOTTE DE WELLE, Bayane
hal.structure.identifierLaboratoire de Physique des Plasmas [LPP]
dc.contributor.authorAUNAI, Nicolas
hal.structure.identifierLaboratoire d'Astrophysique de Bordeaux [Pessac] [LAB]
dc.contributor.authorLAVRAUD, Benoit
hal.structure.identifierInstitut de recherche en astrophysique et planétologie [IRAP]
dc.contributor.authorGÉNOT, Vincent
hal.structure.identifierLaboratoire de Physique des Plasmas [LPP]
dc.contributor.authorJEANDET, Alexis
hal.structure.identifierDPHY, ONERA, Université de Toulouse [Toulouse]
dc.contributor.authorNGUYEN, Gautier
hal.structure.identifierLaboratoire de Physique des Plasmas [LPP]
dc.contributor.authorGHISALBERTI, Ambre
hal.structure.identifierLaboratoire de Physique des Plasmas [LPP]
dc.contributor.authorSMETS, Roch
dc.date.issued2024-08-05
dc.identifier.issn2296-987X
dc.description.abstractEnThe properties of the magnetosheath are of pivotal importance in determining the coupling between the magnetosphere and interplanetary medium. In particular, the magnetic flux pileup and plasma depletion layer (PDL) modify the boundary conditions of magnetopause reconnection. However, the spatial distribution of the magnetic field strength and plasma density in the magnetosheath and their functional dependence on the interplanetary magnetic field (IMF) orientation remain poorly understood. This study characterizes these aspects in detail through the statistical processing of decades of data from Cluster, Double Star, THEMIS, and Magnetospheric Multiscale (MMS) missions. The first part of this study focuses on the poorly known variations across the magnetosheath, from the shock to the magnetopause. The magnetic pileup and PDL are significantly correlated, with a strong dependence on the IMF cone angle. Their dependence on the IMF clock angle is found only near the magnetopause, consistent with the expected effect of magnetic reconnection. The second part of this study examines the asymmetry in the magnetic field amplitude and density between the quasi-parallel and quasi-perpendicular sides of the equatorial magnetosheath. These asymmetries are characterized for different relative distances to the magnetopause and bow shock boundaries and for different IMF orientation. The magnetic field amplitude, observed to be higher on the quasi-perpendicular side of the magnetosheath, becomes more symmetric as it approaches the magnetopause. The quasi-parallel magnetosheath exhibits a higher plasma density near the magnetopause. However, this asymmetry reverses at approximately the mid-magnetosheath with a decreasing IMF cone angle.
dc.description.sponsorshipPlasma Science and Training - ANR-18-EURE-0014
dc.language.isoen
dc.publisherFrontiers Media
dc.rights.urihttp://creativecommons.org/licenses/by/
dc.subject.enmagnetosheath
dc.subject.enmagnetic pileup
dc.subject.enplasma depletion layer
dc.subject.enasymmetry
dc.subject.enplasma density
dc.subject.enmagnetic field amplitude
dc.subject.enmagnetopause
dc.title.enSpatial distribution of plasma density and magnetic field amplitude in the dayside magnetosheath as a function of the IMF orientation
dc.typeArticle de revue
dc.identifier.doi10.3389/fspas.2024.1427791
dc.subject.halPhysique [physics]
dc.subject.halSciences de l'ingénieur [physics]
bordeaux.journalFrontiers in Astronomy and Space Sciences
bordeaux.volume11
bordeaux.peerReviewedoui
hal.identifierhal-04736104
hal.version1
hal.popularnon
hal.audienceInternationale
hal.origin.linkhttps://hal.archives-ouvertes.fr//hal-04736104v1
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