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dc.contributor.authorPezzini, L.
dc.contributor.authorZhukov, A.N.
dc.contributor.authorBacchini, F.
dc.contributor.authorArrò, G.
dc.contributor.authorLópez, R.A.
dc.contributor.authorMicera, A.
dc.contributor.authorInnocenti, M.E.
dc.contributor.authorLapenta, G.
dc.date2024
dc.date.accessioned2025-04-18T09:31:28Z
dc.date.available2025-04-18T09:31:28Z
dc.identifier.urihttps://orfeo.belnet.be/handle/internal/14025
dc.descriptionThe expanding solar wind plasma ubiquitously exhibits anisotropic nonthermal particle velocity distributions. Typically, proton velocity distribution functions (VDFs) show the presence of a core and a field-aligned beam. Novel observations made by the Parker Solar Probe (PSP) in the innermost heliosphere have revealed new complex features in the proton VDFs, namely anisotropic beams that sometimes experience perpendicular diffusion. In this study, we use a 2.5D fully kinetic simulation to investigate the stability of proton VDFs with anisotropic beams observed by PSP. Our setup consists of a core and an anisotropic beam population that drift with respect to each other. This configuration triggers a proton beam instability from which nearly parallel fast magnetosonic modes develop. Our results demonstrate that before this instability reaches saturation, the waves resonantly interact with the beam protons, causing perpendicular heating at the expense of the parallel temperature.
dc.languageeng
dc.titleFully Kinetic Simulations of Proton-beam-driven Instabilities from Parker Solar Probe Observations
dc.typeArticle
dc.subject.frascatiPhysical sciences
dc.audienceScientific
dc.source.titleAstrophysical Journal
dc.source.volume975
dc.source.issue1
dc.source.pageA37
Orfeo.peerreviewedYes
dc.identifier.doi10.3847/1538-4357/ad7465
dc.identifier.url


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