Evolution of the Electron Distribution Function in the Whistler Wave Turbulence of the Solar Wind

dc.contributor.author	Pierrard, V.
dc.contributor.author	Lazar, M.
dc.contributor.author	Schlickeiser, R.
dc.date	2011
dc.date.accessioned	2016-03-29T12:43:52Z
dc.date.available	2016-03-29T12:43:52Z
dc.identifier.uri	https://orfeo.belnet.be/handle/internal/3114
dc.description	The electron distribution functions from the solar corona to the solar wind are determined in this paper by considering the effects of the external forces, of Coulomb collisions and of the wave - particle resonant interactions in the plasma wave turbulence. The electrons are assumed to be interacting with right-handed polarized waves in the whistler regime. The acceleration of electrons in the solar wind seems to be mainly due to the electrostatic potential. Wave turbulence determines the electron pitch-angle diffusion and some characteristics of the velocity distribution function (VDF) such as suprathermal tails. The role of parallel whistlers can also be extended to small altitudes in the solar wind (the acceleration region of the outer corona), where they may explain the energization and the presence of suprathermal electrons.
dc.language	eng
dc.title	Evolution of the Electron Distribution Function in the Whistler Wave Turbulence of the Solar Wind
dc.type	Article
dc.subject.frascati	Physical sciences
dc.audience	Scientific
dc.source.title	Solar Physics
dc.source.volume	269
dc.source.issue	2
dc.source.page	421-438
Orfeo.peerreviewed	Yes
dc.identifier.doi	10.1007/s11207-010-9700-7
dc.identifier.scopus	2-s2.0-79952696710