Core, Halo and Strahl Electrons in the Solar Wind

dc.contributor.author	Pierrard, V.
dc.contributor.author	Maksimovic, M.
dc.contributor.author	Lemaire, J.
dc.date	2001
dc.date.accessioned	2017-05-04T09:17:18Z
dc.date.available	2017-05-04T09:17:18Z
dc.identifier.uri	https://orfeo.belnet.be/handle/internal/5245
dc.description	Electron velocity distribution functions (VDF) observed in the low speed solar wind How are generally characterized by 'core' and 'halo' electrons. In the high speed solar wind, a third population of 'strahl' electrons is generally observed. New collisional models based on the solution of the Fokker-Planck equation can he used to determine the importance of the different electron populations as a function of the radial distance. Typical electron velocity distribution functions observed at I AU from the Sun are used as boundary conditions for the high speed solar wind and for the low speed solar wind. Taking into account the effects of external forces and Coulomb collisions with a background plasma, suprathermal tails are found to be present in the electron VDF at low altitudes in the corona when they exist at large radial distances.
dc.language	eng
dc.title	Core, Halo and Strahl Electrons in the Solar Wind
dc.type	Article
dc.subject.frascati	Physical sciences
dc.audience	Scientific
dc.source.title	Astrophysics and Space Science
dc.source.volume	277
dc.source.issue	1-2
dc.source.page	195-200
Orfeo.peerreviewed	Yes
dc.identifier.doi	10.1023/A:1012218600882
dc.identifier.scopus	2-s2.0-0035642826