On the exospheric approach for the solar wind acceleration

dc.contributor.author	Maksimovic, M.
dc.contributor.author	Pierrard, V.
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/5248
dc.description	We present the basics of the exospheric models of the solar wind acceleration. In these models the plasma is assumed fully collisionless above a typical altitude in the corona. The solar wind is accelerated by the interplanetary electrostatic potential which is needed to warrant the equality of the proton and electron fluxes. These models suggest that the fast wind emanating from the polar regions could be due to the presence of non-thermal electron distributions in the corona.
dc.language	eng
dc.title	On the exospheric approach for the solar wind acceleration
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	181-187
Orfeo.peerreviewed	Yes
dc.identifier.doi	10.1023/A:1012250027289
dc.identifier.scopus	2-s2.0-0035600533