Fitting of hydrodynamic and kinetic solar wind models

dc.contributor.author	Brasseur, G.
dc.contributor.author	Lemaire, J.
dc.date	1977
dc.date.accessioned	2017-09-05T10:19:17Z
dc.date.available	2017-09-05T10:19:17Z
dc.identifier.uri	https://orfeo.belnet.be/handle/internal/6142
dc.description	In isothermal models of the expanding solar corona there exists in general an exobase level where the collision mean free path becomes equal to the density scale height. At this level the hydrodynamic approximations of the transport equations fail to be justified and a kinetic approach is more appropriate. This exobase is located below the altitude of the critical point proper to the hydrodynamic solutions. The bulk velocity at the exobase is subsonic and smaller than the expansion velocity at the critical point. Therefore the transition to a supersonic solar wind velocity occurs in the collisionless ion-exosphere.
dc.language	eng
dc.title	Fitting of hydrodynamic and kinetic solar wind models
dc.type	Article
dc.subject.frascati	Physical sciences
dc.audience	Scientific
dc.source.title	Planetary and Space Science
dc.source.volume	25
dc.source.issue	2
dc.source.page	201-203
Orfeo.peerreviewed	Yes
dc.identifier.doi	10.1016/0032-0633(77)90028-9
dc.identifier.scopus	2-s2.0-0007009037