Toward a 3D Kinetic Model of the Solar Wind

dc.contributor.author	Pierard, V.
dc.contributor.author	Pieters, M.
dc.date	2014
dc.date.accessioned	2016-03-25T09:42:11Z
dc.date.available	2016-03-25T09:42:11Z
dc.identifier.isbn	9781583818527
dc.identifier.uri	https://orfeo.belnet.be/handle/internal/2868
dc.description	The kinetic approach is used to develop a three-dimensional model of the solar wind. As a first approximation, we consider an exospheric model taking into account the effects of the external forces (gravitational and electromagnetic) in a magnetic field decreasing as r-2 where r is the radial distance. The rotation of the Sun deforms the solar streams into the Parker's spiral shape. Using typical solar observations in the solar corona or at 1 AU as boundary conditions, we determine the solar wind characteristics in the meridian and the ecliptic plane from the solar corona to larger distances.
dc.language	eng
dc.title	Toward a 3D Kinetic Model of the Solar Wind
dc.type	Conference
dc.subject.frascati	Physical sciences
dc.audience	Scientific
dc.source.title	Astronomical Society of the Pacific Conference Series
dc.source.volume	484
dc.source.page	168
Orfeo.peerreviewed	No