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dc.contributor.authorPierard, V.
dc.contributor.authorPieters, M.
dc.date2014
dc.date.accessioned2016-03-25T09:42:11Z
dc.date.available2016-03-25T09:42:11Z
dc.identifier.isbn9781583818527
dc.identifier.urihttps://orfeo.belnet.be/handle/internal/2868
dc.descriptionThe 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.languageeng
dc.titleToward a 3D Kinetic Model of the Solar Wind
dc.typeConference
dc.subject.frascatiPhysical sciences
dc.audienceScientific
dc.source.titleAstronomical Society of the Pacific Conference Series
dc.source.volume484
dc.source.page168
Orfeo.peerreviewedNo


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