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Theoretical plasma distributions consistent with ulysses magnetic field observations in a solar wind tangential discontinuity

dc.contributor.authorDe Keyser, J.
dc.contributor.authorRoth, M.
dc.contributor.authorLemaire, J.
dc.contributor.authorTsurutani, B.T.
dc.contributor.authorHo, C.M.
dc.contributor.authorHammond, C.M.
dc.date1996
dc.date.accessioned2017-05-23T12:08:33Z
dc.date.available2017-05-23T12:08:33Z
dc.identifier.urihttps://orfeo.belnet.be/handle/internal/5550
dc.descriptionThe overall multi-layer structure of the magnetic field profile observed by Ulysses across a broad solar wind tangential discontinuity can be reproduced fairly well by means of a kinetic model. Such a simulation provides complementary information about the velocity distribution functions, which are not always available from the plasma experiment due to the low time resolution inherent in plasma measurements. The success of such a simulation proves that the kinetic model can be used as a realistic basis for further studies of the structure and stability of solar wind tangential discontinuities.
dc.languageeng
dc.titleTheoretical plasma distributions consistent with ulysses magnetic field observations in a solar wind tangential discontinuity
dc.typeArticle
dc.subject.frascatiPhysical sciences
dc.audienceScientific
dc.source.titleSolar Physics
dc.source.volume166
dc.source.issue2
dc.source.page415-422
Orfeo.peerreviewedYes
dc.identifier.doi10.1007/BF00149407
dc.identifier.scopus2-s2.0-21344473074


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