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Dependence of Martian magnetopause shape and its dimensions on solar wind dynamic pressure according to Phobos-2 data

dc.contributor.authorVerigin, M.
dc.contributor.authorApáthy, I.
dc.contributor.authorKotova, G.
dc.contributor.authorLemaire, J.
dc.contributor.authorRemizov, A.
dc.contributor.authorRosenbauer, H.
dc.contributor.authorSzegö, K.
dc.contributor.authorSlavin, J.
dc.contributor.authorTatrallyay, M.
dc.contributor.authorSchwingenschuh, K.
dc.contributor.authorShutte, N.
dc.date1996
dc.date.accessioned2017-05-23T10:35:52Z
dc.date.available2017-05-23T10:35:52Z
dc.identifier.urihttps://orfeo.belnet.be/handle/internal/5526
dc.descriptionA semi-empirical model of the Martian magnetopause was developed according to data from the TAUS ion-spectrometer and the MAGMA magnetometer of the Phobos-2 spacecraft for a period of solar activity maximum. The model describes a magnetopause position in the Martian magnetotail and a flaring angle depending on solar wind dynamic pressure ρV2 as well as three points of magnetospheric boundary crossing on the dayside. The shape of the magnetopause is determined in the model from the pressure balance equation on this boundary. Both magnetic pressure and ionospheric plasma pressure are taken into account. A characteristic feature of the model is that the position of the magnetopause in the subsolar region is stable for rather large values of solar wind pressure (ρV2 > 6 × 10-9 dyn/cm2).
dc.languageeng
dc.titleDependence of Martian magnetopause shape and its dimensions on solar wind dynamic pressure according to Phobos-2 data
dc.typeArticle
dc.subject.frascatiPhysical sciences
dc.audienceScientific
dc.source.titleCosmic Research
dc.source.volume34
dc.source.issue6
dc.source.page551-558
Orfeo.peerreviewedYes
dc.identifier.scopus2-s2.0-27244457666


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