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The kinetic model of the solar wind influenced by the given magnetic field

Published online by Cambridge University Press:  01 November 2006

Natalia R. Minkova
Natalia R. Minkova
Affiliation:
Department of Mathematical Physics, Tomsk State University, FTF, Lenin Avenue, 36, Tomsk, 634050, Russia email: nminkova@ftf.tsu.ru
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Abstract

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The solar wind is considered as a steady fully ionized hydrogen plasma flow, with rotational symmetry. The Parker-spiral type magnetic field specifies the dependence of the flow speed on the radial distance and meridional angle if the plasma is assumed to be quasi-neutral and currentless. A two-particle kinetic model of the collisionless rotationally symmetrical plasma flow in a magnetic field is formulated and applied to estimate the flux and density of the solar wind. The obtained theoretical results are compared to the observational data.

Keywords

solar windplasmasmagnetic fieldsanalyticalstatistical
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 2 , Symposium S233: Solar Activity and its Magnetic Origin , March 2006 , pp. 311 - 312
Copyright
© 2006 International Astronomical Union