Hostname: page-component-7c8c6479df-24hb2 Total loading time: 0 Render date: 2024-03-28T09:39:26.630Z Has data issue: false hasContentIssue false

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
Affiliation:
Department of Mathematical Physics, Tomsk State University, FTF, Lenin Avenue, 36, Tomsk, 634050, Russia email: nminkova@ftf.tsu.ru
Rights & Permissions [Opens in a new window]

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

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.

Type
Contributed Papers
Copyright
© 2006 International Astronomical Union