Proc. IAU volume 13, issue S335, P121-124 2017 DOI: 10.1017/s1743921317010420 View full text
M. I. Verigin, G. A. Kotova, V. V. Bezrukikh

Abstract: AbstractIt is generally accepted to use the solar wind ram pressure ρV2 and the IMF Bz component for empirical description of the geo-magnetopause position and shape. A specific feature of the present paper is not to use the solar wind ρV2 but the thermal Pth and magnetic field Pmag pressures adjacent to the magnetopause for proper modelling. These pressures are deduced from the results of 3-D MHD runs and analytic solutions for post bow shock MHD flow in Lagrangian variables. The magnetopause shape variation …

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