Collision of an interplanetary rotational discontinuity with the Earth’s bow shock. Hydrodynamic parameters and magnetic field
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- 作者：E. A. Pushkar
- 关键词：solar wind ; interplanetary rotational discontinuity ; Earth’s magnetosphere ; bow shock
- 刊名：Fluid Dynamics
- 出版年：2015
- 出版时间：January 2015
- 年：2015
- 卷：50
- 期：1
- 页码：137-152
- 全文大小：1,563 KB
- 参考文献：1. P?ech, L, Něme?ek, Z, ?afránková, J (2008) Response of Magnetospheric Boundaries to the Interplanetary Shock: Themis Contribution. Geophys. Res. Lett. 35: pp. L17S02
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9. Pushkar, EA (2008) Three-Dimensional MHD Model of Collision of a Solar Wind Shock Wave with the Earth’s Bow Shock. Problems of Modern Mechanics: to the 85th Anniversary of Academician G.G. Chernyi [Collected Articles]. Moscow University Press, Izd-vo “Omega-L- Moscow, pp. 461-475
10. Pushkar, EA (2008) Collision of a Solar Wind Shock Wave and the Earth’s Bow Shock in a Strong Interplanetary Magnetic Field: Three-Dimensional Magnetohydrodynamic Model. Izv. MGIU, Informatsionnye Tekhnologii i Modelirovanie, No. 1 (10). pp. 46-74
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文摘
Hydrodynamic parameters and magnetic fields generated in each of the waves in the neighborhood of the Earth’s bow shock are found within the framework of the ideal magnetohydrodynamic (MHD) model in the three-dimensional non-plane-polarized formulation when the front of an interplanetary rotational discontinuity, which travels from the Sun and rotates the interplanetary magnetic field by a given angle, impinges on the Earth’s bow shock and propagates along its surface. The interaction pattern is constructed in the quasi-steady-state formulation as a mosaic of exact solutions, obtained by means of a computer using an original MHD 3-D Riemann solver, to the Riemann problem of breakdown of a discontinuity between the states downstream of the rotational discontinuity and the bow shock on the traveling line of intersection of their fronts. The calculations are carried out for typical parameters of the quiescent solar wind and the interplanetary magnetic field at the Earth’s orbit. The solutions obtained can be used to interpret measurements carried out by spacecraft in the solar wind and in neighborhood of the Earth’s magnetosphere.