THE SOLAR-WIND FLOW ALONG THE SUBSOLAR LINE IN THE MAGNETIC BARRIER AND RECONNECTION AT THE MAGNETOPAUSE

被引：4

作者：

ERKAEV, NV

MEZENTSEV, AV

BIERNAT, HK

BESSER, BP

BACHMAIER, GA

SEMENOV, VS

RIJNBEEK, RP

FARRUGIA, CJ

机构：

[1] AUSTRIAN ACAD SCI,SPACE RES INST,A-8010 GRAZ,AUSTRIA

[2] ST PETERSBURG STATE UNIV,INST PHYS,ST PETERSBURG,RUSSIA

[3] UNIV ST ANDREWS,DEPT MATH SCI,ST ANDREWS KY16 9SS,SCOTLAND

[4] NASA,GODDARD SPACE FLIGHT CTR,GREENBELT,MD 20771

来源：

MAGNETOSHEATH | 1994年 / 14卷 / 07期

基金：

美国国家航空航天局;

关键词：

D O I：

10.1016/0273-1177(94)90051-5

中图分类号：

V [航空、航天];

学科分类号：

08 ; 0825 ;

摘要：

The magnetic barrier is a significant fraction of the magnetosheath region where magnetic forces react back on the plasma flow. We use a magnetohydrodynamic approach to calculate the solar wind flow around the magnetosphere. The use of so-called frozen-in coordinates, where the flow lines and the magnetic field are coordinate axes, is found to be most appropriate. Numerical solutions are presented for the problem of the flow around a blunt body. The results near the magnetopause are used as input parameters for a model of the reconnection of magnetic field lines based on shock-type structures.

引用

页码：81 / 86

页数：6

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