Magnetic field reconnection theory and the solar wind-magnetosphere interaction - A review

Details Magnetic field reconnection theory and the solar wind-magnetosphere interaction - A review Magnetic field reconnection theory and the solar wind-magnetosphere interaction - A review

Jun 1985

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985ssrv...41....1p&link_type=abstract

Space Science Reviews (ISSN 0038-6308), vol. 41, June 1985, p. 1-89.

Astronomy and Astrophysics

Astronomy

79

Astronomical Models, Earth Magnetosphere, Magnetic Field Configurations, Magnetic Field Reconnection, Solar Terrestrial Interactions, Solar Wind, Magnetohydrodynamic Stability, Planetary Evolution, Plasma Density, Plasma Sheaths

Scientific paper

The theory of magnetic field line reconnection, as related to the problems of interaction between the solar wind (SW) flow and the earth's magnetosphere (MS) is reviewed, together with laboratory and numerical modeling experiments. The models of Sonnerup (1970), Petschek (1964), Parker (1973), Syrovatskii (1979, 1981), and a solution for the plasma sheet structure (Birn et al., 1977) are presented. It is shown that in the presence of a frozen-in magnetic field, the flow differs from that in the pure gasdynamic case by the appearance of a stagnation line, instead of a point, at the subsolar part of the magnetopause, the length and location of which determine the character of the interaction of the SW with the MS. A theory of that interaction was developed for a steady-state case, and a qualitative model of the SW-MS interaction in the nonsteady-state case is proposed.

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