Open and closed magnetospheric tail configurations and their stability

Details Open and closed magnetospheric tail configurations and their stability Open and closed magnetospheric tail configurations and their stability

Jul 1975

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1975ap%26ss..35..389b&link_type=abstract

Astrophysics and Space Science, vol. 35, July 1975, p. 389-402. Research supported by the Deutsche Forschungsgemeinschaft.

Astronomy and Astrophysics

Astrophysics

50

Geomagnetic Tail, Magnetic Field Configurations, Magnetospheric Instability, Topology, Asymptotic Methods, Lines Of Force, Mach Number, Magnetohydrodynamic Stability, Solar Wind Velocity

Scientific paper

The asymptotic theory valid for magnetospheric-tail configurations that vary only weakly in the antisolar direction is used to derive a number of explicit properties. The conditions under which the magnetopause converges to form a closed magnetosphere or diverges (open magnetosphere) are identified and discussed. It is shown that the presence of the high-latitude low-pressure tail lobes guarantees the open solution. The large value of the Mach number of the unperturbed solar wind is the reason for the slow variation of the plasma and field quantities along the tail. Criteria for (two-dimensional) stability are discussed, and it is shown that they can be expressed in terms of simple topological properties of the equilibria. Closed magnetospheres turn out to be stable, while open magnetospheres with sufficiently stretched field lines are subject to an instability which may be the cause of magnetospheric substorms.

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