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An approximate formulation of the steady-state Chapman-Ferraro problem, given recently by Davis and Beard, is used to calculate the coordinates of the complete boundary of the geomagnetic field. Field lines are then computed in the magnetic meridian plane containing the free-stream direction of the solar wind, taking into account the distorting effects of currents flowing in the boundary. Numerical results are given for the case where the geomagnetic dipole axis is perpendicular to the direction of the solar wind. (auth).
The response of the magnetosphere boundary in a steady solar wind to small initial departures from equilibrium is investigated in accordance with the classical model of Chapman and Ferraro. If the wavelength and amplitude are sufficiently small that curvature and second-order effects can be disregarded, all perturbations, except those having wave fronts aligned with the direction of the local magnetic field, are found to damp exponentially with time and to drift along the boundary with the tangential component of the solar wind. Aligned waves, which neither damp nor amplify in this approximation, are examined further by inclusion of curvature and higher order effects. A first-order analysis shows that curvature introduces a destabilizing effect in small regions in the vicinity of the neutral points and a stabilizing effect elsewhere. Possible geophysical consequences, such as the persistent magnetic agitation of the polar regions, are discussed. An exact solution for an aligned cylindrical solitary wave having an initial form of a circular arc is also presented to illustrate a mode of response that appears to permit injection of elongated and widely separated columns of solar wind plasma into the magnetosphere under certain conditions and to provide a mechanism for momentum transfer from the solar wind to the ambient magnetosphere plasma.
The theory of the boundary of the cavity surrounding a magnetic dipole immersed in a steadily flowing stream of plasma is reviewed, and the various results compared with satellite observations of the termination of the geomagnetic field. The shape on the solar side is roughly hemispherical with some theoretical uncertainty over the poles, the shape on the antisolar side is probably raindrop shaped but depends critically on the direction and relative magnitude of the interplanetary magnetic field and possible nonadiabatic processes such as shock phenomena. (auth).