Interaction of non-perpendicular/parallel solar wind shock waves with the earth's magnetosphere

Abstract

The interaction of travelling interplanetary shock waves with the bow shock-magnetosphere system is considered. We consider the general case when the interplanetary magnetic field is oblique to the Sun-planetary axis, thus, the interplanetary shock is neither parallel nor perpendicular. We find that an ensemble of shocks are produced after the interaction for a representative range of shock Mach numbers. First, we find that the system S + R − CS − S + appears after the collision of travelling fast shock waves S + (Mach number M = 2 to 7) with the bow shock. Here, S − and R − represent the slow shock wave and slow rarefaction wave, and C represents the contact surface. It is shown that in the presence of an interplanetary field that is inclined by 45° to the radial solar wind velocity vector, the waves R − and S − are weak waves and, to the first degree of approximation, the situation is similar to the previously studied normal perpendicular case. The configuration, R + C m S − S + or R + C m R − S + where C m is the magnetopause, appears as the result of the fast shock wave's collision with the magnetopause. In this case the waves S − and R − are weak. The fast rarefaction wave reflected from the magnetosphere is developed similar to the case for the collision of a perpendicular shock. The shock wave intensity is varied for Mach numbers from 2 to 10. Thus, in the limits of the first approximation, the validity of the one-dimensional consideration of the nonstationary interaction of travelling interplanetary shock waves with the bow shock-magnetosphere system is proved. The appearance of the fast rarefaction wave, R 4, decreasing the pressure on the magnetosphere of the Earth after the abrupt shock-like contraction, is proved. A possible geomagnetic effect during the global perturbation of the SSC or SI+ type is discussed.