Abstract
AbstractWe present results of global magnetohydrodynamic simulations which reconsider the relationship between the solar wind dynamic pressure (Pd) and magnetopause standoff distance (RSUB). We simulate the magnetospheric response to increases in the dynamic pressure by varying separately the solar wind density or velocity for northward and southward interplanetary magnetic field (IMF). We obtain different values of the power law indices N in the relation depending on which parameter, density, or velocity, has been varied and for which IMF orientation. The changes in the standoff distance are smaller (higher N) for a density increase for southward IMF and greater (smaller N) for a velocity increase. An enhancement of the solar wind velocity for a southward IMF increases the magnetopause reconnection rate and Region 1 current that move the magnetopause closer to the Earth than it appears in the case of density increase for the same dynamic pressure.
Highlights
SAMSONOV ET AL.: MAGNETOPAUSE STANDOFF DISTANCE the magnetopause current layer) (Borovsky & Birn, 2014)
Large peaks of the electric current density correspond to the magnetopause, and small peaks correspond to the bow shock
Vertical dotted lines indicate the boundary points on both sides of the current layers determined by condition J=0.15 JMAX where JMAX is the maximal current density at the subsolar magnetopause
Summary
SAMSONOV ET AL.: MAGNETOPAUSE STANDOFF DISTANCE the magnetopause current layer) (Borovsky & Birn, 2014). We use the following formula for the absolute reconnection rate (in units of electric field) Where indices s and m indicate magnetic fields and densities on the magnetosheath and magnetospheric sides of the magnetopause current (reconnection) layer.
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