Abstract
Global magnetohydrodynamic models predict that plasma velocities vary
almost linearly from 0 km s-1 along the stagnation
streamline leading from the nose of the stationary magnetopause to 0.25
VSW at the nose of the bow shock, where
VSW is the solar wind velocity. This paper presents a
proof-of-concept study showing how two-point measurements of the plasma
velocity in the subsolar magnetosheath can be used to determine
gradients in the plasma velocity and consequently the steady-state or
slowly-moving locations of both the nose of the magnetopause and the
nose of the bow shock. The results may be of use to those binning
magnetosheath observations to develop empirical models, those testing
models for magnetopause erosion or deposition in response to magnetic
reconnection, and those determining the stand-off distance of the bow
shock as a function of solar wind conditions.