Response of ionospheric convection to changes in the interplanetary magnetic field: Lessons from a MHD simulation

Characteristics of magnetospheric and high-latitude ionospheric convection pattern responses to abrupt changes in the interplanetary magnetic field (I MF) orientation have been investigated using an MHD model with a step funct ion reversal of IMF polarity (positive to negative By) in otherwise steady solar wind conditions. By examining model outputs at 1 min intervals, we ha ve tracked the evolution of the IMF polarity reversal through the magnetosp here, with particular attention to changes in the ionosphere and at the mag netopause. For discussion, times are referenced relative to the time of fir st contact (t = 0) of the IMF reversal with the subsolar nose of the magnet opause at similar to 10.5 R-E. The linear change in large-scale ionospheric convection pattern begins at t = 8 min, reproducing the difference pattern results of Ridley et al. [1997, 1998]. Field-aligned current difference pa tterns, similarly derived, show an initial two-cell pattern earlier, at t = 4 min. The current difference two-cell pattern grows slowly at first, then faster as the potential pattern begins to change. The first magnetic respo nse to the impact of the abrupt IMF transition at the magnetopause nose is to reverse the tilt of the last-closed field lines and of the "first"-open field lines. This change in tilt occurs within the boundary layer before me rging of IMF with closed magnetospheric field lines starts. In the case of steady state IMF By, IMF field lines undergo merging or "changing partners" with other IMF field lines, as they approach the nose and tilt in response to currents. When the By reversal approaches the magnetopause nose, IMF fi eld lines from behind the reversal overtake and merge with those in front o f the reversal, thus puncturing the reversal front and uncoupling the layer of solar wired plasma in the reversal zone from the magnetosphere. The unc oupled layer propagates tailward entirely within the magnetosheath. Merging of closed magnetospheric field lines with the new polarity IMF begins at t = 3 min and starts to affect local currents near the cusp 1 min later. Whi le merging starts early and controls the addition of open flux to the polar cap, large-scale convection pattern changes are tied to the currents, whic h are controlled in the boundary layers. The resulting convection pattern i s an amalgamation of these diverse responses. These results support the con clusion of Maynard et al. [2001b], that the small convection cell is driven from the opposite hemisphere in By-dominated situations.