LATITUDINAL DEPENDENCE OF THE RADIAL IMF COMPONENT - CORONAL IMPRINT

Measurements by Ulysses have confirmed that there is no significant gr adient with respect to heliomagnetic latitude in the radial component, B-r, of the interplanetary magnetic field. In the corona, the plasma beta is << 1, except directly above streamers, so longitudinal and lat itudinal gradients in field strength will relax due to the transverse magnetic pressure gradient force as the solar wind carries magnetic fl ux away from the Sun. This happens quickly enough so that the field is essentially uniform by 5 - 10 R., apparently remaining so as it is ca rried to beyond 1 AU. Here, we illustrate the coronal relaxation with a qualitative physical argument and by reference to a detailed MHD sim ulation.