Structure of magnetospheric convection at the southward and northward directions of the interplanetary magnetic field.

It is shown that differences in the structure of the magnetospheric magnetic field for southward and northward directions of the IMF are due to different reconnection processes. In the northward case, the reconnection occurs at two neutral points of the magnetic field and has an essentially three-dimensional character. In the southward case, a two-dimensional pattern arises, which is analogous to line-type reconnection.