The shape of the magnetopause and the field due to magnetopause currents are calculated from the requirement that the pressure in the magnetosheath be balanced by magnetic pressure inside the magnetosphere. The field due to magnetopause currents is calculated to be consistent with the iteratively adjusted magnetopause shape. The field due to current systems inside the magnetosphere is taken from the T96 model [Tsyganenko, 1996>, which carries information from ~47,000 magnetic field observations. Many different magneto-spheric configurations were found for a variety of conditions. Changes in the shape of the magnetopause with varying dipole tilt angle stood out. The magnetotail and the nose (the point closest to the Sun) were found to shift vertically, in opposite directions, for nonzero dipole tilt. The vertical offset of the nose from the Earth-Sun line varied linearly with dipole tilt angle, reaching ~3RE for maximal tilt and having a weak dependence on solar wind dynamic pressure. The formation of a secondary stagnation point just above the sunward cusp was indicated for absolute dipole tilts in excess of 15¿. The magnitude of the field strength at its local maximum just behind the cusp was determined as a function of dipole tilt angle and the subsolar field strength. Calculated magnetopause shapes and observed magnetopause crossings were found to be consistent when the tilt angle was taken into account. Variations in the latitude of the magnetic cusps with dynamic pressure, interplanetary magnetic field Bz, and dipole tilt were reasonably consistent with observed variations in the latitude of the particle cusp. ¿ 1999 American Geophysical Union