We obtain a class of steady three-dimensional magnetohydrodynamic (MHD) solar wind solutions from a primary radial MHD wind which is spherically symmetric. The energetic source for modifying the given primary MHD wind is the Poynting flux into the solar corona due to interactions of rotation, random flows, and magnetic field at the solar surface. The total energy flux associated with the perturbative MHD flow is conserved beyond several solar radii for typical solar wind parameters. Our main results are as follows: (1) clarification of the issue of possible transverse magnetic field configurations in heliospheric polar regions which can significantly influence the transport of galactic cosmic rays; (2) explicit demonstration that in the presence of nonaxisymmetric MHD perturbations over the solar poles such as a typical misalignment of the rotation and magnetic axes as well as random MHD perturbations, the transverse magnetic field eventually dominates the radial component over the polar heliosphere at large radial distance; (3) an analytical MHD model for latitudinal variation of heliospheric magnetic field due to the solar differential rotation; and (4) a MHD model of a warped heliospheric current sheet and its deformation due to the solar differential rotation. Our class of MHD wind solutions provides a new theoretical basis for developing numerical MHD codes and for modeling modulation of galactic cosmic rays by the heliospheric magnetic field. ¿ American Geophysical Union 1992