The direct problem for two-dimensional transonic outflow of gas from the surface of a slowly-rotating star

A procedure for solving the direct problem for the case of transonic outflow of gas from the surface of a slowly rotating star is formulated in the framework of ideal, two-dimensional hydrodynamics. This is possible because of the existence of a previously known exact analytical solution - that for spherically-symmetric stellar wind. Analytical expressions for the stream function, gas density, velocity, etc. are obtained for asymptotically distant regions. The solution displays a tendency for the formation of a disk in the equatorial plane.