  We discuss steady-state transonic outflows obtained by direct numerical
solution of the hydrodynamic and magnetohydrodynamic equations. We make use of
the Versatile Advection Code, a software package for solving systems of
(hyperbolic) partial differential equations. We proceed stepwise from a
spherically symmetric, isothermal, unmagnetized, non-rotating Parker wind to
arrive at axisymmetric, polytropic, magnetized, rotating models. These
represent 2D generalisations of the analytical 1D Weber-Davis wind solution,
which we obtain in the process. Axisymmetric wind solutions containing both a
`wind' and a `dead' zone are presented.
  Since we are solving for steady-state solutions, we efficiently exploit fully
implicit time stepping. The method allows us to model thermally and/or
magneto-centrifugally driven stellar outflows. We particularly emphasize the
boundary conditions imposed at the stellar surface. For these axisymmetric,
steady-state solutions, we can use the knowledge of the flux functions to
verify the physical correctness of the numerical solutions.
