We discuss numerical simulations of stellar winds and accretion-type flows obtained with the Versatile Advection Code (http://www.phys.uu.nl/~toth/), a software package for solving systems of conservation laws. The wind models include both steady-state and time-dependent transonic outflows from magnetized, rotating stars (Keppens & Goedbloed, 1998, accepted by A&A). Specifically, we present an axisymmetric, stationary solar wind solution that takes account of both the solar differential rotation and the presence of an equatorial dead zone. Subsequently, coronal mass ejections are induced within this solar wind by means of an enforced mass flux. Sufficiently violent forcing triggers shocked ejecta. These axisymmetric MHD simulations of stellar outflows in a meridional cross-section are then confronted with HD, shocked inflows restricted to the equatorial plane. Molteni, Toth & Kuznetsov (1998, accepted by ApJ) recently demonstrated how axisymmetric, shocked rotating accretion flows onto compact objects can be unstable to non-axisymmetric azimuthal perturbations. Steadily rotating, deformed shock patterns can thereby develop. Fully 3D time-dependent outflow and inflow simulations will build upon the insights gained from both studies.