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.