AGB (Asymptotic Giant Branch) stars generate a massive dust
driven stellar wind at the end of their lives. Ideally, this
mass loss is spherical if the physical conditions are
homogeneous at the stellar surface (e.g. temperature) and the
stellar vicinity (e.g. density). Indeed, several physical
processes induce deviations from these ideal conditions. This
will affect the condensation of dust and therefore the mass loss
rate. Inhomogeneities can also caused by cool spots at the
stellar surface. These inhomogeneities of the temperature are
able to emanate from a magnetic field or a huge convection cell
within the stellar envelope. Both options are possible at the
surface of AGB-stars. This thesis introduces a model for the
investigation of the mass loss above cool spots. For that
purpose a radiation hydrodynamic simulation (including a gas, a
dust and a radiation component) has been used and modified for
the special purposes of this problem. A geometry has been chosen
which could have been produced by a magnetic