2D models for the winds of AGB stars

New 2D models for C-star winds including hydrodynamics with radiation pressure on dust grains, chemistry, time-dependent dust formation and simplified grey radiative transfer are presented. These models reveal a much more complex picture of the dust formation and wind acceleration compared to existing 1D models. Excited by hydrodynamical, radiative and thermal instabilities, dust forms from time to time in limited areas close to the star. These clouds are then accelerated outward by radiation pressure. At the same time, less dust containing matter is falling back from the outside at different places. A highly dynamical and turbulent dust formation zone is created in this way, which again creates a strongly inhomogeneous dust distribution. Further away from the star, flow instabilities (e.g. Rayleigh-Taylor) have time to modify and further shape the dust clouds produced in the dust formation zone.