Abstract
Mass loss of asymptotic giant branch (AGB) stars is commonly attributed to the combined effects of pulsation‐induced shocks and radiation pressure on dust grains formed in the outer atmospheric layers. This paper discusses recent results of detailed radiation‐hydrodynamical wind models, regarding the composition of silicate grains in M‐type AGB stars, the influence of grain size dependent opacities, and basic differences in dust‐driven outflows of C‐ and M‐type AGB stars.
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