Mass loss is a crucial component in stellar evolution models, since it largely determines the rate of evolution at the later stages of a star’s life. The dust-driven outflows from AGB stars are particularly important in this regard. Including AGB dust formation in a stellar evolution model does also require a model of these outflows. Since AGB stars exhibit large-amplitude pulsation, a model based on time-dependent radiation hydrodynamics (RHD) is needed in order to capture all the important physical aspects of dust formation. However, this cannot be afforded in a stellar evolution model. Here, a mean-flow model is presented, which include corrections to the steady-state model currently being used in AGB evolution models with dust formation.

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