  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.
