  The slow, dense winds observed in evolved asymptotic giant branch (AGB) stars
are usually attributed to a combination of dust formation in the dynamical
inner atmosphere and momentum transfer from stellar photons interacting with
the newly formed dust particles. Wind models calculated with the DARWIN code,
using this mass-loss scenario, have successfully produced outflows with
dynamical and photometric properties compatible with observations, for both
C-type and M-type AGB stars. Presented here is an overview of the DARWIN models
currently available and what output these models produce, as well as future
plans.
