  Microlensing surveys have proven to be tremendously fruitful in providing
valuable data products for many fields of astrophysics, from eclipse
lightcurves for substellar candidates to limb darkening in stellar atmospheres.
We report on a program of modeling observables from microlensing of
circumstellar envelopes, particularly those of red giant stars that are the
most likely to show finite source effects. We will summarize work for how
polarization light curves can be used to infer envelope properties and will
describe recent modeling of the time dependent spectral energy distributions
(SEDs) for microlensing of dusty winds. One of the most exciting developments
is the possibility of measuring variable polarization from microlensing in a
suitable source using the RINGO polarimeter at La Palma. Also quite interesting
is the possibility of probing a dusty wind using IRAC data for a suitable
source in the event that Spitzer has a ``warm'' cycle.
