  Hydrogen atmosphere white dwarfs with metal lines, so-called DAZs, show
evidence for ongoing accretion of material onto their surfaces. Some DAZs are
known to have unresolved M dwarf companions, which could account for the
observed accretion through a stellar wind. I combine observed Ca abundances of
the DAZs with information on the orbital separation of their M dwarf companions
to infer the mass loss rate of the M dwarfs. I find that for three of the six
known DAZs with M dwarf companions, a stellar wind can plausibly explain the
observed accretion on the white dwarfs assuming Bondi-Hoyle accretion of solar
abundance stellar winds on the order of 10$^{-14}-10^{-16}\Msun$ yr$^{-1}$. The
rest of the sample have companions with orbits $\gtorder$ 1~AU, and require
companion mass loss rates of $> 10^{-11}\Msun$ yr$^{-1}$. I conclude that there
must be an alternative explanation for accretion of material onto DAZs with
widely separated companions. The inferred winds for two of the close binaries
are orders of magnitude smaller than typically assumed for the angular momentum
loss of red dwarf-white dwarf pairs due to magnetic braking from a stellar wind
and may seriously affect predictions for the formation rate of CVs with low
mass companions.
