  We consider the formation of dwarf carbon stars via accretion from a carbon
AGB companion in light of the new 107 object sample of Downes et al. (2004).
This sample is now large enough to allow good mass determination via comparison
of a composite spectrum to theoretical atmospheric models. Carbon dwarfs of
spectral type M are indeed main sequence M dwarfs with enhanced metallicity and
carbon abundance. We also calculate the predicted abundance of both M and of
F/G carbon dwarfs, and show that the latter should be falsifiable in the near
future.
