  We present a new theoretical estimate for the birthrate of R Coronae Borealis
(RCB) stars that is in agreement with recent observational data. We find the
current Galactic birthrate of RCB stars to be $\approx$ 25% of the Galactic
rate of Type Ia supernovae, assuming that RCB stars are formed through the
merger of carbon-oxygen and helium-rich white dwarfs. Our new RCB birthrate
($1.8 \times 10^{-3}$ yr$^{-1}$) is a factor of 10 lower than previous
theoretical estimates. This results in roughly 180--540 RCB stars in the
Galaxy, depending on the RCB lifetime. From the theoretical and observational
estimates, we calculate the total dust production from RCB stars and compare
this rate to dust production from novae and born-again asymptotic giant branch
(AGB) stars. We find that the amount of dust produced by RCB stars is
comparable to the amounts produced by novae or born-again post-AGB stars,
indicating that these merger objects are a viable source of carbonaceous
pre-solar grains in the Galaxy. There are graphite grains with carbon and
oxygen isotopic ratios consistent with the observed composition of RCB stars,
adding weight to the suggestion that these rare objects are a source of
stardust grains.
