Abstract:
Surface abundances of 14 (11 majority class and three minority class) R Coronae Borealis stars (RCBs) along with
the final-flash object, V4334 Sgr (Sakurai’s object) are revised based on their carbon abundances measured from
the observed C2 bands; note that the earlier reported abundances were derived using an assumed carbon abundance
due to the well-known carbon problem. The hot RCB star MV Sgr is not subject to a carbon problem; it is
remarkable to note that MV Sgr’s carbon abundance lies in the range that is measured for the majority and minority
class RCBs. The revised iron abundances for the RCBs are in the range log e (Fe) = 3.8 to log e (Fe) = 5.8 with the
minority class RCB star V854 Cen at the lower end and the majority class RCB star R CrB at the higher end of this
range. Indications are that the revised RCBs’ metallicity range is roughly consistent with the metal-poor population
contained within the bulge. The revised abundances of RCBs are then compared with extreme helium stars (EHes),
the hotter relatives of RCBs. Clear differences are observed between RCBs and EHes in their metallicity
distribution, carbon abundances, and the abundance trends observed for the key elements. These abundances are
further discussed in light of their formation scenarios.
