Detalles de publicación
PP 09008
CNO abundances of HdC and RCB stars: a view of the nucleosynthesis in a white dwarf merger
(1): Instituto de Astrofisica de Canarias (IAC)
(2): National Optical Astronomy Observatory (NOAO)
(3): W. J. McDonald Observatory. The University of Texas at Austin
(4): Department of Physics and Astronomy, Uppsala University
We present high-resolution (R~50,000) observations of near-IR transitions of CO
and CN of the five known hydrogen-deficient carbon (HdC) stars and four R
Coronae Borealis (RCB) stars. We perform an abundance analysis of these stars by
using spectrum synthesis and state-of-the-art MARCS model atmospheres for cool
hydrogen-deficient stars. Our analysis confirms reports by Clayton and
colleagues that those HdC stars exhibiting CO lines in their spectrum and the
cool RCB star S Aps are strongly enriched in 18O (with 16O/18O ratios ranging
from 0.3 to 16). Nitrogen and carbon are in the form of 14N and 12C,
respectively. Elemental abundances for CNO are obtained from CI, C2, CN, and CO
lines. Difficulties in deriving the carbon abundance are discussed. Abundances
of Na from NaI lines and S from SI lines are obtained. Elemental and isotopic
CNO abundances suggest that HdC and RCB stars may be related objects and that
they probably formed from a merger of a He white dwarf with a C-O white dwarf.
and CN of the five known hydrogen-deficient carbon (HdC) stars and four R
Coronae Borealis (RCB) stars. We perform an abundance analysis of these stars by
using spectrum synthesis and state-of-the-art MARCS model atmospheres for cool
hydrogen-deficient stars. Our analysis confirms reports by Clayton and
colleagues that those HdC stars exhibiting CO lines in their spectrum and the
cool RCB star S Aps are strongly enriched in 18O (with 16O/18O ratios ranging
from 0.3 to 16). Nitrogen and carbon are in the form of 14N and 12C,
respectively. Elemental abundances for CNO are obtained from CI, C2, CN, and CO
lines. Difficulties in deriving the carbon abundance are discussed. Abundances
of Na from NaI lines and S from SI lines are obtained. Elemental and isotopic
CNO abundances suggest that HdC and RCB stars may be related objects and that
they probably formed from a merger of a He white dwarf with a C-O white dwarf.