The Metallicity and Lithium Abundances of the Recurring Novae T CrB and RS Oph

Details The Metallicity and Lithium Abundances of the Recurring Novae T CrB and RS Oph The Metallicity and Lithium Abundances of the Recurring Novae T CrB and RS Oph

May 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008pasp..120..492w&link_type=abstract

The Publications of the Astronomical Society of the Pacific, Volume 120, Issue 867, pp. 492-497.

Astronomy and Astrophysics

Astronomy

5

Stars

Scientific paper

We report on high-resolution spectra of the two recurring novae, T CrB and RS Oph, obtained in 2004 when no outbursts were in progress. Selected regions of the spectra between 6500 and 8800 Åwere measured for equivalent widths and analyzed for metallicity. Lines of Fe I, Ni I, Si I, and Ti I were used to establish the effective temperature. The metallicity as derived using models is near solar with an uncertainty estimated to be near a factor of 2 for both stars. Both stars show a strong lithium line at 6707.8 . Approximate Li abundances were derived using model atmospheres for a direct comparison with the nearby Fe I line at 6710.31 Å and the Ca I ground level line at 6572.78 Å. The Li abundances are near log N(Li) = 1.2 for RS Oph and 0.8 for T CrB on the scale of log N(H) = 12.0. Such Li abundances are high for single K and M giants. A survey of symbiotic stars with cool components of types K and M showed no recognizable Li line in 28 stars with high quality spectra. This makes the two repeating novae different from the other symbiotics that consist of a red giant and a white dwarf.

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