Astronomy and Astrophysics – Astronomy
Scientific paper
Jun 1986
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986dchn.reptq....w&link_type=abstract
Semiannual Report, 1 Oct. 1984 - 31 Mar. 1985 Dartmouth Coll., Hanover, NH. Dept. of Physics and Astronomy.
Astronomy and Astrophysics
Astronomy
Convection, Iue, Line Spectra, Stellar Mass Accretion, Ultraviolet Spectroscopy, White Dwarf Stars, Carbon, Helium, Stellar Composition
Scientific paper
A theoretical analysis was carried out in order to interpret the ultraviolet spectra of DB white dwarfs obtained earlier with the International Ultraviolet Explorer (IUE) satellite. Here the results of the IUE ultraviolet spectroscopy combined with visual data and model atmospheres of DB white dwarfs are reported. In particular, a search for spectra lines due to the element carbon using the ultraviolet was made. In no case is there a positive detection of carbon and from these data, and upper limits for carbon by number relative to helium are derived in the range of C: He 10 to the minus 5 power to 10 to the minus 7 power for the 16 DB stars with ultraviolet spectra in the temperature range 11400 K TEFF less than 2300 K. The low carbon abundances found in the atmospheres of the DB stars agree well with the hypothesis that the atmospheric carbon observed in the cooler DQ members of the helium-rich white dwarf sequence is produced by a convective dredging mechanism.
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