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“Carbon-Rich” White Dwarfs

Published online by Cambridge University Press:  12 April 2016

I. Bues
I. Bues*
Affiliation:
I. Mathem. Inst. Freie Universität Berlin

Extract

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8 white dwarfs of spectral type λ4670, LP 93-21, EG182, BPM 27606, EG82, G257-38, EG148, G99-37 and L97-3, with more or less well observed carbon bands in their spectra, have been analyzed by detailed model atmosphere techniques. For the very strong band stars the blanketing effect of the molecular band systems of the Swan band and the Deslandres-d’Azambuja band had to be included in the computation of the models. The best fit of the fluxes with scanner observations and spectra is obtained for abundance ratios of 103 ≤ He/H ≤ 105, 800 ≤ He/C ≤ 5000, with LP 93-21 being the most carbon-rich object. The results are summarized in Table 1.

Type
Colloquium Session III
Information
International Astronomical Union Colloquium , Volume 53: White Dwarfs and Variable Degenerate Stars , August 1979 , pp. 186 - 187
Copyright
Copyright © The University of Rochester 1979

References

Eggen, O.J., Greenstein, J.L. 1965, Ap.J., 141, 83.CrossRefGoogle Scholar
Humphreys, R.M., Liebert, J., Romanishin, W., Strittmatter, P.A. 1979, Publ. A.S.P., 91, 107.Google Scholar
Wegner, G. 1975, M.N.R.A.S., 171, 637.Google Scholar