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The Effect of Varying Helium and Hydrogen Layer Masses on the Pulsation Properties of White Dwarf Models

Published online by Cambridge University Press:  12 April 2016

P.A. Bradley ,
D.E. Winget  and
M.A. Wood

Extract

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Currently, there are disagreements on the theoretical pulsation properties of DA white dwarf models. Winget and his group (cf Winget 1981, Winget and Fontaine 1982, Winget et al. 1981, 1982) use 0.6M⊙ evolutionary white dwarf models, to find that (Teff)blue is sensitive to the mass of the hydrogen layer and very sensitive to the treatment of convective efficiency. However, (Teff)blue is relatively insensitive to the helium layer mass. Winget and collaborators also find that the hydrogen layer must be restricted to 10−8 > MH/M* > 10−12 for (Teff)blue to occur at ∼ 10,500K in models with ML1 convection (see below). More efficient (ML2) convection pushes the blue edge up to ∼ 12,200K, which is still short of the observed blue edge of ∼ 13,000K.

Type
Research Article
Information
International Astronomical Union Colloquium , Volume 114: White Dwarfs , 1989 , pp. 286 - 289
Copyright
Copyright © Springer-Verlag 1989

References

[1] Acouragi, J.P. and Fontaine, G., 1980, Ap. J., 242, 1208.Google Scholar
[2] Böhm, K.-H. and Cassinelli, J. 1971, Astr. Ap., 12, 21.Google Scholar
[3] Böhm-Vitense, E. 1958, Zs. f. Ap., 46, 108.Google Scholar
[4] Cox, A.N., Starrfield, S.G., Kidman, R.B., and Pesnell, W.D. 1987, Ap. J., 317, 303.Google Scholar
[5] Fontaine, G., Tassoul, M., and Wesemael, F. 1984, in Theoretical Problems in Stellar Stability and Oscillations: Proc. of the 25th Int. Ap. Colloq., ed. Noels, A. and Gabriel, M., (Coint-Ougree, Belgium: Universite de Liege), 328.Google Scholar
[6] Kawaler, S.D., 1986, Ph. D. Thesis, University of Texas.Google Scholar
[7] Kepler, S.O., Vauclair, G., Nather, R.E., Winget, D.E., and Robinson, E.L. 1988, these proceedings.Google Scholar
[8] Tomaney, A.B. 1987, in IAU Colloquium No. 95: The Second Conference on Faint Blue Stars, ed. Philip, A.G.D., Hayes, D.S., and Liebert, J.W., (Schenectady; Davis Press), p. 673.Google Scholar
[9] Winget, D.E., 1981, Ph. D. Thesis, University of Rochester.Google Scholar
[10] Winget, D.E., van Horn, H.M., and Hansen, C.J. 1981, Ap. J., 245, L33.Google Scholar
[11] Winget, D.E., and Fontaine, G. 1982, in Pulsations of Classical and Cataclysmic Variable Stars, ed. Cox, J.P. and Hansen, C.J., (Boulder; University of Colorado Press), p. 46.Google Scholar
[12] Winget, D.E., van Horn, H.M., Tassoul, M., Hansen, C.J., Fontaine, G., and Carroll, B.W. 1982, Ap. J., 252, L65.Google Scholar