Hostname: page-component-78c5997874-ndw9j Total loading time: 0 Render date: 2024-11-02T20:20:00.743Z Has data issue: false hasContentIssue false
  • English
  • Français

Spectroscopic Studies and Atmospheric Parameters of ZZ Ceti Stars

Published online by Cambridge University Press:  12 April 2016

D. Daou ,
F. Wesemael ,
P. Bergeron ,
G. Fontaine  and
J. B. Holberg
D. Daou
Affiliation:
Département Physique, Université de Montréal
F. Wesemael
Affiliation:
Département Physique, Université de Montréal
P. Bergeron
Affiliation:
Département Physique, Université de Montréal
G. Fontaine
Affiliation:
Département Physique, Université de Montréal
J. B. Holberg
Affiliation:
Lunar and Planetary Laboratory, University of Arizona

Extract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

The pulsating ZZ Ceti stars cover a narrow range of effective temperatures along the cooling sequence of DA white dwarfs (see, eg., Winget and Fontaine 1982). Fast-photometric searches for pulsating stars in that class have provided strong evidence that the ZZ Ceti phase is an evolutionary phase through which all cooling DA stars will eventually go through (Fontaine et al. 1982). Recent investigations, based on optical or ultraviolet photometry and spectrophotometry, have set the boundaries of the instability strip at temperatures near 10,000-11,000 K and 12,000-13,000 K, respectively (McGraw 1979; Greenstein 1982; Weidemann and Koester 1984; Fontaine et al. 1985; Wesemael, Lamontagne, and Fontaine 1986; Lamontagne, Wesemael, and Fontaine 1987, 1988).

Type
Research Article
Information
International Astronomical Union Colloquium , Volume 114: White Dwarfs , 1989 , pp. 244 - 248
Copyright
Copyright © Springer-Verlag 1989

References

Bergeron, P., Wesemael, F., and Fontaine, G. 1987, IAU Colloq. No. 95, The Second Conference on Faint Blue Stars, Davis Philip, A.G., Hayes, D.S., and Liebert, J.W., eds., L. Davis Press, p. 661.Google Scholar
Bergeron, P., Wesemael, F., and Fontaine, G. 1988, these Proceedings.Google Scholar
Brassard, P., Wesemael, F., and Fontaine, G. 1987, IAU Colloq. No. 95, The Second Conference on Faint Blue Stars, Davis Philip, A.G., Hayes, D.S., and Liebert, J..W., eds., L. Davis Press, p 669.Google Scholar
Döppen, V., Anderson, L., and Mihalas, D. 1987, Astrophys. J., 319, 195 CrossRefGoogle Scholar
Fontaine, G., Bergeron, P., Lacombe, P., Lamontagne, R., and Talon, A. 1985, Astron. J. 90, 1094.CrossRefGoogle Scholar
Fontaine, G., McGraw, J.T., Dearborn, D.S.P., Gustafson, J., and Lacombe, P. 1982, Astrophys. J., 258, 651 CrossRefGoogle Scholar
Greenstein, J.L. 1982, Astrophys. J., 258, 661.CrossRefGoogle Scholar
Hummer, D.G. and Mihalas, D. 1988, Astrophys. J. in press.Google Scholar
Kepler, S.O., Robinson, E.L., and Nather, R.E. 1983, Astrophys. J., 271, 744.CrossRefGoogle Scholar
Lamontagne, R., Wesemael, F., and Fontaine, G. 1987, IAU Colloq. No. 95, The Second Conference on Faint Blue Stars, Davis Philip, A.G., Hayes, D.S., and Liebert, J.V., eds., L. Davis Press, p. 677.Google Scholar
Lamontagne, R., Wesemael, F., and Fontaine, G. 1988, these Proceedings.Google Scholar
McGraw, J.T. 1979, Astrophys. J., 229, 203.CrossRefGoogle Scholar
Nelan, E.P. and Wegner, G. 1985, Astrophys. J., 289, L31.CrossRefGoogle Scholar
Schulz, H. and Wegner, G. 1981, Astron. Astrophys., 94, 272 Google Scholar
Weidemann, V. and Koester, D. 1980, Astron. Astrophys., 85, 208.Google Scholar
Weidemann, V. and Koester, D. 1984, Astron. Astrophys., 132, 195.Google Scholar
Wesemael, F., Lamontagne, R., and Fontaine, G. 1986, Astron. J., 91, 1376.CrossRefGoogle Scholar
Winget, D.E. and Fontaine, G. 1982, in Pulsations in Classical and Cataclysmic Variable Stars, Cox, J.P. and Hansen, C.J., eds., Joint Institute for Laboratory Astrophysics, Boulder, p. 46.Google Scholar