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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

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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

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