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Radial Pulsation Analyses of DA Dwarfs*

Published online by Cambridge University Press:  12 April 2016

S. Starrfield ,
A. N. Cox  and
S. W. Hodson
S. Starrfield
Affiliation:
Theoretical Division, Los Alamos Scientific Laboratory, Los Alamos, NM
A. N. Cox
Affiliation:
Theoretical Division, Los Alamos Scientific Laboratory, Los Alamos, NM
S. W. Hodson
Affiliation:
Theoretical Division, Los Alamos Scientific Laboratory, Los Alamos, NM

Extract

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There are now twelve ZZ Ceti stars known and their properties are summarized by Nather (1978) and McGraw (1977, 1979). They have normal DA spectra and their colors range from a B-V of 0.18 mag to 0.22 mag. This places them on the HR diagram in a region which is an extension to the white dwarfs of the Cepheid instability strip. This would suggest that the cause of their pulsation could be analogous to the κ and γ mechanisms of the Cepheids except for the fact that the periods of the ZZ Ceti stars range from 200 to 1200 seconds, three orders of magnitude larger than the radial pulsation periods for white dwarfs.

Type
Colloquium Session VI
Information
International Astronomical Union Colloquium , Volume 53: White Dwarfs and Variable Degenerate Stars , August 1979 , pp. 382 - 387
Copyright
Copyright © The University of Rochester 1979

Footnotes

†

also at Department of Physics, Arizona State University, Tempe, AZ.

*

Supported in part by NSF Grant AST77-23190 to Arizona State University.

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