Radial Pulsation Analyses of DA Dwarfs

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 th...

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Bibliographic Details
Published in:International Astronomical Union Colloquium 1979-08, Vol.53, p.382-387
Main Authors: Starrfield, S., Cox, A. N., Hodson, S. W.
Format: Article
Language:English
Subjects:
640102 - Astrophysics & Cosmology- Stars & Quasi-Stellar, Radio & X-Ray Sources
CLASSICAL AND QUANTUM MECHANICS, GENERAL PHYSICS
CONVECTION
DATA
DATA FORMS
DENSITY
DWARF STARS
EIGENFUNCTIONS
FUNCTIONS
GRAPHS
INFORMATION
INSTABILITY
INTEGRALS
LAGRANGIAN FUNCTION
NUMERICAL DATA
PHYSICAL PROPERTIES
PULSATIONS
STARS
TEMPERATURE DEPENDENCE
THEORETICAL DATA
TIME DEPENDENCE
WORK FUNCTIONS
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Description
Summary: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.
ISSN:0252-9211
DOI:10.1017/S0252921100076235