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Pulsations of White Dwarf Stars with Thick Hydrogen or Helium Surface Layers

Published online by Cambridge University Press:  03 August 2017

Arthur N. Cox ,
Sumner G. Starrfield ,
Russell B. Kidman  and
W. Dean Pesnell
Arthur N. Cox
Affiliation:
Theoretical Division, MS B288, Los Alamos National Laboratory, Los Alamos, New Mexico 87544
Sumner G. Starrfield
Affiliation:
Theoretical Division, MS B288, Los Alamos National Laboratory, Los Alamos, New Mexico 87544
Russell B. Kidman
Affiliation:
Theoretical Division, MS B288, Los Alamos National Laboratory, Los Alamos, New Mexico 87544
W. Dean Pesnell
Affiliation:
Theoretical Division, MS B288, Los Alamos National Laboratory, Los Alamos, New Mexico 87544

Extract

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In order to see if there could be agreement between results of stellar evolution theory and those of nonradial pulsation theory, calculations of white dwarf models have been made for hydrogen surface masses of 10−4M⊙. Earlier results by Winget et al. (1982) indicated that surface masses greater than 10−8M⊙ would not allow nonradial pulsations, even though all the driving and damping is in surface layers only 10−12 of the mass thick. We show that the surface mass of hydrogen in the pulsating white dwarfs (ZZ Ceti variables) can be any value as long as it is thick enough to contain the surface convection zone.

Type
Chapter 5: Seismological Investigations of Compact Stars
Information
Symposium - International Astronomical Union , Volume 123: Advances In Hello- and Asteroseismology , 1988 , pp. 333 - 337
Copyright
Copyright © Reidel 1988 

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