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Mode trapping in pulsating white dwarfs

  • Part VI Seismology of Stars
  • Conference paper
  • First Online:
Progress of Seismology of the Sun and Stars

Part of the book series: Lecture Notes in Physics ((LNP,volume 367))

Abstract

White dwarfs undergo nonradial g-mode pulsation in three separate instability regions during their cooling history. The coolest pulsating white dwarfs are the ZZ Ceti stars, and the hottest correspond to the pulsating PG1159 stars. The adiabatic pulsation properties of stellar models accurately reproduce many of the observed properties of the pulsations. In particular, trapping of modes by composition transition regions near the surface of these stars is an adiabatic phenomenon. Here we present models of ZZ Ceti stars which show trapped modes with periods that are very close to those observed, and illustrate a technique for using these periods to determine the mass of the surface hydrogen layer.

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Author information

Authors and Affiliations

  1. Department of Physics, Iowa State University, 50011, Ames, IA, USA

    Steven D. Kawaler

  2. Department of Astronomy, Yale University, 06511, New Haven, CT, USA

    Philip Weiss

Authors
  1. Steven D. Kawaler
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  2. Philip Weiss
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Editor information

Y. Osaki H. Shibahashi

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© 1990 Springer-Verlag

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Kawaler, S.D., Weiss, P. (1990). Mode trapping in pulsating white dwarfs. In: Osaki, Y., Shibahashi, H. (eds) Progress of Seismology of the Sun and Stars. Lecture Notes in Physics, vol 367. Springer, Berlin, Heidelberg. https://doi.org/10.1007/3-540-53091-6_110

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  • DOI: https://doi.org/10.1007/3-540-53091-6_110

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  • Publisher Name: Springer, Berlin, Heidelberg

  • Print ISBN: 978-3-540-53091-6

  • Online ISBN: 978-3-540-46645-1

  • eBook Packages: Springer Book Archive

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