Hostname: page-component-8448b6f56d-jr42d Total loading time: 0 Render date: 2024-04-18T14:22:24.472Z Has data issue: false hasContentIssue false
  • English
  • Français

White Dwarf Seismology: Inverse Problem of g-Mode Oscillations

Published online by Cambridge University Press:  12 April 2016

Hiromoto Shibahashi ,
Takashi Sekii  and
Steven Kawaler
Hiromoto Shibahashi
Affiliation:
Department of Astronomy, Faculty of Science, University of Tokyo, Bunkyo-ku, Tokyo 113, Japan
Takashi Sekii
Affiliation:
Department of Astronomy, Faculty of Science, University of Tokyo, Bunkyo-ku, Tokyo 113, Japan
Steven Kawaler
Affiliation:
Center for Solar and Space Research, Yale University 260 Whitney Aven., P.O. Box 6666, New Haven, CT 06511, U.S.A.

Extract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

Since light variability in white dwarfs was first discovered twenty years ago, eighteen DA white dwarfs, several pulsating DB white dwarfs, and hotter pre-white dwarfs have so far been found to be pulsating variables. The most conspicuous characteristics of pulsations in these stars are that they seem to consist of multiple g-modes of nonradial oscillations. Attention should be paid to multiplicity of modes. Stimulated by the success of helioseimology, a research field called ‘asteroseismology’, in which we may probe the internal structure of stars by means of observations of their oscillations, is going to develop. How well such a seismological approach succeeds is dependent on how many modes are observed in each of stars. Since the number of modes of an individual pulsating white dwarf is larger than those of other types of pulsating stars but for the Sun, the seismological study may be the most promising as to the white dwarfs. In fact, by applying the asymptotic relations among eigenfrequencies of high order g-modes with low degree, the degree l, and the radial order n, Kawaler(1987a,b,c) succeeded to get some constraints on the physical quantities of some of pulsating white dwarfs.

Type
Part I. Chemical Peculiarities as Probe of Stellar Evolution
Information
International Astronomical Union Colloquium , Volume 108: Atmospherics Diagnostics of Stellar Evolution: Chemical Peculiarity, Mass Loss, and Explosion , 1988 , pp. 86 - 87
Copyright
Copyright © Springer-Verlag 1988

References

Kawaler, S. 1986, Ph.D. thesis, University of Texas at Austin.Google Scholar
Kawaler, S. 1987a, in Stellar Pulsation, ed. Cox, A.N., Sparks, W.M., and Starrfield, S.G. (Springer, Berlin), p.367.Google Scholar
Kawaler, S. 1987b, in IAU Symp. No.123, Advances in Helio- and Asteroseismolgy, ed. Christensen-Dalsgaard, J. (Reidel, Dordrecht), in press.Google Scholar
Kawaler, S. 1987c, in IAU Colloq. No. 95, The Second Conference on Faint Blue Stars, in press.Google Scholar
Sekii, T. and Shibahashi, H 1987, in Stellar Pulsation, ed. Cox, A.N., Sparks, W.M., and Starrfield, S.G. (Springer, Berlin), p.322.Google Scholar
Shibahashi, H. 1986, in Hydrodynamic and Magnetohydrodynamic Problems in the Sun and Stars, ed. Osaki, Y. (University of Tokyo, Tokyo), p.195.Google Scholar
Shibahashi, H. 1987, in IAU Symp. No.123, Advances in Helio- and Asleroseismology, ed. Christensen-Dalsgaard, J. (Reidel, Dordrecht), in press.CrossRefGoogle Scholar
Tassoul, M. 1980, Astrophys. J. Suppl, 43, 469.Google Scholar