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Seismic Inversions for White Dwarf Stars

Published online by Cambridge University Press:  12 April 2016

M. Takata  and
M.H. Montgomery
M. Takata
Affiliation:
Institute of Astronomy, Madingley Road, Cambridge CB3 0HA, UK
M.H. Montgomery
Affiliation:
Institute of Astronomy, Madingley Road, Cambridge CB3 0HA, UK

Abstract

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Inversion methods have been used successfully for the Sun. The stars with the next richest set of observed frequencies are the white dwarfs. We consider here the viability of numerical inversions for these stars. We find that, while the number of presently observed modes in the white dwarf GD 358 is too small for structural inversions, such inversions would be possible if the frequencies of all modes with 1 ≤ l ≤ 3 were observed. This is possible for space observations by e.g. Eddington.

Type
Part 6. Asteroseismology from Space and from the Ground
Information
International Astronomical Union Colloquium , Volume 185: Radial and Nonradial Pulsations as Probes of Stellar Physics , 2002 , pp. 606 - 607
Copyright
Copyright © Astronomical Society of the Pacific 2002

References

Gough, D.O., 1996, In The Structure of the Sun, ed. Cortes, T.R. & Sánchez, F. (Cambridge: Cambridge University Press), 141 Google Scholar
Kawaler, S.D., Sekii, T., & Gough, D.O., 1999, ApJ, 516, 349 CrossRefGoogle Scholar
Montgomery, M.H., Winget, D.E., 1999, ApJ, 526, 976 Google Scholar
Shibahashi, H., Sekii, T., & Kawaler, S.D., 1988, in Atmospheric Diagnostics of Stellar Evolution: Chemical Peculiarity, Mass Loss, And Explosion, IAU Colloq. No. 108, ed. K.Nomoto, (Berlin: Springer-Verlag), 86 CrossRefGoogle Scholar