Hostname: page-component-78c5997874-94fs2 Total loading time: 0 Render date: 2024-11-02T20:19:07.394Z Has data issue: false hasContentIssue false
  • English
  • Français

Discovery of the sixth DBV Star: CBS 114

Published online by Cambridge University Press:  12 April 2016

D. E. Winget  and
C. F. Claver
D. E. Winget
Affiliation:
McDonald Observatory and Department of Astronomy, The University of Texasat Austin
C. F. Claver
Affiliation:
McDonald Observatory and Department of Astronomy, The University of Texasat Austin

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.

Though widely spread across the H-R diagram the compact pulsators have much in common. All are multi-periodic, and most have extremely complex light curves. All appear to be pulsating in nonradial g-modes, with temperature variations responsible for the bulk of the light modulations. The g-modes are global in nature and, typically, many are excited in each pulsator, so they are a rich source of seismological information about the interior regions of the white dwarf stars.

The pulsating DB white dwarf stars (DBV’s) form one of the three distinct classes of pulsating compact objects currently known. We find these classes nearly uniformly distributed in log Te spanning virtually the whole range of the white dwarf cooling sequence, from the hot DOV stars at log Te ~ 5 to the DAV (ZZ Ceti) stars at log Te ~ 4; the DBV stars, with logTe ~ 4.5, fall in the middle.

Type
Research Article
Information
International Astronomical Union Colloquium , Volume 114: White Dwarfs , 1989 , pp. 290 - 292
Copyright
Copyright © Springer-Verlag 1989

References

Pesch, P., and Sanduleak, N. 1986, Ap. J. Suppl, 60, 543.Google Scholar
Wagner, R.M., Sion, E.M., Liebert, J., Starrfield, S.G. 1988, Ap. J., 328, 213.Google Scholar
Winget, D.E., Seismological Investigations of Compact Stars, in Advances in Helio- and Asteroseismology, eds. Christensen, J. and Frandsen, S. (Copywrite 1988 by the IAU.).Google Scholar