Hostname: page-component-5c6d5d7d68-thh2z Total loading time: 0 Render date: 2024-08-29T13:28:34.047Z Has data issue: false hasContentIssue false
  • English
  • Français

On the Origin of Helium Rich Stars

Published online by Cambridge University Press:  12 April 2016

A. Tutukov
A. Tutukov*
Affiliation:
Astronomical Council of the USSR Academy of Sciences Pyatnitskaya St. 48 Moscow, USSR

Abstract:

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.

The modem theory of stellar evolution leads to several possible scenaria for the formation of many types of hydrogen deficient (usually helium rich) stars. Some of these scenaria are briefly discussed in this paper to provide possible explanations for origins of R Cr B, hot helium and Wolf-Rayet stars; hot sub dwarfs, non-DA degenerate dwarfs and helium stars in binaries like KS Per. The merger of two degenerate stars in close binaries due to the radiation of gravitational waves can lead to several types of helium and carbon rich stars as well as to supernova explosions.

Type
IX Theory
Information
International Astronomical Union Colloquium , Volume 87: Hydrogen Deficient Stars and Related Objects , 1985 , pp. 483 - 487
Copyright
Copyright © Reidel 1986

References

Beaudet, G., Salpeter, E.E. 1969, Ap.J. 155, 203.Google Scholar
Greenstein, J.L., Sargent, A.I. 1974, Ap.J. Suppl. 28, 157.Google Scholar
Heber, U. 1985, Astron. Astrophys. (in press).Google Scholar
Iben, I. Jr., Tutukov, A.V. 1985, Ap.J. Suppl. 58, 661.Google Scholar
Iben, I. Jr., Tutukov, A.V. 1986, Ap.J. (in press).Google Scholar
Tutukov, A.V., Yungelson, L.R. 1979, Acta. Astr. 29, 665.Google Scholar
Warner, B. 1967, Mon. Not. R. astr. Soc. 137, 113.Google Scholar