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Mass Loss Associated with X-Ray Bursts of Neutron Stars*

Published online by Cambridge University Press:  12 April 2016

D. Sugimoto ,
T. Ebisuzaki ,
T. Hanawa  and
M. Kato
D. Sugimoto
Affiliation:
Department of Earth Science and Astronomy, College of General Education, University of Tokyo
T. Ebisuzaki
Affiliation:
Department of Earth Science and Astronomy, College of General Education, University of Tokyo
T. Hanawa
Affiliation:
Department of Earth Science and Astronomy, College of General Education, University of Tokyo
M. Kato
Affiliation:
Department of Earth Science and Astronomy, College of General Education, University of Tokyo

Extract

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Basic features of observed Type I X-ray bursts are thought to be interpreted in terms of helium shell-flash near the surface of the accreted neutron stars (Lewin and Joss 1981). Numerical models of the helium shell-flash show that the luminosity grows very close to the Eddingotn luminosity just after the peak of energy generation.

Type
Research Article
Information
International Astronomical Union Colloquium , Volume 72: Cataclysmic Variables and Related Objects , 1983 , pp. 293 - 298
Copyright
Copyright © Reidel 1983

Footnotes

*

Details of this work are submitted for publication by Ebisuzaki et al. (1982) and by Kato (1982).

References

Ebisuzaki, T., Hanawa, T., and Sugimoto, D. 1982, submitted for publication to Publ. Astron. Soc. Japan.Google Scholar
Kato, M. 1982, submitted for publication to Publ. Astron. Soc. Japan.Google Scholar
Lewin, W.H.G., and Joss, P.C. 1981, Space Sci. Rev., 28, 3.Google Scholar
Ruggles, C.L.N., and Bath, G.T. 1979, Astron. Astrophys., 80, 97.Google Scholar
Zytkow, A. 1972, Acta Astron., 22, 103.Google Scholar