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Helium Shell-Flashes in Accreting White Dwarfs

Published online by Cambridge University Press:  12 April 2016

M. Y. Fujimoto  and
D. Sugimoto
M. Y. Fujimoto
Affiliation:
Takada Branch, Faculty of Education, Niigata University
D. Sugimoto
Affiliation:
Department of Earth Science and Astronomy, College of General Education, University of Tokyo

Extract

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When gas is accreted onto a carbon-oxygen white dwarf, a hydrogen shell-flash is triggered. Recently such phenomena are studied by many authors in relation to nova explosions and rekindling of white dwarfs. Unless all of the accreted gas is ejected by the process of the nova, a helium zone is formed as a result of hydrogen shell-burning. As the hydrogen shell-flashes recur many times, the helium zone grows gradually in mass. Then the helium shell-flash will be ignited as in the deep interior of ordinary red giant stars. We have investigated such process, simulating it by helium accretion at a constant rate. In the present paper we show that the helium shell-flashes result in a variety of strengths depending upon situations.

Type
Colloquium Session IV
Information
International Astronomical Union Colloquium , Volume 53: White Dwarfs and Variable Degenerate Stars , August 1979 , pp. 285 - 289
Copyright
Copyright © The University of Rochester 1979

References

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