Hostname: page-component-cd9895bd7-q99xh Total loading time: 0 Render date: 2024-12-25T16:02:21.797Z Has data issue: false hasContentIssue false
  • English
  • Français

Models for R Coronae Borealis Stars

Published online by Cambridge University Press:  12 April 2016

P. Biermann  and
R. Kippenhahn

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.

If we believe in the spectral analysis of the atmospheres of RCrB stars these objects should have a pure helium envelope slightly enriched in carbon (SEARLE 1961, DANZIGER 1965). However, they cannot be homogeneous helium stars since in that case they should be on the helium main sequence in the Hertzsprung-Russell-diagram, whereas they are found in the region of late supergiants. Their internal chemical structure must therefore be more complicated than that of a homogeneous helium star. From the viewpoint of stellar evolution the next degree of complexity would be to have a carbon-oxygen core.

Type
I. New Phenomena in Very Cool, or Very Young, or Very Peculiar Variables
Information
International Astronomical Union Colloquium , Volume 15: New Directions and Frontiers in Variable Stars Research , 1971 , pp. 54 - 59
Copyright
Copyright © Cambridge University Press 1971

References

Baker, N., Kippenhahn, R., 1962, Z. f. A. 54, 114.Google Scholar
Beaudet, G., Petrostan, V., and Salpeter, E. E., 1967, Ap. J. 150, 979.Google Scholar
Biermann, P., and Kippenhahn, R., 1971, Astron. & Astroph. 14, 32.Google Scholar
Danziger, I. J., 1965, M. N. R. A. S. 130, 199.Google Scholar
Paczynski, B., 1971, Acta Astron. 21, 1.Google Scholar
Searle, L., 1961, Ap. J. 133, 531.Google Scholar
UUS, U., 1970, Nantchnije Informazii 17, 25.Google Scholar
Warner, B., 1967, M. N. R. A. S. 137, 119.Google Scholar