Hostname: page-component-848d4c4894-nr4z6 Total loading time: 0 Render date: 2024-05-17T22:36:32.463Z Has data issue: false hasContentIssue false
  • English
  • Français

Spectra of Symbiotic Stars

Published online by Cambridge University Press:  12 April 2016

Hagai Netzer ,
Elia M. Leibowitz  and
Gary Ferland
Hagai Netzer
Affiliation:
Department of Physics and Astronomy and the Wise Observatory, Tel Aviv University
Elia M. Leibowitz
Affiliation:
Department of Physics and Astronomy and the Wise Observatory, Tel Aviv University
Gary Ferland
Affiliation:
Department of Physics, University of Kentucky, Lexington

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.

We have observed Z And and other symbiotic stars at the Wise Observatory and have obtained absolute flux measurements of many emission lines. Preliminary analysis of the data shows that the line emitting gas is probably photoionized by a hot, T* ≳ 200,000 OK continuum, which can explain the extremely strong Hell lines. The hydrogen Balmer line intensities are different from what is predicted by recombination theory and the optical depths in Hα and Hβ must be significant. Our photoionization model can be used to deduce the geometry, density and temperature of the line emitting gas, and the nature of the hot companion.

Type
Research Article
Information
International Astronomical Union Colloquium , Volume 72: Cataclysmic Variables and Related Objects , 1983 , pp. 35 - 40
Copyright
Copyright © Reidel 1983

References

REFERENCES

Altamore, A., Baratta, G.B., Cassatella, A., Friedjung, M., Giangrande, A., Ricciardi, O. and Viotti, R., 1981, Ap. J. 245, 630 CrossRefGoogle Scholar
Ferland, G. and Netzer, H., 1979, Ap. J. 229, 274 CrossRefGoogle Scholar
Netzer, H., 1975, M.N.R.A.S. 171, 395 CrossRefGoogle Scholar
Nussbaumer, H. and Storey, P.J., 1982 (preprint) Google Scholar
Williams, R.E., 1971, Ap. J. Lett. 167, 27 Google Scholar