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Title:
Energy distributions of symbiotic novae
Authors:
Bryan, Greg L.; Kwok, Sun
Affiliation:
AA(Calgary, University, Canada), AB(Joint Institute for Laboratory Astrophysics, Boulder, CO)
Publication:
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 368, Feb. 10, 1991, p. 252-260. Research supported by NSERC. (ApJ Homepage)
Publication Date:
02/1991
Category:
Astrophysics
Origin:
STI
NASA/STI Keywords:
Infrared Spectra, Novae, Spectral Energy Distribution, Symbiotic Stars, Asymptotic Giant Branch Stars, Emission Spectra, Infrared Astronomy Satellite, Iue, Radiative Transfer, Stellar Envelopes
DOI:
10.1086/169688
Bibliographic Code:
1991ApJ...368..252B

Abstract

The IRAS low-resolution spectra of three recent symbiotic novae are fitted with a dust continuum radiative transfer model. It is found that the dust shells are detached from the photosphere and that the sizes of the inner radii are correlated with times since outburst. An analysis of the IUE spectra of HM Sge at different epochs suggests that the strength of the 2200 A feature is decreasing with times and the grains responsible for the feature are probably formed in the white dwarf ejecta. A complete accounting of the entire energy budget from radio to X-ray shows that most of the energy is emitted by the cool component in the infrared, and a significant fraction of the flux of the hot component is escaping in the far-ultraviolet. The density-bounded nature of the circumstellar gas nebulae could be the result of a bipolar geometry of the nebulae. Unlike classical novae, the optical outburst of symbiotic novae is due to the ionization of the preexisting envelope of the cool component and is not the result of a sudden ejection by the hot component.

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