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The Hot Winds of Novae

Published online by Cambridge University Press:  12 April 2016

Peter H. Hauschildt ,
S. Starrfield ,
E. Baron  and
F. Allard
Peter H. Hauschildt
Affiliation:
Department of Physics & Astronomy, Arizona State University, Tempe, AZ 85287
S. Starrfield
Affiliation:
Department of Physics & Astronomy, Arizona State University, Tempe, AZ 85287
E. Baron
Affiliation:
Department of Physics & Astronomy, University of Oklahoma, Norman, OK 73019-0225
F. Allard
Affiliation:
Department of Physics, Wichita State University, Wichita, KS 67260-0032

Abstract

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We discuss the physical effects that are important for the formation of the late wind spectra of novae. Nova atmospheres are optically thick, rapidly expanding shells with almost flat density profiles, leading to geometrically very extended atmospheres. We show how the properties of nova spectra can be interpreted in terms of this basic model and discuss some important effects that influence the structure and the emitted spectrum of nova atmospheres, e.g., line blanketing, NLTE effects, and the velocity field. Most of the radiation from hot nova winds is emitted in the spectral range of the EUVE satellite. Therefore, we present predicted EUVE spectra for the later stages of nova outbursts. Observations of novae with EUVE could be used to test our models for the nova outburst.

Type
VIII. Novae, X-ray Binaries
Information
International Astronomical Union Colloquium , Volume 152: Astrophysics in the Extreme Ultraviolet , 1996 , pp. 413 - 417
Copyright
Copyright © Kluwer 1996

References

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