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The Outburst of Symbiotic Novae

Published online by Cambridge University Press:  07 August 2017

H. Nussbaumer
H. Nussbaumer*
Affiliation:
Institute of Astronomy ETH-Zentrum CH-8092 Zürich Switzerland

Abstract

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We present the basic properties of symbiotic novae, and show how they differ from classical novae. Differences are observationally particularly noticeable in the luminosity curve, the rise of which is much slower, but its return to pre-outburst level takes much longer than in classical novae. Special emphasis is given to the intial phase, for which two different evolutionary paths have been observed. The outburst may lead into a supergiant phase lasting for several years, which is being followed by the nebular phase, or it may lead straight into the nebular phase. The total energy radiated during an outburst is at least as large as the energy loss of classical novae. Mass-loss during outburst may be sufficiently small to lead eventually to a supernova on the white dwarf.

Type
Oral and Contributed Papers
Information
Symposium - International Astronomical Union , Volume 151: Evolutionary Processes in Interacting Binary Stars , 1992 , pp. 429 - 433
Copyright
Copyright © Kluwer 1992 

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