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The Long Term Behaviour of Classical Old Novae

Published online by Cambridge University Press:  12 April 2016

A. Bianchini
A. Bianchini*
Affiliation:
Osservatorio Astronomico, 35100-Padova, Italy

Abstract

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Quiescent novae are more stable against mass transfer rate than dwarf novae. They may however show cyclical variations of their quiescent magnitudes on time scales of years, probably caused by solar–type cycles of activity of the secondary. The probability density function of the periods of the cycles observed in CVs is similar to that for single stars. Sometimes, periodic or quasi periodic light variations on time scales of tens to hundreds of days are also observed. Although the magnitudes of prenovae and postnovae are essentially the same, the definition of the magnitude of a quiescent nova is still uncertain. At present, the hibernation theory for old novae seems to be supported only by the observations of two very old novae.

Type
1a. Basic Properties of Novae
Information
International Astronomical Union Colloquium , Volume 122: Physics of Classical Novae , 1990 , pp. 13 - 23
Copyright
Copyright © Springer-Verlag 1990

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