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A Beat Phenomenon in Dwarf Nova Eruptions

Published online by Cambridge University Press:  12 April 2016

N. Vogt
N. Vogt*
Affiliation:
European Southern Observatory, Casilla 16317, Santiago 9, Chile

Extract

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Photoelectric observations of the dwarf nova VW Hyi, obtained at the end of the December 1975 supermaximum, are presented. After decline from the outburst, the superhump period (0ḍ07622) combines with the orbital period (0ḍ07427) to a beat phenomenon: the O-C’s and the light curves of the orbital hump vary systematically with the phase of the beat period for at least one week after recovery from the supermaximum. It is suggested that the red secondary component, which rotates non-synchroneously with the superhump period, expands slightly at the beginning of a supermaximum and is heated up asymmetrically, probably due to instabilities in its convection zone. In addition, the increased mass transfer rate may trigger the long eruption in the accretion disc while short eruptions originate in the disc without participation of the secondary.

Type
Part II: Cataclysmic Variables
Information
International Astronomical Union Colloquium , Volume 42: The Interaction of Variable Stars with their Environment , 1977 , pp. 227 - 233
Copyright
Copyright © Veröff. Der Remeis-Sterwarte 1977

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