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Observations of Eclipsing Dwarf Novae

Published online by Cambridge University Press:  12 April 2016

J. Wood
J. Wood*
Affiliation:
Institute of Astronomy, Cambridge, U.K.

Abstract

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High Speed Photometry of four eclipsing dwarf novae, Z Cha, OY Car, HT Cas and IP Peg, is used to determine the orbital parameters and the masses of the two stars in each system. The mass ratio, q, and inclination, i, are found by constraining theoretical stream trajectories (Lubow and Shu 1975) to pass through the observed light centre of the bright spot eclipse. The light centre is defined as the point corresponding to the half flux points in the ingress and egress of the eclipse of the compact part of the bright spot. The theoretical stream width indicates that the centre of the stream must intersect the bright spot close to this point.

Type
II. Radio, IR and Optical Observations
Information
International Astronomical Union Colloquium , Volume 93: Cataclysmic Variables: Recent Multi-Frequency Observations and Theoretical Developments , 1987 , pp. 81 - 83
Copyright
Copyright © Reidel 1987

References

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Wood, J.H., Borne, K.D., Wade, R.A., Berriman, G. 1987 Mon. Not. R. astr. Soc. in preparationGoogle Scholar