Observations of Eclipsing Dwarf Novae

Details Observations of Eclipsing Dwarf Novae Observations of Eclipsing Dwarf Novae

Feb 1987

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987ap%26ss.130...81w&link_type=abstract

Astrophysics and Space Science, Volume 130, Issue 1-2, pp. 81-83

Astronomy and Astrophysics

Astrophysics

3

Scientific paper

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. The length of ingress and egress in the primary eclipse, constrains the radius of the central object relative to the orbital separation. The shape of this eclipse and the temperature of the central objects in z Cha, OY Car and HT Cas imply that the measured

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