The dwarf nova Z Chamaeleontis. I - Photometry

Details The dwarf nova Z Chamaeleontis. I - Photometry The dwarf nova Z Chamaeleontis. I - Photometry

Jun 1979

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1979mnras.187..645b&link_type=abstract

Monthly Notices of the Royal Astronomical Society, vol. 187, June 1979, p. 645-653.

Other

69

Astronomical Photometry, Eclipsing Binary Stars, Light Curve, White Dwarf Stars, Brightness, Stellar Luminosity, Stellar Mass Ejection, Telescopes, Time Dependence

Scientific paper

High-speed photometric observations of the dwarf nova Z Cha are presented. The eclipse light curves clearly show the presence of two eclipsed objects which are identified with the white dwarf, and the bright spot on the edge of the accretion disk. The mid-point of the white dwarf eclipse yields a precise eclipse timing, an order of magnitude more accurate than is possible in any other eruptive binary system. The white dwarf eclipse duration has been used to derive a relationship between q and i. The bright spot is found to be variable in brightness on both long and short time-scales and also varies in position.

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