Walraven observations of the April 1987 superoutburst of the eclipsing dwarf nova Z Chamaeleontis

Details Walraven observations of the April 1987 superoutburst of the eclipsing dwarf nova Z Chamaeleontis Walraven observations of the April 1987 superoutburst of the eclipsing dwarf nova Z Chamaeleontis

Dec 1991

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991a%26a...252..605k&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 252, no. 2, Dec. 1991, p. 605-617. Research supported by NWO.

Astronomy and Astrophysics

Astrophysics

14

Accretion Disks, Eclipsing Binary Stars, Light Curve, Novae, Stellar Spectrophotometry, Cataclysmic Variables, Dwarf Stars, Mass Transfer

Scientific paper

Optical (3200 A - 6000 A) photometry of the SU Ursae Majoris type dwarf nova Z Chamaeleontis are made during the superoutburst in April 1987. The rise to maximum of the precursor is wavelength-dependent. During the precursor a large pre-eclipse dip develops in the orbital light curve, stretching from orbital phase of about 0.6 to about 0.9 (eclipse is identical to phase 0.0). The dip is strongest at the shortest wavelengths. It may be caused by an occultation of the inner parts of the accretion disk. At the end of the precursor the mean (out-of-eclipse and out-of-dip) fluxes decrease. The decrease is largest at the shortest wavelengths. This may signify a wavelength-dependent rise to the second (main) part of the superoutburst. After the precursor has ended, the well-known superhumps appear, which become less prominent as the outburst proceeds. The large dip before eclipse, now occurring between orbital phases 0.6 and 0.8, also gradually declines in prominence throughout the superoutburst. Various features in the light curves are described which were also found in several other SU UMa systems during superoutburst.

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