High-speed photometry of Z Chamaleontis during outbursts

Details High-speed photometry of Z Chamaleontis during outbursts High-speed photometry of Z Chamaleontis during outbursts

Aug 1988

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1988mnras.233..705w&link_type=abstract

Monthly Notices of the Royal Astronomical Society (ISSN 0035-8711), vol. 233, Aug. 15, 1988, p. 705-738. Research supported by t

Astronomy and Astrophysics

Astronomy

56

Accretion Disks, Astronomical Photometry, Dwarf Novae, Eclipsing Binary Stars, Light Curve, Stellar Flares, Correlation, Infrared Photometry, Maximum Entropy Method, White Dwarf Stars

Scientific paper

High-speed white-light photometry of the dwarf nova Z Cha at time resolutions of 4 or 5 s is presented for six supermaxima and one ordinary maxima during the period 1973-1984. It is found that at early stages of the superoutburst, the source of the superhump light is partially eclipsed by the secondary star. Therefore the source of the this light is not a bright spot on the secondary. Synthetic light curves are computed to assist in locating the source of the superhump light and simulations are obtained by modulating the intensity of a bright ring at the outer edge of the disk at the superhump period. MEM deconvolution of eclipse light curves is used to discuss the structural changes that take place during a superoutburst. The observed light curve shows unusual dips at maximum light at phases 0.25 and 0.75. At the end of superoutburst, it is found that the disk has almost completely disappeared, leaving a central source whose size is only that of a few white dwarf radii.

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