High-speed photometry of Z Chamaeleontis in the quiescent state

Details High-speed photometry of Z Chamaeleontis in the quiescent state High-speed photometry of Z Chamaeleontis in the quiescent state

Apr 1984

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984mnras.207..705c&link_type=abstract

Monthly Notices of the Royal Astronomical Society (ISSN 0035-8711), vol. 207, April 15, 1984, p. 705-729.

Astronomy and Astrophysics

Astronomy

70

Dwarf Novae, Light Curve, Starspots, Stellar Mass Accretion, Stellar Spectrophotometry, Stellar Structure, Accretion Disks, Mass Ratios, Orbital Elements, Radial Velocity, Stellar Motions, White Dwarf Stars

Scientific paper

High-speed photometry of the dwarf nova Z Cha is presented. The total duration of the primary eclipse implies a lower limit of about 0.51 + or - 0.08 solar mass for the mass of the white dwarf. The eclipse of the hotspot is more pronounced in comparison with previous observations, and shows at least two types of structure. Using the relationship between the mass ratio and inclination in this system, together with theoretical stream trajectories, it is found that a mass ratio of between 5 and 7 is required to explain the phasing of the hotspot eclipse relative to the primary eclipse. The hotspot varies in size and location in the disc, but always indicates an outer radius for the accretion disc/ring which is about twice that of theoretical inviscid discs. The mass ratio limits, coupled with limitations on the size of the central source, indicate that the central source may have a disc component. It is found that, on occasion, the hotspot extends into the innermost regions of the accretion disc indicating that the stream thickness is, at times, larger than that of th outer disc. It is suggested that these extended hotspots have consequences for the interpretation of radial velocity measurements from the wings of emission lines.

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