An infrared and visual study of the structure and variability of the cataclysmic binary V2051 Ophiuchi

Details An infrared and visual study of the structure and variability of the cataclysmic binary V2051 Ophiuchi An infrared and visual study of the structure and variability of the cataclysmic binary V2051 Ophiuchi

Oct 1986

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986mnras.222..871b&link_type=abstract

Monthly Notices of the Royal Astronomical Society (ISSN 0035-8711), vol. 222, Oct. 15, 1986, p. 871-893. SERC-supported research

Astronomy and Astrophysics

Astronomy

12

Cataclysmic Variables, Dwarf Novae, Eclipsing Binary Stars, Infrared Astronomy, Stellar Structure, Visible Spectrum, Accretion Disks, Brown Dwarf Stars, Main Sequence Stars, Red Dwarf Stars, Stellar Flares

Scientific paper

The quiescent phase of V2051 Oph is characterized on the basis of photometric observations obtained in H and JHK with the 4.5-m MMT on Apr. 16-17, 1984; in HK with the 3.9-m UKIRT on Apr. 26, 1984; and in UH with the 3.9-m AAT on Apr. 27, 1985. The data and the results of eclipse simulations are presented in extensive tables and graphs and discussed. Nearly sinuosidal optically thin light-curve humps are attributed to disk-temperature (or hotter) material near the white dwarf. These humps (along with superimposed rapid, optically thick, 8000-K flares) are shown to explain most of the gross variability of the accretion-disk eclipses. A model with an optically thin accretion disk and a normal main-sequence red dwarf secondary and an alternative model with an opaque disk and a 2000-K brown dwarf (implying a distance of 110 pc or less) are considered.

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