Spectrophotometry of the eclipsing dwarf novae V2051 Ophiuchi

Details Spectrophotometry of the eclipsing dwarf novae V2051 Ophiuchi Spectrophotometry of the eclipsing dwarf novae V2051 Ophiuchi

Jun 1985

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985esasp.236...55w&link_type=abstract

In ESA Recent Results on Cataclysmic Variables p 55-59 (SEE N86-20287 10-93)

Computer Science

Accretion Disks, Dwarf Novae, Stellar Spectrophotometry, Stellar Mass, Stellar Mass Accretion, Stellar Spectra, Stellar Temperature, White Dwarf Stars

Scientific paper

An optical and UV spectrophotometric study of the eclipsing dwarf nova V2051 Oph is presented. The optical and UV spectra are typical of a dwarf nova at quiescence. The observed semiamplitude K1=111 km/sec with a crossing at phase 0.13. This anomalous phase can be reproduced by an asymmetric disk with the trailing lune brighter by 60% than the leading lune. This yields a revised K1=91 km/sec and implies a white dwarf mass of 0.43 M and a companion of mass 0.11 M and radius 0.15 R. The UV to optical continuum can be well fitted by a steady-state optically thick disk model with a turnover at 2500A. If this is related to the maximum temperature of the accretion disk then the system parameters are: maximum disk temperature of 15,500K, M dot = 1.3 times 10 to the minus 10th power M/yr, and distance between 90 and 150 pc.

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