The eclipses of cataclysmic variables. II - U Geminorum

Details The eclipses of cataclysmic variables. II - U Geminorum The eclipses of cataclysmic variables. II - U Geminorum

Oct 1987

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987apj...321..813z&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 321, Oct. 15, 1987, p. 813-821.

Statistics

Computation

35

Cataclysmic Variables, Dwarf Novae, Eclipsing Binary Stars, Light Curve, Radial Velocity, Stellar Mass Accretion, Computational Astrophysics, High Temperature, Roche Limit, Stellar Luminosity, Ultraviolet Spectra, White Dwarf Stars

Scientific paper

U Gem is an eclipsing dwarf nova with an orbital period of 4 h 15 m. High-speed, multicolor photometric observations of U Gem in its quiescent state were obtained. A program was used that synthesizes the light curves of cataclysmic variables to derive the properties of U Gem from its eclipses. Using radial velocity curves published by Wade (1981) and by Stover (1981), it was found that i = 69.7 + or - 0.7 deg, M1 = 1.12 + or - 0.13 solar masses, and M2 = 0.53 + or - 0.06 solar mass. The radial temperature distribution across the accretion disk in U Gem shows that the disk is a hollow ring around the white dwarf with R(out) = 0.30 + or - 0.04 and R(in) = 0.12 + or - 0.05 a, where a is the separation of the two stars. The temperature of the ring is 4800 + or - 300 K. The model also reproduces the published infrared light curves and ultraviolet spectral distributions of U Gem. A mass transfer rate of 7.8 x 10 to the -10th solar mass/yr is derived. The structure of the ring around the white dwarf is consistent with the current theories of accretion disk instabilities in dwarf novae.

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