Other
Scientific paper
Sep 2001
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001aca....51..279s&link_type=abstract
Acta Astronomica, v.51, pp.279-293, (2001).
Other
22
Binaries: Eclipsing, Novae, Cataclysmic Variables, Stars: Individual: U Gem
Scientific paper
Radial velocities measured from peaks of the emission lines (Smak 1976, Stover 1981), analyzed within the three-body approximation, give K_1 consistent with that measured directly from the absorption lines of the white dwarf (Long and Gilliland 1999). This implies that the three-body approximation is essential for correct description of the outer parts of the disk. Wings of the emission lines profiles are likely to be contaminated by contributions from parts of the stream which are overflowing the disk close to the white dwarf. Radial velocities measured from wings (Kraft 1962, Stover 1981), analyzed only in phase intervals free of contamination, give K_1 consistent with other determinations. New analysis of the spot eclipses gives i=69 arcdeg+/-2 arcdeg and shows that during outburst the disk expands up to about r_d approx 0.40 - 0.45 approx 0.9 r_Roche, while during quiescence it contracts from r_d approx 0.75 r_Roche to r_d approx 0.65 r_Roche. However, the radius of the disk during quiescence obtained from V_d sin i appears larger: r_d approx 0.85 - 0.95 r_Roche. System parameters are: M_1=1.07 +/- 0.08 M_odot, M_2=0.39 +/- 0.02 M_odot, R_1=4.7 +/- 0.7 times 10^8 cm, R_2=0.45 +/- 0.01 R_odot, and distance d=96 +/- 4 pc. The radius of the secondary component, when compared with its mass, shows that the secondary is a normal main sequence star.
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