Eclipses in Cataclysmic Variables with Stationary Accretion Disks. V. RW Tri

Details Eclipses in Cataclysmic Variables with Stationary Accretion Disks. V. RW Tri Eclipses in Cataclysmic Variables with Stationary Accretion Disks. V. RW Tri

Jan 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995aca....45..259s&link_type=abstract

Acta Astronomica, v.45, pp.259-277, (1995).

Astronomy and Astrophysics

Astronomy

11

Binaries: Eclipsing, Novae: Cataclysmic Variables, Stars: Individual: Rw Tri

Scientific paper

New B, V light curves of RW Tri were obtained in September 1994. No major variations in the maximum brightness or in the shape of eclipse occurred during the time interval covered by these observations. An inspection of all available light curves of RW Tri shows that they belong to the peculiar type: in the phase interval, where the hot spot hump should normally be present, they are either flat or even show a depression. This indicates strong absorption effects due to circumdisk material located predominantly around the hot spot region. Light curves observed in 1994 were decomposed into their disk and spot components using a procedure involving a simple formula for the phase dependence of the absorption effects. The resulting spot light curves are well defined, showing the spot eclipse, and allowing the determination of the phases of its ingress and -- at least in some cases -- of its egress. The analysis of the disk and spot eclipses based on the mean B and V light curves, together with the value of K_1 (Kaitchuck et al. 1983), gave the following system parameters: M_1=(0.45pm0.15)Modot, M_2=(0.63pm0.10)Modot, A=(1.13pm0.13)times1011 cm, i=70.^d5pm2.5, R_d/A=0.25pm0.03, dot M=(4.0pm2.0)times1017 g/s, and the distance d=270pm40 pc. The disk eclipse is partial. Long-term variations of RW Tri in 1957 (Walker 1963) were rediscussed and shown to be due to variations in the mass-transfer/accretion rate.

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