Abstract
We observed V1974 Cygni with a CCD camera attached to the 1-m telescope of the Wise Observatory for 32 nights during the years 1994 and 1995. The two periodicities identified in the light curve, 0.0812585 day 1.95 hours and 0.085 d P..1 2.04 hr, are interpreted as the orbital period of the binary system and a superhump period, respectively. These results and the interpretation imply that no later than 2.5 years after the outburst of the nova an accretion disk is present in the nova stellar system. They also imply that the disk is in the state of “permanent superhump”. Using the precessing disk model of the superhump phenomenon and utilizing additional published observational results we estimate a mass of 0.75–1.07 M⊙ for the white dwarf in this nova system.
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