A theoretical light-curve model for the 1985 outburst of RS Ophiuchi

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Abstract
A theoretical light-curve model of the 1985 outburst of RS Ophiuchi is presented based on a thermonuclear runaway (TNR) model. The system consists of a very massive white dwarf (WD) with an accretion disk (ACDK) and a red giant (RG). The early phase of the V light curve is well reproduced only by the bloated WD photosphere of the TNR model on a 1.35 +/- 0.01 M_sun WD while the later phase is dominated both by the irradiated ACDK and by the irradiated RG underfilling the inner critical Roche lobe. The UV light curve is also well reproduced by the same model with the distance of 0.6 kpc to RS Oph. The envelope mass at the optical peak is estimated to be 2 x 10^{-6} M_sun, indicating a rather high mass accretion rate of 1.2 x 10^{-7} M_sun yr^{-1} between the 1967 and the 1985 outbursts. About 90% of the envelope mass is blown off in the outburst wind while the residual 10% (2 x 10^{-7} M_sun) has been left and added to the helium layer of the WD. The net increasing rate of the WD mass is 1.2 x 10^{-8} M_sun yr^{-1}. Thus, RS Oph is certainly a strong candidate for a Type Ia supernova progenitor.

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