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An unexpectedly slow evolution in the pre-optical-maximum phase was suggestedin the very short recurrence period nova M31N 2008-12a. To obtain reasonablenova light curves we have improved our calculation method by consistentlycombining optically thick wind solutions of hydrogen-rich envelopes with whitedwarf (WD) structures calculated by a Henyey-type evolution code. The wind massloss rate is properly determined with high accuracy. We have calculated lightcurve models for 1.2 and 1.38 M_sun WDs with mass accretion rates correspondingto recurrence periods of 10 and 1 yr, respectively. The outburst lasts 590/29days in which the pre-optical-maximum phase is 82/16 days, for 1.2/1.38 M_sun,respectively. Optically thick winds start at the end of X-ray flash and ceaseat the beginning of supersoft X-ray phase. We also present supersoft X-raylight curves including a prompt X-ray flash and later supersoft X-ray phase.

A Self-Consistent Model for a Full Cycle of Recurrent Novae -- Wind Mass Loss Rate and X-Ray Luminosity