Abstract
The mass-loss process during nova outbursts is studied for a 1.3 solar mass white dwarf. A sequence consisting of steady mass-loss solutions and static solutions for the dwarf are constructed, and the mass accmulation ratio is calculated using this sequence. The amount of processed helium is estimated, and the accumulation ratio is determined for the case of infinitely large sizes of the Roche lobe. It is found that a complete nova cycle for such a dwarf is followed by a sequence consisting of static and steady mass-loss solutions. Once a hydrogen shell flash occurs, an optically thick wind always follows it. The occurrence of the wind is independent of the initial envelope mass. The mass accumulation ratio depends on the mass transfer rate from the companion. If the size of the outer critical Roche lobe is as small as as few solar radii or less, the mass accumulation ratio depends also on the Roche lobe size.
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