Optically Thick Winds from Degenerate Dwarfs. I. Classical Nova of Populations I and II

Twenty six sequences of optically thick wind solutions have calculated which mimic time-dependent evolution of classical novae of populations I and II. The peak of the new opacity around log T = 5:2 due to iron lines is found to be strong enough to accelerate the winds even in very low iron abundance such as Z=0.001 for massive white dwarfs ( 0:8M ). The old population novae show the slow light curve, the long X-ray turn-o time, the small expansion velocity and the small wind mass-loss rate. The X-ray turn-o time is a good indicator of the white dwarf mass because of its strong dependence on the white dwarf mass and weak dependence on the populations. The white dwarf mass is estimated to be 0:6 M for GQ Mus and 1:0M for V1974 Cyg. The systematic di erence of the wind velocity is predicted between novae in globular clusters and in