THE ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES, 113:121, 1997 November

               OPTICALLY THICK WINDS FROM DEGENERATE DWARFS. I.
                    CLASSICAL NOVA OF POPULATIONS I AND II

                                  MARIKO KATO
  Department of Astronomy, Keio University, Kouhoku-ku, Yokahoma, 223 Japan;
                           mariko@educ.cc.keio.ac.jp

                                   ABSTRACT

        Twenty-six sequences of optically thick wind solutions have been
     calculated which mimic the 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 (>= 0.8Msun).  The old population novae show the slow light
     curve, the long X-ray turn-off time, the small expansion velocity and
     the small wind mass-loss rate. The X-ray turn-off 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 Msun for GQ Mus and ~1.0 Msun for
     V1974 Cyg.  The systematic difference of the wind velocity is
     predicted between novae in globular clusters and in galactic disk.
        Twenty-six tables are presented in the computer readable form of
     CD-ROM that consists of solutions of the optically thick wind and the
     static for the decay phase of classical novae with composition of
     X=0.35, C=0.1 and O=0.2 and heavy elements content Z=0.001, 0.004,
     0.02, 0.05 and 0.1 for the white dwarf masses of 0.4, 0.6, 0.7, 0.8,
     0.9, 1.0, 1.2 and 1.35 Msun. These tables list the characteristic
     values of the envelope such as the photospheric temperature, the
     velocity, the wind mass-loss rate and fluxes of four wavelength bands.
     The updated OPAL opacity (1996) is used.

     Subject headings: novae, cataclysmic variables -- stars: evolution --
                       stars: interior -- stars: mass-loss -- white dwarfs
                       -- X-rays: stars