J/ApJS/113/121 J/ApJS/113/121 Optically thick winds from degenerate dwarfs. I. M Kato Astrophys. J. Suppl. Ser. 113 121 1997 1997ApJS..113..121K Novae Models, evolutionary novae, cataclysmic variables stars: evolution stars: interior stars: mass-loss white dwarfs X-rays: stars 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 (>=0.8M_{sun}_). 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 ~0.6M_{sun}_ for GQ Mus and ~1.0M_{sun}_ 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 1.35M_{sun}_. 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 (Iglesias & Rogers, 1996ApJ...464..943I) is used.

Table Table number (in the printed paper) --- Model Model name --- MassWD White dwarf mass solMass Z Heavy elements content --- RowWS Number of rows of (wind + static) solutions --- RowTot Number of rows total --- MassWD White dwarf mass solMass Z Heavy elements content --- log(Tph) Photospheric temperature [K] log(Lph) Photospheric luminosity [10-7W] log(Rph) Photospheric radius [solRad] log(Vph) Photospheric velocity [cm/s] log(Menv) Envelope mass [solMass] log(dM/dtw) Mass loss rate due to optically thick wind (log dM/dt (wind)) [solMass/yr] log(dM/dtn) Mass loss rate due to Hydrogen nuclear burning (log dM/dt (nuc)) [solMass/yr] Radcr Radius at the critical point solRad Velcr Velocity at the critical point cm/s time Evolutional time yr Mbol Bolometric magnitude mag Mvis Visual magnitude mag log(FUV) Flux in UV (912.3250{AA}) log(FNN) = log(L_NN_/4{pi}D^2^), D=1.0 kpc (NN=UV, EUV or SSXR) For log(FSSXR), values less than -30.000 are listed as just -30.000. [solLum/kpc2] log(FEUV) Flux in EUV (100.912{AA}) [solLum/kpc2] log(FSSXR) Flux in supersoft X-ray (30.100{AA}) [solLum/kpc2] UNKNOWN 1998Feb06 J_ApJS_113_121.xml