J/ApJS/113/121 Optically thick winds from degenerate dwarfs. I. (Kato 1997)
Optically thick winds from degenerate dwarfs. I.
Classical nova of populations I and II
Kato M.
<Astrophys. J. Suppl. Ser. 113, 121 (1997)>
=1997ApJS..113..121K 1997ApJS..113..121K
ADC_Keywords: Novae ; Models, evolutionary
Keywords: novae, cataclysmic variables - stars: evolution - stars: interior -
stars: mass-loss - white dwarfs - X-rays: stars
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 (≥0.8M☉). 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☉ for GQ Mus and ∼1.0M☉
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☉. 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 1996ApJ...464..943I) is
used.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
header.dat 33 26 Overall model parameters for all tables
tables.dat 125 662 Envelope solutions for classical novae
(table1 to table26)
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Byte-by-byte Description of file: header.dat
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Field Format Units Label Explanations
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1- 2 I2 --- Table Table number (in the printed paper)
4-13 A10 --- Model Model name
14-18 F5.1 solMass MassWD White dwarf mass
19-25 F7.3 --- Z Heavy elements content
26-29 I4 --- RowWS Number of rows of (wind + static) solutions
30-33 I4 --- RowTot Number of rows total
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Byte-by-byte Description of file: tables.dat
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Bytes Format Units Label Explanations
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1- 4 F4.2 solMass MassWD White dwarf mass
6- 10 F5.3 --- Z Heavy elements content
12- 17 F6.3 [K] log(Tph) Photospheric temperature
20- 25 F6.3 [10-7W] log(Lph) Photospheric luminosity
28- 33 F6.3 [solRad] log(Rph) Photospheric radius
35- 40 F6.3 [cm/s] log(Vph) Photospheric velocity
42- 47 F6.3 [solMass] log(Menv) Envelope mass
49- 55 F7.3 [solMass/yr] log(dM/dtw) Mass loss rate due to optically thick
wind (log dM/dt (wind))
57- 63 F7.3 [solMass/yr] log(dM/dtn) Mass loss rate due to Hydrogen nuclear
burning (log dM/dt (nuc))
65- 70 F6.3 solRad Radcr Radius at the critical point
72- 77 F6.3 cm/s Velcr Velocity at the critical point
79- 87 E9.3 yr time Evolutional time
89- 94 F6.3 mag Mbol Bolometric magnitude
96-101 F6.3 mag Mvis Visual magnitude
103-109 F7.3 [solLum/kpc2] log(FUV) *Flux in UV (912.3250Å)
111-117 F7.3 [solLum/kpc2] log(FEUV) *Flux in EUV (100.912Å)
119-125 F7.3 [solLum/kpc2] log(FSSXR) *Flux in supersoft X-ray (30.100Å)
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Note on log(FUV), log(FEUV) and log(FSSXR):
log(FNN) = log(LNN/4πD2), D=1.0 kpc (NN=UV, EUV or SSXR)
For log(FSSXR), values less than -30.000 are listed as just -30.000.
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Origin: AAS CD-ROM series, Volume 9, 1997 Lee Brotzman [ADS] 27-Aug-97
(End) [CDS] 06-Feb-1998