Modeling of the Super-Eddington Phase for Classical Novae: Five IUE Novae - INSPIRE

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Modeling of the Super-Eddington Phase for Classical Novae: Five IUE Novae

Mariko Kato
(
- Keio U.
)
,
Izumi Hachisu
(
- Tokyo U., Earth Sci. Dept.
)

Nov, 2006

9 pages

Published in:

Astrophys.J. 657 (2007) 1004-1012

e-Print:

astro-ph/0611594 [astro-ph]

DOI:

10.1086/511058

View in:

ADS Abstract Service

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Abstract: (arXiv)

We present a light curve model for the super-Eddington luminosity phase of five classical novae observed with IUE. Optical and UV light curves are calculated based on the optically thick wind theory with a reduced effective opacity for a porous atmosphere. Fitting a model light curve with the UV 1455 \AA light curve, we determine the white dwarf mass and distance to be (1.3 M_sun, 4.4 kpc) for V693 CrA, (1.05 M_sun, 1.8 kpc) for V1974 Cyg, (0.95 M_sun, 4.1 kpc) for V1668 Cyg, (1.0 M_sun, 2.1 kpc) for V351 Pup, and (1.0 M_sun, 4.3 kpc) for OS And.

novae, cataclysmic variables
stars: individual (OS Andromedae, V693 Coronae Australis, V1974 Cygni, V1668 Cygni, V351 Puppis)

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(
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)
,
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(
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)

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)

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