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

Abstract

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 Ålight 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.

arXiv comment9 pages including 8 figures, to appear in the Astrophysical Journal

References in corpus (7)

• A Universal Decline Law of Classical Novae
• The Theory of Steady State Super-Eddington Winds and its Application to Novae
• A study of the expanding envelope of Nova V1974 Cyg 1992 based on IUE high resolution spectroscopy
• Toward a unified light curve model for multi-wavelength observations of V1974 Cygni (Nova Cygni 1992)
• Non-LTE model atmosphere analysis of the early ultraviolet spectra of nova OS Andromedae 1986
• A Modeling of the Super-Eddington Luminosity in Nova Outbursts: V1974 Cygni
• Classical Novae as Super-Eddington Objects

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