A Modeling of the Super-Eddington Luminosity in Nova Outbursts: V1974 Cygni

Abstract

We have modeled nova light curves exceeding the Eddington luminosity. It has been suggested that a porous structure develops in nova envelopes during the super Eddington phase and the effective opacity is much reduced for such a porous atmosphere. Based on this reduced opacity model, we have calculated envelope structures and light curves of novae. The optically thick wind model is used to simulate nova winds. We find that the photospheric luminosity and the wind mass-loss rate increase inversely proportional to the reducing factor of opacities, but the wind velocity hardly changes. We also reproduce the optical light curve of V1974 Cygni (Nova Cygni 1992) in the super-Eddington phase, which lasts 13 days from the optical peak 1.7 mag above the Eddington luminosity.

8 pages, 4 figures, to appear in ApJL

References in corpus (3)

• 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)
• Six months of mass outflow and inclined rings in the ejecta of V1494 Aql

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