2005/10/02 by Mariko Kato, Izumi Hachisu · 1 citation
Physics and Astronomy · #Astronomy and Astrophysical Research #Astrophysical Phenomena and Observations #Eddington luminosity #Envelope (radar) #Gamma-ray bursts and supernovae #Light curve #Luminosity #Nova (rocket) #Opacity #Radiative transfer #astro-ph
paper · pdf · doi:10.1086/498300
published as Astrophys.J.633:L117-L120,2005 · 8 pages, 4 figures, to appear in ApJL
arxiv created 2005/10/02 · openalex publication_date 2005/10/24 · arxiv updated 2009/12/01 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/05
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 that 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 that 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.