2006/02/10 by Zhanwen Han, Philipp Podsiadlowski · 4 citations
Physics and Astronomy · #Astro and Planetary Science #Astrophysics and Star Formation Studies #Gamma-ray bursts and supernovae #astro-ph
paper · pdf · doi:10.1111/j.1365-2966.2006.10185.x
published as Mon.Not.Roy.Astron.Soc.368:1095-1100,2006 · 7 pages, 8 figures, accepted by MNRAS
arxiv created 2006/02/10 · openalex publication_date 2006/03/23 · arxiv updated 2009/12/01 · openalex created_date 2025/10/10 · openalex updated_date 2026/07/28
Supernova 2002ic was an atypical Type Ia supernova (SN Ia) with evidence for substantial amounts of hydrogen associated with the system. Contrary to previous claims, we show that its unusual properties can be understood within the framework of one of the most favoured progenitor models, the so-called supersoft channel. This requires that the donor star was initially relatively massive (∼3 M⊙) and that the system experienced a delayed dynamical instability, leading to a large amount of mass-loss from the system in the last few 104 yr before the explosion. This can produce the inferred hydrogen-rich circumstellar environment, most likely with a disc-like geometry. However, in order for this model to be feasible, it requires a larger accretion efficiency on to the white dwarf than is assumed in present parametrizations. If this is confirmed, it would most likely increase estimates for the frequency of the single-degenerate channel. Based on population synthesis simulations we estimate that not more than 1 in 100 SNe Ia should belong to this subgroup of SNe Ia.