2011/07/01 by Yasuomi Kamiya
Physics and Astronomy · #Astro and Planetary Science #Astrophysics #Chandrasekhar limit #Extinction (optical mineralogy) #Galaxy #Gamma-ray bursts and supernovae #Geology #Light curve #Optics #Physics #Pulsars and Gravitational Waves Research #Stars #Supernova #Type (biology) #White dwarf #astro-ph.HE #astro-ph.SR
paper · pdf · doi:10.1017/s1743921312015268
published in Proceedings of the International Astronomical Union 7(S281), 314-315 (Cambridge University Press) · 2 pages, 1 figure, published in the Proceedings of the IAU Symposium No. 281 "Binary Paths to Type Ia Supernova Explosions" held in Padova (July 4-8, 2011)
openalex publication_date 2011/07/01 · arxiv created 2013/02/14 · arxiv updated 2013/02/15 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
Abstract Simplified explosion models of super-Chandrasekhar-mass C-O white dwarfs (WDs) are constructed with parameters such as WD mass and 56 Ni mass. Their light curves are obtained by solving one-dimensional equations of radiation hydrodynamics, and compared with the observations of SN 2009dc, one of the overluminous Type Ia supernovae, to estimate its properties. As a result, the progenitor of SN 2009dc is suggested to be a 2.2–2.4- M ⊙ C-O WD with 1.2–1.4 M ⊙ of 56 Ni, if the extinction by its host galaxy is negligible.