TL;DR
This paper models super-Chandrasekhar-mass white dwarf explosions to explain the luminous supernova SN 2009dc, estimating its progenitor's mass and nickel content through radiation hydrodynamics simulations.
Contribution
It introduces simplified explosion models for super-Chandrasekhar-mass white dwarfs and compares their light curves with observations to estimate progenitor properties.
Findings
Progenitor likely a 2.2-2.4 solar mass white dwarf.
Nickel-56 mass estimated between 1.2 and 1.4 solar masses.
Model matches observed light curves assuming negligible host galaxy extinction.
Abstract
Simplified explosion models of super-Chandrasekhar-mass C-O white dwarfs (WDs) are constructed with parameters such as WD mass and Ni-56 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- to 2.4-solar-mass C-O WD with 1.2 to 1.4 solar masses of Ni-56, if the extinction by its host galaxy is negligible.
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