Survival of the Fittest: Numerical Modeling of SN 2014C

Initially classified as a Type Ib supernova (SN), ∼100 days after the explosion SN 2014C made a transition to a Type II SN, presenting a gradual increase in the H α emission. This has been interpreted as evidence of interaction between the SN shock wave and a massive shell previously ejected from th...

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Bibliographic Details
Published in:The Astrophysical journal 2022-05, Vol.930 (2), p.150
Main Authors: Vargas, Felipe, De Colle, Fabio, Brethauer, Daniel, Margutti, Raffaella, Bernal, Cristian G.
Format: Article
Language:English
Subjects:
Astrophysics
Bremsstrahlung
Density stratification
Ejecta
Explosions
Genetic algorithms
H alpha line
High energy astrophysics
Mathematical models
Numerical models
Numerical simulations
Radiation
Shells (structural forms)
Shock waves
Stellar physics
Supernova
Supernova dynamics
X-ray astronomy
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Summary:Initially classified as a Type Ib supernova (SN), ∼100 days after the explosion SN 2014C made a transition to a Type II SN, presenting a gradual increase in the H α emission. This has been interpreted as evidence of interaction between the SN shock wave and a massive shell previously ejected from the progenitor star. In this paper we present numerical simulations of the propagation of the SN shock through the progenitor star and its wind, as well as the interaction of the SN ejecta with the massive shell. To determine with high precision the structure and location of the shell, we couple a genetic algorithm to a hydrodynamic and a bremsstrahlung radiation transfer code. We iteratively modify the density stratification and location of the shell by minimizing the variance between X-ray observations and synthetic predictions computed from the numerical model, allowing the shell structure to be completely arbitrary. By assuming spherical symmetry, we found that our best-fit model has a shell mass of 2.6 M ⊙ ; extends from 1.6 × 10 16 cm to 1.87 × 10 17 cm, implying that it was ejected ∼ 60/( v w /100 km s −1 ) yr before the SN explosion; and has a density stratification with an average behavior ∼ r −3 but presenting density fluctuations larger than one order of magnitude. Finally, we predict that if the density stratification follows the same power-law behavior, the SN will break out from the shell by mid-2022, i.e., 8.5 yr after explosion.
ISSN:0004-637X
1538-4357
DOI:10.3847/1538-4357/ac649d