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SN 2020sck: Deflagration in a Carbon-Oxygen White Dwarf
Journal
Astrophysical Journal
ISSN
0004637X
Date Issued
2022-02-01
Author(s)
Dutta, Anirban
Sahu, D. K.
Anupama, G. C.
Joharle, Simran
Kumar, Brajesh
Nayana, A. J.
Singh, Avinash
Kumar, Harsh
Bhalerao, Varun
Barway, Sudhansu
Dutta, Anirban
Abstract
We present optical UBVRI photometry and low-to-medium resolution spectroscopic observations of type Iax supernova SN 2020sck spanning -5.5 days to +67 days from maximum light in the B-band. From the photometric analysis we find m B (15) = 2.03 ± 0.05 mag and M B = -17.81 ± 0.22 mag. Radiation diffusion model fit to the quasi-bolometric light curve indicates 0.13 ± 0.02 M Ȯ of 56Ni and 0.34 M Ȯ of ejecta are synthesized in the explosion. Comparing the observed quasi-bolometric light curve with the angle-averaged bolometric light curve of a three-dimensional pure deflagration explosion of M ch carbon-oxygen white dwarf, we find agreement with a model in which 0.16 M Ȯ of 56Ni and 0.37 M Ȯ of ejecta is formed. By comparing the +1.4 days spectrum of SN 2020sck with synthetic spectrum generated using SYN++, we find absorption features due to C ii, C iii, and O i. These are unburned materials in the explosion and indicate a C-O white dwarf. One-dimensional radiative transfer modeling of the spectra with TARDIS shows higher density in the ejecta near the photosphere and a steep decrease in the outer layers with an ejecta composition dominated mostly by C, O, Si, Fe, and Ni. The star-formation rate of the host galaxy computed from the luminosity of the Hα (λ6563) line is 0.09 M Ȯ yr-1, indicating a relatively young stellar environment.
Volume
925
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