Astrophys. J., 925, 217-217 (2022/February-2)
SN 2020sck: Deflagration in a Carbon-Oxygen White Dwarf.
DUTTA A., SAHU D.K., ANUPAMA G.C., JOHARLE S., KUMAR B., NAYANA A.J., SINGH A., KUMAR H., BHALERAO V. and BARWAY S.
Abstract (from CDS):
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 ΔmB(15) = 2.03 ± 0.05 mag and MB = -17.81 ± 0.22 mag. Radiation diffusion model fit to the quasi-bolometric light curve indicates 0.13 ± 0.02 M☉ of 56Ni and 0.34 M☉ 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 Mch carbon-oxygen white dwarf, we find agreement with a model in which 0.16 M☉ of 56Ni and 0.37 M☉ 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☉ yr–1, indicating a relatively young stellar environment.
© 2022. The Author(s). Published by the American Astronomical Society.
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