Abstract
We investigate the phenomenon of a dense circumstellar (CS) shell and powerful emission of the (type IIP) SN 2020tlf progenitor. Our modeling of the H\(\alpha\) line and the circumstellar (CS) interaction suggests a CS shell radius of \({\sim}10^{15}\) cm and a mass of \({\sim}\)0.2 \(M_{\odot}\) lost by the supernova (SN) progenitor within \(\sim\)6 yr before the explosion. Spectroscopy and photometry of the SN after the explosion show no clear signatures of the material lost by the SN progenitor in the period of its high luminosity. However, this material could be present in the inner zone of the CS shell. We propose a hydrodynamic model of the consequences of a flash with an energy of \(5\times 10^{48}\) erg in the convective nuclear burning zone. The model predicts the ejection of outer layers of the SN progenitor (\(\sim\)0.1\(M_{\odot}\)) and a luminosity of \(10^{40}\) erg s\({}^{-1}\) for hundreds of days in agreement with the observed SN progenitor luminosity. We propose the Lighthill mechanism of acoustic wave generation by turbulence in the convective nuclear burning zone to account for the phenomenon of confined CS shells in core-collapse SNe.
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Funding
This study was supported by the Russian Scientific Foundation (project no. 19-12-00229) and the Russian Foundation for Basic Research and the Deutsche Forschungsgemeinschaft (project no. 21-52-12032).
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Translated by V. Astakhov
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Chugai, N.N., Utrobin, V.P. Circumstellar Shell and Emission of the SN 2020tlf Progenitor. Astron. Lett. 48, 275–283 (2022). https://doi.org/10.1134/S1063773722060020
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DOI: https://doi.org/10.1134/S1063773722060020