Circumstellar shell and presupernova emission of SN 2020tlf

TL;DR

This paper models the dense circumstellar shell and presupernova emission of SN 2020tlf, revealing the shell's properties, the ejection of outer layers, and proposing a turbulence-driven acoustic wave mechanism for shell formation.

Contribution

It introduces a hydrodynamic model of presupernova outbursts and proposes a novel turbulence-induced acoustic wave mechanism for the formation of the circumstellar shell.

Findings

CS shell radius of ~10^15 cm and mass of ~0.2 solar masses

Ejection of ~0.1 solar masses during a flash event

Predicted luminosity matches observations over hundreds of days

Abstract

We address a phenomenon of a confined circumstellar (CS) dense shell and powerful presupernova emission of SN 2020tlf (type IIP). Modeling the \ha\ line and the circumstellar interaction implies the CS shell radius of $\sim$10$^{15}$ cm and the mass of $\sim0.2M_{\odot}$ lost during $\sim$6 yr prior to the explosion. Spectra and photometry of the supernova after the explosion do not show apparent signature of the material lost by the presupernova during its powerful luminosity. This material presumably resided in the inner zone of the CS shell. We present a hydrodynamic model of the outcome of a flash with the energy of $5\times10^{48}$ erg in the convective nuclear burning zone. The model predicts the ejection of outer layers of the presupernova ($\sim0.1M_{\odot}$) and the luminosity of $10^{40}$ erg s$^{-1}$ during several hundreds days in accord with observations. We propose the Lighthill mechanism of acoustic waves generation by the turbulence of the convective nuclear burning zone to account for the phenomenon of a compact CS shell of supernovae related to the core collapse.