Shock breakouts from red supergiants: analytical and numerical predictions

Abstract

Shock breakout (SBO) signal is the first signature of the supernova explosion apart from gravitational waves and neutrinos. Observational properties of SBO, such as bolometric luminosity and colour temperature, connect to the supernova progenitor and explosion parameters. Detecting SBO or SBO-cooling will constrain the progenitor and explosion models of collapsing stars. In the light of recently launched eROSITA telescope, the rate for detection of SBO is a few events during a year. In the current study, we examine the analytic formulae derived by Shussman et al. (2016). We use four red supergiant models from their study, while running explosions with the radiation hydrodynamics code STELLA. We conclude that there is a good agreement between analytic and numerical approaches for bolometric luminosity and colour temperature during SBO. The analytic formulae for the SBO signal based on the global supernova parameters can be used instead of running time-consuming numerical simulations. We define spectral range where analytic formulae for the SBO spectra are valid. We provide improved analytical expression for the SBO spectral energy distribution. We confirm dependence of colour temperature on radius derived by analytical studies and suggest to use early time observations to confine the progenitor radius. Additionally we show the prediction for the SBO signal from red supergiants as seen by eROSITA instrument.

The low-luminosity type II SN\,2016aqf: A well-monitored spectral evolution of the Ni/Fe abundance ratio

“…The large uncertainties come mainly from the velocity, specifically from the instrumental resolution, and from the distance uncertainty used in calculating the absolute magnitude. We compared these results with similar relations found in the literature (e.g., Kasen & Woosley 2009;Shussman et al 2016;Sukhbold et al 2016;Kozyreva et al 2019;Goldberg et al 2019;Kozyreva et al 2020), obtaining similar results.…”