Optical to X-rays supernovae light curves following shock breakout through a thick wind

TL;DR

This paper models supernova shock breakouts through thick winds, predicting diverse temperatures and spectral components, with implications for detecting X-ray emissions days to months after the explosion.

Contribution

It provides a detailed analysis of the evolution of supernova shock breakout signals, including the temperature variation and spectral components, extending understanding of observable signatures in optical, UV, and X-ray bands.

Findings

Breakout temperature varies from 10^4 to 5×10^6 K due to thermal equilibrium deviations.

Post-breakout emission includes both optical/UV and hard X-ray components.

X-ray emission becomes prominent 10-50 days after the explosion for certain breakout times.

Abstract

Recent supernovae (SNe) observations have motivated renewed interest in SN shock breakouts from stars surrounded by thick winds. In such events the interaction with the wind powers the observed luminosity, and predictions include observable hard X-rays. Wind breakouts on timescales of a day or longer are currently the most probable for detection. Here we study the signal that follows such events. We start from the breakout of the radiation mediated shock, finding that the breakout temperature can vary significantly from one event to another ($10^4 - 5 \times 10^6$ K) due to possible deviation from thermal equilibrium. In general, events with longer breakout pulse duration, $t_{bo}$, are softer. We follow the observed radiation through the evolution of the collisionless shock which forms after the breakout of the radiation mediated shock. We restrict the study of the collisionless shock evolution to cases where the breakout itself is in thermal equilibrium, peaking in optical/UV. In these cases the post-breakout emission contains two spectral components - soft (optical/UV) and hard (X-rays and possibly soft $\gamma$-rays). Right after the breakout pulse X-rays are strongly suppressed, and they carry only a small fraction of the total luminosity. The hard component becomes harder and its luminosity rises quickly afterwards, gaining dominance at $\sim 10-50 \,t_{bo}$. The ratio of the peak optical/UV to the peak X-ray luminosity depends mostly on the breakout time. In terms of prospects for X-ray and soft gamma-ray detections, it is best to observe 100-500 days after explosions with breakout timescales between a week and a month.