Shock breakout theory

TL;DR

This paper reviews supernova shock breakout theory, explaining how early emission signatures reveal progenitor star properties and mass-loss history, and discusses recent observational advances and future prospects.

Contribution

It provides a pedagogical overview of shock breakout theory, synthesizing recent observational findings and outlining necessary advancements for future research.

Findings

Shock breakout signatures reveal progenitor star structure.

Circumstellar material affects breakout duration.

Observations constrain supernova progenitor properties.

Abstract

The earliest supernova (SN) emission is produced when the optical depth of the plasma lying ahead of the shock, which ejects the envelope, drops below c/v, where v is the shock velocity. This "breakout" may occur when the shock reaches the edge of the star, producing a bright X-ray/UV flash on time scales of seconds to a fraction of an hour, followed by UV/optical "cooling" emission from the expanding cooling envelope on a day time-scale. If the optical depth of circumstellar material (CSM) ejected from the progenitor star prior to the explosion is larger than c/v, the breakout will take place at larger radii, within the CSM, extending its duration to days time scale. The properties of the early, breakout and cooling, emission carry unique signatures of the structure of the progenitor star (e.g. its radius and surface composition) and of its mass-loss history. The recent progress of wide-field transient surveys enable SN detections on a day time scale, and are being used to set unique constraints on the progenitors of SNe of all types. This chapter includes a pedagogical description of SN breakout theory, and a concise overview of what we have learned from observations so far, and of advances in observational capabilities that are required in order to make further significant progress.