Shock Breakout from Stellar Envelopes: The relativistic limit

TL;DR

This paper models the emission from relativistic shock breakouts in stellar envelopes, predicting gamma-ray and X-ray signatures, and compares these predictions with observed gamma-ray bursts, providing insights into supernova explosions and compact object events.

Contribution

It introduces an analytic framework for shock breakout emission in relativistic regimes, including pair production effects, and applies it to gamma-ray bursts and supernovae.

Findings

Shock breakouts produce ~200 keV photons in pair-loaded regions.

Some low-luminosity gamma-ray bursts are consistent with relativistic shock breakout models.

Type Ia supernovae emit ~10^{41} erg in ~1 MeV photons during shock breakout.

Abstract

We calculate the observed luminosity and spectrum following the emergence of a relativistic shock wave from a stellar edges. Shock waves propagating at $0.6<\Gamma_\text{sh}\beta_\text{sh}$, where $\Gamma_\text{sh}$ is the shock Lorentz factor and $\beta_\text{sh}$ is its associated reduced velocity, heat the stellar envelope to temperatures exceeding $\sim 50$ keV, allowing for a vigorous production of electron and positron pairs. Pairs significantly increase the electron scattering optical depth and regulate the temperature through photon generation, producing distinct observational signatures in the escaping emission. Assuming Wien equilibrium, we find analytic expressions for the temperature and pair density profiles in the envelope immediately after shock passage, and compute the emission during the expansion phase. Our analysis shows that in pair loaded regions, photons are produced at a roughly uniform rest frame energy of $\sim 200$ keV, and reinforces previous estimates that the shock breakout signal will be detected as a short burst of energetic $\gamma$-ray photons, followed by a longer phase of X-ray emission. We test our model on a sample of low-luminosity gamma ray bursts using a closure relation between the $\gamma$-ray burst duration, the radiation temperature and the $\gamma$-ray isotropic equivalent energy, and find that some of the events are consistent with the relativistic shock breakout model. Finally, we apply our results to explosions in white dwarfs and neutron stars, and find that typical type Ia supernovae emit $\sim 10^{41}$ erg in the form of $\sim 1$ MeV photons.