Inverse-Compton drag on a Highly Magnetized GRB jet in Stellar Envelope

TL;DR

This paper investigates how inverse-Compton scattering in stellar envelopes significantly slows down highly magnetized GRB jets, leading to observable high-energy flashes, and finds that pair screens do not prevent this drag.

Contribution

It demonstrates that strong inverse-Compton drag affects Poynting flux dominated GRB jets in stellar envelopes, especially for high initial magnetization, and explores the role of pair screens in this process.

Findings

Jets with high magnetization are slowed to sub-relativistic speeds.

A fraction of jet energy is emitted as a bright 1-100 MeV flash.

Pair screens do not effectively shield the jet from inverse-Compton drag.

Abstract

The collimation and evolution of relativistic outflows in $\gamma$-ray bursts (GRBs) are determined by their interaction with the stellar envelope through which they travel before reaching the much larger distance where the energy is dissipated and $\gamma$-rays are produced. We consider the case of a Poynting flux dominated relativistic outflow and show that it suffers strong inverse-Compton (IC) scattering drag near the stellar surface and the jet is slowed down to sub-relativistic speed if its initial magnetization parameter ($\sigma_0$) is larger than about 10$^5$. If the temperature of the cocoon surrounding the jet were to be larger than about 10 keV, then an optically thick layer of electrons and positrons forms at the interface of the cocoon and the jet, and one might expect this pair screen to protect the interior of the jet from IC drag. However, the pair screen turns out to be ephemeral, and instead of shielding the jet it speeds up the IC drag on it. Although a high $\sigma_0$ jet might not survive its passage through the star, a fraction of its energy is converted to 1-100 MeV radiation that escapes the star and appears as a bright flash lasting for about 10 s.