Prompt Gamma-Ray Burst Emission from Internal Shocks -- New Insights

TL;DR

This paper proposes that synchrotron emission from internal shocks, involving both forward and reverse shocks, can naturally explain key features of prompt gamma-ray burst emission, including spectral shapes and pulse evolution.

Contribution

It introduces a model where synchrotron emission from both shocks accounts for observed GRB spectral features without fine-tuning.

Findings

Explains GRB pulse shapes and spectral evolution.

Accounts for low-energy spectral components and doubly-broken spectra.

Maintains high radiative efficiency in the model.

Abstract

Internal shocks are a leading candidate for the dissipation mechanism that powers the prompt $\gamma$-ray emission in gamma-ray bursts (GRBs). In this scenario a compact central source produces an ultra-relativistic outflow with varying speeds, causing faster parts or shells to collide with slower ones. Each collision produces a pair of shocks -- a forward shock (FS) propagating into the slower leading shell and a reverse shock (RS) propagating into the faster trailing shell. The RS's lab-frame speed is always smaller, while the RS is typically stronger than the FS, leading to different conditions in the two shocked regions that both contribute to the observed emission. We show that optically-thin synchrotron emission from both (weaker FS + stronger RS) can naturally explain key features of prompt GRB emission such as the pulse shapes, time-evolution of the $\nu{}F_\nu$ peak flux and photon-energy, and the spectrum. Particularly, it can account for two features commonly observed in GRB spectra: (i) a sub-dominant low-energy spectral component (often interpreted as ``photospheric''-like), or (ii) a doubly-broken power-law spectrum with the low-energy spectral slope approaching the slow cooling limit. Both features can be obtained while maintaining high overall radiative efficiency without any fine-tuning of the physical conditions.