Simulation of high energy emission from gamma-ray bursts

TL;DR

This paper presents new relativistic shock simulations of gamma-ray bursts that replicate observed high-energy emissions up to GeV energies, offering insights into jet physics and particle acceleration.

Contribution

It introduces a dynamically consistent relativistic shock model for GRB prompt emission, including magnetic fields, improving understanding of high-energy radiation mechanisms.

Findings

Model reproduces observed burst properties up to GeV energies.

Provides insights into relativistic jet characteristics.

Enhances understanding of particle acceleration in GRBs.

Abstract

Gamma-Ray Bursts (GRBs) are the must violent explosions after the Big-Bang. Their high energy radiation can potentially carry information about the most inner part of the accretion disk of a collapsing star, ionize the surrounding material in the host galaxy and thereby influence the process of star formation specially in the dense environment at high redshifts. They can also have a significant contribution in the formation of high energy cosmic-rays. Here we present new simulations of GRBs according to a dynamically consistent relativistic shock model for the prompt emission, with or without the presence of an magnetic field. They show that the properties of observed bursts are well reproduced by this model up to GeV energies. They help to better understand GRB phenomenon, and provide an insight into characteristics of relativistic jets and particle acceleration which cannot yet be simulated with enough precision from first principles.