Radiation from accelerated particles in relativistic jets with shocks, shear-flow, and reconnection

TL;DR

This paper investigates particle acceleration and radiation in relativistic jets with shocks, shear flows, and reconnection, revealing how magnetic fields influence spectra and providing insights into high-energy astrophysical phenomena.

Contribution

It presents self-consistent calculations of radiation from electrons in turbulent magnetic fields generated by shocks and shear instabilities in relativistic jets, advancing understanding of their spectral properties.

Findings

Spectra depend on jet Lorentz factor, temperature, and magnetic field strength.

Magnetic fields from shocks and shear instabilities influence electron acceleration.

Results aid interpretation of gamma-ray burst and supernova remnant emissions.

Abstract

We have investigated particle acceleration and shock structure associated with an unmagnetized relativistic jet propagating into an unmagnetized plasma. Strong magnetic fields generated in the trailing jet shock lead to transverse deflection and acceleration of the electrons. We have self-consistently calculated the radiation from the electrons accelerated in the turbulent magnetic fields. We find that the synthetic spectra depend on the bulk Lorentz factor of the jet, the jet temperature, and the strength of the magnetic fields generated in the shock. We have also begun study of electron acceleration in the strong magnetic fields generated by kinetic shear (Kelvin-Helmholtz) instabilities. Our calculated spectra should lead to a better understanding of the complex time evolution and/or spectral structure from gamma-ray bursts, relativistic jets, and supernova remnants.