Magnetic acceleration of ultra-relativistic GRB and AGN jets

TL;DR

This paper uses numerical simulations to study how magnetic fields accelerate ultra-relativistic jets in astrophysical objects, showing efficient conversion of magnetic energy into kinetic energy and extended acceleration regions.

Contribution

It demonstrates that magnetically driven jets can achieve high Lorentz factors with extended acceleration, aligning with observations and semi-analytic models, and highlights differences between jet and wind solutions.

Findings

Over half of Poynting flux converted to kinetic energy in jets.

Acceleration efficiency depends on jet confinement shape.

Pulsar winds may remain Poynting dominated at termination shock.

Abstract

We present numerical simulations of cold, axisymmetric, magnetically driven relativistic outflows. The outflows are initially sub-Alfv\'enic and Poynting flux-dominated, with total--to--rest-mass energy flux ratio up to $\mu \sim 620$. To study the magnetic acceleration of jets we simulate flows confined within a funnel with rigid wall of prescribed shape, which we take to be $z\propto r^a$ (in cylindrical coordinates, with $a$ ranging from 1 to 2). This allows us to eliminate the numerical dissipative effects induced by a free boundary with an ambient medium. We find that in all cases they converge to a steady state characterized by a spatially extended acceleration region. For the jet solutions the acceleration process is very efficient - on the outermost scale of the simulation more than half of the Poynting flux has been converted into kinetic energy flux, and the terminal Lorentz factor approached its maximum possible value ($\Gamma_\infty \simeq \mu$). The acceleration is accompanied by the collimation of magnetic field lines in excess of that dictated by the funnel shape. The numerical solutions are generally consistent with the semi-analytic self-similar jets solutions and the spatially extended acceleration observed in some astrophysical relativistic jets. In agreement with previous studies we also find that the acceleration is significantly less effective for wind solutions suggesting that pulsar winds may remain Poynting dominated when they reach the termination shock.