Magnetic dissipation in short gamma-ray burst jets. I. Resistive relativistic MHD evolution in a model environment

TL;DR

This study uses resistive relativistic MHD simulations to explore how magnetic dissipation affects short gamma-ray burst jets during their initial propagation in a magnetized environment, revealing significant structural and turbulence differences.

Contribution

It introduces the first detailed resistive relativistic MHD simulations of short gamma-ray burst jets, highlighting the impact of finite plasma resistivity on jet structure and turbulence.

Findings

Resistivity influences jet structure and turbulence.

Regions with resistive electric fields may enhance particle acceleration.

Dissipated power depends on resistivity models.

Abstract

Short gamma-ray bursts originate when relativistic jets emerge from the remnants of binary neutron star mergers. Both the jet and the remnant are believed to be strongly magnetized, and the presence of magnetic fields is known to influence the jet propagation across the surrounding post-merger environment. In the magnetic interplay between the jet and the environment itself, effects due to a finite plasma conductivity may be important, especially in the first phases of the jet propagation. We aim to investigate such effects, from jet launching to its final breakout from the post-merger environment. 2D axisymmetric and full 3D resistive relativistic MHD simulations, are performed with the PLUTO numerical code. Different models for physical resistivity, which must be small but still above the numerical one (producing unwanted smearing of structures in any ideal MHD code) are considered and compared. All simulations are performed by using an axisymmetric analytical model for the jet propagation environment; we leave the case of jet propagation in a realistic environment (i.e. imported from actual binary neutron star merger simulation) to a later study. Significant differences in the jet structure and induced turbulence are clearly seen in 2D axisymmetric simulations. Regions with a resistive electric field parallel to the magnetic field form and non-thermal particle acceleration may be enhanced there. The level of dissipated Ohmic power is also dependent on the various recipes for resistivity. Most of the differences arise before breakout from the magnetized environment, whereas once the jet enters the external atmosphere these differences are preserved during further propagation despite the lower grid refinement. Finally, we show and discuss the 3D evolution of the jet within the same environment, in order to highlight the emergence of non-axisymmetric features.