Approaching ballistic motion in 3D simulations of gamma-ray burst jets in realistic binary neutron star merger environments

TL;DR

This study extends 3D magnetohydrodynamic simulations of gamma-ray burst jets in neutron star merger environments to nearly ballistic regimes, providing more accurate models of jet evolution and structure for observational comparison.

Contribution

It advances 3D jet simulations to longer timescales, capturing the transition to ballistic motion and detailed angular structure in realistic merger environments.

Findings

Jet struggles to pierce dense surroundings, resulting in asymmetrical outflows.

98% of jet energy is in kinetic form at simulation end.

Angular structure becomes frozen, suitable for afterglow modeling.

Abstract

Context. The concomitant observation of gravitational wave and electromagnetic signals from a binary neutron star (BNS) merger in 2017 confirmed that these events can produce relativistic jets responsible for short Gamma-Ray Bursts (sGRBs). The complex interaction between the jet and the surrounding post-merger environment shapes the angular structure of the outflow, which is then imprinted in the prompt and afterglow sGRB emission. Aims. The outcome of relativistic (magneto)hydrodynamic simulations of jets piercing through post-merger environments is often used as input to compute afterglow signals to be compared with observations. However, for reliable comparisons, the jet propagation should be followed until nearly ballistic regimes, in which the jet acceleration is essentially over and the angular structure is no longer evolving. This condition is typically reached in 2D simulations, but not in 3D. Our goal is to extend a (specific) jet simulation in 3D up to a nearly ballistic phase, analysing the overall dynamical evolution from the jet breakout. Methods. Our work is based on a previous 3D magnetohydrodynamic jet simulation employing a realistic environment imported from a BNS merger simulation, extended here far beyond the evolution time originally covered. After approximately 3 seconds of the jet evolution on the original spherical grid, we remap the system into a uniform Cartesian grid and reach about 10 seconds without loss of resolution. Results. The specific jet considered here struggles to pierce the dense surroundings, resulting in a rather asymmetrical emerging outflow with relatively low Lorentz factor. The analysis of the energy conversion processes and corresponding acceleration shows that at the end of our simulation 98% of the energy is in kinetic form. Moreover, at that time the angular structure is frozen. We thus obtain suitable inputs for...