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

¹ SISSA, Via Bonomea 265, I-34136 Trieste, Italy
² INAF, Osservatorio Astronomico di Padova, Vicolo dell’Osservatorio 5, I-35122 Padova, Italy
³ INFN, Sezione di Trieste, Via Valerio 2, I-34127 Trieste, Italy
⁴ INFN, Sezione di Padova, Via Francesco Marzolo 8, I-35131 Padova, Italy
⁵ INAF, Osservatorio Astronomico di Brera, via Bianchi 46, I-23807 Merate, Italy
⁶ IFPU, Via Beirut 2, I-34151 Trieste, Italy

^⋆ Corresponding authors; edreas@sissa.it; riccardo.ciolfi@inaf.it

Received: 29 July 2024
Accepted: 11 January 2025

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 that can 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 ones. Our goal is to extend a (specific) jet simulation in 3D up to a nearly ballistic phase and analyse 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 remapped the system into a uniform Cartesian grid and reached about 10 seconds without loss of resolution.

Results. The specific jet considered here struggled to pierce the dense surroundings, resulting in a rather asymmetrical emerging outflow with a relatively low Lorentz factor. Analysis of the energy conversion processes and corresponding acceleration showed 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 obtained suitable inputs for computing the afterglow emission. Our procedure is general and applicable to any jet simulation of the same kind.