Simulations of substructures in relativistic jets

TL;DR

This paper introduces a new Fortran 90 code for simulating relativistic jets from accretion disks around black holes, capturing substructures and lobes through stable GRMHD solutions.

Contribution

A novel numerical code employing a Nessyahu-Tadmor scheme for stable GRMHD simulations of relativistic jets with substructure formation.

Findings

Successful simulation of jet substructures and lobes.

Stable numerical solutions with controlled oscillations.

Jets ejected over distances twenty times the black hole radius.

Abstract

We present a set of simulations of relativistic jets from accretion disk initial setup with a new code in Fortran 90 to get numerical solutions of a system of General Relativistic Magnetohydrodynamics (GRMHD) partial differential equations in a fixed Black Hole (BH) spacetime which is able to show substructures formations inside the jet as well as a lobe formation on the disk. For this, a central scheme of finite volume method without dimensional split and no Riemann solvers (a Nessyahu-Tadmor method) was implemented. Thus, we were able to obtain stable numerical solutions with spurious oscillations under control and no excessive numerical dissipation. We setup a magnetized accretion disk uncharged plasma surrounding a central Schwarzschild BH immersed in a magnetosphere which evolve to the ejection of matter in the form of jet with its substructures over a distance of almost twenty times the BH radius.