Numerical study of relativistic jet propagation inside uniform interstellar medium issuing from an Active Galactic Nuclei

Abstract

A direct numerical simulation (DNS) of two-dimensional axisymmetric relativistic jet propagation through a uniform interstellar medium was carried out by solving the relativistic magnetohydrodynamic (RMHD) equations with the PLUTO solver (Mignone et al., 2007). Moreover, a comprehensive discussion of the detailed flow features involved in this propagation is provided throughout this study. The physics underlying shock-vorticity interaction during relativistic jet propagation through a uniform interstellar medium has been thoroughly described in this present study. Additionally, the probability density distribution (p.d.f) of enstrophy ($ϵ$) indicates that the highest intensity of fluid rotation, and consequently turbulence, is manifested within the cocoon instead of the frontal region of the relativistic jet.