Numerical study of three-dimensional relativistic jet/spherical cloud interaction in astrophysical galactic outflows

In this Letter, the direct numerical simulation (DNS) of three-dimensional relativistic jet/spherical cloud interaction has been performed by solving the hydrodynamic relativistic equations using PLUTO solver [Mignone et al., “PLUTO: A numerical code for computational astrophysics,” Astrophys. J. Suppl. Ser. 170, 228 (2007)]. The detailed flow features involved during this relativistic jet/spherical cloud interaction have been thoroughly discussed in this study. The flow physics associated with shock-turbulence amplification/attenuation has been carried out by using the divergence of Lamb vector analysis [Pal et al., “Numerical studies of shock–vortex interaction over a wedge during shock-wave diffraction—A new approach,” Phys. Fluids 35, 106106 (2023); Hamman et al., “On the lamb vector divergence in Navier–Stokes flows,” J. Fluid Mech. 610, 261–284 (2008); Chen et al., “Numerical investigation of the compressible flow past an aerofoil,” J. Fluid Mech. 643, 97–126 (2010).]. The study also reveals that the presence of a spherical cloud in the trajectory of relativistic jet could produce more turbulence over absence of cloud.