Unveiling Relativistic Jet Dynamics with Dynamic Mode Decomposition

In the present investigation, a magnetized relativistic jet originating from an active galactic nucleus is numerically simulated by solving the relativistic magneto-hydrodynamic equations, employing a high-order finite volume methodology as implemented in the PLUTO solver. The vortical coherent modes, identified through dynamic mode decomposition during the propagation of a relativistic jet through a uniform interstellar medium, exhibit spatio-temporal decay behavior due to strong dissipation induced by the jet head shock. The conversion of jet kinetic energy into thermal energy leads to pronounced dissipation, primarily resulting from the deceleration of the relativistic jet by the jet head shock.