Formation of relativistic MHD jets: stationary state solutions & numerical simulations

TL;DR

This paper combines stationary solutions and numerical simulations to study the formation, acceleration, and spectral properties of relativistic MHD jets, providing insights into jet collimation and emission mechanisms.

Contribution

It introduces a comprehensive approach integrating stationary models, spectral analysis, and simulations to advance understanding of relativistic MHD jet formation and acceleration.

Findings

Stationary solutions illustrate jet collimation and acceleration processes.

Spectral analysis shows Doppler effects on jet emission.

Simulations demonstrate acceleration from low to high velocities.

Abstract

We discuss numerical results of relativistic magnetohydrodynamic (MHD) jet formation models. We first review some examples of stationary state solutions treating the collimation and acceleration process of relativistic MHD jets. We provide an a posteriori check for the MHD condition in highly magnetized flows, namely the comparison of particle density to Goldreich-Julian density. Using the jet dynamical parameters calculated from the MHD model we show the rest-frame thermal X-ray spectra of the jet, from which we derive the overall spectrum taking into account a variation of Doppler boosting and Doppler shift of emission lines along the outflow. Finally, we present preliminary results of relativistic MHD simulations of jet formation demonstrating the acceleration of a low velocity (0.01c) disk wind to a collimated high velocity (0.8c).