Jet propagation through inhomogeneous media and shock ionization

TL;DR

This paper presents the first numerical simulations of relativistic jets propagating through galaxy centers, highlighting shock ionization effects and matching observed gas velocities, with preliminary results indicating long cooling times in low-density media.

Contribution

First numerical simulations of relativistic outflows in galaxy centers including atomic hydrogen and ionization cooling effects.

Findings

Efficient shock ionization of atomic hydrogen in interstellar clouds.

Simulated gas velocities align with observational data.

Long cooling times due to low-density environments.

Abstract

In this contribution we present the first numerical simulations of a relativistic outflow propagating through the inner hundreds of parsecs of its host galaxy, including atomic and ionised hydrogen, and the cooling effects of ionisation. Our results are preliminary, but we observe efficient shock ionization of atomic hydrogen in interstellar clouds. The mean density of the interstellar medium in these initial simulations is lower than that expected in typical galaxies, which makes cooling times longer and thus no recombination is observed inside the shocked region. The velocities achieved by the shocked gas in the simulations are in agreement with observational results, although with a wide spectrum of values.