Structure of Magnetic Tower Jets in Stratified Atmospheres

Abstract

Based on a new approach on modeling the magnetically dominated outflows from AGNs (Li et al. 2006), we study the propagation of magnetic tower jets in gravitationally stratified atmospheres (such as a galaxy cluster environment) in large scales (> tens of kpc) by performing three-dimensional magnetohydrodynamic (MHD) simulations. We present the detailed analysis of the MHD waves, the cylindrical radial force balance, and the collimation of magnetic tower jets. As magnetic energy is injected into a small central volume over a finite amount of time, the magnetic fields expand down the backgroun d density gradient, forming a collimated jet and an expanded “lobe” due to the gradually decreasing background density and pressure. Both the jet and lobes are magnetically dominated. In addition, the injection and expansion produce a hydrodynamic shock wave that is moving ahead of and enclosing the magnetic tower jet. This shock can eventually break the hydrostatic equilibrium in the ambient medium and cause a global gravitational contraction. This contraction produces a strong compression at the head of the magnetic tower front and helps to collimate radially to produce a slendershaped jet. At the outer edge of the jet, the magnetic pressur e is balanced by the background (modified) gas pressure, without any significant contribution from the hoo p stress. On the other hand, along the central axis of the jet, hoop stress is the dominant force in shaping the cent ral collimation of the poloidal current. The system, which possesses a highly wound helical magnetic configurati on, never quite reaches a force-free equilibrium state though the evolution becomes much slower at late stages. The simulations were performed without any initial perturbations so the overall structures of the jet r emain mostly axisymmetric. Subject headings:magnetic fields — galaxies: active — galaxies: jets — methods : numerical — magnetohydrodynamics (MHD)