Formation and collimation of relativistic MHD jets - simulations and radio maps

Abstract

We present results of magnetohydrodynamic (MHD) simulations of jet formation and propagation, discussing a variety of astrophysical setups. In the first approach we consider simulations of relativistic MHD jet formation, considering jets launched from the surface of a Keplerian disk, demonstrating numerically - for the first time - the self-collimating ability of relativistic MHD jets. We obtain Lorentz factors up to about 10 while acquiring a high degree of collimation of about 1 degree. We then present synchrotron maps calculated from the intrinsic jet structure derived from the MHD jet formation simulation. We finally present (non-relativistic) MHD simulations of jet lauching, treating the transition between accretion and ejection. These setups include a physical magnetic diffusivity which is essential for loading the accretion material onto the outflow. We find relatively high mass fluxes in the outflow, of the order of 20-40 % of the accretion rate.

7 pages, 4 figures, conference proceedings HEPRO 4

References in corpus (5)

• Magnetic acceleration of relativistic AGN jets
• Accretion-Powered Stellar Winds II: Numerical Solutions for Stellar Wind Torques
• A fully covariant mean-field dynamo closure for numerical 3+1 resistive GRMHD
• Bipolar jets launched from magnetically diffusive accretion disks. I. Ejection efficiency vs field strength and diffusivity
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Cited by in corpus (3)

• TANAMI monitoring of Centaurus A: The complex dynamics in the inner parsec of an extragalactic jet
• The Magnetic Field and Polarization Properties of Radio Galaxies in Different Accretion States
• On the Radio Image of Relativistic Jets -- I. Internal Structure, Doppler Boosting, and Polarization Maps