General Relativistic Magnetohydrodynamic Simulations of Jet Formation with a Thin Keplerian Disk

Details General Relativistic Magnetohydrodynamic Simulations of Jet Formation with a Thin Keplerian Disk General Relativistic Magnetohydrodynamic Simulations of Jet Formation with a Thin Keplerian Disk

2006-09-13

arxiv.org/abs/astro-ph/0609344v2

Astronomy and Astrophysics

Astrophysics

12 pages, 3 figures, revised version based on referee's comments

Scientific paper

We have performed several simulations of black hole systems (non-rotating, black hole spin parameter a=0.0 and rapidly rotating, a=0.95) with a geometrically thin Keplerian disk using the newly developed RAISHIN code. The simulation results show the formation of jets driven by the Lorentz force and the gas pressure gradient. The jets have mildly relativistic speed (\sim 0.4c). The matter is continuously supplied from the accretion disk and the jet propagates outward until each applicable terminal simulation time (non-rotating: t/\tau_S = 275 and rotating: t/tau_S = 200, \tau_S \equiv r_S/c). It appears that a rotating black hole creates an additional, faster, and more collimated matter-dominated inner outflow (\sim 0.5c) formed and accelerated by the twisted magnetic field resulting from frame-dragging in the black hole ergosphere. This is the first known simulation confirming the formation of an inner magnetically-driven, matter-dominated jet by the frame-dragging effect from a black hole co-rotating with a thin Keplerian disk threaded by a vertical magnetic field. This result indicates that jet kinematic structure depends on black hole rotation and on the initial magnetic field configuration and strength.

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