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

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 (> 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 = r_S/c). It appears that a rotating black hole creates an additional, faster, and more collimated inner outflow (> 0.5c) formed and accelerated by the twisted magnetic field resulting from frame-dragging in the black hole ergosphere. This new result indicates that jet kinematic structure depends on black hole rotation