General Relativistic Simulations of Jet Formation by a Rapidly Rotating Black Hole

Recent observations of Galactic Black Hole Candidates (BHCs) suggest that those that are superluminal jet sources have more rapid black hole spin rates than otherwise normal BHCs. This provides observational support for models of relativistic jet formation that extract rotational energy of the central black hole. To investigate this mechanism, we have developed a new general relativistic magnetohydrodynamic code in Kerr geometry. Here we report on the first numerical simulation of the formation of a relativistic jet in a rapidly-rotating (a = 0.95) Kerr black hole magnetosphere. We assume that the initial velocity of the disk is zero. We find that the maximum velocity of the jet reaches 0.93c (Lorentz factor, 2.7) and the terminal velocity of the jet is 0.85c (Lorentz factor, 1.9). On the other hand, for a non-rotating (a = 0) Schwarzschild black hole, the maximum jet velocity is less than 0.6c as far as we calculated with the similar condition of the magnetosphere to that of the Kerr black hole case. These numerical results show the importance of the rapidly rotating black hole for the relativistic jet formation clearly.