AAS 202nd Meeting, May 2003
Session 6 Black Holes and Pulsars
Poster, Monday, May 26, 2003, 9:20am-6:30pm, West Exhibit Hall

## [6.02] The Formation of relativistic jets from Kerr Black Holes

K.-I. Nishikawa, G. Richardson, R. Preece (NSSTC), P. Hardee (Univ. Alabama, Tuscaloosa), S. Koide (Toyama Univ.), K. Shibata (Kyoto Univ.), T. Kudoh (Univ. Western Ontario), H. Sol (Obs. de Paris-Meudon), J. P. Hughes (Rutgers Univ.), J. Fishman (NSSTC)

We have performed the first fully three-dimensional general relativistic magnetohydrodynamics (GRMHD) simulation for Schwarzschild and Kerr black holes with a free falling corona and thin accretion disk. The initial simulation results with a Schwarzschild metric show that a jet is created as in the previous axisymmetric simulations with mirror symmetry at the equator. However, the time to form the jet is slightly longer than in the 2-D axisymmetric simulation. We expect that the dynamics of jet formation are modified due to the additional freedom in the azimuthal dimension without axisymmetry with respect to the z axis and reflection symmetry with respect to the equatorial plane. This simulation ran for 128.9 light-crossing time (\tau\rm S = r\rm S/c) which is much larger than the previous simulation time 52 \tau\rm S. The jet which is initially formed due to the twisted magnetic fields and shocks becomes a wind at the later time. The wind flows out with a much wider angle than the initial jet. The twisted magnetic fields at the earlier time were untwisted and less pinched. The accretion disk became thicker than the initial condition. Further simulations with initial perturbations will provide insights for accretion dynamics with instabilities such as magnetorotational instability (MRI) and accretion-eject instability (AEI). These instabilities may contribute to variablities observed in microquasars and AGN jets.