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K.-I. Nishikawa (Rutgers Univ.), S. Koide (Toyama Univ.), K. Shibata (Kyoto Univ.), T. Kudoh (NAO, Japan), H. Sol (Obs. de Paris-Meudon), J. P. Hughes (Rutgers Univ.)
We have investigated the dynamics of an accretion disk around Schwarzschild black holes initially threaded by a uniform poloidal magnetic field in a non-rotating corona (either in a steady-state infalling state) around a non-rotating black hole using a 3-D GRMHD with the ``axisymmetry'' along the z-direction. Magnetic field is tightly twisted by the rotation of the disk, and plasmas in the shocked region of the disk are accelerated by J \times B force to form bipolar relativistic jets. In order to investigate variabilities of generated relativistic jets and magnetic field structure inside jets, we have performed calculations using the 3-D GRMHD code with a full 3-dimensional system. We will investigate how the third dimension affects the global disk dynamics and jet generation.
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