[Previous] | [Session 69] | [Next]
K.-I. Nishikawa (Rutgers Univ.), S. Koide (Toyama Univ.), K. Shibata (Kyoto Univ.), T. Kudoh (NAO, Japan), J. Frank (LSU), H. Sol (Obs. de Paris-Meudon)
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 or in hydrostatic equilibrium) 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.
If you would like more information about this abstract, please follow the link to http://www.physics.rutgers.edu/~kenichi. This link was provided by the author. When you follow it, you will leave the Web site for this meeting; to return, you should use the Back comand on your browser.
The author(s) of this abstract have provided an email address for comments about the abstract: kenich@physics.rutgers.edu