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G. A. Richardson, K.-I. Nishikawa, R. Preece (NSSTC), P. Hardee (Univ. Alabama, Tuscaloosa), S. Koide (Toyama Univ.), K. Shibata (Kyoto Univ.), T. Kudoh (Univ. of Western Ontario), H. Sol (Obs. de Paris-Meudon), J. P. Hughes (Rutgers Univ.), J. Fishman (NSSTC)
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 (in a steady-state infalling state) around a non-rotating black hole using 3-D GRMHD with the ``axisymmetry'' along the z-direction. The magnetic field is tightly twisted by the rotation of the accretion disk, and plasmas in the shocked region of the disk are accelerated by the J \times B force to form bipolar relativistic jets.
In order to investigate variabilities of generated relativistic jets and the magnetic field structure inside jets, we have performed calculations using the 3-D GRMHD code with a full 3-dimensional system without the axisymmetry. We have investigated how the third dimension affects the global disk dynamics and jet generation. We will perform simulations with various incoming flows from an accompanying star.
If you would like more information about this abstract, please follow the link to http:/gammaray.nsstc.nasa.gov/~nishikawa. 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: georgia.richardson@msfc.nasa.gov
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Bulletin of the American Astronomical Society, 34, #4
© 2002. The American Astronomical Soceity.