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General Relativistic Magnetohydrodynamic Simulations of CollapsarsWe have performed 2.5-dimensional general relativistic magnetohydrodynamic (MHD) simulations of collapsars including a rotating black hole. Initially, we assume that the core collapse has failed in this star. A rotating black hole of a few solar masses is inserted by hand into the calculation. The simulation results show the formation of a disklike structure and the generation of a jetlike outflow near the central black hole. The jetlike outflow propagates and accelerated mainly by the magnetic field. The total jet velocity is approximately 0.3c. When the rotation of the black hole is faster, the magnetic field is twisted strongly owing to the frame-dragging effect. The magnetic energy stored by the twisting magnetic field is directly converted to kinetic energy of the jet rather than propagating as an Alfven wave. Thus, as the rotation of the black hole becomes faster, the poloidal velocity of the jet becomes faster.
Document ID
20050205820
Acquisition Source
Marshall Space Flight Center
Document Type
Preprint (Draft being sent to journal)
Authors
Mizuno, Yosuke
(National Space Science and Technology Center Huntsville, AL, United States)
Yamada, S.
(Waseda Univ. Tokyo, Japan)
Koider, S.
(Toyama Univ. Toyama, Japan)
Shipata, K.
(Kyoto Univ. Japan)
Date Acquired
August 23, 2013
Publication Date
January 1, 2005
Subject Category
Plasma Physics
Meeting Information
Meeting: Ultra-Relativistic Jets in Astrophysics Observations, Theory, Simulations
Location: Banff, Alberta
Country: Canada
Start Date: July 11, 2005
End Date: July 15, 2005
Distribution Limits
Public
Copyright
Work of the US Gov. Public Use Permitted.

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