General relativistic magnetohydrodynamic simulations of collapsars: Rotating black hole cases

Mizuno, Y. and Yamada, S. and Koide, S. and Shibata, K. (2005) General relativistic magnetohydrodynamic simulations of collapsars: Rotating black hole cases. Il nuovo cimento C, 28 (3). pp. 423-426. ISSN 1826-9885

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We 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 ∼ 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 Alfv´en wave. Thus, as the rotation of the black hole becomes faster, the poloidal velocity of the jet becomes faster.

Item Type: Article
Additional Information: Paper presented at the “4th Workshop on Gamma-Ray Burst in the Afterglow Era”, Rome, October 18-22, 2004.
Uncontrolled Keywords: γ-ray sources; γ-ray bursts ; Magnetohydrodynamics and plasmas ; Relativity and gravitation
Subjects: 500 Scienze naturali e Matematica > 520 Astronomia e scienze connesse
Depositing User: Marina Spanti
Date Deposited: 16 Mar 2020 10:49
Last Modified: 16 Mar 2020 10:49

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