General Relativistic Magnetohydrodynamic Simulations of Black Hole Accretion Disks(Session 4 : Theoretical/Numerial Approaches to the Accretion Physics)

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概要

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• Observations are providing increasingly detailed quantitative information about the accretion flows that power such high energy systems as X-ray binaries and active galactic nuclei. Analytic models of such systems must rely on assumptions such as regular flow geometry and a simple, parameterized stress. Global numerical simulations offer a way to investigate the basic physical dynamics of accretion flows without these assumptions. For black hole accretion studies one solves the equations of general relativistic magnetohydro-dynamics. Magnetic fields are of fundamental importance to the structure and evolution of accretion disks because magnetic turbulence is the source of the anomalous stress that drives accretion. We have developed a three-dimensional general relativistic magnetohydrodynamic simulation code to evolve time-dependent accretion systems self-consistently. Recent global simulations of black hole accretion disks suggest that the generic structure of the accretion flow is usefully divided into five regimes : the main disk, the inner disk, the corona, the evacuated funnel, and the funnel wall jet. The properties of each of these regions are summarized.

• 理論物理学刊行会の論文
• 2004-11-15

著者

• De Villiers

  Department Of Astronomy University Of Virginia

• HAWLEY John

  Department of Astronomy, University of Virginia

• Hawley John

  Department Of Astronomy University Of Virginia

• DE VILLIERS

  Department of Astronomy, University of Virginia

関連論文

• General Relativistic Magnetohydrodynamic Simulations of Black Hole Accretion Disks(Session 4 : Theoretical/Numerial Approaches to the Accretion Physics)
• General Relativistic Magnetohydrodynamic Simulations of Black Hole Accretion Disks(Session 4 : Theoretical/Numerial Approaches to the Accretion Physics)

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