Radiatively Inefficient Accretion Flows(Session 4 : Theoretical/Numerial Approaches to the Accretion Physics)

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概要

• 論文の詳細を見る

• Black hole accretion flows could be radiatively inefficient when a mass supply rate is either much less or much larger than the Eddington rate. Because of lack of radiative cooling, such flows are hot and geometrically thick. This article will review different models and different approaches to study radiatively inefficient accretion flows. Initially, the flows were studied as purely hydrodynamic viscous flows. It was shown analytically and numerically that the hydrodynamic flows are convectively unstable. Convection significantly changes the flow structure, flattening the radial density profile and decreasing the accretion rate. More recently, numerical MHD models of the flows have been developed by several groups. In these models the problems of angular momentum transport and dissipation of binding energy can be solved self-consistently. The MHD models show the flow's strong dependence on the topology of the magnetic field, and some models show efficient convection.

• 理論物理学刊行会の論文
• 2004-11-15

著者

• IGUMENSHCHEV Igor

  Laboratory for Laser Energetics, University of Rochester

• Igumenshchev I

  Univ. Rochester Ny Usa

• Igumenshchev Igor

  Laboratory For Laser Energetics University Of Rochester

関連論文

• Magnetically Arrested Disk : an Energetically Efficient Accretion Flow
• Radiatively Inefficient Accretion Flows(Session 4 : Theoretical/Numerial Approaches to the Accretion Physics)
• Radiatively Inefficient Accretion Flows(Session 4 : Theoretical/Numerial Approaches to the Accretion Physics)

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