Stability of accretion disk around rotating black holes: a pseudo-general-relativistic fluid dynamical study

Abstract

We discuss the solution of accretion disk when the black hole is chosen to be rotating. We study, how the fluid properties get affected for different rotation parameters of the black hole. We know that no cosmic object is static in Universe. Here the effect of the rotation of the black hole to the space-time is considered following an earlier work of the author, where the pseudo-Newtonian potential was prescribed for the Kerr geometry. We show that, with the inclusion of rotation of the black hole, the valid disk parameter region dramatically changes and disk becomes unstable. Also we discuss about the possibility of shock in accretion disk around rotating black holes. When the black hole is chosen to be rotating, the sonic locations of the accretion disk get shifted or disappear, making the disk unstable. To bring it in the stable situation, the angular momentum of the accreting matter has to be reduced/enhanced (for co/counter-rotating disk) by means of some physical process.

24 Latex pages including 7 figures; Accepted for publication in Astrophysical Journal

References in corpus (4)

• Description of Pseudo-Newtonian Potential for the Relativistic Accretion Disk around Kerr Black Holes
• Stability of Accretion Disks in Presence of Nucleosynthesis
• Effect of Coriolis force on Accretion Flows around Rotating Compact Object
• Hydrodynamical Study of Advective Accretion flow around Neutron Stars

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