Magnetorotational Instability around a Rotating Black Hole

Abstract

The magnetorotational instability(MRI) in the Kerr spacetime is studied on a 3+1 viewpoint. The Maxwell's equations are expressed in a circularly orbiting observer's frame that co-rotates with matter in Keplerian orbits. There exist large proper growth rates in MRI around a rapidly rotating black hole. The large "centrifugal force" and the rapid variations of magnetic fields are caused by the rotation of spacetime geometry. As the result, in the extreme Kerr case the maximum proper growth rate at $r=r_{ms}$ becomes about twelve times as large as that in Schwartzshield case.

18pages, 9figures

References in corpus (11)

• Hyper-Accreting Black Holes and Gamma-Ray Bursts
• A Measurement of the Electromagnetic Luminosity of a Kerr Black Hole
• Magnetically Driven Accretion Flows in the Kerr Metric I: Models and Overall Structure
• Neutrino trapping and accretion models for Gamma-Ray Bursts
• Magnetically Driven Accretion in the Kerr Metric III: Unbound Outflows
• Can neutrino-cooled accretion disk be an origin of gamma-ray bursts?
• Magnetically Driven Accretion Flows in the Kerr Metric II: Structure of the Magnetic Field
• Magnetically Driven Accretion Flows in the Kerr Metric IV: Dynamical Properties of the Inner Disk
• Advection Dominated Accretion Flows in the Kerr Metric: I. Basic Equations
• Global General Relativistic Magnetohydrodynamic Simulations of Accretion Tori
• The Magnetorotational Instability in the Kerr Metric

Cited by in corpus (5)

• Numerical 3+1 general relativistic magnetohydrodynamics: a local characteristic approach
• Magnetorotational instability in neutron star mergers: impact of neutrinos
• Analog rotating black holes in a magnetohydrodynamic inflow
• Magnetic amplification in premerger neutron stars through resonance-induced magnetorotational instabilities
• Resistive Accretion Flows around a Kerr Black Hole