A General Relativistic Magnetohydrodynamic Model of High Frequency Quasi-periodic Oscillations in Black Hole Low-Mass X-ray Binaries

Abstract

We suggest a possible explanation for the high frequency quasi-periodic oscillations (QPOs) in black hole low mass X-ray binaries. By solving the perturbation general relativistic magnetohydrodynamic equations, we find two stable modes of the Alfven wave in the the accretion disks with toroidal magnetic fields. We suggest that these two modes may lead to the double high frequency QPOs if they are produced in the transition region between the inner advection dominated accretion flow and the outer thin disk. This model naturally accounts for the 3 : 2 relation for the upper and lower frequencies of the QPOs, and the relation between the black hole mass and QPO frequency.

Accepted for publication in The Astrophysical Journal

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Cited by in corpus (4)

• Super-Strong Magnetic Fields of Neutron Stars in Be X-Ray Binaries Estimated with New Torque and Magnetosphere Models
• Stochastic oscillations of general relativistic disks
• The Magneto Hydro Dynamical Model of KHz Quasi Periodic Oscillations in Neutron Star Low Mass X-ray Binaries (II)
• A possible explanation of the parallel tracks in kilohertz quasi-periodic oscillations from low-mass-X-ray binaries