Abstract
We performed 1.5D general relativistic simulations using a Kerr metric without disk viscosity for a model of high frequency quasi-periodic oscillations (QPOs) in microquasars. We found that quasi-periodic inward shock waves propagate from the accretion disk toward the black hole when we initially inject a disturbance into the disk. The frequency of the shock formation is approximately equal to the maximum epicyclic frequency in the disk (κ m a x ), which is on the order of the frequency of high frequency QPOs in microquasars. κ m a x depends on the rotation of the black hole, and therefore we can estimate the value of the spin parameter of a black hole candidate (BHC) in a microquasar by comparing the high frequency QPO with κ m a x . We found that such values can be roughly estimated as 0.0 < a < 0.4 for CIRS 1915+105 and 0.85 < a < 1.0 for GRO J1655-40.
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