Abstract
The observed quasi-periodic oscillations (QPOs) in neutron star and black hole X-ray binaries have been suggested to be probably related to the oscillation modes in a relativistic accretion disk. Here we studied the non-damping feature of some oscillation modes by considering the radial perturbations and viscosity effects. We found that the non-damping fundamental modes can be amplified significantly in the inner disk when the viscosity parameter increases. Three of these non-damping modes are trapped in the inner disk and their trapping sizes depend on the radial wavenumber, Mach number and the spin of the central object. Some observed properties of kilohertz QPOs in neutron star X-ray binaries and hundred-hertz QPOs in black hole X-ray binaries may be explained by these trapped non-damping oscillation modes.
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