Adding a quadratic radial correction changes the predicted lower QPO frequency near the ISCO, but fits to eight neutron stars show it is insufficient to rescue the relativistic precession model.
QPOs in Cataclysmic Variables and in X-ray Binaries
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abstract
Recent observations, reported by Warner and Woudt, of Dwarf Nova Oscillations (DNOs) exhibiting frequency drift, period doubling, and 1:2:3 harmonic structure, can be understood as disc oscillations that are excited by perturbations at the spin frequency of the white dwarf or of its equatorial layers. Similar quasi-periodic disc oscillations in black hole low-mass X-ray binary (LMXB) transients in a 2:3 frequency ratio show no evidence of frequency drift and correspond to two separate modes of disc oscillation excited by an internal resonance. Just as no effects of general relativity play a role in white dwarf DNOs, no stellar surface or magnetic field effects need be invoked to explain the black hole QPOs.
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Generalizing the relativistic precession model of quasi-periodic oscillations through anharmonic corrections
Adding a quadratic radial correction changes the predicted lower QPO frequency near the ISCO, but fits to eight neutron stars show it is insufficient to rescue the relativistic precession model.