A toy model for coupling accretion disk oscillations to the neutron star spin

Abstract

Lee, Abramowicz & Kluzniak (2004) demonstrated numerically that rotation of neutron star couples with oscillations of its accretion disk, and excites resonances. No specific coupling was assumed, but magnetic field was suggested as the most likely one. Following this idea, we show (Petri 2005) that if the neutron star is non-axially symmetric and rotating, its gravity may provide the coupling and excite resonances. Here, we return to the original suggestion that the coupling is of a magnetic origin, and demonstrate how does it work in terms of a simple, analytic toy-model.

Accepted by A&A

References in corpus (6)

• Non-linear resonance in nearly geodesic motion in low-mass X-ray binaries
• Quasi-periodic X-ray brightness fluctuations in an accreting millisecond pulsar
• Resonance in Forced Oscillations of an Accretion Disk and Kilohertz Quasi Periodic Oscillations
• An explanation for the kHz-QPO twin peaks separation in slow and fast rotators
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Cited by in corpus (6)

• On mass-constraints implied by the relativistic precession model of twin-peak quasi-periodic oscillations in Circinus X-1
• Resonant radii of kHz quasi-periodic oscillations in Keplerian discs orbiting neutron stars
• A new model for QPOs in accreting black holes: application to the microquasar GRS 1915+105
• Forced oscillations in a hydrodynamical accretion disk and QPOs
• Evidences of an innermost stable bound orbit predicted by general relativity from the amplitude of the twin-peak quasi-periodic oscillations
• Constraining the mass and moment of inertia of neutron stars from quasi-periodic oscillations in X-ray binaries