The Relativistic Precession Model for QPOs in Low Mass X-ray Binaries

Details The Relativistic Precession Model for QPOs in Low Mass X-ray Binaries The Relativistic Precession Model for QPOs in Low Mass X-ray Binaries

2000-11-21

arxiv.org/abs/astro-ph/0011395v1

Astronomy and Astrophysics

Astrophysics

12 pages, 2 embedded figures, Proceedings of X-ray Astronomy '999 - Stellar Endpoints, AGN and the Diffuse Background, 2000. G

Scientific paper

10.1063/1.1434649

The relativistic precession model for quasi periodic oscillations, QPOs, in low mass X-ray binaries is reviewed. The behaviour of three simultaneous types of QPOs is well matched in terms of the fundamental frequencies for geodesic motion in the strong field of the accreting compact object for reasonable star masses and spin frequencies. The model ascribes the higher frequency kHz QPOs, the lower frequency kHz QPOs and the horizontal branch oscillations to the Keplerian, periastron precession and nodal precession frequencies of matter inhomogeneities orbiting close to the inner edge of the accretion disk. The remarkable correlation between the centroid frequency of QPOs in both neutron star and black hole candidate low mass X-ray binaries is very well fit by the model. QPOs from low mass X-ray binaries might provide an unprecedented laboratory to test general relativity in the strong field regime.

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