Lense-Thirring Precession and QPOs in Low Mass X-Ray Binaries

Details Lense-Thirring Precession and QPOs in Low Mass X-Ray Binaries Lense-Thirring Precession and QPOs in Low Mass X-Ray Binaries

1997-09-10

arxiv.org/abs/astro-ph/9709085v1

Astrophys.J. 492 (1998) L59

Astronomy and Astrophysics

Astrophysics

Accepted for publication in Astrophysical Journal Letters. AASTEX needed

Scientific paper

10.1086/311075

We show in this Letter that relativistic dragging of inertial frames around fast rotating collapsed stars is substantial and can give rise to observable effects. We apply this to the kHz quasi periodic oscillations (QPOs) sources, low mass X-ray binaries (LMXRBs) containing an accreting neutron star. Within the beat frequency model, both the Keplerian frequency of the innermost region of the accretion disk (~0.3-1.2 kHz) and the neutron star spin frequency (~0.3-0.4 kHz) are directly observed. From these the Lense-Thirring precession frequency (tens of Hz) of the same material in the innermost disk regions which gives rise to the kHz QPOs is determined within a factor of ~4, depending on the neutron star equation of state. The classical contribution from neutron star oblateness decreases the precession frequency slightly. The broad peaks at frequencies ~20-40 Hz in the power spectra of the Atoll-sources 4U1728-34, 4U0614+091 and KS1731-260 and their variations with the higher kHz QPO frequency are well matched by Lense-Thirring precession of material in the innermost disk region. We also suggest that the ~15-50 Hz horizontal branch QPOs of GX5-1 and GX17+2 (and likewise other Z-type low mass X-ray binaries) arise from the same mechanism.

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