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

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arxiv astro-ph/9709085 v1 pith:EMLBNJOU submitted 1997-09-10 astro-ph

Luigi Stella , Mario Vietri This is my paper · ORCID
classification astro-ph
keywords frequencyneutronprecessionqposstarbinariesdiskinnermost
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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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Cited by 11 Pith papers

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    Treating QPO-emitting disk clumps as spinning test bodies reproduces the observed twin kHz QPOs without the effective de Sitter term, with fits preferring n≈2 thin-disk structures for Schwarzschild and n≈1 for Kerr.

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    GRB 090510 is modeled as a merger of two ~1.2 solar mass neutron stars that forms a spinning 2.36 solar mass black hole, with each emission phase traced to a different energy source.

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    The paper derives spin precession frequencies for a rotating naked singularity spacetime, shows they match Kerr in the weak field, and uses quasi-periodic oscillations to constrain and disfavor the model.

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    astro-ph.HE 2025-01 conditional novelty 5.0 of 10

    Type-C QPOs in the 2021 outburst of 4U 1630-472 show a strong photon index versus frequency correlation and a significant Q-factor break at about 2.31 Hz.

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  7. A 0.03 Hz Radio Quasi-periodic Oscillation During the 2025 Flare of GRS 1915+105

    astro-ph.HE 2026-06 unverdicted novelty 4.0 of 10

    A recurring 0.03 Hz radio QPO was detected in the 2025 flare of GRS 1915+105 at >5.9 sigma in one epoch, identical across S- and X-bands and prior years, indicating an intrinsic accretion-jet timescale.

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    For a nonminimally coupled magnetic AdS black hole, the Lyapunov exponent and QPO frequencies both reproduce the swallowtail branch structure of the Van der Waals-like thermodynamic phase transition.

  11. Constraints on extra charges in dyonic Kerr-Newman-Kasuya-Taub-NUT black hole from the observations of quasi-periodic oscillations

    astro-ph.HE 2025-07 conditional novelty 4.0 of 10

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