Tidal disruption of small satellites orbiting black holes

TL;DR

This paper models how tidal forces deform small orbiting clumps around black holes, producing simulated light curves and power spectra that match observed high-frequency QPOs in LMXBs, revealing insights into accretion dynamics.

Contribution

It introduces a numerical simulation approach to reproduce twin high-frequency QPOs caused by tidal deformation near black holes, aligning with observational data.

Findings

Simulated power spectra match observed high-frequency QPOs in XTE J1550-564.

Twin peaks correspond to Keplerian and combined frequencies.

Tidal deformation can explain the origin of high-frequency QPOs.

Abstract

Low Mass X-ray Binaries (LMXBs) with either a black hole or a neutron star show power spectra characterised by Quasi Periodic Oscillations (QPOs). Twin peak high frequency QPOs are characterised by frequencies that are typical for matter orbiting within 10 r_g from the compact object. We consider clumps of material orbiting a Schwarzschild black hole, that are deformed by tidal interaction. We present some preliminary calculations of corresponding light curves and power spectra. We were able to fit the simulated power spectra with the high frequency part of the power spectra observed in the LMXB XTE J1550-564 containing a black hole. Our numerical simulations reproduce the twin high frequency QPOs and the power-law. The lower peak corresponds to the Keplerian frequency, the upper one to the sum of the Keplerian and the radial frequency.