A new model for QPOs in accreting black holes: application to the microquasar GRS 1915+105

TL;DR

This paper proposes a resonant oscillation model involving spiral density waves and vertical epicyclic oscillations in accretion disks around black holes, successfully explaining high-frequency QPOs in GRS 1915+105 and constraining black hole parameters.

Contribution

It introduces a new resonance-based model for QPOs in black hole binaries, applying Kerr spacetime to match observed frequencies and predict additional spectral features.

Findings

Reproduces observed HF-QPO frequencies in GRS 1915+105.

Predicts additional spectral features at specific frequencies.

Constrains black hole mass and spin from QPO data.

Abstract

(abridged) In this paper we extend the idea suggested previously by Petri (2005a,b) that the high frequency quasi-periodic oscillations observed in low-mass X-ray binaries may be explained as a resonant oscillation of the accretion disk with a rotating asymmetric background (gravitational or magnetic) field imposed by the compact object. Here, we apply this general idea to black hole binaries. It is assumed that a test particle experiences a similar parametric resonance mechanism such as the one described in paper I and II but now the resonance is induced by the interaction between a spiral density wave in the accretion disk, excited close to the innermost stable circular orbit, and vertical epicyclic oscillations. We use the Kerr spacetime geometry to deduce the characteristic frequencies of this test particle. The response of the test particle is maximal when the frequency ratio of the two strongest resonances is equal to 3:2 as observed in black hole candidates. Finally, applying our model to the microquasar GRS 1915+105, we reproduce the correct value of several HF-QPOs. Indeed the presence of the 168/113/56/42/28 Hz features in the power spectrum time analysis is predicted. Moreover, based only on the two HF-QPO frequencies, our model is able to constrain the mass $M_{\rm BH}$ and angular momentum $a_{\rm BH}$ of the accreting black hole.