Simple analytic formula relating the mass and spin of accreting compact objects to their rapid X-ray variability

TL;DR

This paper derives a simple analytic formula linking the mass and spin of accreting compact objects to their high-frequency QPOs, extending previous models to include rotation and oblateness effects.

Contribution

It introduces an extended formula applicable to rotating Kerr and Hartle-Thorne spacetimes, unifying predictions of the CT and RP models for QPO frequencies.

Findings

The formula accurately reproduces QPO frequencies in Schwarzschild and Kerr spacetimes.

It demonstrates better fits to NS QPO data than the relativistic precession model.

The model is compatible with realistic NS mass and spin values.

Abstract

Following the previous research on epicyclic oscillations of accretion disks around black holes (BHs) and neutron stars (NSs), a new model of high-frequency quasi-periodic oscillations (QPOs) has been proposed (CT model), which deals with oscillations of fluid in marginally overflowing accretion tori (i.e., tori terminated by cusps). According to preliminary investigations, the model provides better fits of the NS QPO data compared to the relativistic precession (RP) model. It also implies a significantly higher upper limit on the Galactic microquasars BH spin. A short analytic formula has been noticed to well reproduce the model's predictions on the QPO frequencies in Schwarzschild spacetimes. Here we derive an extended version of this formula that applies to rotating compact objects. We start with the consideration of Kerr spacetimes and derive a formula that is not restricted to a particular specific angular momentum distribution of the inner accretion flow, such as Keplerian or constant. Finally, we consider Hartle-Thorne spacetimes and include corrections implied by the NS oblateness. For a particular choice of a single parameter, our relation provides frequencies predicted by the CT model. For another value, it provides frequencies predicted by the RP model. We conclude that the formula is well applicable for rotating oblateness NSs and both models. We briefly illustrate application of our simple formula on several NS sources and confirm the expectation that the CT model is compatible with realistic values of the NS mass and provides better fits of data than the RP model.