Twin peak HF QPOs as a spectral imprint of dual oscillation modes of accretion tori

TL;DR

This paper models twin peak HF QPOs as spectral signatures of dual oscillation modes in accretion tori around compact objects, using relativistic simulations to match observed frequency ratios and iron line profiles.

Contribution

It introduces a novel spectral modeling approach linking twin peak QPOs to specific oscillation modes in accretion tori, incorporating relativistic ray-tracing and analysis of inclination and spin effects.

Findings

Power spectra show dominant peaks with 3/2 frequency ratio across various inclinations and spins.

Iron line profiles significantly depend on observer inclination.

Simulation results align with observed twin peak QPO characteristics.

Abstract

High frequency (millisecond) quasi-periodic oscillations (HF QPOs) are observed in the X-ray power-density spectra of several microquasars and low mass X-ray binaries. Two distinct QPO peaks, so-called twin peak QPOs, are often detected simultaneously exhibiting their frequency ratio close or equal to 3/2. Following the analytic theory and previous studies of observable spectral signatures, we aim to model the twin peak QPOs as a spectral imprint of specific dual oscillation regime defined by a combination of the lowest radial and vertical oscillation mode of optically thick slender tori with constant specific angular momentum. We examined power spectra and fluorescent K$\alpha$ iron line profiles for two different simulation setups with the mode frequency relations corresponding to the epicyclic resonance HF QPOs model and modified relativistic precession QPOs model. We use relativistic ray-tracing implemented in parallel simulation code LSDplus. In the background of the Kerr spacetime geometry, we analyze the influence of the distant observer inclination and the spin of the central compact object. Relativistic optical projection of the oscillating slender torus is illustrated by images in false colours related to the frequency shift. We show that performed simulations yield power spectra with the pair of dominant peaks corresponding to the frequencies of radial and vertical oscillation modes with the proper ratio equal to 3/2 on a wide range of inclinations and spin values. We also discuss exceptional cases of a very small and very high inclination as well as unstable high spin relativistic precession-like configuration predicting constant frequency ratio equal to 1/2. We demonstrate signifiant dependency of broadened K$\alpha$ iron line profiles on the inclination of the distant observer.