X-ray variability time scales in Active Galactic Nuclei

TL;DR

This paper links X-ray variability time scales in AGN to clumpy accretion flow models, deriving a characteristic time scale that matches observed PSD break times, supporting a physical interpretation of variability origins.

Contribution

It introduces a model-based derivation of X-ray variability time scales in AGN that aligns with observed PSD break times, incorporating black hole mass and accretion rate dependencies.

Findings

Derived a characteristic X-ray time scale $ au_{X}$ consistent with observed PSD breaks.

Model reproduces the empirical relation between break time scale and black hole parameters.

Supports the physical interpretation of variability time scales in terms of accretion flow shocks.

Abstract

X-ray variability in Active Galactic Nuclei (AGN) is commonly analysed in terms of the Power Spectral Density (PSD). The break observed in the power spectrum can be interpreted as a characteristic X-ray variability time scale. Here we study variability properties within the framework of clumpy accretion flows, in which shocks between accreting elements account for the UV and X-ray emissions. We derive a characteristic X-ray time scale, $\tau_{X}$, and compare it with the measured PSD break time scale, $T_{B}$. A quite good agreement is found in both magnitude and trend. In particular, the model dependence on black hole mass and accretion rate precisely reproduces the empirical relation obtained by McHardy et al. (2006). We suggest a possible physical interpretation of the break time scale and briefly discuss the related aspects of optical/UV variability and correlations between different wavelengths.