Truncated accretion discs in black hole X-ray binaries: dynamics and variability signatures

TL;DR

This study uses GRMHD simulations to explore how truncated accretion discs around black holes oscillate and influence X-ray variability, revealing correlations between magnetic fields, oscillation frequencies, and shock phenomena.

Contribution

It introduces a detailed GRMHD simulation framework for truncated accretion discs, linking disc dynamics with observable X-ray variability signatures in black hole binaries.

Findings

Inner disc edge oscillates quasi-periodically, producing low-frequency QPOs.

Magnetic field strength and resistivity influence QPO frequency.

Transient shocks form during high accretion stages, affecting radiative properties.

Abstract

Variable features in black hole X-ray Binaries (BH-XRBs) are observed in different energy ranges and time scales. The physical origin of different spectral states in BH-XRBs and their relations with the underlying accretion disc are still elusive. To investigate the intermediate state of BH-XRBs during outburst, we simulate a truncated accretion disc around a Kerr black hole using a general relativistic magneto-hydrodynamical (GRMHD) framework under axisymmetry with adaptively refined mesh. Additionally, we have also carried out radiative transfer calculations for understanding the implications of disc dynamics on emission. Dynamically, the inner edge of the truncated accretion disc oscillates in a quasi-periodic fashion (QPO). The QPO frequency of oscillations $(\nu_{\rm QPO, max})$ increases as the magnetic field strength and magnetic resistivity increase. However, as the truncation radius increases, $\nu_{\rm QPO, max}$ decreases. In our simulation models, frequency varies between $7\times(10M_{\odot}/M_{\rm BH})$ Hz $\lesssim\nu_{\rm QPO, max}\lesssim20 \times (10M_{\odot}/M_{\rm BH})$ Hz, which is in the range of low-frequency QPOs. We further find evidence of transient shocks in the highly accreting stage during oscillation. Such a transient shock acts as an extended hot post-shock corona around the black hole that has an impact on its radiative properties. The radiative transfer calculations show signatures of these oscillations in the form of modulation in the edge-brightened structure of the accretion disc.