Dual-Corona Comptonization model for the Type-B Quasi-Periodic Oscillations in GX 339-4

TL;DR

This paper models the type-B QPOs in GX 339-4 using a dual-corona Comptonization approach, fitting spectral and timing data to reveal the physical properties of the inner accretion regions during outburst.

Contribution

It introduces a dual-corona Comptonization model that explains the spectral and timing features of type-B QPOs in GX 339-4, linking variability to interacting Comptonizing regions.

Findings

Fractional rms spectrum remains constant below 1.8 keV and increases at higher energies.

Lag spectrum shows a U-shape, decreasing then increasing with energy.

Model constrains physical parameters of the Comptonizing regions.

Abstract

Characterising the fast variability in black-hole low-mass X-ray binaries (BHXBs) can help us understand the geometrical and physical nature of the innermost regions of these sources. Particularly, type-B quasi-periodic oscillations (QPOs), observed in BHXBs during the soft-intermediate state (SIMS) of an outburst, are believed to be connected to the ejection of a relativistic jet. The X-ray spectrum of a source in the SIMS is characterised by a dominant soft blackbody-like component - associated with the accretion disc - and a hard component - associated with a Comptonizing region or corona. Strong type-B QPOs were observed by NICER and AstroSat in GX 339$-$4 during its 2021 outburst. We find that the fractional rms spectrum of the QPO remains constant at $\sim$1 per cent for energies below $\sim$1.8 keV and then increases with increasing energy up to $\sim$17 per cent at 20$-$30 keV. We also find that the lag spectrum is "U-shaped", decreasing from $\sim$1.2 rad at 0.7 keV to 0 rad at $\sim$3.5 keV, and increasing again at higher energies up to $\sim$0.6 rad at 20$-$30 keV. Using a recently developed time-dependent Comptonization model, we fit simultaneously the fractional rms and lag spectra of the QPO and the time-averaged energy spectrum of GX 339$-$4 to constrain the physical parameters of the region responsible for the variability we observe. We suggest that the radiative properties of the type-B QPOs observed in GX 339$-$4 can be explained by two physically-connected Comptonizing regions that interact with the accretion disc via a feedback loop of X-ray photons.