Type-B QPOs in the black hole source H1743-322 and their association with Comptonization region and Jet

TL;DR

This study investigates the nature of type-B QPOs in H1743-322, linking them to jet activity and Comptonization region structure, through spectral, timing, and radio observations, and proposes a model involving jet and precession effects.

Contribution

It provides new insights into the production mechanism of type-B QPOs, suggesting their association with jets and the structure of the Comptonization region, supported by spectral and radio analysis.

Findings

Type-B QPOs are linked to jet activity in H1743-322.

Spectral analysis shows differences in Comptonization region structure between QPO types.

Radio and spectral trends support jet involvement in type-B QPOs.

Abstract

The connection of type-B QPOs to the hot flow in the inner accretion disk region is vaguely understood in black hole X-ray binaries. We performed spectral and timing studies of twenty-three observations where type-C and type-B QPOs with similar centroid frequencies (~ 6 Hz) occurred. Their spectral differences were used to understand the production mechanism of type-B QPOs, along with the quasi-simultaneous radio observations. Based on the spectral results, we did not notice many variations in the Comptonization parameters and the inner disk radius during type-C and type-B QPOs. We found that the structure of the Comptonization region has to be different for observations associated with type-C and type-B QPOs based on the CompTT model. Radio flux density vs QPO width, soft to hard flux ratio, and QPO width vs inner disk temperature, were found to follow certain trends, suggesting that a jet could be responsible for the type-B QPOs in H1743-322. Further studies are required to uniquely constrain this scenario. In a case study where a gradual transition from type-C to type-B QPO was noticed, we found that the spectral changes could be explained by the presence of a jet or a vertically extended optically thick Comptonization region. The geometrical Lense-Thirring precession model with a hot flow and a jet in the inner region was incorporated to explain the spectral and timing variations.