Spectro-temporal studies of rapid transition of the quasi periodic oscillations in the black hole source H1743-322

TL;DR

This study investigates rapid transitions of quasi-periodic oscillations (QPOs) in black hole source H1743-322, revealing their association with jet activity and corona dynamics through spectral and timing analysis of RXTE data.

Contribution

It identifies and characterizes eight rapid QPO transition events and links them to jet and corona behavior, providing new insights into accretion-ejection mechanisms.

Findings

Eight QPO transition events identified with different QPO types.

QPO disappearance correlates with stable inner disk radius but varying power-law indices.

Type-B QPOs linked to precessing weak jets; Type-C QPOs associated with stronger jets.

Abstract

An appearance or disappearance of QPOs associated with the variation of X-ray flux can be used to decipher the accretion ejection mechanism of black hole X-ray sources. We searched and studied such rapid transitions in H1743-322 using RXTE archival data and found eight such events, where QPO vanishes suddenly along with the variation of X-ray flux. The appearance/disappearance of QPOs were associated to the four events exhibiting type-B QPOs at $\sim$ 4.5 Hz, one with type-A QPO at $\nu$ $\sim$ 3.5 Hz, and the remaining three were connected to type-C QPOs at $\sim$ 9.5 Hz. Spectral studies of the data unveiled that an inner disk radius remained at the same location around 2-9 r$_g$ , depending on the used model but power-law indices were varying, indicating that either corona or jet is responsible for the events. The probable ejection radii of corona were estimated to be around 4.2-15.4 r$_g$ based on the plasma ejection model. Our X-ray and quasi-simultaneous radio correlation studies suggest that the type-B QPOs are probably related to the precession of a weak jet though a small and weak corona is present at its base and the type-C QPOs are associated to the base of a relatively strong jet which is acting like a corona.