  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.
