  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.
