  We report the detection of type-B quasi-periodic oscillation (QPO) of the
black hole X-ray binary Swift J1728.9-3613 observed by NICER during the 2019
outburst. A type- B QPO was observed for the first two days and it disappeared
as flux increased, but again appeared at $\sim$ 7.70 Hz when flux was
dramatically decreased. The source was found in the soft-intermediate state
during these observations. We further studied the energy dependence of the QPO.
We found that QPO was observed only for a higher energy range implying that the
origin of QPO is possibly due to the corona emitting higher energy photons by
the inverse Compton process. The variation of spectral parameters can be
explained with the disk truncation model. The fractional rms found to be
monotonically increased with energy. The phase lag spectrum followed the
U-shaped curve. The rms and phase lag spectrum are modelled and explained with
the single-component comptonization model vkompthdk.
