  Coronal bright points (BPs) are small-scale luminous features seen in the
solar corona. Quasi-periodic brightenings are frequently observed in the BPs
and are generally linked with underneath magnetic flux changes. We study the
dynamics of a BP seen in the coronal hole using the Atmospheric Imaging
Assembly (AIA) images, the Helioseismic and Magnetic Imager (HMI) magnetogram
on board the Solar Dynamics Observatory (SDO) and spectroscopic data from the
newly launched Interface Region Imaging Spectrograph (IRIS). The detailed
analysis shows that the BP evolves throughout our observing period along with
changes in underlying photospheric magnetic flux and shows periodic
brightenings in different EUV and FUV images. With highest possible spectral
and spatial resolution of IRIS, we attempted to identify the sources of these
oscillations. IRIS sit and stare observation provided a unique opportunity to
study the time evolution of one foot point of the BP as the slit position
crossed it. We noticed enhanced line profile asymmetry, enhanced line width,
intensity enhancements and large deviation from the average Doppler shift in
the line profiles at specific instances which indicate the presence of sudden
flows along the line of sight direction. We propose that transition region
explosive events (EEs) originating from small scale reconnections and the
reconnection outflows are affecting the line profiles. The correlation between
all these parameters is consistent with the repetitive reconnection scenario
and could explain the quasi-periodic nature of the brightening.
