  Intensity oscillations of coronal bright points (BPs) have been studied for
past several years. It has been known for a while that these BPs are closed
magnetic loop like structures. However, initiation of such intensity
oscillations is still an enigma. There have been many suggestions to explain
these oscillations, but modeling of such BPs have not been explored so far.
Using a multithreaded nanoflare heated loop model we study the behavior of such
BPs in this work. We compute typical loop lengths of BPs using potential field
line extrapolation of available data (Chandrashekhar et al. 2013), and set this
as the length of our simulated loops. We produce intensity like observables
through forward modeling and analyze the intensity time series using wavelet
analysis, as was done by previous observers. The result reveals similar
intensity oscillation periods reported in past observations. It is suggested
these oscillations are actually shock wave propagations along the loop. We also
show that if one considers different background subtractions, one can extract
adiabatic standing modes from the intensity time series data as well, both from
the observed and simulated data.
