  We present results of multi-epoch (fourteen nights during 2007-2010) $V$-band
photometry of the cluster NGC 1893 region to identify photometric variable
stars in the cluster. The study identified a total of 53 stars showing
photometric variability. The members associated with the region are identified
on the basis of spectral energy distribution, $J-H/H-K$ two colour diagram and
$V/V-I$ colour-magnitude diagram. The ages and masses of the majority of
pre-main-sequence sources are found to be $\lesssim$ 5 Myr and in the range 0.5
$\lesssim$ $M/M_{\odot}$ $\lesssim$ 4, respectively. These pre-main-sequence
sources hence could be T Tauri stars. We also determined the physical
parameters like disk mass and accretion rate from the spectral energy
distribution of these T Tauri stars. The periods of majority of the T Tauri
stars range from 0.1 to 20 day. The brightness of Classical T Tauri stars is
found to vary with larger amplitude in comparison to Weak line T Tauri stars.
It is found that the amplitude decreases with increase in mass, which could be
due to the dispersal of disks of massive stars.
