  The total-to-selective extinction RV in the direction of a cluster is found
to be 3.12 +/- 0.2 (close to its normal value). We derive the luminosity and
mass functions for the cluster main sequence stars. The mass function slope is
found to be -2.29 +/- 0.20 which is close to Salpeter value. We find evidence
of mass segregation process in the cluster which is not yet dynamically
relaxed. We have performed time series photometric observations to detect
variable stars within star cluster NGC 1960. The DAOPHOT-II package is utilized
to estimate the apparent stellar magnitudes of stars. The secondary
standardization method is applied to the transformation of these apparent
magnitudes into standard values. The magnitude-time diagrams (light curves) of
stars are constructed to identify possible variability nature within them. The
stars, having sufficient magnitude variation with time, are considered to be
variable stars and their period values have computed through PERIOD04 package.
These periodic values of variables are used to construct their corresponding
phase diagrams. Here, we are reporting short periodic variables through the
photometric analysis of science frames of whole night observations. Their type
and variability nature, have been prescribed on the basis of information about
amplitude, period and shape of phase diagrams. The location of variables on
colour-magnitude-diagram is effective to constrain the history of stellar
evolution. Our present analysis indicates that the variability fraction of
massive stars is found to be high in the comparison of lighter members.
