  We present a comprehensive multi-wavelength study of the star-forming region
NGC 1893 to explore the effects of massive stars on low-mass star formation.
Using near-infrared colours, slitless spectroscopy and narrow-band $H\alpha$
photometry in the cluster region we have identified candidate young stellar
objects (YSOs) distributed in a pattern from the cluster to one of the nearby
nebulae Sim 129. The $V, (V-I)$ colour-magnitude diagram of the YSOs indicates
that majority of these objects have ages between 1 to 5 Myr. The spread in the
ages of the YSOs may indicate a non-coeval star formation in the cluster. The
slope of the KLF for the cluster is estimated to be $0.34\pm0.07$, which agrees
well with the average value ($\sim 0.4$) reported for young clusters. For the
entire observed mass range $0.6 < M/M_\odot \le 17.7$ the value of the slope of
the initial mass function, $`\Gamma$', comes out to be $-1.27\pm0.08$, which is
in agreement with the Salpeter value of -1.35 in the solar neighborhood.
However, the value of $`\Gamma$' for PMS phase stars (mass range $0.6 <
M/M_\odot \le 2.0$) is found to be $-0.88\pm0.09$ which is shallower than the
value ($-1.71\pm0.20$) obtained for MS stars having mass range $2.5 < M/M_\odot
\le 17.7$ indicating a break in the slope of the mass function at $\sim 2
M_\odot$. Estimated $`\Gamma$' values indicate an effect of mass segregation
for main-sequence stars, in the sense that massive stars are preferentially
located towards the cluster center. The estimated dynamical evolution time is
found to be greater than the age of the cluster, therefore the observed mass
segregation in the cluster may be the imprint of the star formation process.
There is evidence for triggered star formation in the region, which seems to
govern initial morphology of the cluster.
