  The interactions between the Magellanic Clouds significantly affect the shape
and distribution of the young stellar population, particularly in the periphery
of the Small Magellanic Cloud (SMC). We present the first far-UV (FUV) map of
the north-east SMC-Shell region using the Ultra Violet Imaging Telescope (UVIT)
onboard AstroSat. The detected FUV stars are combined with Gaia Early Data
Release 3 data to create a FUV-optical catalog of ~ 14,400 stars. FUV-optical
colour-magnitude diagrams are used along with isochrones to estimate the
stellar ages. The detected stars are formed in multiple episodes. We identified
two episodes of star formation (~ 60 and ~ 260 Myr ago) where the episode at ~
260 Myr is linked to the recent interaction with the Large Magellanic Cloud
(LMC) and the episode at ~ 60 Myr is linked to the pericentric passage of the
SMC around our Galaxy. The median proper motion (PM) and velocity dispersion
are found to be similar to the SMC main body, indicating that this region has
not experienced significant tidal effects. The FUV stellar surface density and
the dispersion in PM suggest an extent of the inner SMC in the north-east
direction to be around 2.2 deg. We detect arm-like and arc-like structures in
the FUV stellar density map, and their kinematics appear to be similar to the
SMC main body. These extended outer features are the spatial stellar
overdensities formed over multiple episodes of star formation, but without
apparent kinematic distinction.
