  We study partial tidal disruption and present a quantitative analysis of the
orbital dynamics of the remnant self-bound core. We perform smoothed particle
hydrodynamical simulations to show that partial disruption of a star due to the
tidal field of a black hole leads to a jump in the specific orbital energy and
angular momentum of the core. It directly leads to deviation in the core's
trajectory apart from getting a boost in its velocity. Our analysis shows that
the variations in the specific orbital energy and angular momentum are higher
when the pericentre distance is lower. We conclude that higher mass asymmetry
of the two tidal tails increases the magnitude of the trajectory deviations.
Our study reveals that observable deviations are only possible when mass ratio
$q \lesssim 10^3 $, which indicates the range of intermediate-mass black holes.
