  To enhance our understanding of the impact of galaxy mergers on the
kinematics of early-type galaxies (ETGs), we examine differences in specific
stellar angular momentum within the half-light radius ($\lambda_{R_e}$) among
ETGs with different types of tidal features and those without such features.
This is accomplished by categorizing tidal features, which serve as direct
evidence of recent mergers, into shells, streams, and tails, through deep
images from the DESI Legacy Survey, and by using MaNGA data for the analysis of
the kinematics of 1244 ETGs at $z<0.055$. We find that ETGs with tidal features
typically have reduced $\lambda_{R_e}$ values that are lower by 0.12 dex than
ETGs without tidal features. ETGs with shells contribute most to the reduction
in $\lambda_{R_e}$. Consequently, nearly half of ETGs with shells are
classified as slow rotators, a fraction that is more than twice as high as that
of ETGs with tails or streams, and over three times higher than that of ETGs
without tidal features. These trends generally remain valid even when ETGs are
divided into several mass bins. Our findings support the idea that radial
mergers, which are more effective at reducing $\lambda_{R_e}$ than circular
mergers, are more closely associated with the formation of shells rather than
streams or tails. The detection of shells in slightly more massive ETGs
compared to streams and tails may be attributed to the fact that massive
satellite galaxies are more likely to be accreted through radial orbits, due to
the nature of dynamical friction.
