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Using 324 numerically modelled galaxy clusters as provided by THE THREEHUNDRED project, we study the evolution of the kinematic properties of thestellar component of haloes on first infall. We select objects withM$_{\textrm{star}}>5\times10^{10} h^{-1}M_{\odot}$ within $3R_{200}$ of themain cluster halo at $z=0$ and follow their progenitors. We find that althoughhaloes are stripped of their dark matter and gas after entering the maincluster halo, there is practically no change in their stellar kinematics. Forthe vast majority of our `galaxies' -- defined as the central stellar componentfound within the haloes that form our sample -- their kinematic properties, asdescribed by the fraction of ordered rotation, and their position in thespecific stellar angular momentum$-$stellar mass plane $j_{\rm star}$ --M$_{\rm star}$, are mostly unchanged by the influence of the central hostcluster. However, for a small number of infalling galaxies, stellar mergers andencounters with remnant stellar cores close to the centre of the main cluster,particularly during pericentre passage, are able to spin-up their stellarcomponent by $z=0$.

The Three Hundred Project: The stellar angular momentum evolution of cluster galaxies