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