  We study the origin of misalignments between the stellar and star-forming gas
components of simulated galaxies in the EAGLE simulations. We focus on galaxies
with stellar masses $\geq 10^9$ M$_\odot$ at 0$\leq$z$\leq$1. We compare the
frequency of misalignments with observational results from the SAMI survey and
find that overall, EAGLE can reproduce the incidence of misalignments in the
field and clusters, as well as the dependence on stellar mass and optical
colour within the uncertainties. We study the dependence on kinematic
misalignments with internal galaxy properties and different processes related
to galaxy mergers and sudden changes in stellar and star-forming gas mass. We
found that despite the environment being relevant in setting the conditions to
misalign the star-forming gas, the internal galaxy properties play a crucial
role in determining whether the gas quickly aligns with the stellar component
or not. Hence, galaxies that are more triaxial and more dispersion dominated
display more misalignments because they are inefficient at realigning the
star-forming gas towards the stellar angular momentum vector.
