  We present a study of kinematic asymmetries from the integral field
spectroscopic surveys MAGPI and SAMI. By comparing the asymmetries in the
ionsied gas and stars, we aim to disentangle the physical processes that
contribute to kinematic disturbances. We normalise deviations from circular
motion by $S_{05}$, allowing us to study kinematic asymmetries in the stars and
gas, regardless of kinematic temperature. We find a similar distribution of
stellar asymmetries in galaxies where we do and do not detect ionised gas,
suggesting that whatever is driving the stellar asymmetries does not always
lead to gas removal. In both MAGPI and SAMI, we find an anti-correlation
between stellar asymmetry and stellar mass, that is absent in the gas
asymmetries. After stellar mass and mean-stellar-age matching distributions, we
find that at all stellar masses, MAGPI galaxies display larger stellar
asymmetry compared to SAMI galaxies. In both MAGPI and SAMI galaxies, we find
that star-forming galaxies with old mean-stellar-ages typically have larger
asymmetries in their gas compared to their stars, whereas galaxies with young
mean-stellar-ages have larger asymmetries in their stars compared to their gas.
We suggest that this results from continuous, clumpy accretion of gas.
