  We study the role of star formation and stellar feedback in a galaxy being
ram pressure stripped on its infall into a cluster. We use hydrodynamical
wind-tunnel simulations of a massive galaxy ($M_\text{star} = 10^{11} M_\odot$)
moving into a massive cluster ($M_\text{cluster} = 10^{15} M_\odot$). We have
two types of simulations: with and without star formation and stellar feedback,
SF and RC respectively. For each type we simulate four realisations of the same
galaxy: a face-on wind, edge-on wind, $45^\circ$ angled wind, and a control
galaxy not subject to ram pressure. We directly compare the stripping evolution
of galaxies with and without star formation. We find that stellar feedback has
no direct effect on the stripping process, i.e. there is no enhancement in
stripping via a velocity kick to the interstellar medium gas. The main
difference between RC and SF galaxies is due to the indirect effect of stellar
feedback, which produces a smoother and more homogeneous interstellar medium.
Hence, while the average gas surface density is comparable in both simulation
types, the scatter is broader in the RC galaxies. As a result, at the galaxy
outskirts overdense clumps survive in RC simulation, and the stripping proceeds
more slowly. At the same time, in the inner disc, underdense gas in the RC
holes is removed faster than the smoothly distributed gas in the SF simulation.
For our massive galaxy, we therefore find that the effect of feedback on the
stripping rate is almost negligible, independent of wind angle.
