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We use the EAGLE simulations to study the effects of the intra-cluster medium(ICM) on the spatially resolved star-formation activity in galaxies. We studythree cases of galaxy asymmetry dividing each galaxy in two halves using theplane (i) perpendicular to the $\rm \texttt{velocity}$ direction,differentiating the galaxy part approaching to the cluster center, hereafterdubbed as the "leading half", and the opposite one "trailing half", (ii)perpendicular to the $\rm \texttt{radial}$ position of the satellite to thecentre of the cluster, (iii) that maximizes the star-formation rate ($\rm SFR$)difference between the two halves. For (i), we find an enhancement of the $\rmSFR$, star formation efficiency ($\rm SFE$), and interstellar medium pressurein the leading half with respect to the trailing one and normal star-forminggalaxies in the EAGLE simulation, and a clear overabundance of gas particles intheir trailing. These results suggest that ram pressure (RP) is boosting thestar formation by gas compression in the leading half, and transporting the gasto the trailing half. This effect is more pronounced in satellites ofintermediate stellar masses $\rm 10^{9.5-10.5} M_{\odot}$, with gas massesabove $\rm 10^{9} M_{\odot}$, and located within one virial radius or in themost massive clusters. In (iii) we find an alignment between the velocity andthe vector perpendicular to the plane that maximizes the $\rm SFR$ differencebetween the two halves. It suggests that finding this plane in real galaxiescan provide insights into the velocity direction.

The better half -- Asymmetric star-formation due to ram pressure in the EAGLE simulations