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The removal of the interstellar medium (ISM) of disk galaxies through rampressure stripping (RPS) has been extensively studied in numerous simulations.Nevertheless, the role of magnetic fields (MF) on the gas dynamics in thisprocess has been hardly studied, although the MF influence on the large-scaledisk structure is well established. With this in mind, we present a 3Dmagnetohydrodynamic (MHD) simulation of face-on RPS of a disk galaxy to studythe impact of the galactic MF in the gas stripping. The main effect ofincluding a galactic MF is a flared disk. When the intracluster medium (ICM)wind hits this flared disk, oblique shocks are produced at the interactioninterface, where the ISM is compressed, generating a gas inflow from largeradii towards the central regions of the galaxy. This inflow is observed for$\sim 150$ Myr and may supply the central parts of the galaxy with material forstar formation while the outskirts of the disk are being stripped of gas, thusthe oblique shocks can induce and enhance the star formation in the remainingdisk. We also observed that the MF alters the shape and structure of the sweptgas, giving a smooth appearance in the magnetized case and clumpier andfilamentary-like morphology in the hydro case. Finally, we estimated thetruncation radius expected for our models using the Gunn-Gott criterion andfound that is in agreement with the simulations.

MHD simulations of ram pressure stripping of a disk galaxy