The removal of the interstellar medium (ISM) of disc galaxies through ram pressure stripping (RPS) has been extensively studied in numerous simulations. Nevertheless, the role of magnetic fields (MF) on the gas dynamics in this process has been hardly studied, although the MF influence on the large-scale disc structure is well established. With this in mind, we present 3D magnetohydrodynamic (MHD) simulations of disc galaxies subject to RPS, with different disc inclination to study the evolution of the galactic MF and its impact in the gas stripping. When the intracluster medium (ICM) wind hits a galaxy, the gas in the disc is compressed, leading to an enhancement of the MF intensity in the upstream side in our simulations. Since the gas is bound by the MF, we observe that in nearly face-on discs, the gas is swept by the wind in ring-like structures and dragging the field lines with it. In the case of nearly edge-on discs, the field lines are compressed in the upstream side and more extended towards the downstream side. The ICM is magnetized in the downstream side from 0.2 to 0.7 micro Gauss, where nearly face-on discs contribute the most, given that the developed tail is more extended than in nearly edge-on models.
Enviado por m.ramos@irya.unam.mx, 2019 Oct