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A dynamical model including ram pressure stripping is applied to the stronglyHI deficient Virgo spiral galaxy NGC 4522. A carefully chosen model snapshot iscompared with existing VLA HI observations. The model successfully reproducesthe large-scale gas distribution and the velocity field. However it fails toreproduce the large observed HI linewidths in the extraplanar component, forwhich we give possible explanations. In a second step, we solve the inductionequation on the velocity fields of the dynamical model and calculate the largescale magnetic field. Assuming a Gaussian distribution of relativisticelectrons we obtain the distribution of polarized radio continuum emissionwhich is also compared with our VLA observations at 6 cm. The observed maximumof the polarized radio continuum emission is successfully reproduced. Our modelsuggests that the ram pressure maximum occurred only ~50 Myr ago. Since NGC4522 is located far away from the cluster center (~1 Mpc) where theintracluster medium density is too low to cause the observed stripping if theintracluster medium is static and smooth, two scenarios are envisaged: (i) thegalaxy moves very rapidly within the intracluster medium and is not even boundto the cluster; in this case the galaxy has just passed the region of highestintracluster medium density; (ii) the intracluster medium is not static butmoving due to the infall of the M49 group of galaxies. In this case the galaxyhas just passed the region of highest intracluster medium velocity. This studyshows the strength of combining high resolution HI and polarized radiocontinuum emission with detailed numerical modeling of the evolution of the gasand the large-scale magnetic field.Comment: 15 pages, 11 figures, accepted for publication in A&

A dynamical model for the heavily ram pressure stripped Virgo spiral galaxy NGC 4522