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The magnetic field of galaxies is believed to be produced by internal dynamoaction, but can be affected by motion of the galaxy through the surroundingmedium. Observations of polarized radio emission of galaxies located in galaxyclusters have revealed noticeable features of large-scale magneticconfigurations, including displacements of the magnetic structures from theoptical images and tails, which are possible imprints of ram pressure effectsarising from motion of the galaxies through the intracluster medium. We presenta quantitative dynamo model which attempts to describe the above effects. Incontrast to the traditional problem of a wind affecting a body with aprescribed magnetic field, we investigate how a non-magnetized wind flowaffects a magnetic field that is being self-excited by galactic dynamo action.In order to isolate the leading physical effects we exploit a simple dynamomodel that can describe relevant effects. In particular, we use what is knownas the 'no-z' approximation for the mean-field dynamo equations. In a suitableparametric range we obtain displacements of the large-scale magnetic field, aswell as magnetic tails. However, the specific details of their locations arequite counterintuitive. The direction of displacement is perpendicular to,rather than parallel to, the wind direction. The point at which the tailemerges from the galaxy depends on details of the model. The tail is eventuallydirected downstream. In the simplest case the magnetic tail begins in theregion where the wind decreases the total gas velocity. Any wind thatpenetrates the galaxy modifies the intrinsic dynamo action. These features aredifferent from those found in ram-pressure models. Any determination ofgalactic motion through the cluster medium from observational data needs totake the effects of dynamo action into account.

Ram pressure effects in the galactic plane and galactic dynamos in the no-z approximation