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The relation between the resolved star formation rate per unit area and thenon-thermal radio continuum emission is studied in 21 Virgo cluster galaxiesand the two nearby spiral galaxies, NGC6946 and M51. For the interpretation andunderstanding of our results we used a 3D model where star formation, 2D cosmicray (CR) propagation, and the physics of synchrotron emission are included.Based on the linear correlation between the star formation rate per unit areaand the synchrotron emission and its scatter radio-bright and radio-dim regionscan be robustly defined for our sample of spiral galaxies. We identified CRdiffusion or streaming as the physical causes of radio-bright regions ofunperturbed symmetric spiral galaxies as NGC6946. We identified the probablecauses of radio-bright regions in several galaxies as CR transport, via eithergravitational tides (M51) or galactic winds (NGC4532) or ram pressure stripping(NGC4330 and NGC4522). Three galaxies are overall radio-dim: NGC4298, NGC4535,and NGC4567. Based on our model of synchrotron-emitting disks we suggest thatthe overall radio-dim galaxies have a significantly lower magnetic field thanexpected by equipartition between the magnetic and turbulent energy densities.Radio-bright regions frequently coincide with asymmetric ridges of polarizedradio continuum emission, and we found a clear albeit moderate correlationbetween the polarized radio continuum emission and the radio/SFR ratio. Whencompression or shear motions of the interstellar medium (ISM) are present inthe galactic disk, the radio-bright regions are linked to the commonly observedasymmetric ridges of polarized radio continuum emission and represent a usefultool for the interaction diagnostics. Based on our results, we propose ascenario for the interplay between star formation, CR electrons, and magneticfields in spiral galaxies.

Deciphering the radio-star formation correlation on kpc-scales III. Radio-dim and bright regions in spiral galaxies