We describe the basic process of coupling between dynamo and density waves in galaxies. The growth rate of magnetic field as a result of coupling is derived, applying the method of multiple time scales to the marginal state of disk dynamo. It is shown that the 1st-order resonance in a perturbation of density and thus the linear swing excitation, is possible. Moreover, the growth rate of magnetic field is always positive and does not depend on the initial phase difference between the magnetic and density waves. Both the numerical and analytical calculations show that ω = 2ω0 (ω: density-wave freq., ω0: dynamo freq.) is still the best condition for resonance due to the linear effect of swing excitation.

The evolution of galactic magnetic fields under the influence of spiral arms is investigated numerically by 2-dimensional simulation. We compute several models, especially when the swing-excitation mechanism works. We consider also the modification of the mean velocity fields driven by the Lorentz force of the growing magnetic fields. The characteristic structure of magnetic fields around the arm in each model is compared with the observations.