Resonance centrifugal effects as a factor in the formation of solar magnetic arcades. Influence of dynamical radiative cooling

This article continues our studies of the development of an MHD, waveguide, centrifugalresonance instability as a possible mechanism for the formation of solar magnetic arcades; here, we take into account the non-isentropic nature of this process associated with the presence of dynamical radiative cooling. In contrast to the results of our previous study, our computational data show that five, rather than two, waveguide-resonance families of unstable modes are able to develop in a cylindrical, rotating layer of magnetized plasma. This substantially expands the spectrum of associated wave processes, so that the joint action of all these growing wave harmonics can lead in the non-linear stage of their development to morphologies close to those observed in solar magnetic arcades—to the formation both of the magnetic arcades themselves and of fine structure in such arcades.