9 Conclusions
Recently achieved spatial and temporal resolution performance of coronal telescopes and spectral
instruments, space-borne as well as ground-based, makes possible systematic observational investigations of
various waves and oscillations in the corona. The theory of interaction of MHD modes with plasma
structures, in particular, of the MHD modes of a magnetic cylinder, developed in early eighties, provides the
theoretical basis for interpretation of the phenomena. Observationally determined properties of MHD modes
of solar coronal structures, such as active region loops, polar plumes, and other open structures, showed an
excellent agreement with the theory. The combination of the observationally gained knowledge with MHD
wave theory and direct numerical simulations of the phenomena, gives rise to a new method of investigation
of coronal plasmas, the MHD seismology of the corona. This makes the investigation of coronal MHD
waves and oscillations to be an interesting, rapidly developing, and promising branch of solar
physics.
Some important topics, such as the coronal Moreton or EIT wave, oscillations in coronal bright points,
sub-second radio pulsations, nonlinear effects, and other, remained out of the scope of the present version of
this review, and will be covered in the next edition.
