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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.


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