Abstract
Quiescent solar prominences are highly dynamic structures which, among other features, display oscillatory motions. The presence of these oscillations has been confirmed by means of ground- and space-based observations, and they have been classified in small and large amplitude oscillations. Since prominences are magnetized structures, the theoretical interpretation of their oscillations has been mostly done in terms of magnetohydrodynamic (MHD) waves. This interpretation has allowed the development of prominence seismology as a tool to determine prominence physical parameters (magnetic field, Alfven speed, inhomogeneity scale, etc.) which are difficult to measure by direct means.
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