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Solar filament eruptions play a crucial role in triggering coronal massejections (CMEs). More than 80 % of eruptions lead to a CME. This correlationhas been studied extensively during the past solar cycles and the last longsolar minimum. The statistics made on events occurring during the rising phaseof the new solar cycle 24 is in agreement with this finding. Both filaments andCMEs have been related to twisted magnetic fields. Therefore, nearly all theMHD CME models include a twisted flux tube, called a flux rope. Either the fluxrope is present long before the eruption, or it is built up by reconnection ofa sheared arcade from the beginning of the eruption. In order to initiateeruptions, different mechanisms have been proposed: new emergence of flux,and/or dispersion of the external magnetic field, and/or reconnection of fieldlines below or above the flux rope. These mechanisms reduce the downwardmagnetic tension and favor the rise of the flux rope. Another mechanism is thekink instability when the configuration is twisted too much. In this paper weopen a forum of discussions revisiting observational and theoretical papers tounderstand which mechanisms trigger the eruption. We conclude that all theabove quoted mechanisms could bring the flux rope to an unstable state.However, the most efficient mechanism for CMEs is the loss-of-equilibrium ortorus instability, when the flux rope has reached an unstable thresholddetermined by a decay index of the external magnetic field.

Solar filament eruptions and their physical role in triggering Coronal Mass Ejections