Using some observational evidences of filament disturbances associated with microflares we point out the following results:
1. The filament destabilization begins at one of its footpoint,
2. Glose to this footpoint one of two pores are observed, they move with an anomalous velocity as seen in white light pictures.
3. Bríghtenings in Hα and in C IV overlie the location of the pores. The pores may be the signature of new emerging flux.
4. The dynamics observed in Hα filament is generally associated with heating of the filament transitíon zone.
5. The excess energy is released at different places along the filament, but this process does not seem to imply a heating conduction front.
During the Maximum Year, preflare and preeruptive phenomena have been observed which give a new idea on the association of eruptive prominences and coronal transients. The propagation of a C IV brightening through a prominence is related to the onset of a
MHD wave. It is followed by the activation of the prominence and its eruption some two hours later. A coronal transient is observed above 1.6 Rs. It is argued that the eruption of the prominence is
the result of perturbations in the magnetic field configuration initiated by the MHD waves. The consequence would be that more generally the primary initiation of the eruption may happen up to
several hours before the rlse of the prominence.
During the maximum activity year 1980, chromospheric mass ejections were observed with the Multichannel Subtractive Double Pass Spectrograph operating at Mcudon (MSDP), while the UV and X ray emissions were observed respectively with Ultra Violet Spectrograph (UVSP) and HXIS instruments on board the SMM satellite. These ejections are not related directly to flares but are located in active regions near sunspots. As the magnetic field is frozen in the matter, the study of the velocity field leads to the geometry of the magnetic structures and to the temporal evolution
of the magnetic field lines. Ejections of matter recur often with a period of 10 to 20 minutes. In CIV, the bright loops colncide with the Hα surge but are more extended. Associated with the events are either X ray emission or type III bursts. We interprete these signatures by invoking, respectively closed or open structures. The estimate of the energy involved gives constraints on the mechanism responsible for the surge.