The spectra of three surges observed on September 20 and October 2, 1979 havebeen analysed. Rotational velocities have been evaluated for the wide range of heights above the chromosphere. The obtained results show that the rotational velocity decreases from above a hundred km/s at the surge bases to tens km/s at the surge tops. Generally, this tendency is independent of the surge evolution stage.
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.