VELOCITY-FIELDS IN THE SOLAR CORONA DURING MASS EJECTIONS AS OBSERVEDWITH UVCS-SOHO

This Letter presents the observations of the first two coronal mass ej ections (CMEs) obtained with the Ultraviolet Coronagraph Spectrometer of SOHO. Both CMEs were observed at high spectral resolution in the ul traviolet domain. The first event on 1996 June 6-7 was observed in H I Ly alpha lambda 1216 and Ly beta lambda 1026, O VI lambda lambda 1032 and 1037, Si XII lambda lambda 499 and 521 and imaged within 1.5 and 5 R-.. The second event on 1996 December 23 was observed in several H I lines and cool lines such as C III lambda 977, N III lambda lambda 9 90-992, and O V lambda 630. The analysis of line profiles has allowed us to determine the line-of-sight velocities of the extended corona du ring a mass ejection. In particular there is evidence for mass motions consistent with untwisting magnetic fields around an erupted flux tub e in one of the events and line of sight velocities of 200 km s(-1) in the early phase of the second event presumably related to the expansi on of the leading arch of the transient.