Abstract
The D3 emission lines observed on a prominence over the solar east limb on 1984 May 5, which were found to consist of two components, i.e. the main and the broadened components, have been successfully calculated using the two-cloud model method with the multiplet of helium (3 D-3(3,2,1)-2 P-3(2,1,0)) taken into account. The results obtained show that the ejecta in front of the prominence are formed by the intermittent ejections of the matter from the plage region around the prominence, because there exist at least three distinguishable phases of the line-of-sight velocity, increasing during the observations. The turbulent velocity of the ejecta is rather large, about 29 km s(-1). The Doppler width of the ejecta is mainly the result of the non-thermal effect, and the thermal effect can be neglected compared with the non-thermal effect. The prominence is quiet and characterized by typical properties.
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