Abstract　

I will summarize the results obtained over recent years on the formation of the helium spectrum in solar prominences. The radiative transfer problem in non-LTE conditions is solved to compute the profiles of the resonance lines of He I and He II. The structure of the prominence-to-corona transition region (PCTR) has a major influence on the resulting spectrum of these lines since they are formed mostly in this part of the prominence. However, even lines formed in the central part of the prominence are affected by the existence of the PCTR. Diagnostic techniques using the absorption of coronal radiation by the cool prominence plasma will be demonstrated. I will also present the technique of Doppler dimming / brightening to study the radial motion of moving prominences. Future steps in this kind of modelling will be addressed. I will conclude by a presentation of a new effort in the construction of a solar prominence catalogue.