1997A&A...321..867M

We report a parameter study of emission lines arising from a disc surrounding a Be star, using parameters appropriate to the Be star ψ Per. We concentrate on the Hα line and on some IR recombination lines (Brα, Brγ, Pfγ and HI 17-6). The model we use is a simple cone-like disc model, first proposed by Waters (1986A&A...162..121W). This model has been successful in explaining the continuum energy distribution of Be stars, and we now wish to study the emission line spectrum emerging from such a disc. We find that line shapes and ratios of line strengths are strongly dependent on the temperature structure of the disc. Infrared recombination lines will therefore be very useful in determining the physical state of the circumstellar envelopes of Be stars.