MODELLING RADIATIVE STELLAR WINDS WITH THE SIMECA CODE

Observatoire de la Côte d'Azur, Département Fresnel UMR 6528, Site de Grasse-Roquevignon, Avenue Copernic, 06130 Grasse, France

Abstract

Using the SIMECA code developped by Stee & Araùjo (1994), we report theoretical HI visible and near-IR line profiles, i.e. Hα (6562 Å), Hβ (4861 Å) and Brγ (21 656 Å), and intensity maps for a large set of parameters representative of early to late Be spectral types. We have computed the size of the emitting region in the Br γ line and its nearby continuum which both originate from a very extended region, i.e. at least 40 stellar radii which is twice the size of the Hα emitting region. We predict the relative fluxes from the central star, the envelope contribution in the given lines and in the continuum for a wide range of parameters characterizing the disk models. Finally, we have also studied the effect of changing the spectral type on our results and we obtain a clear correlation between the luminosity in Hα and in the infrared.