Observatoire de la Côte d'Azur - Site de Grasse-Roquevignon
Avenue Copernic
SF2A-
06130
GRASSE, France
Presentation 1 : None
Modeling Hot stellar winds for the VLTI with the SIMECA Code.
Ph. Stee
Thanks to the SIMECA code, we present theoretical HI visible and near-IR line profiles, i.e H [\( \alpha \)] (6562 Å), H [\( \beta \)] (4861 Å) and Br [\( \gamma \)] (21656 Å), and intensity maps for a large set of parameters (density, temperature, envelope geometry, inclination angle), representative of early to late Be spectral types. We have computed the size of the emitting region in the Br [\( \gamma \)] 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 H [\( \alpha \)] 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.All these results are used to prepare future VLTI interferometric observation programs for the AMBER and MIDI instruments.