Observatoire de la Côte d'Azur,
Département FRESNEL, CNRS UMR 6528,
Site de Grasse-Roquevignon, Avenue Copernic,
06130 Grasse, France
Using the SIMECA code developed by Stee & Araùjo (1994)
for Be stars we obtain a correlation between the mass loss rates
and the
Br
continuum luminosity as a function of the
opening angle of the disk. We show that this correlation is similar to those obtain by
Scuderi et al. for O-B supergiants. We found that the wind density at the base of the
photosphere, from a sample
of 8 Be stars, lies between 10-13 and 10-12 g cm-3.
We also present a relationship
between the mass of the circumstellar disk and the
2.16 µm flux.
Finally we emphasize how
interferometric measurements can help to estimate the wind density and
we present a sample of 16
Be stars with predicted visibilities that can be observed with the VLTI.
continuum emission
and interferometric measurements
and the
Br
continuum luminosity as a function of the
opening angle of the disk. We show that this correlation is similar to those obtain by
Scuderi et al. for O-B supergiants. We found that the wind density at the base of the
photosphere, from a sample
of 8 Be stars, lies between 10-13 and 10-12 g cm-3.
We also present a relationship
between the mass of the circumstellar disk and the
2.16 µm flux.
Finally we emphasize how
interferometric measurements can help to estimate the wind density and
we present a sample of 16
Be stars with predicted visibilities that can be observed with the VLTI.