Estrellas B con Líneas de Emisión en la Banda L.

GRANADA, ANAHÍ

Córdoba, Argentina

Jornada; Primeras Jornadas sobre Astrofisica Estelar; 2008

OALP

Hydrogen and helium lines in the optical and UV spectral ranges have already proved to be useful tools to study the wind structure in early-type stars. In order to describe the contribution of the stellar wind to the IR line flux of B-type stars with different luminosity classes, we calculate NLTE hydrogen line profiles considering expanding media with different beta velocity laws and temperature distributions. We build a grid of synthetic emission line profiles in order to compare them with observations and infer  properties of the circumstellar medium, such as velocity fields, temperature structures and mass loss rates. The velocity/density gradient plays an important role in the shape and intensity  of the lines and sets constraints to the size of their forming regions.