Espectro infrarrojo de líneas de H en estrellas tempranas

We study the physical conditions in extended atmospheres of hot stars by means of a theoretical analysis of the hidrogen line spectrum in the infrared region. We use the radiative transfer theory, in order to describe the thermal and kinematic conditions and the line forming regions, looking for correlations between our model's parameters and the profiles of the Paschen lines. We compute NLTE spherically symmetric models with velocity fields and strong departures of radiative equilibrium.