Abstract
AB Aurigae is the brightest Ae Herbig star in the northern hemisphere and it shows evidence of accretion and ejection processes in its circumstellar region. Moreover the Hα line shows a P-Cygni type profile which is a common indication of wind. Its Hα line is very variable, and most of this variation occurs in its blue-shifted side. One of the processes that can be used to explain this variation is a disk wind similar to those of the classical T Tauri stars. AB Aurigae has been observed using spectral interferometry in the optical region, by the VEGA spectrometer in the CHARA-array, which can resolve details of milliseconds of arc in size: in the case of AB Aur represent sizes smaller than 1 AU. With this resolution, it's possible to observe the region where the wind is being ejected. Using a radiative transfer code that already had been used to model the Hα line profiles in classical T Tauri stars, and adapting it to model the Hα line in AB Aur, we calculate an intensity map showing the region where this line is being formed, and then we compare it with data from the interferometric observations. This work will give us a better understanding of the ejection and accretion mechanism that are responsible for the formation of the Hα line around AB Aur and in some of the Herbig Ae/Be stars, and whether a disk wind mechanism can explain or not this line in these objects.
