Spectroscopic survey of emission line stars in open clusters

Abstract

We summarize a study of emission-line stars in young open clusters. The study was done in two phases. The first phase was the survey, where the emission stars in young open clusters were identified using the slitless spectral images. The identified emission stars were then studied in detail using their slit spectra in the 3700–9000 °A range. The results of the study suggest that there could be two mechanisms responsible for the Be phenomenon. The early type B stars are likely to become Be stars in the second half of their MS lifetime, whereas the late type B stars are likely to be born as Be stars.