2012/12/29 by G. Catanzaro · 3 citations
Physics and Astronomy · Social Sciences · #Angular velocity #Astronomical spectroscopy #Astronomy and Astrophysical Research #Atlas (anatomy) #Balmer series #Educational Leadership and Practices #Emission spectrum #Line (geometry) #Radial velocity #Spectral line #Stars #Stellar, planetary, and galactic studies #astro-ph.SR
paper · pdf · doi:10.1051/0004-6361/201220357
20 pages. arXiv admin note: text overlap with arXiv:astro-ph/0609602 by other authors
arxiv created 2012/12/29 · openalex publication_date 2012/12/29 · arxiv updated 2015/06/12 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/05
Context. Be stars are fast-rotating early-type emission line stars. It is generally assumed that observed emission is generated in a rotating disk-like envelope, as supported by the observed correlation between the stellar projected rotational velocity vsini and the width of the emission lines. Then, high-resolution spectroscopic observations of Balmer lines profiles play an important role in putting constraints on Be stars modeling.