R. H. D. Townsend, S. P. Owocki, I. D. Howarth
Abstract
Be stars are near-main-sequence, B-type stars that have been observed to show Balmer-line emission. It is approaching a century and a half since the discovery of the first Be star (Secchi 1867), and in recent decades compelling empirical
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Be stars are near-main-sequence, B-type stars that have been observed to show Balmer-line emission. It is approaching a century and a half since the discovery of the first Be star (Secchi 1867), and in recent decades compelling empirical
Key concepts: Physics, Rotation (mathematics), Astrophysics, Stars, Line (geometry), Astronomy, Star (game theory), Observational study