2006/09/26 by R. S. Schnerr, H. F. Henrichs, R. D. Oudmaijer +1 · 35 citations
Physics and Astronomy · #Astro and Planetary Science #Astronomy #Astrophysics #Astrophysics and Star Formation Studies #Context (archaeology) #Geology #Geometry #Physics #Rotation (mathematics) #Stars #Stellar, planetary, and galactic studies #astro-ph
paper · pdf · doi:10.1051/0004-6361:20066392
published in Astronomy and Astrophysics 459(1), L21-L24 (EDP Sciences) · 4 pages, 3 figures. Accepted by A&A Letters
openalex publication_date 2006/09/26 · arxiv created 2006/10/06 · arxiv updated 2014/10/13 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/05
Context.Be stars, which are characterised by intermittent emission in their hydrogen lines, are known to be fast rotators. This fast rotation is a requirement for the formation of a Keplerian disk, which in turn gives rise to the emission. However, the pulsating, magnetic B1IV star β Cephei is a very slow rotator that still shows Hα emission episodes like in other Be stars, contradicting current theories.