Be Stars: Rapidly Rotating Pulsators
arXiv:1210.0784 · doi:10.1007/978-3-642-29630-7_46
Abstract
I will show that Be stars are, without exception, a class of rapidly rotating stars, which are in the majority of cases pulsating stars as well, while none of them does possess a large scale (i.e. with significant dipolar contribution) magnetic field.
Review talk given at "XX Stellar Pulsation Conference Series: Impact of new instrumentation and new insights in stellar pulsations", Granada, 5-9 September 2011, in press in AIP Conf. Ser
References in corpus (5)
- Effects of gravitational darkening on the determination of fundamental parameters in fast rotating B-type stars
- On the incidence of weak magnetic fields in DA white dwarfs
- On the Determination of the Rotational Oblateness of Achernar
- Magnetic survey of emission line B-type stars with FORS1 at the VLT
- Evidence for weak magnetic fields in early-type emission stars
Cited by in corpus (5)
- High-resolution, H band Spectroscopy of Be Stars with SDSS-III/APOGEE: I. New Be Stars, Line Identifications, and Line Profiles
- Pulsation among TESS A and B stars and the Maia variables
- TESS observations of Be stars: a new interpretation
- The Circumstellar Disk of the Be Star ~Aquarii
- The B and Be States of the Star EM Cepheus