# Classical Be stars

@article{Rivinius2013ClassicalBS,
title={Classical Be stars},
author={Th. Rivinius and Alex C. Carciofi and Christophe Martayan},
journal={The Astronomy and Astrophysics Review},
year={2013},
volume={21},
pages={1-86}
}
• Published 2013
• Physics
• The Astronomy and Astrophysics Review
In the past decade, a consensus has emerged regarding the nature of classical Be stars: They are very rapidly rotating main sequence B stars, which, through a still unknown, but increasingly constrained process, form an outwardly diffusing gaseous, dust-free Keplerian disk. In this work, first the definition of Be stars is contrasted to similar classes, and common observables obtained for Be stars are introduced and the respective formation mechanisms explained. We then review the current state… Expand
238 Citations

#### Figures and Tables from this paper

A high fraction of Be stars in young massive clusters: evidence for a large population of near-critically rotating stars
Recent photometric analysis of the colour-magnitude diagrams (CMDs) of young massive clusters (YMCs) have found evidence for splitting in the main sequence and extended main sequence turn-offs, bothExpand
The disk physical conditions of 48 Persei constrained by contemporaneous H{\alpha} spectroscopy and interferometry
• Physics
• 2017
We utilize a multi-step modelling process to produce synthetic interferometric and spectroscopic observables, which are then compared to their observed counterparts. Our extensive set ofExpand
Photoionization Models of the Inner Gaseous Disk of the Herbig Be Star BD+65 1637
• Physics
• 2015
We attempt to constrain the physical properties of the inner, gaseous disk of the Herbig Be star BD+65 1637 using non-LTE, circumstellar disk codes and observed spectra (3700 to 10,500 \r{A}) fromExpand
Spectral and spatial imaging of the Be+sdO binary phi Persei
The rapidly rotating Be star phi Persei was spun up by mass and angular momentum transfer from a now stripped-down, hot subdwarf companion. Here we present the first high angular resolution images ofExpand
Be X-ray binaries in the SMC as indicators of mass-transfer efficiency
Be X-ray binaries (BeXRBs) consist of rapidly rotating Be stars with neutron star companions accreting from the circumstellar emission disk. We compare the observed population of BeXRBs in the SmallExpand
Catalogue of new Herbig Ae/Be and classical Be stars
The intermediate-mass pre-main sequence Herbig Ae/Be stars are key to understanding the differences in formation mechanisms between low- and high-mass stars. The study of the general properties ofExpand
Stellar Inclination Angles from Be-star Hα Emission Line Profiles
• Physics
• 2020
We demonstrate that the angle between star's rotation axis and the observer's line-of-sight, usually called the inclination angle, can be reliably determined for Be stars via H$\alpha$ emission-lineExpand
An investigation of the photometric variability of confirmed and candidate Galactic Be stars using ASAS-3 data
We present an investigation of a large sample of confirmed (N = 233) and candidate (N = 54) Galactic classical Be stars (mean V magnitude range of 6.4-12.6 mag), with the main aim of characterizingExpand
Computing the Polarimetric and Photometric Variability of Be Stars
• Physics
• 2018
We investigate variations in the linear polarization as well as in the V-band and B-band colour-magnitudes for classical Be star disks. We present two models: disks with enhanced disk density andExpand
Improved Main-sequence Turnoff Ages of Young Open Clusters: Multicolor UBV Techniques and the Challenges of Rotation
• Physics
• 2018
Main sequence turnoff ages in young open clusters are complicated by turnoffs that are sparse, have high binarity fractions, can be affected by differential reddening, and typically include a numberExpand

#### References

SHOWING 1-10 OF 391 REFERENCES
A representative sample of Be stars V: Hvariability
• Physics
• 2013
Aims. We attempt to determine if a dependency on spectral subtype or vsini exists for stars undergoing phase-changes between B and Be states, as well as for those stars exhibiting variability in HαExpand
Mode visibilities in rapidly rotating stars
• Physics
• 2013
Context: Mode identification is a crucial step to comparing observed frequencies with theoretical ones, but has proven to be difficult in rapidly rotating stars. Aims: To further constrain modeExpand
Astron Astrophys 550:A77, DOI 10.1051/0004-6361/201220506 Reid WA, Parker QA (2012) Emission-line stars discovered in the UKST Hα survey of the Large Mag
• 2012
Mass loss from hot massive stars
• Physics
• 2008
Mass loss is a key process in the evolution of massive stars, and must be understood quantitatively if it is to be successfully included in broader astrophysical applications such as galactic andExpand
κ-mechanism excitation of retrograde mixed modes in rotating B-type stars
• Mon Not R Astron Soc 364:573–582,
• 2005
Be-star rotation: how close to critical?
• Physics
• 2003
We argue that, in general, observational studies of Be-star rotation have paid insufficient attention to the effects of equatorial gravity darkening. We present new line-profile calculations thatExpand
Rotation and magnetic field in the Be star omega Orionis
Ori is a B2IIIe star for which rotational modulation and non-radial pulsations (NRP) have been recently investi- gated from two independent observational campaigns in 1998 and 1999. Putting the dataExpand
Dynamical Models of Winds from Rotating Hot Stars
The hottest and most massive stars (spectral types O, B, Wolf-Rayet) have strong stellar winds that are believed to be driven by line scattering of the star's continuum radiation eld. The atmospheresExpand
CHARRON: CODE FOR HIGH ANGULAR RESOLUTION OF ROTATING OBJECTS IN NATURE∗
Rotation is one of the fundamental physical parameters governing stellar physics and evolution. At the same time, spectrally resolved optical/IR long-baseline interferometry has proven to be anExpand