Rotational Velocities of B Stars

By Helmut A. Abt, H. Levato, M. Grosso. 2002

296 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/fe4ad537ffbac3949eae64423473e327821531eb

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Citations in the corpus

An investigation of the close environment of β Cephei with the VEGA/CHARA interferometer (2010, background): “The magnetic axis is almost 90 degrees from the rotational axis, whose inclination is 60 degrees compared to the line-of-sight (Abt et al. 2002).”
Observational Evidence for Tidal Interaction in Close Binary Systems (2007, background): “Abt et al. (2002) derived the rotational period of their samples from the stellar line broadening, and concluded that all B-type stars with orbital periods shorter than 2.4 days are synchronized, while binaries with periods between 2.4 days and 5.0 days are ‘nearly synchronized’.”
The VLT FLAMES Survey of Massive Stars: Rotation and Nitrogen Enrichment as the Key to Understanding Massive Star Evolution (2007, result): “This population is dominated by field stars, which are known to rotate slower than cluster stars, and our velocity distribution is comparable to the Galactic field stars of Abt et al. (2002).”
Rotational velocities of A-type stars. III. Velocity distributions (2006, methodology): “The gray histogram is for B9-type stars in Abt et al. (2002).”
The Progenitor Stars of Gamma-Ray Bursts (2005, background): “About 0.3% of B stars have rotational speeds on the main sequence in excess of two-thirds times the break up speed, and the average is 25% of break up (Abt et al. 2002).”
The VLT-FLAMES survey of massive stars: surface chemical compositions of B-type stars in the Magellanic Clouds (2006, background): “Recent observational studies (Huang & Gies 2005 and Abt et al. 2002) have shown that binary systems experience more spin down than single stars and this is attributed to tidal interaction causing synchronization.”
Mind Your Ps and Qs: The Interrelation between Period (P) and Mass-ratio (Q) Distributions of Binary Stars (2016, background): “Early-type stars, including those in binaries with P & 10 days where tidal synchronization is inefficient, are rotationally broadened by 〈vrot〉 ≈ 100 - 200 km s−1 (Abt et al. 2002; Levato & Grosso 2013).”
A STELLAR ROTATION CENSUS OF B STARS: FROM ZAMS TO TAMS (2010, background): “The results are also in qualitative agreement with those of Abt et al. (2002) and Abt (2003) who examined a similar number of B stars and found that between luminosity class V (unevolved) and class III (evolved) the mean projected rotational velocity declines by ≈ 15% for early-B types and by ≈ 40%…”
Fourier method of determining the rotational velocities in OB stars (2007, unknown): “Slettebak 1975; Herrero et al. 1992; Abt et al. 2002; Strom et al. 2005).”