Volume 537, January 2012
|Number of page(s)||22|
|Section||Stellar structure and evolution|
|Published online||19 January 2012|
IV. Evolution of rotational velocities
1 Institut d’Astrophysique de Paris, UMR 7095 CNRS – Université Pierre & Marie Curie, 98bis boulevard Arago, 75014 Paris, France
2 GEPI/CNRS UMR 8111, Observatoire de Paris – Université Paris Denis Diderot, 5 place Jules Janssen, 92195 Meudon Cedex, France
Received: 13 July 2011
Accepted: 1 December 2011
Context. In previous works of this series, we have shown that late B- and early A-type stars have genuine bimodal distributions of rotational velocities and that late A-type stars lack slow rotators. The distributions of the surface angular velocity ratio Ω/Ωcrit (Ωcrit is the critical angular velocity) have peculiar shapes according to spectral type groups, which can be caused by evolutionary properties.
Aims. We aim to review the properties of these rotational velocity distributions in some detail as a function of stellar mass and age.
Methods. We have gathered vsini for a sample of 2014 B6- to F2-type stars. We have determined the masses and ages for these objects with stellar evolution models. The (Teff,log L/L⊙)-parameters were determined from the uvby–β photometry and the HIPPARCOS parallaxes.
Results. The velocity distributions show two regimes that depend on the stellar mass. Stars less massive than 2.5 M⊙ have a unimodal equatorial velocity distribution and show a monotonical acceleration with age on the main sequence (MS). Stars more massive have a bimodal equatorial velocity distribution. Contrarily to theoretical predictions, the equatorial velocities of stars from about 1.7 M⊙ to 3.2 M⊙ undergo a strong acceleration in the first third of the MS evolutionary phase, while in the last third of the MS they evolve roughly as if there were no angular momentum redistribution in the external stellar layers. The studied stars might start in the ZAMS not necessarily as rigid rotators, but with a total angular momentum lower than the critical one of rigid rotators. The stars seem to evolve as differential rotators all the way of their MS life span and the variation of the observed rotational velocities proceeds with characteristic time scales δt ≈ 0.2 tMS, where tMS is the time spent by a star in the MS.
Key words: stars: early-type / stars: rotation / stars: evolution
Full Table 1 is only available at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (126.96.36.199) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/537/A120
Appendices are available in electronic form at http://www.aanda.org
© ESO, 2012
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