Rotational velocities of A-type stars IV. Evolution of rotational velocities

TL;DR

This study analyzes the evolution of rotational velocities in A-type stars, revealing mass-dependent velocity distributions and suggesting differential rotation throughout their main sequence lifespan, challenging some theoretical predictions.

Contribution

It provides a detailed analysis of rotational velocity distributions as a function of stellar mass and age, highlighting unexpected acceleration patterns and differential rotation in A-type stars.

Findings

Stars less than 2.5 Msun have unimodal velocity distributions and accelerate monotonically with age.

Stars between 1.7 and 3.2 Msun show strong early acceleration, then slow down.

Stars evolve as differential rotators throughout their main sequence life.

Abstract

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 \Omega/\Omega_crit (\Omega_crit is the critical angular velocity) have peculiar shapes according to spectral type groups, which can be caused by evolutionary properties. We aim to review the properties of these rotational velocity distributions in some detail as a function of stellar mass and age. We have gathered v sin i 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/Lsun)-parameters were determined from the uvby-\beta photometry and the HIPPARCOS parallaxes. The velocity distributions show two regimes that depend on the stellar mass. Stars less massive than 2.5 Msun 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 Msun to 3.2 Msun 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 \delta(t)\sim 0.2 t_MS, where t_MS is the time spent by a star in the MS.