1996/11/18 by S. Talon, Suzanne Talon, Jean-Paul Zahn +8
Physics and Astronomy · #Astro and Planetary Science #Astronomy and Astrophysical Research #Astrophysics (astro-ph) #FOS: Physical sciences #Stellar, planetary, and galactic studies #astro-ph
paper · pdf · doi:10.48550/arxiv.astro-ph/9611131
10 pages latex file using l-aa.sty, 11 postscript figures, accepted by A&A
arxiv created 1996/11/18 · openalex publication_date 1996/11/18 · arxiv updated 2009/12/01 · openalex created_date 2025/10/10 · openalex updated_date 2026/07/28
We describe the main-sequence evolution of a rotating 9 M_\odot star. Its interior rotation profile is determined by the redistribution of angular momentum through the meridian circulation and through the shear turbulence generated by the differential rotation; the possible effect of internal waves is neglected. We examine the mixing of chemicals produced by the same internal motions. Our modelization is based on the set of equations established by Zahn (1992) and completed in Matias, Talon & Zahn (1996). Our calculations show that the amount of mixing associated with a typical rotation velocity of ∼ 100 km/s yields stellar models whose global parameters are very similar to those obtained with the moderate overshooting (d/HP ≃ 0.2) which has been invoked until now to fit the observations. Fast rotation (∼ 300 km/s) leads to significant changes of the C/N and O/N surface ratios, but the abundance of He is barely increased. The modifications of the internal composition profile due to such rotational mixing will certainly affect the post--main-sequence evolution.