Astronomy and Astrophysics – Astrophysics
Scientific paper
May 1987
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987a%26a...178..159m&link_type=abstract
Astronomy and Astrophysics (ISSN 0004-6361), vol. 178, no. 1-2, May 1987, p. 159-169.
Astronomy and Astrophysics
Astrophysics
195
Blue Stars, Stellar Evolution, Supermassive Stars, Baroclinic Instability, Critical Velocity, Mixing, Stellar Rotation, Stellar Structure, Turbulent Diffusion, Viscosity
Scientific paper
The effects of rotationally induced mixing on the evolution of massive stars is examined. The mechanism considered results from baroclinic instability due to differential rotation which produces two-dimensional meteorological-like turbulent motions; the mixing is produced by the small-scale three-dimensional tail of the turbulent spectrum. The models show that, due to the high viscosity, the diffusion coefficient would be sufficiently large to mix most massive stars during their MS lifetime. However, below some critical rotation velocity, diffusive mixing is efficiently prevented by the mu-gradient. Below critical rotiation, the evolution is essentially classical with unmodifed redwards tracks in the HR diagram. Above critical rotation, the evolutionary tracks go upwards and bluewards, very close to those of fully homogeneous evolution. Comparisons with observations indicate that turbulent diffusion can account for the ON stars lying close to the zero-age sequence.
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