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Constraints on Mixing Processes from Abundance Anomalies

Published online by Cambridge University Press:  26 May 2016

G. Michaud ,
J. Richer  and
O. Richard
G. Michaud
Affiliation:
Département de physique, Université de Montréal, Montréal, PQ, Canada, H3C 3J7; CEntre de Recherche en Calcul Appliqué (CERCA), 5160 boul. Décarie, bureau 400, Montréal, PQ, Canada, H3X 2H9
J. Richer
Affiliation:
Département de physique, Université de Montréal, Montréal, PQ, Canada, H3C 3J7; CEntre de Recherche en Calcul Appliqué (CERCA), 5160 boul. Décarie, bureau 400, Montréal, PQ, Canada, H3X 2H9
O. Richard
Affiliation:
Département de physique, Université de Montréal, Montréal, PQ, Canada, H3C 3J7; CEntre de Recherche en Calcul Appliqué (CERCA), 5160 boul. Décarie, bureau 400, Montréal, PQ, Canada, H3X 2H9

Abstract

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Abundance anomalies in the Sun, main sequence F, A and B stars, turnoff Pop II stars, the horizontal branch and white dwarfs are caused at least partly by particle transport processes. Detailed evolutionary models have been calculated for most of those objects taking into account the gravitational settling, thermal diffusion and radiative accelerations of 28 isotopes (24 atomic species). These will be used together with the observed abundances to put constraints on the mixing that rotationnally induced turbulence may lead to. The link between abundance anomalies and rotation on the HB is explained by the variation with log g of the ratio of the Eddington-Sweet and atomic diffusion velocities.

Type
Session 4 Rotation and Stellar Evolution
Information
Symposium - International Astronomical Union , Volume 215: Stellar Rotation , 2004 , pp. 457 - 466
Copyright
Copyright © Astronomical Society of the Pacific 2004 

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