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Chemical Separation vs Rotation in a and F-Stars

Published online by Cambridge University Press:  12 April 2016

Paul Charbonneau
Paul Charbonneau*
Affiliation:
High Altitude Observatory, National Center for Atmospheric Research1, P.O. Box 3000, Boulder, CO 80307, U.S.A.

Abstract

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The role played by rotationally-induced mixing in the diffusion-based models for non-magnetic chemically peculiar stars is investigated. This paper focuses on one specific rotationally controlled mixing mechanism, namely thermally-driven meridional circulation. Its effects on the time evolution of chemical abundances are illustrated by means of three specific examples. The first two concern the diffusion model for FmAm stars, where it is shown that while circulation has a determining influence on the settling of Helium, it has no significant effect on the diffusion of heavier metals once the He superficial convection zone has disappeared. The third example is concerned with the diffusion/mass loss model for λBootis stars. It is shown that the inclusion of circulation prevents the appearance of generalized underabundances at any epoch of the evolution, indicating that the diffusion/mass loss model for these objects must be abandoned.

Keywords

AbundancesDiffusionRotation
Type
V. Theory of CP Star Photospheres
Information
International Astronomical Union Colloquium , Volume 138: Peculiar versus Normal Phenomena in A-Type and Related Stars , 1993 , pp. 474 - 489
Copyright
Copyright © Astronomical Society of the Pacific 1993

References

Abt, H.A., & Levy, S.G. 1985, Ap. J. Suppl., 59, 229 CrossRefGoogle Scholar
Baglin, A., Morel, P.J., & Schatzman, E. 1985, Astr. Ap., 149, 309 Google Scholar
Baschek, B., & Searle, S. 1969, Ap. J., 155, 537 Google Scholar
Baschek, B., & Slettebak, A. 1988, Astr. Ap., 207, 112 Google Scholar
Berthet, S. 1992, Astr. Ap., 253, 451 Google Scholar
Bohlender, D.A., & Landstreet, J.D. 1990, M. N. R. A. S., 247, 606 Google Scholar
Brown, A., Vealé, A., Judge, P., Bookbinder, J.A., & Hubeny, I. 1990, Ap. J., 361, 220 Google Scholar
Burkhart, C., & Coupry, M.-F. 1991, Astr. Ap., 249, 205 Google Scholar
Cayrel, R., Burkhart, C., & Van’t Veer, C. 1991, in IAU symp. 145, Evolution of Stars: The Photospheric Abundance Connection, eds. Michaud, G & Tutukov, A., 99 Google Scholar
Chaboyer, B., & Zahn, J.-P. 1992, Astr. Ap., 253, 173 Google Scholar
Charbonneau, P. 1991, Ap. J., 372, L33 Google Scholar
Charbonneau, P. 1992a, J. Roy. Astron. Soc. Canada, 86, 31 Google Scholar
Charbonneau, P. 1992b, Astr. Ap., 259, 134 Google Scholar
Charbonneau, P. 1992c, preprintGoogle Scholar
Charbonneau, P., & Michaud, G. 1988, Ap. J., 327, 809 Google Scholar
Charbonneau, P., & Michaud, G. 1991, Ap. J., 370, 693 CrossRefGoogle Scholar
Charbonnel, C., Vauclair, S., & Zahn, J.-P. 1992, Astr. Ap., 255, 191 Google Scholar
Gray, R.O. 1988, Astron. J., 95, 220 Google Scholar
Holweger, H., Gigas, D., & Steffen, M. 1986b, Astr. Ap., 155, 58 Google Scholar
Holweger, H., Steffen, M., & Gigas, D. 1986b, Astr. Ap., 163, 333 Google Scholar
King, J.R., & Patten, B.M. 1992, M. N. R. A. S., 256, 571 CrossRefGoogle Scholar
Lanz, T., & Catala, C. 1992, Astr. Ap., 257, 663 Google Scholar
Latour, J., Toomre, J., & Zahn, J.-P. 1981, Ap. J., 248, 1081 Google Scholar
Lemke, M. 1989, Astr. Ap., 225, 125 Google Scholar
MacGregor, K.B., & Stencel, R. 1992, Ap. J., 397, in pressGoogle Scholar
Michaud, G. 1982, Ap. J., 258, 349 Google Scholar
Michaud, G. 1987, Phys. Scripta, 36, 112 Google Scholar
Michaud, G., & Charland, Y. 1986, Ap. J., 311, 326 Google Scholar
Michaud, G., & Charland, Y., Vauclair, S., & Vauclair, G. 1976, Ap. J., 210, 447 Google Scholar
Michaud, G., Tarasick, D., Charland, Y., & Pelletier, C. 1983, Ap. J., 269, 239 Google Scholar
Pinsonneault, M.H., Kawaler, S.D., Sofia, S., & Demarque, P. 1989, Ap. J., 338, 424 Google Scholar
Preston, G.W. 1974, Ann. Rev. Astr. Ap., 12, 257 Google Scholar
Proffitt, C.R., & Michaud, G. 1989, Ap. J., 345, 998 Google Scholar
Schatzman, E. 1969, Astr. Ap., 3, 331 Google Scholar
Schatzman, E. 1977, Astr. Ap., 56, 211 Google Scholar
Sadakane, K., & Nishida, M. 1986, PASP, 98, 685 Google Scholar
Sakurai, T. 1991, M. N. R. A. S., 248, 457 Google Scholar
Sofia, S., & Chan, K.L. 1984, Ap. J., 282, 550 Google Scholar
Tassoul, J.-L. 1978, Theory of Rotating Stars (Princeton: Princeton University Press)Google Scholar
Tassoul, J.-L. 1990, in Angular Momentum and Mass Loss for Hot Stars, eds. Willson, L.A. & Stalio, R. (Kluwer), 7 Google Scholar
Tassoul, J.-L., and Tassoul, M. 1982, Ap. J. Suppl., 49, 317 Google Scholar
Vauclair, G., Vauclair, S., & Michaud, G. 1978, Ap. J., 223, 920 Google Scholar
Vauclair, S. 1988, Ap. J., 335, 971 Google Scholar
Venn, K.A., & Lambert, D.L. 1990, Ap. J., 363, 234 CrossRefGoogle Scholar
Zahn, J.-P. 1987, in The Internai Solar Angular Velocity, Durney, B. & Sofia, S. (Dordrecht: Reidel), p. 201 Google Scholar
Zahn, J.-P. 1992, submitted to Astron. Ap. Google Scholar