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Chemical Inhomogeneities and Pulsation1

Published online by Cambridge University Press:  12 April 2016

S. Turcotte
S. Turcotte*
Affiliation:
Lawrence Livermore National Laboratory, L-413, P. O Box 808, Livermore, CA 94551, USA; e-mail:sturcotte@igpp.ucllnl.org

Abstract

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Major improvements in models of chemically peculiar stars have been achieved in the past few years. With these new models it has been possible to test quantitatively some of the processes involved in the formation of abundance anomalies and their effect on stellar structure. The models of metallic A (Am) stars have shown that a much deeper mixing has to be present to account for observed abundance anomalies. This has implications on their variability, which these models also reproduce qualitatively. These models also have implications for other chemically inhomogeneous stars such as HgMn B stars which are not known to be variable and λ Boötis stars which can be. The study of the variability of chemically inhomogeneous stars can provide unique information on the dynamic processes occurring in many types of stars in addition to modeling of the evolution of their surface composition.

Type
Part 2.3. Chemically Peculiar Stars
Information
International Astronomical Union Colloquium , Volume 185: Radial and Nonradial Pulsations as Probes of Stellar Physics , 2002 , pp. 257 - 265
Copyright
Copyright © Astronomical Society of the Pacific 2002

Footnotes

1

This work was performed under the auspices of the U.S. Department of Energy, National Nuclear Security Administration by the University of California, Lawrence Livermore National Laboratory under contract No. W-7405-Eng-48.

References

Babel, J. 1996, A&A, 309, 867 Google Scholar
Charbonneau, P. 1993, ApJ, 405, 720 CrossRefGoogle Scholar
Charpinet, S., Fontaine, G., Brassard, P., & Dorman, B. 1996, ApJ, 471, 103 CrossRefGoogle Scholar
Cox, A.N., Hodson, S.W., & King, D.S. 1979, ApJ, 231, 798 CrossRefGoogle Scholar
Fowler, W.A., Burbidge, E.M., Burbidge, G.R., & Hoyle, F. ApJ, 142, 423 CrossRefGoogle Scholar
Gonzalez, J.-F., Bohlender, D.A., Matthews, J.M., & Yang, S. 1998, in Fundamental Stellar Properties: The Interaction between Observation and Theory, ed. Bedding, T., (University of Sydney), 132 Google Scholar
Grevesse, N. & Noels, A. 1993, in Origin and Distribution of the Elements, eds. Prantzos, N., Vangioni-Flam, E., Cassé, M., (Cambridge Univ. Press), 15 Google Scholar
Guthrie, B.N.G. 1971, Ap&SS, 13, 168 Google Scholar
Kurtz, D.W. 1978, ApJ, 221, 869 CrossRefGoogle Scholar
Kurtz, D.W. 2000, in ASP Conf. Ser., Vol. 210, Delta Scuti and Related Stars, eds. Breger, M. & Montgomery, M., (San Francisco ASP), 287 Google Scholar
Kurtz, D.W. & Wegner, G. 1979, ApJ, 232, 510 CrossRefGoogle Scholar
Richer, J., Michaud, G., & Turcotte, S. 2000, ApJ, 529, 338 CrossRefGoogle Scholar
Solano, E., Paunzen, E., Pintado, O.I., Córdoba, , & Varela, J. 2001, A&A, 374, 957 Google Scholar
Turcotte, S. & Charbonneau, P. 1993, ApJ, 413, 456 CrossRefGoogle Scholar
Turcotte, S., Richer, J., Michaud, G., & Christensen-Dalsgaard, J. 2000, A&A, 360, 603 Google Scholar
Venn, K.A. & Lambert, D.L. 1990, ApJ, 363, 234 CrossRefGoogle Scholar