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Helioseismic Constraints on the Structure of the Present Sun

Published online by Cambridge University Press:  12 April 2016

V.A. Baturin  and
S.V. Ajukov
V.A. Baturin
Affiliation:
Sternberg Astronomical Institute, Moscow 119899, Russia
S.V. Ajukov
Affiliation:
Sternberg Astronomical Institute, Moscow 119899, Russia

Extract

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Given the chemical composition (essentially the hydrogen abundance), mass and the physics of the interior, the structure of a star is uniquely determined. The usual method for the determination of the hydrogen-abundance profile of the present Sun is via evolutionary calculations. But the existing uncertainties in the physics and evolutionary history suggest considering a more extended set of possible solar models. Here, we examine models with solar values of radius, luminosity and mass, but with arbitrary profiles of the hydrogen abundance in the core. Of course, the profiles X(m/M) must satisfy some (rather weak) restrictions, so that the solar values (determined by fitting) can be attained.

Type
I. Setting the stage: Sun, Stars Galaxies and the Universe
Information
International Astronomical Union Colloquium , Volume 137: Inside the Stars , 1993 , pp. 69 - 71
Copyright
Copyright © Astronomical Society of the Pacific 1993

References

Christensen–Dalsgaard, J. 1988, Computational Procedures for GONG Solar Model Project.Google Scholar
Christensen–Dalsgaard, J. 1991, in Challenges to Theories of the Structure of Moderate-mass Stars, pp. 11–36, ed. Gough, D.O. and Toomre, J. (Lecture Notes in Physics, 388, Springer, Heidelberg, 1991).Google Scholar
Christensen–Dalsgaard, J. 1992, Geophys. Astrophys. Fluid Dynamics, in press.Google Scholar
Courtaud, D., Damamme, G., Genot, E., Vuillemin, M., and Turck-Chièze, S. 1990, Solar Phys., 128, 49–60.CrossRefGoogle Scholar
Kim, Y.-C., Demarque, P., and Guenther, D.B. 1991, ApJ, 377, 407–412.CrossRefGoogle Scholar
Mihalas, D., Däppen, W., and Hummer, D.G. 1988, ApJ, 331, 815–825.CrossRefGoogle Scholar
Sackmann, I.-J., Boothroyd, A.I., and Fowler, W. 1990, ApJ, 360, 727–736.CrossRefGoogle Scholar
Vorontsov, S.V., Baturin, V.A., and Pamyatnykh, A.A. 1991, Nature, 349, 49–51.CrossRefGoogle Scholar