Physics
Scientific paper
Oct 1985
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985soph..100...21r&link_type=abstract
Solar Physics (ISSN 0038-0938), vol. 100, Oct. 1985, p. 21-51.
Physics
30
Solar Interior, Solar Magnetic Field, Stellar Evolution, Stellar Models, Stellar Structure, Carbon 12, Convective Flow, Magnetohydrodynamic Stability, Nuclear Reactions, Solar Flux, Solar Neutrinos, Stellar Rotation, Turbulent Mixing
Scientific paper
The standard model of solar evolution is reviewed and a number of problems are highlighted. A fundamental question is whether there is any mixing of matter in the central regions, since such mixing could radically alter the model of the present sun and modify our understanding of the evolution of other stars. Standard models of solar evolution become unstable to He-3 driven global oscillations at an age of 3x10 to the 8th years and this may drive some mixing; even if this is not the case, the finite amplitude limit of these oscillations is likely to produce modifications in the standard model. The internal rotation of the sun remains an enigma and absence of knowledge of any internal magnetic field makes it difficult to study the problem. Rotationally driven instabilities are ineffective in the central chemically inhomogeneous regions but may contribute to the inward diffusion of lithium from the convective zone. These and other problems are considered but few solutions are proposed.
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