Other
Scientific paper
Mar 1985
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985apj...290..344g&link_type=abstract
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 290, March 1, 1985, p. 344-346.
Other
5
Nuclear Fusion, Solar Oscillations, Stellar Cores, Stellar Evolution, Thermonuclear Reactions, Abundance, Helium Isotopes, Kelvin-Helmholtz Instability, Perturbation Theory, Solar Neutrinos, Thermal Instability
Scientific paper
A search for coupled thermal-nuclear oscillations in the solar core is made using a stellar evolution code with a full nuclear reaction network. The Kelvin-Helmholtz time scale for the whole sun is 3 x 10 to the 7th yr, but only 3 x 10 to the 6th yr for the nuclear-burning core. The lifetime of He-3 in the solar core is more than about 10 to the 5th yr and increases rapidly outward. Processing of He-3 accounts for about two-thirds of the energy released in the dominant p-p reaction chains in the sun. Oscillations of the nuclear species could generate solar luminosity variations on time scales of 10 to the 5th to 10 to the 7th yr. Evolution sequences following large-amplitude perturbations of He-3 and other minor nuclear species show strong damping with equilibrium being restored on the Kelvin-Helmholtz time scale. Consistent with previous linear analyses, no evidence for thermonuclear instability in the sun is found.
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