The stability of a solar model to non-radial oscillations

Details The stability of a solar model to non-radial oscillations The stability of a solar model to non-radial oscillations

Dec 1974

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1974mnras.169..429c&link_type=abstract

Monthly Notices of the Royal Astronomical Society, vol. 169, Dec. 1974, p. 429-445.

Physics

67

Astronomical Models, Gravity Waves, Oscillations, Solar Physics, Thermal Instability, Abundance, Luminosity, Main Sequence Stars, Neutrinos, Solar Constant, Stellar Evolution, Thermonuclear Reactions

Scientific paper

The stability of a solar model to low-order gravity modes has been investigated in quasi-adiabatic approximation, neglecting any direct effects of convection on the oscillations. The zero age main sequence model was found to be stable, but after about 200 m.y. the g1 (l = I) mode became unstable. The dominant destabilization comes from the dependence of the pp chain reaction rate on the abundances of He-3 and H when nuclear equilibrium is disturbed, and is felt once a sufficient He-3 inhomogeneity is established in the energy generating core.

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