The stability of a solar model to non-radial oscillations.
Abstract
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.
- Publication:
-
Monthly Notices of the Royal Astronomical Society
- Pub Date:
- December 1974
- DOI:
- 10.1093/mnras/169.3.429
- Bibcode:
- 1974MNRAS.169..429C
- Keywords:
-
- Astronomical Models;
- Gravity Waves;
- Oscillations;
- Solar Physics;
- Thermal Instability;
- Abundance;
- Luminosity;
- Main Sequence Stars;
- Neutrinos;
- Solar Constant;
- Stellar Evolution;
- Thermonuclear Reactions;
- Solar Physics