Nonadiabatic nonradial oscillations of a solar model
Abstract
The stability of a solar model on the main sequence to linearized nonadiabatic nonradial oscillations has been studied. In the inner 99.9 per cent b.y. radius the eigenfunctions were barely distinguishable from those of the adiabatic approximation. The integrated effect of this region is to stabilize the oscillations at zero age, but after a time of order .1 b.y. the destabilizing effect of the 3He (3He, 2p) 4He reactions exceeds the damping. However, there is much more severe damping in a nonadiabatic shell beneath the photosphere about 300 km thick, which dominates the entire effect from the rest of the star interior to this shell.
- Publication:
-
Memoires of the Societe Royale des Sciences de Liege
- Pub Date:
- 1975
- Bibcode:
- 1975MSRSL...8..309C
- Keywords:
-
- Astronomical Models;
- Eigenvectors;
- Main Sequence Stars;
- Solar Atmosphere;
- Stable Oscillations;
- Vibration Mode;
- Adiabatic Conditions;
- Boundary Value Problems;
- Measure And Integration;
- Newton-Raphson Method;
- Nuclear Fusion;
- Oscillation Dampers;
- Perturbation Theory;
- Photosphere;
- Radiative Transfer;
- Spherical Harmonics;
- Stellar Interiors;
- Astrophysics