Research on the solar model and oscillation in 1990s (I): progress in solar models.
Abstract
The study of solar models is the most important way to understand the global structure and properties of the Sun. Developments in solar modelling in the 1990s are reviewed. The use of the MHD and OPAL equations of states and of the OPAL opacity has moved the theoretical solar oscillation frequencies much closer to the observed values. The introduction of turbulent spectrum in the local convection theory and the 3D hydrodynamic simulation convection models have increased the knowledge of convective energy transportation, as well as its influence on the global Sun. The difference of surface helium abundance between models and inversion results has been filled by diffusion effects. Surface lithium may be depleted by turbulent diffusion or big mass loss. An astrophysical solution for the solar neutrino fluxes looks unlikely. A higher probability exists for a solution from particle physics.
- Publication:
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Progress in Astronomy
- Pub Date:
- December 1998
- Bibcode:
- 1998PABei..16..287G
- Keywords:
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- Solar Models;
- Solar Oscillations;
- Solar Neutrinos