The study of solar models is the most important way for us to understand the global structure and properties of the Sun. Developments in solar modeling in 1990s are reviewed in this paper. 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 intrduction of turbulent spectrum in local convection theory and the 3D hydrodynamic simulation convection models have increased our knowledge of convective enery transportaion, 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 effect. 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.
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