90年代太阳模型和太阳震荡研究进展(I):太阳模型研究进展(英)

Research on the Solar Model and Oscillation in 1990s (I): Progress in Solar Models

太阳模型的研究是了解太阳整体结构和性质的极为重要的手段。90年代以来太阳模型研究取得了进展。随着MHD及OPAL物态方程的引入，理论上的太阳振荡频率与观测值的差别已大为减小，而考虑湍流频谱分布的局域对流理论和三维流体动力学模拟结果可对太阳内部对流能量传输过程有更深刻的理解．以前所发现的理论模型与反演结果得到的初始氦丰度的差别已能由扩散过程加以解释，而太阳表面锂丰度亏损问题也可以由扩散过程或早期演化星风来加以解决，太阳中微子问题则似应由粒子物理而不是天体物理来解决。

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 introduction of turbulent spectrum in local convection theory and the 3D hydrodynamic simulation convection models have increased our 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 effect. Surface lithium may be depleted by turbulent diffusion or big mass loss. An astrophysical solution for the solar neutrino flaxes looks unlikely. A higher probability exists for a solution from particle physics.