摘要
太阳振荡研究现已成为研究太阳内部性质的新手段，也成为检验太阳模型构造时输入物理参量的最重要工具。90年代以来理论与观测日震频率的差别已随输入物理参量及太阳振荡理论的改进而大为减小，可是现有的差别仍远大于观测误差。由日震反演可对太阳内部对流区、表面氦丰度及自转随纬度和径向的分布都有更多了解。太阳振荡的湍动随机激发及激发源的位置都已得到研究，不过现在问题还未完全解决。今后一方面要探测更多的振动方式，另一方面也需要解决不同观测者得到的结果存在系统差的问题，而最外层的非绝热现象及理论与观测存在差别仍是最关键的难题。
Helioseismology has become a new tool for the study of the solar interior as well as one of the most important devices to determine the quality of the the input physics that enters the solar models. The discrepancy between theoretical and observational frequencies has drastically decreased in the 1990s due to modified input physics and improved stellar oscillation theory. However, the discrepancy is still bigger than the observational error. From frequency inversion studies we know more about the solar convection zonet the surface helium abundance and rotational velocity distribution as a function of depth and latitude. The stochastic excitation mechanism by turbulence and the location of the excitation sources are well studied, but not completely understood. More work is needed for the detection of new oscillation modes and also to explain the systematic discrepancy between different observers. The non-adiabatic physics in the outermost layer and the difference between theoretical and observational frequencies especially require closer attention.
出处
《天文学进展》
CSCD
北大核心
1998年第4期305-320,共16页
Progress In Astronomy
关键词
太阳
基本参量
太阳震荡
太阳模型
Sun
oscillations-Sun
fundamental parameters-Sun
interior
