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 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 imporoved stellar oscillation theory. However, the discrepancy is still bigger than the observational error. From frequency inversion studies we know more about the solar convection zone, the surface helium abundance and rotional velocity distribution as a function of depth and latitude. The stochastic excitation mechanism by turbulence and the location of the excitaion 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 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.
Gong ZG,Yuan YQ,Li Y,et al. Research on the Solar Model and Oscillation in 1990s (II): Progress in Research on the Solar Oscillations[J]. 天文学进展,1998,16(4):305-320.
APA
龚志刚,袁永泉,李焱,W．D ppen,&彭美仙.(1998).Research on the Solar Model and Oscillation in 1990s (II): Progress in Research on the Solar Oscillations.天文学进展,16(4),305-320.
MLA
龚志刚,et al."Research on the Solar Model and Oscillation in 1990s (II): Progress in Research on the Solar Oscillations".天文学进展 16.4(1998):305-320.
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