Abstract
The variety and precision of the observed frequencies of solar oscillations allow a detailed investigation of the foundations of computations of stellar models. This is of obvious importance to our understanding of the structure of other stars of moderate mass. Furthermore, we may hope to use the solar data to obtain information about the basic properties of matter under solar conditions.
To exploit the solar data it is crucial to understand and limit the uncertainties in the computation of solar models and frequencies. In addition, we must explore the sensitivity of the models to the properties of the physics of the solar interior and to the simplifying assumptions made in the calculations. I discuss numerical tests of the calculations, including comparisons of independently computed models. Furthermore, I present results of modifying the assumed physics, in particular the equation of state and the opacity. At the level of the observational precision the frequencies are highly sensitive to even quite subtle details of the physics.
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Christensen-Dalsgaard, J. (1991). Solar oscillations and the physics of the solar interior. In: Gough, D., Toomre, J. (eds) Challenges to Theories of the Structure of Moderate-Mass Stars. Lecture Notes in Physics, vol 388. Springer, Berlin, Heidelberg. https://doi.org/10.1007/3-540-54420-8_47
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DOI: https://doi.org/10.1007/3-540-54420-8_47
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