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Paper: Challenges in Solar and Stellar Model Physics
Volume: 478, Fifty Years of Seismology of the Sun and Stars
Page: 351
Authors: Guzik, J. A.
Abstract: We are reaching relative maturity and standardization in one-dimensional single-star stellar evolution and pulsation modeling, and are making advances in binary and 2D and 3D models. However, many physical inputs are still uncertain or neglected in models of the Sun and of other stars. Thanks to the Kepler, CoRoT, and MOST spacecraft, and ground-based networks, we now have pulsation data for stars that are of comparable quality to that for the Sun to constrain models and test physical assumptions. Here I will focus on main sequence (core H-burning) or slightly post-main sequence (shell H-burning) stellar models, and some of the unsolved problems for these stars. I will revisit the solar abundance problem, and show the effects of modified electron screening, dark matter, and early mass loss on solar models. I will discuss the γ Dor/δ Sct hybrid stars, the mismatch between predicted and observed frequencies for δ Sct stars, and how seismology of stars more massive than the Sun, e.g. the brightest Kepler target θ Cyg, could help us constrain physical processes such as diffusive settling, test pulsation driving mechanisms, and provide clues to the solar abundance problem.
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