Abstract
Solar Oscillations, with frequencies between 2 and 5 mHz, can be identified as p modes with well-determined degree 1 and overtone number n, but minor discrepancies, of order 10 MHZ, between observed and calculated frequencies remain. We describe the computation of solar models and their frequencies of oscillation, check the accuracy of the numerical results, and study the influence of the atmosphere. Attempts to improve the calculated frequencies for low degree and intermediate order (n=10…20) have so far been unsuccessful.
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Stix, M., Knölker, M. (1987). On the Frequencies of Solar Oscillations. In: Hillebrandt, W., Meyer-Hofmeister, E., Thomas, HC. (eds) Physical Processes in Comets, Stars and Active Galaxies. Springer, Berlin, Heidelberg. https://doi.org/10.1007/978-3-642-72640-8_7
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DOI: https://doi.org/10.1007/978-3-642-72640-8_7
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