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Turbulence and Solar p-Mode Oscillations

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Abstract

The discrepancy between observed and theoretical mode frequencies can be used to examine the reliability of the standard solar model as a faithful representation of solar real situation. With the help of an improved time-dependent convective model that takes into account contribution of the full spatial and temporal turbulent energy spectrum, we study the influence of turbulent pressure on structure and solar p-mode frequencies. For the radial modes we find that the Reynolds stress produces signification modifications in structure and p-mode spectrum. Compared with an adiabatic approximation, the discrepancy is largely removed by the turbulent correction.

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Authors and Affiliations

  1. Yunnan Observatory, NAOCAS, Chinese Academy of Sciences, Kunming, 650011, P.R. China

    S.L. Bi & H.Y. Xu

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  1. S.L. Bi
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  2. H.Y. Xu
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Bi, S., Xu, H. Turbulence and Solar p-Mode Oscillations. Astrophysics and Space Science 279, 191–202 (2002). https://doi.org/10.1023/A:1015136218125

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  • DOI: https://doi.org/10.1023/A:1015136218125

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