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Origin of the Near-Surface Shear Layer of Solar Rotation

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Abstract

Helioseismology has revealed an increase in the rotation rate with depth in a thin (\({\sim}30\) Mm) near-surface layer. The normalized rotational shear in this layer does not depend on latitude. This rotational state is shown to be a consequence of the short characteristic time of near-surface convection compared to the rotation period and radial anisotropy of convective turbulence. Analytical calculations within mean-field hydrodynamics reproduce the observed normalized rotational shear and are consistent with numerical experiments on radiative hydrodynamics of solar convection. The near-surface shear layer is the source of global meridional flow important for the solar dynamo.

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Fig. 1

Notes

  1. https://docs.mesastar.org

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Funding

This work was financially supported by the Ministry of Science and High Education of the Russian Federation.

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Authors and Affiliations

  1. Institute of Solar–Terrestrial Physics, Russian Academy of Sciences, Siberian Branch, 664033, Irkutsk, Russia

    L. L. Kitchatinov

  2. Pulkovo Astronomical Observatory, Russian Academy of Sciences, 196140, St. Petersburg, Russia

    L. L. Kitchatinov

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Correspondence to L. L. Kitchatinov.

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Translated by V. Astakhov

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Kitchatinov, L.L. Origin of the Near-Surface Shear Layer of Solar Rotation. Astron. Lett. 49, 754–761 (2023). https://doi.org/10.1134/S106377372311004X

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