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Outward transport of angular momentum by gas convection and the equatorial acceleration of the Sun

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Abstract

A new mechanism for sustaining enhanced rotational velocity of the outer layers of the solar convective envelope is considered.

The gas density inside turbulent eddies decreases because of centrifugal scattering of matter. The decrease of density in eddies rotating in the same sense as the Sun on the whole is larger than that in eddies rotating in the opposite sense. As a result, the former ascend while the latter sink down, thus producing a continuous outward flux of angular momentum.

A distribution of angular velocity in the radius of the solar convective envelope in the equatorial plane was obtained in the approximation of the ‘mixing length’ theory of thermal convection. The results agree rather well with observations.

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Authors and Affiliations

  1. A. F. Ioffe Physical-Technical Institute, Academy of Sciences of the USSR, K-21, Leningrad, U.S.S.R.

    E. M. Drobyshevski

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  1. E. M. Drobyshevski
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Drobyshevski, E.M. Outward transport of angular momentum by gas convection and the equatorial acceleration of the Sun. Sol Phys 51, 473–479 (1977). https://doi.org/10.1007/BF00216380

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  • DOI: https://doi.org/10.1007/BF00216380

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