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The rotation of the solar atmosphere

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Abstract

A model of the solar atmosphere is presented in which we discuss the conservation of angular momentum for the two basic states in which the solar gas can be: namely, either confined by closed field lines or outflowing along open magnetic field lines. It can be shown that the boundary conditions are in general different for these two cases. From this we obtain the results that in the closed configuration the gas can corotate at the solar surface with the magnetic field lines and its angular velocity will then increase with height, whereas for a gas flowing along an open field line the angular velocity will decrease. An exception to the latter case can be found where the open magnetic field lines are strongly nonradial and where the density is a slowly varying function of radius. In such regions the angular velocity may initially increase with height, reach a maximum and then decrease.

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Authors and Affiliations

  1. Kitt Peak National Observatory, Tucson, Ariz., U.S.A.

    E. J. Weber

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  1. E. J. Weber
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Kitt Peak National Observatory Contribution No. 439.

Operated by The Association of Universities for Research in Astronomy, Inc., under contract with the National Science Foundation.

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Weber, E.J. The rotation of the solar atmosphere. Sol Phys 9, 150–159 (1969). https://doi.org/10.1007/BF00145735

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  • DOI: https://doi.org/10.1007/BF00145735

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