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Corotating structure in the solar wind

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Abstract

The hydrodynamic equations which describe the radial solar wind expansion are linearized and specialized to treat corotating perturbations. Approximate solutions are found which are time stationary in the corotating reference frame. The solutions predict the behavior of corotating structures for a given boundary condition close to the sun. In particular, the structure resulting from the interaction of fast and slow streams is described. Comparison with sector structure data shows reasonable qualitative and quantitative agreement.

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Authors and Affiliations

  1. Dept. of Physics, Boston College, Chestnut Hill, Mass., U.S.A.

    R. L. Carovillano

  2. Dept. of Meteorology, University of California, Los Angeles, Calif., U.S.A.

    G. L. Siscoe

Authors
  1. R. L. Carovillano
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  2. G. L. Siscoe
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Carovillano, R.L., Siscoe, G.L. Corotating structure in the solar wind. Sol Phys 8, 401–414 (1969). https://doi.org/10.1007/BF00155388

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  • DOI: https://doi.org/10.1007/BF00155388

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