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Meridional (north-south) motions of the solar wind

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Abstract

The steady state hydrodynamic equations which describe the solar wind flow are linearized and used to study the spatial behavior of zonal pressure perturbations. Such perturbations produce meridional (north-south) motions in the solar wind. To simplify the spatial dependence of the zero-order variables and to take advantage of the supersonic regime, the analysis is restricted to heliocentric distances greater than 0.1 AU (astronomical unit). A simplified problem involving a north-south magnetic field asymmetry is also treated. The emphasis of the paper is to determine what pressure perturbations are required at the inner boundary (0.1 AU) to produce at earth north-south deviations from radial flow of 1° to 3°.

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Authors and Affiliations

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

    G. L. Siscoe

  2. Dept. of Planetary and Space Science, University of California, Los Angeles, Calif., U.S.A.

    L. T. Finley

Authors
  1. G. L. Siscoe
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  2. L. T. Finley
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Siscoe, G.L., Finley, L.T. Meridional (north-south) motions of the solar wind. Sol Phys 9, 452–466 (1969). https://doi.org/10.1007/BF02391671

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  • DOI: https://doi.org/10.1007/BF02391671

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