Solar Physics

, Volume 9, Issue 2, pp 452–466 | Cite as

Meridional (north-south) motions of the solar wind

  • G. L. Siscoe
  • L. T. Finley


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°.


Magnetic Field Steady State Solar Wind Spatial Dependence Hydrodynamic Equation 
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Copyright information

© D. Reidel Publishing Company 1969

Authors and Affiliations

  • G. L. Siscoe
    • 1
  • L. T. Finley
    • 2
  1. 1.Dept. of MeteorologyUniversity of CaliforniaLos AngelesU.S.A.
  2. 2.Dept. of Planetary and Space ScienceUniversity of CaliforniaLos AngelesU.S.A.

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