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Fluid dynamics of thin solar wind filaments

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Abstract

This paper gives the radial dependence of the flow parameters in a thin solar wind filament corotating with the Sun. Presuming that the filament flow velocity is different from the external velocity close to the Sun, the solution shows that the radial component of the filament flow is eventually (at distances greater than 1 AU) brought equal to the external radial flow speed by pressures acting on the filament boundary. These pressures also induce azimuthal motion that reaches a maximum near 1 AU. The direction of the azimuthal motion is consistent with that deduced for the fast-slow stream interaction. The longitudinal angular width of the filament changes very little (< 20%) over the length of the filament.

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Authors and Affiliations

  1. Dept. of Meteorology, University of California, 90024, Los Angeles, Calif., U.S.A.

    G. L. Siscoe

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  1. G. L. Siscoe
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Siscoe, G.L. Fluid dynamics of thin solar wind filaments. Sol Phys 13, 490–498 (1970). https://doi.org/10.1007/BF00153568

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  • DOI: https://doi.org/10.1007/BF00153568

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