A leaky magnetohydrodynamic waveguide model for the acceleration of high-speed solar wind streams in coronal holes

Details A leaky magnetohydrodynamic waveguide model for the acceleration of high-speed solar wind streams in coronal holes A leaky magnetohydrodynamic waveguide model for the acceleration of high-speed solar wind streams in coronal holes

Apr 1985

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985apj...291..328d&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 291, April 1, 1985, p. 328-338.

Physics

Optics

33

Coronal Holes, Magnetohydrodynamic Waves, Solar Corona, Solar Wind, Acceleration, Geometrical Optics, Wave Propagation, Waveguides

Scientific paper

It is well established observationally that high-speed solar wind streams originate in coronal hole regions in the solar corona. One suggested source for the additional momentum of these streams is "wave pressure" generated by magnetohydrodynamic (MHD) waves. In the paper the effect of coronal hole magnetic structure on the propagation of MHD waves of all periods is considered. It is found that the coronal hole structure acts as a "leaky" MHD waveguide, i.e., wave flux which enters at the base of the coronal hole is only weakly guided by the coronal hole structure. The force on the coronal hole plasma due to the propagation of the leaky wave modes is calculated. It is found that the net force consists of two terms: (1) magnetic wave pressure and (2) magnetic wave tension. The calculations imply that the coupling of the solar wind plasma to the turbulence in the photosphere may not be as efficient as previous theories of wave propagation in the corona have indicated.

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