Formation of the corona and fast solar-wind streams above coronal holes

Details Formation of the corona and fast solar-wind streams above coronal holes Formation of the corona and fast solar-wind streams above coronal holes

Apr 1988

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1988ge%26ae..28..190c&link_type=abstract

Geomagnetizm i Aeronomiia (ISSN 0016-7940), vol. 28, Mar.-Apr. 1988, p. 190-196. In Russian.

Physics

Coronal Holes, Magnetohydrodynamic Waves, Solar Wind, Space Plasmas, Field Strength, Magnetohydrodynamic Flow, Plasma Density, Plasma Temperature

Scientific paper

A theoretical model with an MHD-wave energy source is used to examine corona formation and solar-wind streams above coronal holes. The magnetic-field structure is assumed to be quasi-monopole in nature. It is shown that the superradial divergence of magnetic field lines leads to a greater effect of the solar-wind outflow on the coronal thermal regime than in a radial field. This leads to lower-than-background values of plasma temperature and density in the corona and to higher speeds of the solar-wind streams.

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