Thermally conductive flows in coronal holes

Details Thermally conductive flows in coronal holes Thermally conductive flows in coronal holes

Nov 1977

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1977soph...55...99s&link_type=abstract

Solar Physics, vol. 55, Nov. 1977, p. 99-109.

Physics

18

Conducting Fluids, Gas Expansion, Solar Corona, Solar Wind, Thermal Conductivity, Astronomical Models, Emission Spectra, Polytropic Processes, Stellar Models

Scientific paper

A treatment of polytropic solar wind flows in non-radial expansion regions, developed by Kopp and Holzer (1976), is extended to include the effect of thermal conduction. Thermal conductive and polytropic flows in the lower corona under specified high-speed stream conditions at 1 AU are compared; the thermally conductive flows more closely model the observed phenomena, though predicted electron density is still too low and the predicted temperature too high. It is suggested that another mechanism (such as wave pressure), in conjunction with thermal conduction, may provide an accurate explanation for solar wind flows originating in coronal holes.

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