Astronomy and Astrophysics – Astrophysics
Scientific paper
Nov 1992
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992apj...400..362s&link_type=abstract
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 400, no. 1, p. 362-368.
Astronomy and Astrophysics
Astrophysics
9
Conductive Heat Transfer, Magnetohydrodynamics, Proton Energy, Solar Corona, Solar Wind, Coulomb Collisions, Electron Density (Concentration), Flux (Rate)
Scientific paper
A two-fluid model of the solar wind was introduced by Sturrock and Hartle (1966) and Hartle and Sturrock (1968). In these studies the proton energy equation was integrated neglecting the heat conductive term. Later several authors solved the equations for the two-fluid solar wind model keeping the proton heat conductive term. Methods where the equations are integrated simultaneously outward and inward from the critical point were used. The equations were also integrated inward from a large heliocentric distance. These methods have been applied to cases with low coronal base electron densities and high base temperatures. In this paper we present a method of integrating the two-fluid solar wind equations using an iteration procedure where the equations are integrated separately and the proton flux is kept constant during the integrations. The technique is applicable for a wide range of coronal base densities and temperatures. The method is used to carry out a parameter study of the two-fluid solar wind.
Holzer Thomas Edward
Leer Egil
Sandbaek Ornulf
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