Solution of three-fluid model equations with anomalous transport coefficients for the quiet solar wind

Details Solution of three-fluid model equations with anomalous transport coefficients for the quiet solar wind Solution of three-fluid model equations with anomalous transport coefficients for the quiet solar wind

Feb 1975

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1975apj...196..205c&link_type=abstract

Astrophysical Journal, vol. 196, Feb. 15, 1975, pt. 1, p. 205-219.

Mathematics

Logic

13

Astronomical Models, Mathematical Models, Multiphase Flow, Solar Wind, Transport Properties, Alpha Particles, Dynamic Models, Friction, Heat Transfer, Interplanetary Magnetic Fields, Perturbation Theory, Solar Corona, Solar Electrons, Solar Protons, Solar Wind Velocity

Scientific paper

A three-fluid model consisting of continuity, momentum, and energy equations is used to describe the average behavior of the electrons, protons, and alpha-particles in the quiet expanding solar corona. Friction forces due to the possible occurrence of different particle streaming velocities are incorporated in the model equations. The transport coefficients are allowed to include phenomenological contributions from turbulent wave-particle interactions existing in the solar wind. The model assumes spherical symmetry and neglects such effects as viscosity, rotation, and magnetic fields. The numerical solution of the equations is achieved by using a perturbation-method procedure in which a two-fluid solution for electrons and protons is followed by a solution for the alpha particles. These model-equations predict the following features of the alpha-particles at 1 AU: (1) equal alpha-particle and proton streaming velocities, (2) an alpha-particle to proton temperature ratio of about 3.5, and (3) an alpha-particle to proton density ratio of about 0.035.

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