On the modeling of the three-fluid structure of the quiet solar wind

Details On the modeling of the three-fluid structure of the quiet solar wind On the modeling of the three-fluid structure of the quiet solar wind

Sep 1981

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1981ap%26ss..79...67c&link_type=abstract

Astrophysics and Space Science, vol. 79, no. 1, Sept. 1981, p. 67-75.

Astronomy and Astrophysics

Astrophysics

6

Alpha Particles, Astronomical Models, Multiphase Flow, Particle Interactions, Plasma Jets, Solar Wind, Electric Fields, Gas Expansion, Interplanetary Gas, Particle Density (Concentration), Solar Corpuscular Radiation, Steady Flow, Stellar Models, Temperature Distribution

Scientific paper

The reciprocal influences of, on the one hand, the electrons and protons of the solar wind, and, on the other, solar wind alpha particles are investigated for the case of the quiet expanding corona within the framework of a conductive three-fluid model. The three-fluid equations incorporating frictional forces due to different streaming velocities are solved in two manners: by the simultaneous solution of the fluid equations for all three species, and by the solution of the two-fluid equations for the electrons and protons followed by the solution of a modified one-fluid equation for the alpha particles. Both methods are found to provide solutions for all three species which are in satisfactory agreement with observations at 1 AU, indicating that differences between the three-fluid and two-fluid characteristics of electrons and protons represent a second-order effect on the alpha particles. The frictional interaction between alpha particles and protons is found to raise the alpha particle streaming velocity to that of the protons and decrease the alpha particle to proton density ratio to about 0.035, while the alpha particles affect the solar wind proton temperature profile through heat exchange, dynamic friction and contributions to the interplanetary electrostatic field.

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