Computer Science – Numerical Analysis
Scientific paper
Feb 1976
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1976apj...203..720a&link_type=abstract
Astrophysical Journal, vol. 203, Feb. 1, 1976, pt. 1, p. 720-738.
Computer Science
Numerical Analysis
11
Astronomical Models, Interplanetary Medium, Solar Wind, Two Fluid Models, Azimuth, Magnetic Fields, Magnetohydrodynamic Flow, Mathematical Models, Numerical Analysis, Solar Wind Velocity, Vlasov Equations
Scientific paper
The two-region model of the solar wind divides the interplanetary space into two regions: it assumes that the solar wind is one-fluid in an inner region within 0.4 AU and two-fluid in an outer region beyond 0.4 AU. This paper includes the angular motion of the solar wind in the two-region model. The flow in the one-fluid region is governed by the one-fluid magnetohydrodynamic equations. The second and third moment equations of the Vlasov equation together with other conservation equations are used to describe the solar-wind flow in the two-fluid region. The predicted azimuthal velocity at 1 AU is less than 2 km/s. All other macroscopic and microscopic properties from this model are in good agreement with experimental quiet-time observations at 1 AU. The numerical results also confirm that when the azimuthal velocity is included in the analysis, the amount of magnetic-field energy converted into kinetic energy in the solar wind is only a small fraction of the total expansion energy flux and has little effect upon the final radial expansion velocity.
Acuña Mario Humberto
Whang Yun C.
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