Computer Science
Scientific paper
Mar 2010
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010aipc.1216..206u&link_type=abstract
TWELFTH INTERNATIONAL SOLAR WIND CONFERENCE. AIP Conference Proceedings, Volume 1216, pp. 206-209 (2010).
Computer Science
1
Solar Wind, Plasma Turbulence, Interplanetary Magnetic Fields, Magnetohydrodynamics, Particle Emission, Solar Wind, Turbulence, Interplanetary Magnetic Fields, Magnetohydrodynamics And Plasmas
Scientific paper
A magnetohydrodynamic model is used to simulate the global steady-state structure of the solar wind in the region from 0.3 to 100 AU. The model is based on a numerical solution of the combined set of solar wind equations and small-scale turbulence transport equations and accounts for apparent heating of the solar wind by a turbulence cascade and interstellar pickup protons. We use the model to study the distribution of plasma and magnetic field parameters and the effects of turbulence dissipation and pickup-proton-associated-heating on the variation of plasma temperature in the outer heliosphere. To illuminate the roles of the turbulent cascade and the pickup protons in heating the solar wind with heliocentric distance, we compare the model results with and without turbulence. The variations of plasma temperature in the outer heliosphere are compared with Voyager 2 observations.
Breech Ben
Goldstein Michel L.
Matthaeus William H.
Usmanov Arcadi V.
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