Physics
Scientific paper
Dec 2008
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008agufmsh42a..02b&link_type=abstract
American Geophysical Union, Fall Meeting 2008, abstract #SH42A-02
Physics
2149 Mhd Waves And Turbulence (2752, 6050, 7836), 2164 Solar Wind Plasma, 7827 Kinetic And Mhd Theory, 7859 Transport Processes, 7863 Turbulence (4490)
Scientific paper
Every fluctuation of MHD turbulence has a flow nature and an Alfven-wave nature. Further, all Alfven waves in a collisionless plasma are subject to Landau damping Hence, for the solar wind all turbulent fluctuations experience dissipation, which can be couched as a shear viscosity of the solar-wind plasma and this shear viscosity can be used to construct Reynolds numbers. The expressions obtained for viscosity are quite simple. For the solar-wind plasma, the Landau-damping viscosity is much stronger than the Braginskii shear viscosity, yielding turbulence Reynolds numbers R of 500,000 to 50,000,000, depending on the model used to describe the solar-wind turbulence. These R values are compared with effective Reynolds numbers obtained from the ratios of the measured correlation lengths to the measured Taylor scales of the solar-wind turbulence. A discussion follows as to whether MHD turbulence obeys the same scalings with Reynolds number as does Navier-Stokes turbulence.
Borovsky Joseph E.
Gary Peter S.
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