Numerical simulations of the turbulence dissipation in the solar wind and corona

Details Numerical simulations of the turbulence dissipation in the solar wind and corona Numerical simulations of the turbulence dissipation in the solar wind and corona

Dec 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008agufmsh31a1646m&link_type=abstract

American Geophysical Union, Fall Meeting 2008, abstract #SH31A-1646

Physics

2159 Plasma Waves And Turbulence, 2164 Solar Wind Plasma, 7829 Kinetic Waves And Instabilities, 7867 Wave/Particle Interactions (2483, 6984), 7868 Wave/Wave Interactions

Scientific paper

The physical mechanism responsible for the turbulence dissipation in the solar wind and corona is not completely understood. Analysis of the observational data shows that the damping rate of the turbulent fluctuations has to depend on their amplitude. This suggests a nonlinear mechanism of dissipation. However, existing theoretical mechanisms of nonlinear wave damping require fluctuation amplitudes that are too high compared to the actual values. We will report the results of hybrid simulations designed to mimic quasi-parallel and quasi-perpendicular turbulent fluctuations in a cold and warm plasma. We will analyze how nonlinearity contributes to the damping of the waves when their amplitudes conform to the limitations imposed by observations. In the in situ solar, the amplitudes are estimated directly wind from the measured magnetic spectra. In the corona, the turbulent fluctuations can become compressional due to certain nonlinear and kinetic effects. This allows us to tie the fluctuation amplitudes to the density spectra inferred from the interplanetary scintillation observations.

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