Hybrid simulations of the two-dimensional cascade of weak solar wind turbulence beyond MHD scales

Details Hybrid simulations of the two-dimensional cascade of weak solar wind turbulence beyond MHD scales Hybrid simulations of the two-dimensional cascade of weak solar wind turbulence beyond MHD scales

Dec 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011agufmsh52a..01v&link_type=abstract

American Geophysical Union, Fall Meeting 2011, abstract #SH52A-01

Physics

Plasma Physics

[7827] Space Plasma Physics / Kinetic And Mhd Theory, [7863] Space Plasma Physics / Turbulence, [7868] Space Plasma Physics / Wave/Wave Interactions

Scientific paper

The nature of solar wind turbulence in the dissipation range beyond the typical large MHD scales is still under debate. A two-dimensional model is presented based on the hybrid code A.I.K.E.F., which treats ions as particles following the Vlasov equation and electrons as a massless neutralizing fluid. Up to a certain wavenumber in the MHD regime, the system is initialized with a superposition of isotropic Alfvén waves with amplitudes following the empirically confirmed spectral power law of Kolmogorov. The turbulence then evolves and cascades into the dispersive spectral range, where also dissipative effects emerge. Under typical solar wind conditions, weak turbulence develops as a superposition of normal modes in the kinetic regime. The spectral analysis in the direction parallel to the background magnetic field reveals a cascade of left-handed Alfvén/ion-cyclotron waves until the resonant absorption sets in and a right-handed fast/whistler component. Perpendicular to the background field, a broad turbulent spectrum is found built up of fluctuations with a strong compressive component. Ion-Bernstein waves are possible normal modes in this direction of propagation.

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