Magnetic Wavenumber Spectrum of Whistler Turbulence: Particle-In-Cell Simulation

Details Magnetic Wavenumber Spectrum of Whistler Turbulence: Particle-In-Cell Simulation Magnetic Wavenumber Spectrum of Whistler Turbulence: Particle-In-Cell Simulation

Dec 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010agufmsh41b1800s&link_type=abstract

American Geophysical Union, Fall Meeting 2010, abstract #SH41B-1800

Physics

Plasma Physics

[2159] Interplanetary Physics / Plasma Waves And Turbulence, [2164] Interplanetary Physics / Solar Wind Plasma, [7863] Space Plasma Physics / Turbulence

Scientific paper

The forward cascade of decaying whistler turbulence is studied in low beta plasma to understand essential properties of the energy spectrum at electron scales, by using a two-dimensional electromagnetic particle-in-cell (PIC) simulation. This simulation demonstrates the turbulence which has larger energy cascade rate than the dissipation rate of turbulence at the electron inertial scales. The PIC simulation shows that the magnetic energy spectrum of forward-cascaded whistler turbulence at the electron scales exhibits an anisotropic property and a very steep power-law spectrum which is consistent with recent solar wind observations. A comparison of the power-law index of steep spectrum with that predicted by phenomenological turbulence scaling expression for the electron inertial scales, suggests that the energy cascade at the scales depends on both magnetic fluctuations and electron velocity fluctuations, and whistler dispersion relation at the electron scales. As the energy cascade rate is enough larger than the dissipation rate of turbulence in the solar wind, not only kinetic Alfven turbulence but also whistler turbulence can explain recent solar wind observations of very steep magnetic spectra at short scales.

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