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Abstract: Whistler waves are present in solar wind plasma. These waves possesscharacteristic turbulent fluctuations that are characterized typically by thefrequency and length scales that are respectively bigger than ion gyrofrequency and smaller than ion gyro radius. The electron inertial length is anintrinsic length scale in whistler wave turbulence that distinguishably dividesthe high frequency solar wind turbulent spectra into scales smaller and biggerthan the electron inertial length. We present nonlinear three dimensional, timedependent, fluid simulations of whistler wave turbulence to investigate theirrole in solar wind plasma. Our simulations find that the dispersive whistlermodes evolve entirely differently in the two regimes. While the dispersivewhistler wave effects are stronger in the large scale regime, they do notinfluence the spectral cascades which are describable by a Kolmogorov-like$k^{-7-3}$ spectrum. By contrast, the small scale turbulent fluctuationsexhibit a Navier-Stokes like evolution where characteristic turbulent eddiesexhibit a typical $k^{-5-3}$ hydrodynamic turbulent spectrum. By virtue ofequipartition between the wave velocity and magnetic fields, we quantify therole of whistler waves in the solar wind plasma fluctuations.



Autor: Dastgeer Shaikh, G. P. Zank

Fuente: https://arxiv.org/







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