A model for the non-universal power-law of the solar wind sub-ion scale magnetic spectrum

Abstract

A phenomenological turbulence model for kinetic Alfvén waves in a magnetizedcollisionless plasma, able to reproduce the non-universalpower-law spectra observed at the sub-ion scales in the solar wind and the terrestrial magnetosphere, is presented.The process of temperature homogenization along distortedmagnetic field lines, induced by Landau damping,affects the turbulencetransfer time and results in a steepening of the sub-ion power-law spectrumof critically-balanced turbulence, whose exponent is sensitive to the ratio between the Alfvén wave period and the nonlinear timescale. Transition from large-scaleweak turbulence to smaller scale strong turbulence is capturedand non local interactions, relevant in the case of steep spectra, are accounted for.

8 pages, 3 figures, 1 table, submitted to ApJL

References in corpus (5)

• Solar wind turbulent spectrum at plasma kinetic scales
• Multiscale nature of the dissipation range in gyrokinetic simulations of Alfvénic turbulence
• Solar wind turbulence from MHD to sub-ion scales: high-resolution hybrid simulations
• The dissipation of solar wind turbulent fluctuations at electron scales
• The signature of evolving turbulence in quiet solar wind as seen by ULYSSES

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