Radial Dependence of the Frequency Break Between Fluid and Kinetic Scales in the Solar Wind Fluctuations

Abstract

We investigate the radial dependence of the spectral break separating the inertial from the dissipation range in power density spectra of interplanetary magnetic field fluctuations, between $0.42$ and $5.3$ AU, during radial alignments between MESSENGER and WIND for the inner heliosphere and between WIND and ULYSSES for the outer heliosphere. We found that the spectral break moves to higher and higher frequencies as the heliocentric distance decreases. The radial dependence of the corresponding wavenumber is of the kind ${\kappa }_b\sim R^{-1.08}$ in good agreement with that of the wavenumber derived from the linear resonance condition for proton cyclotron damping. These results support conclusions from previous studies which suggest that a cyclotron-resonant dissipation mechanism must participate into the spectral cascade together with other possible kinetic noncyclotron-resonant mechanisms.

8 pages, 3 figures, Accepted on Astrophysical Journal Letters

References in corpus (5)

• Small Scale Energy Cascade of the Solar Wind Turbulence
• Solar wind turbulent spectrum at plasma kinetic scales
• Wave turbulence in incompressible Hall MHD
• Multi-scale Hall-MHD turbulence in the solar wind
• Density Fluctuation Spectrum of Solar Wind Turbulence between Ion and Electron Scales

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