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Title: SCALING OF THE ELECTRON DISSIPATION RANGE OF SOLAR WIND TURBULENCE

Electron scale solar wind (SW) turbulence has attracted great interest in recent years. Considerable evidence exists that the turbulence is not fully dissipated near the proton scale, but continues cascading down to electron scales. However, the scaling of the magnetic energy spectra as well as the nature of the plasma modes involved at those small scales are still not fully determined. Here we survey 10 yr of the Cluster STAFF search-coil magnetometer waveforms measured in the SW and perform a statistical study of the magnetic energy spectra in the frequency range [1, 180] Hz. We found that 75% of the analyzed spectra exhibit breakpoints near the electron gyroscale ρ{sub e}, followed by steeper power-law-like spectra. We show that the scaling below the electron breakpoint cannot be determined unambiguously due to instrumental limitations that we discuss in detail. We compare our results to those reported in other studies and discuss their implications for the physical mechanisms involved and for theoretical modeling of energy dissipation in the SW.
Authors:
; ; ; ;  [1] ;  [2] ;  [3]
  1. Laboratoire de Physique des Plasmas, CNRS-Ecole Polytechnique-UPMC, Route de Saclay, F-92120 Palaiseau (France)
  2. School of Electronics and Information, Wuhan University, Wuhan (China)
  3. NASA Goddard Space Flight Center, Code 672, Greenbelt, MD 20771 (United States)
Publication Date:
OSTI Identifier:
22270705
Resource Type:
Journal Article
Resource Relation:
Journal Name: Astrophysical Journal; Journal Volume: 777; Journal Issue: 1; Other Information: Country of input: International Atomic Energy Agency (IAEA)
Country of Publication:
United States
Language:
English
Subject:
79 ASTROPHYSICS, COSMOLOGY AND ASTRONOMY; ASTRONOMY; ASTROPHYSICS; COMPARATIVE EVALUATIONS; COSMIC ELECTRONS; ENERGY LOSSES; ENERGY SPECTRA; MAGNETOMETERS; PLASMA; SOLAR ELECTRONS; SOLAR PROTONS; SOLAR WIND; TURBULENCE; WAVE FORMS