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SOLAR WIND TURBULENT SPECTRUM AT PLASMA KINETIC SCALES

Abstract : The description of the turbulent spectrum of magnetic fluctuations in the solar wind in the kinetic range of scales is not yet completely established. Here, we perform a statistical study of 100 spectra measured by the STAFF instrument on the Cluster mission, which allows us to resolve turbulent fluctuations from ion scales down to a fraction of electron scales, i.e., from ~102 km to ~300 m. We show that for k ⊥ρ e in [0.03, 3] (which corresponds approximately to the frequency in the spacecraft frame f in [3, 300] Hz), all the observed spectra can be described by a general law E(k ⊥)vpropk –8/3 ⊥exp (– k ⊥ρ e ), where k ⊥ is the wavevector component normal to the background magnetic field and ρ e the electron Larmor radius. This exponential tail found in the solar wind seems compatible with the Landau damping of magnetic fluctuations onto electrons.
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https://hal.archives-ouvertes.fr/hal-01553733
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Submitted on : Monday, July 3, 2017 - 4:50:58 PM
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Olga Alexandrova, C. Lacombe, Anne Mangeney, Roland Grappin, M. Maksimovic. SOLAR WIND TURBULENT SPECTRUM AT PLASMA KINETIC SCALES. The Astrophysical Journal, American Astronomical Society, 2012, 760 (2), pp.121. ⟨10.1088/0004-637X/760/2/121⟩. ⟨hal-01553733⟩

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