SOLAR WIND TURBULENT SPECTRUM AT PLASMA KINETIC SCALES

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 flu...

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Bibliographic Details
Published in:The Astrophysical journal 2012-12, Vol.760 (2), p.1-6
Main Authors: ALEXANDROVA, O, LACOMBE, C, MANCENEY, A, GRAPPIN, R, MAKSIMOVIC, M
Format: Article
Language:English
Subjects:
ASTRONOMY
ASTROPHYSICS
ASTROPHYSICS, COSMOLOGY AND ASTRONOMY
Earth, ocean, space
ENERGY SPECTRA
Exact sciences and technology
Fluctuation
FLUCTUATIONS
Fluid dynamics
IONS
LANDAU DAMPING
LARMOR RADIUS
MAGNETIC FIELDS
Physics
PLASMA
Plasma Physics
SOLAR ELECTRONS
SOLAR WIND
Spacecraft
Spectra
TURBULENCE
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Summary: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 ~10 super(2) km to ~300 m. We show that for k sub([perpendicular])[rho]e [isin] [0.03, 3] (which corresponds approximately to the frequency in the spacecraft frame f [isin] [3, 300] Hz), all the observed spectra can be described by a general law E(k sub([perpendicular])) [is proportional to] k super(-8/3) sub([perpendicular]) exp(-k sub([perpendicular])[rho]e), where k sub([perpendicular]) is the wavevector component normal to the background magnetic field and [rho]e the electron Larmor radius. This exponential tail found in the solar wind seems compatible with the Landau damping of magnetic fluctuations onto electrons.
ISSN:0004-637X
1538-4357
DOI:10.1088/0004-637x/760/2/121