Dependence of the Dissipation Range Spectrum of Interplanetary Magnetic Fluctuationson the Rate of Energy Cascade

By Charles W. Smith, Kathleen E. Hamilton, B. Vasquez, R. Leamon. 2006

322 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Molecular Biology

View Paper: https://www.semanticscholar.org/paper/d9005e7e217794c20701cdbad7d5c7255bc74234

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Citations in the corpus

ENHANCED MAGNETIC COMPRESSIBILITY AND ISOTROPIC SCALE INVARIANCE AT SUB-ION LARMOR SCALES IN SOLAR WIND TURBULENCE (2010, background): “This was shown by Hamilton et al. (2008), who repeated the inertial range analysis of Smith et al. (2006b) within the dissipation range and showed that the variance anisotropy followed the empirical power-law relationship δB2⊥/δB 2 ‖ ≡ PSD⊥/PSD‖ ∼ β−0.56p in open field line intervals of the solar…”
SOLAR WIND TURBULENT SPECTRUM AT PLASMA KINETIC SCALES (2012, background): “…degrees of freedom in the vicinity of ion scales is still a matter of debate and is probably at the origin of the spectral variations observed between 0.3 and 3 Hz in the satellite frame: the spectral index here varies between −4 and −2 (Leamon et al. 1998; Smith et al. 2006; Sahraoui et al. 2010).”
Evaluation of the turbulent energy cascade rates from the upper inertial range in the solar wind at 1 AU (2007, methodology): “[32] Hamilton et al. [2005] and Smith et al. [2005, 2006a, 2006b] have constructed a much larger database of one to several hour intervals using the Advanced Composition Explorer (ACE) spacecraft at 1 AU. Smith et al. [2006a, 2006b] evaluated only � Kol but limited the comparison to magnetic field”
ASTROPHYSICAL GYROKINETICS: KINETIC AND FLUID TURBULENT CASCADES IN MAGNETIZED WEAKLY COLLISIONAL PLASMAS (2007, background): “It is certainly a fact that in many solar-wind measurements, the relatively shallow magnetic-energy spectra associated with the KAW cascade (§ 7.5) fail to appear and much steeper spectra are detected (close tok−4; see Leamon et al. 1998; Smith et al. 2006).”
A Model of Turbulence in Magnetized Plasmas: Implications for the Dissipation Range in the Solar Wind (2007, background): “…wind that the above methods have achieved, the mechanisms responsible for the ubiquitous break in the magnetic frequency spectrum between the inertial and dissipation ranges or for the varying spectral index in the dissipation range have still not been unequivocally identified [Smith et al., 2006].”
Solar Wind Turbulence and the Role of Ion Instabilities (2013, background): “Smith et al. (2006) show that within a narrow frequency range [0.4–0.8] Hz, the spectral index α varies between −4 and −2.”
Small-Scale Energy Cascade of the Solar Wind Turbulence (2007, background): “For f > fci the spectrum steepens significantly, but is still described by a power law f s, with s2 (2Y4) (Leamon et al. 1998; Smith et al. 2006).”