Solar wind magnetic fluctuation spectra: Dispersion versus damping

By O. Stawicki, S. Gary, Hui Li. 2001

197 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Molecular Biology

View Paper: https://www.semanticscholar.org/paper/362e70a20a55d4281d05f8c528e4f5ead1ca2092

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Citations in the corpus

Dependence of the Dissipation Range Spectrum of Interplanetary Magnetic Fluctuationson the Rate of Energy Cascade (2006, background): “Stawicki et al. (2001) assert that this results in a spectral form determined by whistler wave propagation beyond the cyclotron resonance (within what we here call the dissipation range).”
Wave turbulence in incompressible Hall magnetohydrodynamics (2006, background): “In addition it is often observed that the high frequency fluctuations of the magnetic field are much smaller than the background magnetic field (see, e.g., Stawicki et al. 2001).”
Coronal Holes and the High-Speed Solar Wind (2002, background): “The situation is slightly better in the in situ interplanetary medium because the fluctuation spectrum can be measured directly (e.g., Leamon et al. 1998, 1999; Stawicki et al. 2001), but even there no self-consistent theoretical picture exists.”
SOLAR WIND TURBULENT SPECTRUM AT PLASMA KINETIC SCALES (2012, background): “…range is usually attributed to the ion dissipation range (Leamon et al. 1998, 1999, 2000; Smith et al. 2012) or to another fluid cascade, which may continue down to electron scales (Biskamp et al. 1996; Stawicki et al. 2001; Li et al. 2001; Galtier & Bhattacharjee 2003; Galtier & Buchlin 2007).”
Solar Wind Turbulence and the Role of Ion Instabilities (2013, background): “2011b), a further small scale turbulent cascade (Biskamp et al. 1996; Ghosh et al. 1996; Stawicki et al. 2001; Li et al. 2001; Galtier 2006; Alexandrova et al. 2007, 2008; Schekochihin et al. 2009; Howes et al. 2011b; Rudakov et al. 2011; Boldyrev and Perez 2012) or a combination of both.”
A Model of Turbulence in Magnetized Plasmas: Implications for the Dissipation Range in the Solar Wind (2007, background): “…[Coleman, 1968; Denskat et al., 1983; Goldstein et al., 1994; Leamon et al., 1998b; Gary , 1999], Landau damping of kinetic Alfvén waves [Leamon et al., 1998a, 1999; Leamon et al., 2000], or the dispersive nature of whistler waves [Stawicki et al., 2001; Krishan and Mahajan, 2004; Galtier , 2006].”
Alfvénic Turbulence in the Extended Solar Corona: Kinetic Effects and Proton Heating (2003, methodology): “We refer to these wavenumber regions below as the MHD and KAW inertial ranges, respectively (see also discussion of the “dispersion range” in interplanetary space by Stawicki et al. 2001).”
Small-Scale Energy Cascade of the Solar Wind Turbulence (2007, background): “Others suggest that after the spectral break another turbulent cascade takes place (Biskamp et al. 1996; Ghosh et al. 1996; Stawicki et al. 2001; Li et al. 2001; Galtier 2006).”
ENHANCED MAGNETIC COMPRESSIBILITY AND ISOTROPIC SCALE INVARIANCE AT SUB-ION LARMOR SCALES IN SOLAR WIND TURBULENCE (2010, background): “…at these scales are dispersive in nature (kinetic Alfvén and Whistler waves), many of the proponents of such theories suggest that what has been dubbed the dissipation range for purely historical reasons, should actually be called the dispersive range (Stawicki et al. 2001; Sahraoui et al. 2012).”
Kinetic Physics of the Solar Corona and Solar Wind (2006, background): “, Stix (1992), Melrose and McPhedran (1991), or Baumjohann and Treumann (1996).”
ASTROPHYSICAL GYROKINETICS: KINETIC AND FLUID TURBULENT CASCADES IN MAGNETIZED WEAKLY COLLISIONAL PLASMAS (2007, background): “8 and § 7.3; cf., e.g., Leamon et al. 1999; Stawicki et al. 2001).”