IDENTIFICATION OF KINETIC ALFVÉN WAVE TURBULENCE IN THE SOLAR WIND

By C. Salem, Gregory G. Howes, D. Sundkvist, S. Bale, C. Chaston, C. Chen, Florian Mozer. 2012

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SCALING OF THE ELECTRON DISSIPATION RANGE OF SOLAR WIND TURBULENCE (2013, background): “…one assumes that turbulence below the ion scale is dominated essentially by highly oblique KAWs, as suggested by several SW observations (Bale et al. 2005; Sahraoui et al. 2009, 2010a; Salem et al. 2012; Podesta & Tenbarge 2012; Kiyani et al. 2013; Chen et al. 2013), such a dependence could exist.”
SOLAR WIND TURBULENT SPECTRUM AT PLASMA KINETIC SCALES (2012, background): “2010; Narita and Gary 2010), others suggest KAW turbulence (Bale et al. 2005; Schekochihin et al. 2009; Sahraoui et al. 2010; Salem et al. 2012), or a combination of both types of linear waves (Podesta and Gary 2011).”
ENHANCED MAGNETIC COMPRESSIBILITY AND ISOTROPIC SCALE INVARIANCE AT SUB-ION LARMOR SCALES IN SOLAR WIND TURBULENCE (2010, methodology): “Within the context of subion Larmor scales, there is a growing body of work showing that the fluctuations at these scales share the characteristic of kinetic Alfvén waves (Leamon et al. 1998b, 1999; Bale et al. 2005; Howes et al. 2008; Sahraoui et al. 2009, 2010; Salem et al. 2012).”
Recent progress in astrophysical plasma turbulence from solar wind observations (2016, background): “Electric field spectra have also been reported to flatten at ion scales (Bale et al. 2005; Sahraoui et al. 2009; Salem et al. 2012), and ion velocity and temperature spectra to steepen (Šafránková et al.”