SPECTRUM OF KINETIC-ALFVÉN TURBULENCE

By S. Boldyrev, Jean C. Perez. 2012

157 citations recorded by the source corpus.

A numerical study of strong kinetic-Alfvén turbulence at scales smaller than the ion gyroscale is presented, and a phenomenological model is proposed that argues that magnetic and density fluctuations are concentrated mostly in two-dimensional structures, which leads to their Fourier energy spectra E(k⊥)∝k−8/3⊥, where k⊥ is the wavevector component normal to the strong background magnetic field. The results may provide an explanation for recent observations of magnetic and density fluctuations in the solar wind at sub-proton scales.

Subfields: Astronomy and Astrophysics, Molecular Biology

View Paper: https://www.semanticscholar.org/paper/401303ba2b7520b805e872d145f38d340cfd5e28

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In Astronomy and Astrophysics

1. C. Chen
2. S. Boldyrev
3. O. Alexandrova
4. S. Bale
5. L. Sorriso-Valvo
6. T. Horbury
7. A. Retinò

In Molecular Biology

1. C. Chen
2. T. Horbury
3. S. Bale

Citations in the corpus

• Recent progress in astrophysical plasma turbulence from solar wind observations (2016, background): “…also been observed in simulations that do † This comparison assumes the Taylor hypothesis, which is thought to be valid for kinetic Alfvén turbulence at 1 AU but not whistler turbulence (Howes et al. 2014; Klein et al. 2014). not contain such damping (Boldyrev & Perez 2012; Franci et al. 2015).”
• Solar Wind Turbulence and the Role of Ion Instabilities (2013, background): “The oblique kinetic Alfvén wave (KAW) turbulence is sensitive to the ion gyroradius ρi (Schekochihin et al. 2009; Boldyrev and Perez 2012) and the transition from MHD to Hall MHD occurs at the ion inertial length λi (Galtier 2006; Servidio et al.”
• SCALING OF THE ELECTRON DISSIPATION RANGE OF SOLAR WIND TURBULENCE (2013, result): “These values are close to those predicted by existing theoretical and numerical simulations (Camporeale & Burgess 2011; Chang et al. 2011; Howes et al. 2011b; Boldyrev & Perez 2012) and to the observations reported in Alexandrova et al. (2012).”
• Nature of Kinetic Scale Turbulence in the Earth's Magnetosheath (2016, background): “…Alexandrova et al. 2009; Kiyani et al. 2009; Chen et al. 2010a, 2012; Sahraoui et al. 2013) and kinetic Alfvén turbulence simulations (e.g., Howes et al. 2011; Boldyrev & Perez 2012), and not far from the k −8/3 ⊥ prediction for intermittent kinetic Alfvén turbulence (Boldyrev & Perez 2012).”