The Anisotropy of Electron Magnetohydrodynamic Turbulence

By Jungyeon Cho, A. Lazarian. 2004

135 citations recorded by the source corpus.

We present numerical studies of three-dimensional electron magnetohydrodynamic (EMHD) turbulence. We investigate the cascade timescale and anisotropy of freely decaying, strong EMHD turbulence with zero electron skin depth. The cascade time scales with k-4/3. Our numerical results clearly show scale-dependent anisotropy. We find that the observed anisotropy is consistent with k∥ ∝ k, where k∥ and k⊥ are wavenumbers parallel and perpendicular to (local) mean magnetic field, respectively.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/62f68fdbbb619de4f5e9cdfe3d66a4ed32ccebc0

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

1. C. Chen
2. Gregory G. Howes
3. E. Quataert
4. Gianfranco Brunetti
5. A. Lazarian
6. A. Schekochihin
7. S. Cowley
8. Gregory W. Hammett

In Nuclear and High Energy Physics

1. Gianfranco Brunetti
2. Gregory G. Howes
3. A. Lazarian
4. E. Quataert
5. C. Chen
6. A. Schekochihin
7. S. Cowley
8. William Dorland

Citations in the corpus

• A Model of Turbulence in Magnetized Plasmas: Implications for the Dissipation Range in the Solar Wind (2007, methodology): “…argument (explained in more detail in § 2.1) is the one-dimensional magnetic energy spectrum EB(k⊥) ∝ k−7/3⊥ and a predicted wavenumber anisotropy that scales as k‖ ∝ k1/3⊥ [Biskmap et al., 1999; Cho and Lazarian, 2004; Krishan and Mahajan, 2004; Shaikh and Zank , 2005; Schekochihin et al., 2007].”
• Recent progress in astrophysical plasma turbulence from solar wind observations (2016, background): “When a critical balance between the whistler timescale and nonlinear timescale is assumed, the scale-dependent anisotropy k‖ ∝ k1/3⊥ is obtained (Cho & Lazarian 2004), a stronger anisotropy than for Alfvénic turbulence.”
• Compressible turbulence in galaxy clusters: physics and stochastic particle re-acceleration (2007, background): “The latter process, however, is somewhat more problematic than the Alfvénic mode scattering, as whistler turbulence is even more anisotropic than the Alfvénic one (Cho & Lazarian 2004).”
• Nature of Kinetic Scale Turbulence in the Earth's Magnetosheath (2016, background): “…principle (Goldreich & Sridhar 1995) is assumed, in which the linear and nonlinear terms of the dynamical equations are comparable, dimensional arguments lead to a perpendicular energy spectrum E(k⊥) ∝ k −7/3 ⊥ , along with an anisotropy k‖ ∝ k 1/3 ⊥ (Cho & Lazarian 2004; Schekochihin et al. 2009).”