The Anisotropy of Magnetohydrodynamic Alfvénic Turbulence

By Jungyeon Cho, Ethan Vishniac. 2000

470 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Molecular Biology

View Paper: https://www.semanticscholar.org/paper/e8eba24a97d8d20ab6c7cd5312d48a163a54b6ae

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Citations in the corpus

Modeling the Pan-Spectral Energy Distribution of Starburst Galaxies. I. The Role of ISM Pressure and the Molecular Cloud Dissipation Timescale (2004, background): “In a m agnetized and turbulentinterstellarm edium ,num ericalsim ulations(e.g.Cho & Vishniac (2000b))have shown thatthe localm agnetic eld willstay in equipartition with thegasturbulentenergy; V B = p 4 : (25) Thisprovides the coupling between the gasdensity and the m agnetic eld which isa…”
Simulations of Incompressible Magnetohydrodynamic Turbulence (2000, methodology): “Our simulations differ from those of Cho & Vishniac (2000) in that they are excited anisotropically so that we can study the deep inertial range of MHD turbulence.”
Anisotropy of Alfvénic turbulence in the solar wind and numerical simulations (2010, methodology): “2) and previous simulations (Cho & Vishniac 2000), the contours are elongated in the parallel direction.”
ASTROPHYSICAL GYROKINETICS: KINETIC AND FLUID TURBULENT CASCADES IN MAGNETIZED WEAKLY COLLISIONAL PLASMAS (2007, background): “Numerical simulations of 3D MHD turbulence do not support the possibility of a parallel Alfvén-wave cascade (Shebalin et al. 1983; Oughton et al. 1994; Cho & Vishniac 2000; Maron & Goldreich 2001; Cho et al. 2002; Müller et al. 2003).”
Dissipation of Magnetohydrodynamic Waves on Energetic Particles: Impact on Interstellar Turbulence and Cosmic-Ray Transport (2005, background): “Numerical simulations have confirmed this concept (Cho & Vishniac 2000).”
Spectral Exponents of Kinetic and Magnetic Energy Spectra in Solar Wind Turbulence (2007, background): “…2000;Müller & Biskamp 2000; Haugen et al. 2003, 2004a, 2004b; Haugen & Brandenburg 2004; Alexakis et al. 2005;Mininni et al. 2005;Mininni &Montgomery 2005) and 3/2 (Cho & Vishniac 2000; Maron & Goldreich 2001; Boldyrev et al. 2006;Mason et al. 2006) have been reported in the literature.”
Density Fluctuations in MHD Turbulence: Spectra, Intermittency, and Topology (2006, methodology): “This is an extension of the procedures employed in Cho & Vishniac (2000) and Cho et al. (2002).”
Wave turbulence in incompressible Hall magnetohydrodynamics (2006, background): “…presence of a mean magnetic field plays a fundamental role in the behavior of compressible or incompressible MHD turbulence (Montgomery and Turner 1981; Shebalin et al. 1983; Oughton et al. 1994; Matthaeus et al. 1996; Kinney and McWilliams 1998; Cho and Vishniac 2000; Oughton and Matthaeus 2005).”
Simulations of Magnetohydrodynamic Turbulence in a Strongly Magnetized Medium (2001, methodology): “Diagnostics for our code can be found in Cho and Vishniac (2000b).”
Compressible Magnetohydrodynamic Turbulence in Interstellar Plasmas (2001, unknown): “Those by Cho & Vishniac (2000b) support both equations (1) and (2), and those by & Biskamp (2000) support equationMu ller (1).”
Acceleration of primary and secondary particles in galaxy clusters by compressible MHD turbulence: from radio haloes to gamma-rays (2010, background): “Their inefficiency stems from the both the spectra being steep in terms of parallel perturbations as well as fluctuations being very anisotropic (Goldreich & Sridhar 1995, Lazarian & Vishniac 1999, Cho & Vishniac 2000, Maron & Goldreich 2001, Cho, Lazarian & Vishniac 2002).”
NUMERICAL TESTS OF FAST RECONNECTION IN WEAKLY STOCHASTIC MAGNETIC FIELDS (2009, background): “Reasonable alternatives are expected to have only marginal impact on the nature of field line stochasticity (see also Cho & Vishniac 2000; Maron & Goldreich 2001; Lithwick & Goldreich 2001; Cho et al. 2002; Cho & Lazarian 2002, 2003), provided that the GS95 scalings are generalized to include the…”
The Milky Way’s Kiloparsec-Scale Wind: A Hybrid Cosmic-Ray and Thermally Driven Outflow (2007, background): “…in the turbulent cascade seen in both experiments and theoretical studies of MHD turbulence (see, e.g. Shebalin et al. 1983; Goldreich & Sridhar 1995; Cho & Vishniac 2000; Milano et al. 2001), which has also been invoked in studies of turbulence in supernovae as well (Ptuskin & Zirakashvili 2003).”
Anisotropy in Fast and Slow Solar Wind Fluctuations (2005, background): “Also, note that for the slow wind the anisotropy is more pronounced at smaller scales than at larger scales, something expected from numerical simulation studies and phenomenological arguments (see, e.g., Oughton et al. 1994; Cho & Vishniac 2000; Milano et al. 2001).”
FAST MAGNETIC RECONNECTION AND SPONTANEOUS STOCHASTICITY (2011, methodology): “The importance of the local system of reference was implicit in Kraichnan (1965) but was first discussed within the GS95 model in subsequent publications (LV99, Cho & Vishniac (2000); Maron & Goldreich (2001); Cho et al. (2002); Cho & Lazarian (2002)). al.”
Cosmic-Ray Propagation: Nonlinear Diffusion Parallel and Perpendicular to Mean Magnetic Field (2007, methodology): “Numerical simulations (see Cho & Vishniac 2000, Maron & Goldreich 2001, Müller & Biskamp 2000, Cho, Lazarian & Vishniac 2002, Cho & Lazarian 2002, 2003, see also book of Biskamp 2003, as well as, Cho, Lazarian & Vishniac (2003) and Elmegreen & Scalo 2004 for reviews), however, do not show 2D…”