Scaling properties of three-dimensional isotropic magnetohydrodynamic turbulence

By D. Biskamp, W. Müller. 2000

229 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Molecular Biology

View Paper: https://www.semanticscholar.org/paper/ab3a23f344dec3217b3605fbd6c3fefe58c631a0

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Citations in the corpus

ASTROPHYSICAL GYROKINETICS: KINETIC AND FLUID TURBULENT CASCADES IN MAGNETIZED WEAKLY COLLISIONAL PLASMAS (2007, background): “Indecaying MHD turbulence simulations, the magnetic energy does indeed appear to be at the outer scale (Biskamp & Müller 2000), so one might expect an Alfvénic cascade deep in the inertial range.”
STATISTICAL ANALYSIS OF DISCONTINUITIES IN SOLAR WIND ACE DATA AND COMPARISON WITH INTERMITTENT MHD TURBULENCE (2009, methodology): “Simulations of magnetohydrodynamic (MHD) turbulence (Politano et al. 1998; Biskamp & Muller 2000) and solar wind observations (Burlaga 1991; Marsch & Tu 1994; Horbury et al. 1997; Sorriso-Valvo et al. 1999; Burlaga et al. 2006) each show evidence for intermittency in the form of characteristic…”
A Model of Turbulence in Magnetized Plasmas: Implications for the Dissipation Range in the Solar Wind (2007, background): “…through detailed numerical simulations [Shebalin et al., 1983; Matthaeus et al., 1996, 1998; Cho and Vishniac, 2000; Müller and Biskamp, 2000; Biskamp and Müller , 2000; Maron and Goldreich, 2001; Cho et al., 2002; Cho and Lazarian, 2003; Vestuto et al., 2003; Oughton et al., 2004; Shaikh…”
Control of star formation by supersonic turbulence (2000, methodology): “The scaling properties of the structure functions of such turbulence was derived from the work of She & Leveque (1994) by Müller & Biskamp (2000; also see Biskamp & Müller 2000) by assuming that dissipation occurs in current sheets.”
Interstellar Turbulence I: Observations and Processes (2004, background): “Biskamp & Müller (1999, 2000) show that for incompressible isotropic MHD turbulence the total and kinetic energies vary as t−1 when there is no magnetic helicity but the total energy varies as t−1/2 with the same t−1 kinetic energy decay when helicity is present and nearly conserved.”
Simulations of the Small-Scale Turbulent Dynamo (2003, methodology): “Indeed, the kinetic and magnetic energy spectra that Biskamp & Müller (2000) found in their self-similarly decaying regime were quite different from those for the forced case: while again there was no equipartition, it was the magnetic energy that dominated the kinetic one at large scales (we…”
Statistical theory of magnetohydrodynamic turbulence: recent results (2004, methodology): “Recent book “Magnetohydrodynamic Turbulence” by Biskamp[14] covers most of the basic topics.”
Imbalanced Strong MHD Turbulence (2006, background): “…literature (Iroshnikov 1963; Kraichnan 1965; Shebalin et al. 1983; Goldreich & Sridhar 1995, 1997; Ng & Bhattacharjee 1996; Cho & Vishniac 2000; Biskamp & Müller 2000; Maron & Goldreich 2001; Cho et al. 2002; Galtier et al. 2000, 2002; Müller et al. 2003; Galtier et al. 2005; Boldyrev 2005;…”