Magnetohydrodynamic Turbulence

By D. Biskamp. 2003

565 citations recorded by the source corpus.

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In Astronomy and Astrophysics

Citations in the corpus

Wave turbulence in incompressible Hall magnetohydrodynamics (2006, background): “Since pure Alfvén waves are exact solutions of the ideal incompressible MHD equations (see, e.g., Pouquet 1993), nonlinear interactions should be suppressed if only one type of wave is present.”
Turbulent Heating of the Solar Wind by Newborn Interstellar Pickup Protons (2006, result): “First, the general scenario of cascade and homogeneous turbulence decay has been found (Hossain et al. 1995; Biskamp 2003) to proceed inMHD in much the same way as in hydrodynamics (Taylor 1935; von Kármán &Howarth 1938).”
Statistical theory of magnetohydrodynamic turbulence: recent results (2004, background): “Pouquet et al. on helical flows. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .333 8.3.3.”
Interstellar Turbulence I: Observations and Processes (2004, methodology): “…of the spectrum or the nature of the low wave number part of the initial spectrum (e.g., Saffman’s invariant, Loitsianskii’s invariant, closures whose results depend on the initial spectrum) give results in this same range (see summaries in Hinze 1975, Lesieur 1990, Frisch 1995, Biskamp 2003).”
Can slow roll inflation induce relevant helical magnetic fields (2010, background): “The inverse cascade is active as long as the Reynolds number of the cosmic fluid at the scale under consideration is larger than one and the fluid is therefore turbulent [57].”
Cascades and transitions in turbulent flows (2018, background): “It is an empirical fact [350, 357] that for B0 = 0 the energies E,E± and the cross helicity Hc cascade forward to the small scales while the magnetic helicity HM cascades inversely to the large scales.”
Astrophysical magnetic fields and nonlinear dynamo theory (2004, background): “Both hydrodynamic and magnetohydrodynamic turbulence are only discussed in their applications, but there are many fundamental aspects that are interesting in their own right; see the text books by Frisch[24] and Biskamp[25] and the work by Goldreich and Sridhar[26]; for a recent review see Ref.”
Evolving turbulence and magnetic fields in galaxy clusters (2005, background): “The decay of the MHD turbulence can be significantly slowed down if the system has non-zero invariants such as magnetic helicity and/or cross-helicity (Biskamp 2003).”
Theory of Star Formation (2007, background): “General references include Frisch (1995), Biskamp (2003), and Falgarone & Passot (2003).”
NUMERICAL TESTS OF FAST RECONNECTION IN WEAKLY STOCHASTIC MAGNETIC FIELDS (2009, background): “Attempt to construct such a model can be traced back to Iroshnikov (1963) and Kraichnan (1965) papers as well as to later fundamental works (e.g. Montgomery & Turner 1981; Shebalin et al. 1983; Higdon 1984, see also book by Biskamp 2003).”
Cosmological Magnetic Fields: Their Generation, Evolution and Observation (2013, background): “This process is extensively studied in various contexts of hydrodynamic and MHD turbulence, both analytically and numerically, see e.g. Biskamp (2003); Tsytovich (1977); Landau and Lifschitz (1990) and more.”