Compressible Magnetohydrodynamic Turbulence in Interstellar Plasmas

By Y. Lithwick, Peter Goldreich. 2001

306 citations recorded by the source corpus.

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In Astronomy and Astrophysics

Citations in the corpus

Compressible turbulence in galaxy clusters: physics and stochastic particle re-acceleration (2007, background): “Lithwick & Goldreich (2001) conjectured that this scaling of incompressible modes is also true for Alfvén modes and slow modes in the presence of compressibility.”
The 511 keV emission from positron annihilation in the Galaxy (2010, background): “The distortion of the wave packets during the interaction produces anisotropic fluctuations elongated along the mean magnetic field (Lithwick and Goldreich, 2001).”
A Model of Turbulence in Magnetized Plasmas: Implications for the Dissipation Range in the Solar Wind (2007, background): “Later studies have examined the effects of compressibility [Lithwick and Goldreich, 2001; Cho and Lazarian, 2003; Vestuto et al., 2003], imbalanced Elsässer fluxes [Maron and Goldreich, 2001; Cho et al., 2002; Lithwick et al., 2007], and a host of other refinements [Oughton et al., 2004; Oughton…”
ASTROPHYSICAL GYROKINETICS: KINETIC AND FLUID TURBULENT CASCADES IN MAGNETIZED WEAKLY COLLISIONAL PLASMAS (2007, methodology): “√ βi √ me mi (115) (see Lithwick & Goldreich 2001 for a discussion of these conditions in application to the ISM).”
Control of star formation by supersonic turbulence (2000, methodology): “A theory of very weakly compressible turbulence has been derived by using the Mach number M ≪ 1 as a perturbation parameter (Lithwick & Goldreich 2001), but no further progress has been made towards analytic models of strongly compressible magnetohydrodynamic (MHD) turbulence with M ≫ 1.”
Turbulent Structure of a Stratified Supernova-driven Interstellar Medium (2005, background): “Its shape contrasts drastically with its counterpart in a weakly compressible medium, where density fluctuations behave as a tracer field and possess a Kolmogorov spectrum (Lithwick & Goldreich 2001).”
Imbalanced Strong MHD Turbulence (2006, background): “3 A wavepacket can be defined more precisely in terms of correlation lengths perpendicular and parallel to the mean field (Lithwick & Goldreich 2001).”
Cosmic-Ray Scattering and Streaming in Compressible Magnetohydrodynamic Turbulence (2004, background): “Itwasconjectured in Lithwick & Goldreich (2001)thatGS95scaling should beapproxim ately trueforAlfv en and slow m odesin m oderately com pressibleplasm a.Form agnetically dom inated,theso-called low plasm a,CL02 showed thatthecoupling ofAlfv enicand com - pressible m odesisweak and thatthe Alfv enic…”
DENSITY STUDIES OF MHD INTERSTELLAR TURBULENCE: STATISTICAL MOMENTS, CORRELATIONS AND BISPECTRUM (2008, background): “Density structures in turbulence can be associated with the slow and fast modes (see Lithwick & Goldreich 2001; Cho & Lazarian 2003; Beresnyak, Lazarian & Cho 2005).”
NUMERICAL TESTS OF FAST RECONNECTION IN WEAKLY STOCHASTIC MAGNETIC FIELDS (2009, background): “…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 case of weak…”
Cosmic-Ray Propagation: Nonlinear Diffusion Parallel and Perpendicular to Mean Magnetic Field (2007, background): “However, while the turbulence injected on large scales may correspond to GS95 model and its extensions to compressible medium (Lithwick & Goldreich 2001, Cho & Lazarian 2002, 2003), one should not disregard the possibilities of generation of additional perturbations by CR themselves.”
Solar Wind Turbulence and the Role of Ion Instabilities (2013, methodology): “This model has been extended to include the passive mixing of the compressive fluctuations by the Alfvénic turbulence (Goldreich and Sridhar 1995, 1997; Lithwick and Goldreich 2001; Schekochihin et al. 2009).”
Acceleration of primary and secondary particles in galaxy clusters by compressible MHD turbulence: from radio haloes to gamma-rays (2010, background): “While the theory of imbalanced turbulence is being intensively developed (see Lithwick & Goldreich 2001; Beresnyak & Lazarian 2008, 2009, 2010; Chandran 2008, Perez & Boldyrev 2009) we do not expect that the effects of imbalance would dominate in the cluster environments.”
LOCATING THE “MISSING” BARYONS WITH EXTRAGALACTIC DISPERSION MEASURE ESTIMATES (2013, background): “Lithwick & Goldreich (2001) argued that in is set by the eddy scale at which the turnover time equals the proton diffusion time across the eddy or in ∼ 6 × 1013 ( 1 kpc out )1/2 (10−4 cm−3 ρe/β )3/2 cm, (6) where β is the plasma beta parameter (the ratio of thermal to magnetic pressure), which is…”
FAST MAGNETIC RECONNECTION AND SPONTANEOUS STOCHASTICITY (2011, background): “The qualifier “local” is important5, as no universal relations exist if eddies are treated in respect to the global mean magnetic field (LV99, Cho & Vishniac (2000); Maron & Goldreich (2001); Lithwick & Goldreich (2001); Cho et al. (2002)).”
Dissipation of Magnetohydrodynamic Waves on Energetic Particles: Impact on Interstellar Turbulence and Cosmic-Ray Transport (2005, methodology): “Although the formalism has been developed for incompressible MHD turbulence, Lithwick & Goldreich (2001) argued that the compressibility does not essentially alter the results on the Alfven wave spectrum.”