In magnetically dominated relativistic collisionless plasmas, Alfvén and slow modes follow anisotropic Goldreich-Sridhar scaling, fast modes are isotropic with larger kinetic energy fraction, and dynamic alignment weakens near kinetic scales due to thermal fluctuations.
R., Federrath C., Klessen R
7 Pith papers cite this work. Polarity classification is still indexing.
7
Pith papers citing it
citation-role summary
background 1
method 1
citation-polarity summary
verdicts
UNVERDICTED 7representative citing papers
Ensemble simulations find linear magnetic energy growth (p_nl=1) in subsonic small-scale dynamos and quadratic growth (p_nl=2) in supersonic ones, with universal conversion efficiency ~1/100 of turbulent kinetic energy flux and nonlinear phase duration ~20 t0.
An a posteriori framework implemented in PyMHD estimates numerical dissipation in Alfvénic, dynamo, and MRI-driven MHD turbulence, showing it has distinct spectral and anisotropic properties from physical dissipation.
The thin-screen approximation for pulsar scintillation arcs has key limitations; 3D volume propagation produces variable curvature and features linked to branched flow from correlated weak scatterings.
Derives and validates via PIC simulations a scaling law for nonthermal spectral tails in mildly to strongly magnetized turbulent plasmas, with application to black-hole coronae.
A review summarizing pitfalls in older CR-MHD models and progress toward more rigorous treatments that connect microphysical CR scales to galactic dynamics.
Review summarizing observational data on the Milky Way's magnetic field structure, including spiral alignment, halo components, turbulence, and correlations with interstellar gas and dust.
citing papers explorer
-
Turbulence Mode Decomposition and Anisotropy in Magnetically Dominated Collisionless Plasmas
In magnetically dominated relativistic collisionless plasmas, Alfvén and slow modes follow anisotropic Goldreich-Sridhar scaling, fast modes are isotropic with larger kinetic energy fraction, and dynamic alignment weakens near kinetic scales due to thermal fluctuations.
-
The universal growth of magnetic energy during the nonlinear phase of subsonic and supersonic small-scale dynamos
Ensemble simulations find linear magnetic energy growth (p_nl=1) in subsonic small-scale dynamos and quadratic growth (p_nl=2) in supersonic ones, with universal conversion efficiency ~1/100 of turbulent kinetic energy flux and nonlinear phase duration ~20 t0.
-
Characterization of Numerical Dissipation in Simulations of Magnetohydrodynamic Turbulence
An a posteriori framework implemented in PyMHD estimates numerical dissipation in Alfvénic, dynamo, and MRI-driven MHD turbulence, showing it has distinct spectral and anisotropic properties from physical dissipation.
-
Pulsar scintillation arcs formed from branched flow
The thin-screen approximation for pulsar scintillation arcs has key limitations; 3D volume propagation produces variable curvature and features linked to branched flow from correlated weak scatterings.
-
On The Nonthermal Power Laws In Magnetized Turbulent Plasmas
Derives and validates via PIC simulations a scaling law for nonthermal spectral tails in mildly to strongly magnetized turbulent plasmas, with application to black-hole coronae.
-
Cosmic Rays on Galaxy Scales: Progress and Pitfalls for CR-MHD Dynamical Models
A review summarizing pitfalls in older CR-MHD models and progress toward more rigorous treatments that connect microphysical CR scales to galactic dynamics.
-
The magnetic field of the Milky Way: an observational perspective
Review summarizing observational data on the Milky Way's magnetic field structure, including spiral alignment, halo components, turbulence, and correlations with interstellar gas and dust.