2009/12/07 by Jean C. Perez, Jean C Perez, Stanislav Boldyrev · 2 citations
Physics and Astronomy · #Ionosphere and magnetosphere dynamics #Solar and Space Plasma Dynamics #Stellar, planetary, and galactic studies #astro-ph.GA #astro-ph.SR
paper · pdf · doi:10.1088/2041-8205/710/1/l63
published as Astrophysical Journal Letters, 710, L63-L66 (2010). · Submitted to ApJL
arxiv created 2009/12/07 · openalex publication_date 2010/01/22 · openalex created_date 2025/10/10 · openalex updated_date 2026/07/31
Magnetohydrodynamics (MHD) is invoked to address turbulent fluctuations in a variety of astrophysical systems. MHD turbulence in nature is often anisotropic and imbalanced, in that Alfvénic fluctuations moving in opposite directions along the background magnetic field carry unequal energies. This work formulates specific requirements for effective numerical simulations of strong imbalanced MHD turbulence with a guide field B 0 . High-resolution simulations are then performed and they suggest that the spectra of the counterpropagating Alfvén modes do not differ from the balanced case, while their amplitudes and the corresponding rates of energy cascades are significantly affected by the imbalance. It is further proposed that the stronger the imbalance the larger the magnetic Reynolds number that is required in numerical simulations in order to correctly reproduce the turbulence spectrum. This may explain current discrepancies among numerical simulations and observations of imbalanced MHD turbulence.