2002/01/29 by Mark Hindmarsh, Mattias Christensson, M. Christensson +5
Biochemistry, Genetics and Molecular Biology · Physics and Astronomy · #Astrophysics (astro-ph) #Cosmology and Gravitation Theories #FOS: Physical sciences #Fluid Dynamics (physics.flu-dyn) #Geomagnetism and Paleomagnetism Studies #High Energy Physics - Phenomenology (hep-ph) #Solar and Space Plasma Dynamics #astro-ph #hep-ph #physics.flu-dyn
paper · pdf · doi:10.48550/arxiv.astro-ph/0201466
Talk presented at COSMO-01, Rovaniemi, Finland, August 29 -- September 4, 2001
arxiv created 2002/01/29 · openalex publication_date 2002/01/29 · arxiv updated 2009/11/30 · openalex created_date 2025/10/10 · openalex updated_date 2026/07/28
We have carried out numerical simulations of freely decaying magnetohydrodynamic (MHD) turbulence in three dimensions, which can be applied to the evolution of stochastic magnetic fields in the early Universe. For helical magnetic fields an inverse cascade effect is observed in which magnetic helicity and energy is transfered from smaller scales to larger scales, accompanied by power law growth in the characteristic length scale of the magnetic field. The magnetic field quickly reaches a scaling regime with self-similar evolution, and power law behaviour at high wavenumbers. We also find power law decay in the magnetic and kinematic energies.