2006/10/31 by Sébastien Galtier, S. Galtier, E. Buchlin +1 · 5 citations
Biochemistry, Genetics and Molecular Biology · Physics and Astronomy · #Astrophysics #Classical mechanics #Computational physics #Geomagnetism and Paleomagnetism Studies #Geometry #Ionosphere and magnetosphere dynamics #Kinetic energy #Magnetic energy #Magnetic field #Magnetic reconnection #Magnetization #Magnetohydrodynamic drive #Magnetohydrodynamic turbulence #Magnetohydrodynamics #Mechanics #Physics #Power law #Quantum mechanics #Scaling #Solar and Space Plasma Dynamics #Solar wind #Turbulence #astro-ph
paper · pdf · doi:10.1086/510423
published as Astrophys.J.656:560-566,2007 · 7 pages, 4 figures
arxiv created 2007/02/01 · openalex publication_date 2007/02/03 · arxiv updated 2009/12/01 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/05
The spectra of solar wind magnetic fluctuations exhibit a significant power-law steepening at frequencies f > 1 Hz. The origin of this multiple scaling is investigated through dispersive Hall magnetohydrodynamics. We perform three-dimensional numerical simulations in the framework of a highly turbulent shell model and show that the large-scale magnetic fluctuations are characterized by a k -5/3 -type spectrum that steepens at scales smaller than the ion inertial length d i , to k -7/3 if the magnetic energy overtakes the kinetic energy, or to k -11/3 in the opposite case. These results are in agreement both with a heuristic description à la Kolmogorov and with the range of power-law indices found in the solar wind.