Multi-scale Hall-MHD turbulence in the solar wind
| dc.creator | Galtier, S. | |
| dc.creator | Buchlin, E. | |
| dc.date | 2006-10-25 | |
| dc.date | 2007-02-01 | |
| dc.date.accessioned | 2026-07-07T10:40:38Z | |
| dc.date.available | 2026-07-07T10:40:38Z | |
| dc.description | Solar wind magnetic fluctuation spectra exhibit a significant power law steepening at frequencies f>1Hz. The origin of this multi-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 which 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 a la Kolmogorov, and with the range of power law indices found in the solar wind. | |
| dc.description | 7 pages, 4 figures | |
| dc.identifier | https://arxiv.org/abs/astro-ph/0610759 | |
| dc.identifier | http://arxiv.org/abs/astro-ph/0610759 | |
| dc.identifier | Astrophys.J.656:560-566,2007 | |
| dc.identifier | doi:10.1086/510423 | |
| dc.identifier.uri | http://salesiana.dossiersoluciones.com/handle/123456789/181390 | |
| dc.subject | Astrophysics | |
| dc.title | Multi-scale Hall-MHD turbulence in the solar wind | |
| dc.type | text |