Sébastien Galtier and Eric Buchlin 2007 ApJ 656 560 doi:10.1086/510423
Sébastien Galtier1 and Eric Buchlin2
Show affiliationsThe 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 di, 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.
Issue 1 (2007 February 10)
Received 2006 September 25, accepted for publication 2006 October 25
Sébastien Galtier and Eric Buchlin 2007 ApJ 656 560
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