Magneto-hydrodynamic turbulence (MHD) with a mean large-scale field is known to produce an anisotropic cascade, with energy mostly in perpendicular scales. We use a shell-model version of the Reduced MHD equations to simulate turbulence in homogeneous periodic conditions, in coronal loops, and in the solar wind. We compare the perpendicular and parallel spectra and show that different regimes of weak turbulence develop in loops and in the solar wind. We briefly comment on the way their characteristic large-scale features influence the weak turbulence spectra and their transition to strong turbulence.

Building small scales in MHD turbulence / A. Verdini;R. Grappin;R. Pinto;M. Velli. - In: AIP CONFERENCE PROCEEDINGS. - ISSN 0094-243X. - STAMPA. - 1539:(2013), pp. 74-77. (Intervento presentato al convegno SOLAR WIND 13: Proceedings of the Thirteenth International Solar Wind Conference.) [10.1063/1.4810993].

Building small scales in MHD turbulence

VERDINI, ANDREA;VELLI, MARCO
2013

Abstract

Magneto-hydrodynamic turbulence (MHD) with a mean large-scale field is known to produce an anisotropic cascade, with energy mostly in perpendicular scales. We use a shell-model version of the Reduced MHD equations to simulate turbulence in homogeneous periodic conditions, in coronal loops, and in the solar wind. We compare the perpendicular and parallel spectra and show that different regimes of weak turbulence develop in loops and in the solar wind. We briefly comment on the way their characteristic large-scale features influence the weak turbulence spectra and their transition to strong turbulence.
2013
SOLAR WIND 13: Proceedings of the Thirteenth International Solar Wind Conference.
SOLAR WIND 13: Proceedings of the Thirteenth International Solar Wind Conference.
A. Verdini;R. Grappin;R. Pinto;M. Velli
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Utilizza questo identificatore per citare o creare un link a questa risorsa: https://hdl.handle.net/2158/865912
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