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Article overview
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Shear Photospheric Forcing and the Origin of Turbulence in Coronal Loops | | A. F. Rappazzo
; M. Velli
; G. Einaudi
; | | Date: |
19 Mar 2010 | | Abstract: | We present a series of numerical simulations aimed at understanding the
nature and origin of turbulence in coronal loops in the framework of the Parker
model for coronal heating. A coronal loop is studied via reduced
magnetohydrodynamics simulations in Cartesian geometry. A uniform and strong
magnetic field threads the volume between the two photospheric planes, where a
velocity field in the form of a 1D shear flow pattern is present. Initially the
magnetic field which developes in the coronal loop is a simple map of the
photospheric velocity field. This initial configuration is unstable to a
multiple tearing instability which develops islands with X and O points in the
plane orthogonal to the axial field. Once the nonlinear stage sets in the
system evolution is characterized by a regime of MHD turbulence dominated by
magnetic energy. A well developed power law in energy spectra is observed and
the magnetic field never returns to the simple initial state mapping the
photospheric flow. The formation of X and O points in the planes orthogonal to
the axial field allows the continued and repeated formation and dissipation of
small scale current sheets where the plasma is heated. | | Source: | arXiv, 1003.3872 | | Services: | Forum | Review | PDF | Favorites | |
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