Bibcode
Rappazzo, A. F.; Velli, M.; Einaudi, G.
Referencia bibliográfica
The Astrophysical Journal, Volume 722, Issue 1, pp. 65-78 (2010).
Fecha de publicación:
10
2010
Revista
Número de citas
50
Número de citas referidas
48
Descripción
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
magnetohydrodynamic (MHD) 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
one-dimensional shear flow pattern is present. Initially, the magnetic
field that develops in the coronal loop is a simple map of the
photospheric velocity field. This initial configuration is unstable to a
multiple tearing instability that 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. We conclude that the observed
turbulent dynamics are not induced by the complexity of the pattern that
the magnetic field-line footpoints follow but they rather stem from the
inherent nonlinear nature of the system.
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