Astronomy and Astrophysics – Astronomy
Scientific paper
Aug 1992
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992apj...394..662g&link_type=abstract
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 394, no. 2, Aug. 1, 1992, p. 662-669. Research supported by University of H
Astronomy and Astrophysics
Astronomy
31
Coronal Loops, Magnetohydrodynamic Turbulence, Solar Magnetic Field, Differential Equations, Energy Spectra, Power Spectra, Solar Convection (Astronomy), Turbulence Models, Velocity Distribution
Scientific paper
It is proposed that a stationary spectrum of magnetohydrodynamic turbulence is generated in solar coronal loops by the interweaving of magnetic field lines driven by the turbulent velocity field in the convective region. Starting from the set of incompressible magnetohydrodynamic equations, two ordinary differential equations describing the stationary turbulent energy spectrum and the frequency of direct energy cascade for a given kinetic energy spectrum of the subphotospheric convective motions are derived. An estimate of the typical dissipation length scale, at which magnetic energy efficiently heats the plasma by Joule dissipation is obtained. The impact of recent results of two-dimensional magnetohydrodynamic numerical simulations on the coronal heating problem is also discussed.
Ferro Fontan Constantino
Gomez Daniel O.
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