Two-dimensional magnetohydrodynamics and turbulent coronal heating

Details Two-dimensional magnetohydrodynamics and turbulent coronal heating Two-dimensional magnetohydrodynamics and turbulent coronal heating

Jun 1997

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997aipc..414..205d&link_type=abstract

The workshop on two-dimensional turbulence in plasmas and fluids. AIP Conference Proceedings, Volume 414, pp. 205-211 (1997).

Computer Science

Plasma Turbulence, Magnetohydrodynamic And Fluid Equation

Scientific paper

We consider the heating of solar coronal active regions within a turbulent scenario. A direct numerical simulation of the equations governing the dynamics of a coronal magnetic loop is performed, assuming that the essential features can be described by an externally driven two-dimensional magnetohydrodynamic system. A stationary and large-scale magnetic forcing was imposed, to model the photospheric motions at the magnetic loop footpoints. A turbulent stationary regime is reached with an energy dissipation rate consistent with the heating requirements of coronal loops. The energy dissipation rate time series shows an intermittent behavior, in the form of impulsive events, superimposed on the stationary component. We associate the impulsive events of magnetic energy dissipation with the so-called nanoflares. A statistical analysis of these events yields a power law distribution as a function of their energies with a slope consistent with those obtained for flare energy distributions reported from X-ray observations. We also show the development of small scales in the spatial distribution of electric currents.

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