Two-dimensional magnetohydrodynamics and turbulent coronal heating
- Departamento de Fisica, Universidad de Buenos Aires, Pabellon I, Ciudad Universitaria, Buenos Aires (1428) (Argentina)
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.
- OSTI ID:
- 21175346
- Journal Information:
- AIP Conference Proceedings, Vol. 414, Issue 1; Conference: Workshop on two-dimensional turbulence in plasmas and fluids, Canberra (Australia), 16 Jun - 11 Jul 1997; Other Information: DOI: 10.1063/1.54430; (c) 1997 American Institute of Physics; Country of input: International Atomic Energy Agency (IAEA); ISSN 0094-243X
- Country of Publication:
- United States
- Language:
- English
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