Heating of Coronal Loops: Weak MHD Turbulence and Scaling Laws.

Details Heating of Coronal Loops: Weak MHD Turbulence and Scaling Laws. Heating of Coronal Loops: Weak MHD Turbulence and Scaling Laws.

May 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007agusmsh23c..07r&link_type=abstract

American Geophysical Union, Spring Meeting 2007, abstract #SH23C-07

Physics

7509 Corona, 7524 Magnetic Fields, 7526 Magnetic Reconnection (2723, 7835), 7549 Ultraviolet Emissions, 7863 Turbulence (4490)

Scientific paper

We have investigated the nonlinear dynamics of the Parker Scenario for coronal heating through Reduced MHD long-time high-resolution simulations. A coronal loop is modeled as an elongated Cartesian box embedded in uniform and strong axial magnetic field, whose footpoints are convected by motions at the top and bottom planes, mimicking the photospere. We unambiguously identify MHD anisotropic turbulence as the physical mechanism responsible for the transport of energy from the large scales, where energy is injected by photosperic motions, to the small scales, where it is dissipated. This allows us to give analytical estimates of the heating rate for coronal loops as a function of the loop parameters, i.e. lengths, Alfvén velocity, forcing intensity. The predicted heating rate is within the lower range of observed active region and quiet-Sun coronal energy losses.

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