Coronal Heating via MHD Turbulence

Details Coronal Heating via MHD Turbulence Coronal Heating via MHD Turbulence

May 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001agusm..sp51c04e&link_type=abstract

American Geophysical Union, Spring Meeting 2001, abstract #SP51C-04 INVITED

Physics

7509 Corona, 7524 Magnetic Fields, 7835 Magnetic Reconnection, 7863 Turbulence

Scientific paper

We present reduced MHD turbulence scenarios for coronal heating in a coronal loop using the 2D cross section approximation (Einaudi and Velli 1999) and the complete boundary value problem 3D simulations. 2D runs are carried out for longer times and greater resolution with different types of forcing, allowing the exploration of the dependence of the heating rates, statistical properties and scalings with the nature of the photospheric forcing. 3D runs are carried out using only some selected photospheric forcings. It is found that line-tying partially inhibits the inverse cascade which dominates the 2D approximation. In 3D the overall behavior of the system is sensitive to the 3 time-scales present in the system, namely propagation time along the loop, dynamical transverse time and photospheric forcing correlation time. Coronal heating scaling laws are reviewed in the light of simulation results

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