Coronal Heating Through Reduced MHD Turbulence

Details Coronal Heating Through Reduced MHD Turbulence Coronal Heating Through Reduced MHD Turbulence

May 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005agusmsp41a..04r&link_type=abstract

American Geophysical Union, Spring Meeting 2005, abstract #SP41A-04

Physics

7509 Corona, 7835 Magnetic Reconnection, 7839 Nonlinear Phenomena, 7863 Turbulence

Scientific paper

We present 3D reduced-MHD simulations modeling the heating of coronal loops in the solar atmosphere via the tangling of coronal field lines by random photospheric footpoint motions, which we represent as eddies having a finite correlation time. The overall behaviour of the system is sensitive to the intrinsic time-scale present, namely Alfvén propagation time along the loop, dynamical transverse time and photospheric forcing correlation time. The line-tying effect associated with the Alfvén wave propagation along the loop and the reflective photospheric boundary conditions limit the extent of the inverse cascade of magnetic energy when compared to 2D approximations and increases intermittency in both kinetic and magnetic energy absorption and dissipation. The simulations show that the corona self-organizes in response to the forcing in what we conjecture to be a state of minimal dissipation compatible with the driving.

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