HR: 0830h
AN: SP41A-04    [Abstracts]
TI: Coronal Heating Through Reduced MHD Turbulence
AU: Rappazzo, F
EM: rappazzo@df.unipi.it
AF: Dipartimento di Fisica, Universit… di Pisa, Largo Bruno Pontecorvo 3, Pisa, PI Italy
AU: * Velli, M
EM: Marco.Velli@jpl.nasa.gov
AF: Jet Propulsion Laboratory, California Inst. of Technology, 4800 Oak Grove Dr., Pasadena, CA 91109 United States
AU: Dahlburg, R
EM: rdahlbur@lcp.nrl.navy.mil
AF: Laboratory for Computational Physics & Fluid Dynamics, NRL, Washington DC 20375, United States
AU: Einaudi, G
EM: einaudi@df.unipi.it
AF: Dipartimento di Fisica, Universit… di Pisa, Largo Bruno Pontecorvo 3, Pisa, PI Italy
AU: Einaudi, G
EM: einaudi@df.unipi.it
AF: partment of Physics and Astronomy, George Mason University, Fairfax, VA 22030, United States
AB: 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.
DE: 7509 Corona
DE: 7835 Magnetic reconnection
DE: 7839 Nonlinear phenomena
DE: 7863 Turbulence
SC: Solar Physics Division - AAS [SP]
MN: 2005 Joint Assembly