HR: 1340h
AN: SH13A-1152 [Abstracts]
TI: Dynamics of Forced MHD Turbulence and Coronal Heating
AU: * Rappazzo, A F
EM: rappazzo@df.unipi.it
AF: Dipartimento di Fisica, Universit\`a di Pisa, Via Buonarroti 2, Ed. C, Pisa, 56127
Italy
AU: * Rappazzo, A F
EM: rappazzo@df.unipi.it
AF: Berkeley Research Associates, Inc, P.O. Box 852, Springfield, VA 22150
United States
AU: Dahlburg, R B
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\`a di Pisa, Via Buonarroti 2, Ed. C, Pisa, 56127
Italy
AU: Einaudi, G
EM: einaudi@df.unipi.it
AF: Department of Physics and Astronomy, George Mason University, Fairfax, VA 22030
United States
AU: Velli, M
EM: velli@arcetri.astro.it
AF: Dipartimento di Astronomia e Scienza dello Spazio, Universit\`a di Firenze, Firenze, 50125
Italy
AU: Velli, M
EM: velli@arcetri.astro.it
AF: Jet Propulsion Laboratory, 4800 Oak Grove Drive, Pasadena, CA 91109
United States
AB:
We present 3D MHD simulations modeling the heating of coronal
loops in the solar atmosphere via the tangling of coronal field lines by
photospheric footpoint motions. The overall behaviour of the system is sensitive to the intrinsic time-scale present, namely
Alfv\'en propagation time along the loop, dynamical transverse time and photospheric forcing correlation time. The
line-tying effect associated with the Alfv\'en 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 increase 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: SPA-Solar and Heliospheric Physics [SH]
MN: 2004 AGU Fall Meeting