HR: 1400h
AN: SH23C-07    [Abstracts]
TI: Heating of Coronal Loops: Weak MHD Turbulence and Scaling Laws.
AU: * Rappazzo, F
EM: rappazzo@jpl.nasa.gov
AF: Jet Propulsion Laboratory, 4800 Oak Grove Drive, Pasadena, CA 91109, United States
AU: Velli, M
EM: mvelli@jpl.nasa.gov
AF: Jet Propulsion Laboratory, 4800 Oak Grove Drive, Pasadena, CA 91109, United States
AU: Einaudi, G
EM: einaudi@df.unipi.it
AF: Dipartimento di Fisica, Università di Pisa, Largo Bruno Pontecorvo 3, Pisa, Italy
AU: Dahlburg, R
EM: rdahlbur@lcp.nrl.navy.mil
AF: Laboratory for Computational Physics and Fluid Dynamics, Naval Research Laboratory, 4555 Overlook Ave., SW, Washington, DC , United States
AB: 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.
DE: 7509 Corona
DE: 7524 Magnetic fields
DE: 7526 Magnetic reconnection (2723, 7835)
DE: 7549 Ultraviolet emissions
DE: 7863 Turbulence (4490)
SC: SPA-Solar and Heliospheric Physics [SH]
MN: 2007 Joint Assembly