Weak Magnetohydrodynamic Turbulence and Coronal Heating and Acceleration (Invited)

Details Weak Magnetohydrodynamic Turbulence and Coronal Heating and Acceleration (Invited) Weak Magnetohydrodynamic Turbulence and Coronal Heating and Acceleration (Invited)

Dec 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009agufmsm41c..01v&link_type=abstract

American Geophysical Union, Fall Meeting 2009, abstract #SM41C-01

Physics

[2149] Interplanetary Physics / Mhd Waves And Turbulence, [2723] Magnetospheric Physics / Magnetic Reconnection

Scientific paper

We will describe the characteristic state of the confined coronal magnetic field as a special case of magnetically dominated magnetohydrodynamic turbulence, where the free energy in the transverse magnetic field is continuously cascaded to small scales, even though the overall kinetic energy is small. The coronal turbulence problem is defined by the photospheric boundary conditions, and these play a role in determining the prevalence of local/vs non-local interactions in the turbulent cascade. Simulations for various forcing models and different coronal loop plasma parameters will be presented together with a phenomenological model describing the anomalous turbulence scaling laws found.

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