The Parker Scenario for Coronal Heating as an MHD Turbulence Problem

Details The Parker Scenario for Coronal Heating as an MHD Turbulence Problem The Parker Scenario for Coronal Heating as an MHD Turbulence Problem

2010-02-12

arxiv.org/abs/1002.2631v1

Proceedings of the NSO Workshop #24 -- Subsurface and Atmospheric Influences on Solar Activity, Eds. R. Howe & R. Komm, ASP Co

Astronomy and Astrophysics

Astrophysics

Solar and Stellar Astrophysics

9 page, 4 figures,

Scientific paper

The Parker or field line tangling model of coronal heating is investigated through long-time high-resolution simulations of the dynamics of a coronal loop in cartesian geometry within the framework of reduced magnetohydrodynamics (RMHD). Slow photospheric motions induce a Poynting flux which saturates by driving an anisotropic turbulent cascade dominated by magnetic energy and characterized by current sheets elongated along the axial magnetic field. Increasing the value of the axial magnetic field different regimes of MHD turbulence develop with a bearing on coronal heating rates. In physical space magnetic field lines at the scale of convection cells appear only slightly bended in agreement with observations of large loops of current (E)UV and X-ray imagers.

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