The Spatial and Temporal Dependence of Coronal Heating by Alfven Wave Turbulence

Abstract

The solar atmosphere may be heated by Alfven waves that propagate up from the convection zone and dissipate their energy in the chromosphere and corona. To further test this theory, we consider wave heating in an active region observed on 2012 March 7. A potential field model of the region is constructed, and 22 field lines representing observed coronal loops are traced through the model. Using a three-dimensional (3D) reduced magneto-hydrodynamics (MHD) code, we simulate the dynamics of Alfven waves in and near the observed loops. The results for different loops are combined into a single formula describing the average heating rate Q as function of position within the observed active region. We suggest this expression may be approximately valid also for other active regions, and therefore may be used to construct 3D, time-dependent models of the coronal plasma. Such models are needed to understand the role of thermal non-equilibrium in the structuring and dynamics of the Sun's corona.

Accepted for publication in the Astrophysical Journal. 12 pages (emulateapj style), 7 figures, 2 tables. Some figure resolutions were degraded to conform with arXiv file size requirements. The final journal version will also have an animated version of Figure 7 included as online supplementary material

References in corpus (5)

• Self-consistent Coronal Heating and Solar Wind Acceleration from Anisotropic Magnetohydrodynamic Turbulence
• High Resolution Observations and Modeling of Dynamic Fibrils
• Microflares and the Statistics of X-ray Flares
• Dynamics of the solar magnetic bright points derived from their horizontal motions
• A nanoflare model of quiet Sun EUV emission

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