Fig. 3


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Overview of the AWSoM and AWSoM-R physics. They solve XMHD equations with separate ion and electron temperatures. The energy densities of parallel and antiparallel propagating turbulence that are self-consistently coupled to each other and to the plasma are solved together with the XMHD equations. Heat conduction and radiative cooling are also taken into account. The turbulence is powered by the Poynting flux leaving the solar photosphere.

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