Modeling of hot plasma in the solar active region core

Magnetically confined plasma with temperatures $⩾5MK$ are a feature of hot coronal loops observed in the core of active regions. In this paper, using observations and MHD modeling of coronal loops, we investigate whether wave heating (Alternating Current) models can describe the high temperature loops observed in the active region of 2012 September 7. We construct three-dimensional MHD models for the Alfvén wave turbulence within loops with high temperature. We find that for the Alfvén waves to create enough turbulence to heat the corona, the rms velocity at the footpoints must be 5–6 $km{s}^{-1}$. We conclude that the Alfvén wave turbulence model may be a candidate for explaining how the hot loops are heated, provided the loops have a high velocity at their photospheric footpoints.