Magnetoturbulent Coronal Heating Hypothesis

How can the solar corona be much hotter than the Sun’s surface? This article explores the question through the magnetoturbulent coronal heating hypothesis, connecting basal magnetic energy input with Alfvén-wave reflection, turbulent dissipation, thermal transport and mass exchange. It focuses on the conditions under which coronal loops can sustain a hot, stable equilibrium. The response framework provides a sufficient condition for linear stability under specified assumptions. An analytical example shows how systems with the same equilibrium and mean heating can nevertheless differ in stability. The article outlines a protocol for independently identifying this response and testing its predictions against numerical models and solar observations. Quantitative reproduction of observed coronal temperatures remains to be established.