  Solar variability investigations that include magnetic energy coupling are
paramount to solving many key solar/stellar physics problems, particularly for
understanding the temporal variability of magnetic energy redistribution and
heating processes. Using three years of observations from the {\it Solar
Dynamics Observatory's} Atmospheric Imaging Assembly and Heliosemic Magnetic
Imager; radiative and magnetic fluxes were measured from gross features and at
full-disk scales, respectively. Magnetic energy coupling analyses support
radiative flux descriptions via a plasma heating connectivity of dominant
(magnetic) and diffuse components, specifically of the predominantly closed
field corona. Our work shows that this relationship favors an energetic
redistribution efficiency across large temperature gradients, and potentially
sheds light on the long withstanding issue of diffuse unresolved low corona
emission. The intimacy of magnetic energy redistribution and plasma conditions
revealed by this work holds significant insight for the field of stellar
physics, as we have provided possible means for probing distant sources in
currently limited and/or undetectable radiation distributions.
