Solar Atmospheric Magnetic Energy Coupling: Broad Plasma Conditions and Temperature Scales

Solar variability investigations that include its magnetic energy coupling are paramount to solving many key solar/stellar physics problems. Particularly 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 coronal hole, quiet Sun, active regions (ARs), AR cores (i.e., inter moss), and at full-disk scales, respectively. Our feature radiative to photospheric magnetic energy coupling analyses supported a temperature dependence. We present mathematical descriptions of magnetic energy coupling across broad temperature gradients, independent of feature for $>$\,10\,G magnetic fluxes. Thus, providing an improved approach for describing magnetic energy redistribution processes of the predominately closed field corona. A general solar atmospheric model is presented that centers on an observationally derived self-similar central engine with possible extension to the cooler atmospheric layers ($\log T$\,$\le$\,6.0) of open field structures. Finally, this work indicates stellar X-ray observations can provide insight to currently limited and/or undetectable radiation distributions, and holds potential for understanding their gross atmospheric feature classes thermodynamic profiles.