Solar Atmospheric Magnetic Energy Coupling: Broad Plasma Conditions and Spectrum Regimes

TL;DR

This study analyzes three years of solar observations to understand magnetic energy coupling and plasma heating, revealing efficient energy redistribution across temperature gradients and insights into unresolved low corona emission.

Contribution

It provides new observational evidence linking magnetic energy coupling to plasma heating and diffuse emission in the solar corona, aiding stellar physics understanding.

Findings

Magnetic energy coupling supports radiative flux models.

Efficient energy redistribution occurs across large temperature gradients.

Insights into unresolved low corona emission are provided.

Abstract

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.