The Divided Nature of the Quiet Sun: Cool and Warm Loops

The magnetic field is undoubtedly the most important but least constrained quantity in the solar atmosphere. In this work we develop an indirect method to probe coronal magnetic fields through connectivity. Connectivity is a physically meaningful quantity in the corona thanks to anisotropic transport processes of the low-beta plasma. We use these properties to observationally probe the question: what fraction of quiet sun magnetic flux in connected to the corona? We analyze four coordinated datasets: Hinode/SOT and SDO/HMI magnetograms, IRIS 1400A slit jaw images, and SDO/AIA 171A and 193A images. These data allow us to constrain where and when transition region plasma has sympathetic interactions with coronal plasma. We use a combination of correlation and regression analysis to map out where these interactions occur and statistically infer the fractional filling factor of coronal loops. Cool non-coronal loops are believed to a significant contributor to transition region emission measure. We work to quantify that contribution in our analysis.