Scaling Laws of Quiet-Sun Coronal Loops

TL;DR

This study investigates the physical parameter relations in quiet-Sun coronal loops using tomography and magnetic field modeling, revealing a density-length scaling law and latitude-dependent temperature variations.

Contribution

It introduces a novel combination of DEMT and PFSS modeling to analyze quiet-Sun loops, providing new scaling laws and insights into temperature distributions.

Findings

Density scales with loop length as N ∼ L^{-0.35}

No significant temperature-length relation found

Equatorial loops tend to be cooler with decreasing temperature along their length

Abstract

We study a series of relations between physical parameters in coronal loops of the quiet Sun reconstructed by combining tomographic techniques and modeling of the coronal magnetic field. We use differential emission measure tomography (DEMT) to determine the three-dimensional distribution of the electron density and temperature in the corona, and we model the magnetic field with a potential-field source-surface (PFSS) extrapolation of a synoptic magnetogram. By tracing the DEMT products along the extrapolated magnetic field lines, we obtain loop-averaged electron density and temperature. Also, loop-integrated energy-related quantities are computed for each closed magnetic field line. We apply the procedure to Carrington rotation 2082, during the activity minimum between Solar Cycles 23 and 24. We find a scaling law between the loop-average density $N$ and loop length $L$, $N_m \sim L^{-0.35}$, but we do not find a significant relation between loop-average temperature and loop length. We confirm though the previously found result that loop-average temperatures at the equatorial latitudes are lower than at higher latitudes. We associate this behavior with the presence at the equatorial latitudes of loops with decreasing temperatures along their length (``down'' loops), which are in general colder than loops with increasing temperatures (``up'' loops). We find that the obtained scalings for quiet-Sun loops do not generally agree with those found in the case of AR loops from previous observational and theoretical studies. We suggest that to better understand the relations found, it is necessary to forward model the reconstructed loops using hydrodynamic codes working under the physical conditions of the quiet-Sun corona.