Scaling laws of coronal loops compared to a 3D MHD model of an Active Region

TL;DR

This study tests established coronal loop scaling laws against a high-resolution 3D MHD model of the solar corona, revealing their limitations and proposing a new law for heat input that accounts for both hot and cooler structures.

Contribution

We compare existing scaling laws with a realistic 3D MHD model and develop a new scaling law for coronal heating applicable to various loop temperatures.

Findings

Support for hot and EUV-emissive loop scaling laws

Identification of offsets in RTV scaling law for the model data

Proposal of a new scaling law for coronal heat input

Abstract

Context. The structure and heating of coronal loops are investigated since decades. Established scaling laws relate fundamental quantities like the loop apex temperature, pressure, length, and the coronal heating. Aims. We test such scaling laws against a large-scale 3D MHD model of the Solar corona, which became feasible with nowadays high-performance computing. Methods. We drive an active region simulation a with photospheric observations and found strong similarities to the observed coronal loops in X-rays and EUV wavelength. A 3D reconstruction of stereoscopic observations showed that our model loops have a realistic spatial structure. We compare scaling laws to our model data extracted along an ensemble of field lines. Finally, we fit a new scaling law that represents well hot loops and also cooler structures, which was not possible before only based on observations. Results. Our model data gives some support for scaling laws that were established for hot and EUV-emissive coronal loops. For the RTV scaling law we find an offset to our model data, which can be explained by 1D considerations of a static loop with a constant heat input and conduction. With a fit to our model data we set up a new scaling law for the coronal heat input along magnetic field lines. Conclusions. RTV-like scaling laws were fitted to hot loops and therefore do not predict well the coronal heat input for cooler structures that are hardly observable. The basic differences between 1D and self-consistent 3D modeling account for deviations between our and earlier scaling laws. We also conclude that a heating mechanism by MHD-turbulent dissipation within a braided flux tube would heat the corona stronger than consistent with our model corona.