Testing a Riemannian twisted solar loop model from EUV data and magnetic topology

TL;DR

This paper tests a Riemannian model of twisted solar magnetic flux tubes against EUV observations, confirming the model's consistency with solar physics data and deriving bounds on loop lengths and plasma vorticity.

Contribution

It introduces a Riemannian flux tube model for solar loops, linking magnetic topology with EUV data and providing new estimates for torsion and loop dimensions.

Findings

Magnetic to torsion energy ratio is about 10^9, indicating weak torsion contribution.

Solar loops up to 5000 km in diameter and 220,000 km in height are modeled.

Torsion estimates align with previous observational data.

Abstract

Compact Riemannian solar twisted magnetic flux tube surfaces model are tested against solar extreme ultraviolet (EUV) lines observations, allowing us to compute the diameter and height of solar plasma loops. The relation between magnetic and torsion energies is found for a nonplanar solar twisted (torsioned) loop to be $10^{9}$, which shows that the contribution of torsion energy to the solar loop is extremely weaker than the magnetic energy contribution. In this case solar loops of up $5000 km$ in diameter can be reached. The height of $220.000 km$ is used to obtain an estimate for torsion based on the Riemannian flux tube surface, which yields ${\tau}_{0}=0.9{\times} 10^{-8} m^{-1}$ which coincides with one of the data of $(0.9{\pm}0.4){\times}10^{-8}m^{-1}$ obtained by Lopez-Fuentes et al (2003). This result tells us that the Riemannian flux tube model for plasma solar loops is consistent with experimental results in solar physics. These results are obtained for a homogeneous twisted solar loop. By making use of Moffatt-Ricca theorem for the bounds on torsional energy of unknotted vortex filaments, applied to magnetic topology, one places bounds on the lengths of EUV solar loops. New results as the vorticity of the plasma flow along the tube is also computed in terms of the flux tube twist.