Formation of the helium EUV resonance lines

TL;DR

This study demonstrates that incorporating non-equilibrium ionisation and radiative transfer effects in 3D simulations explains the high observed intensities of helium EUV resonance lines in the quiet Sun, resolving a long-standing discrepancy.

Contribution

The paper introduces a comprehensive 3D MHD model including non-equilibrium ionisation and radiative transfer to accurately reproduce helium EUV line intensities.

Findings

Helium EUV line intensities are an order of magnitude higher with advanced modeling.

He I 584 enhancement is mainly due to He II recombination cascades.

He II 304 and 256 enhancements are primarily caused by non-equilibrium ionisation.

Abstract

Context: While classical models successfully reproduce intensities of many transition region lines, they predict helium EUV line intensities roughly an order of magnitude lower than the observed value. Aims: To determine the relevant formation mechanism(s) of the helium EUV resonance lines, capable of explaining the high intensities under quiet sun conditions. Methods: We synthesise and study the emergent spectra from a 3D radiation-magnetohydrodynamics simulation model. The effects of coronal illumination and non-equilibrium ionisation of hydrogen and helium are included self-consistently in the numerical simulation. Results: Radiative transfer calculations result in helium EUV line intensities that are an order of magnitude larger than the intensities calculated under the classical assumptions. The enhanced intensity of He I 584 is primarily caused by He II recombination cascades. The enhanced intensity of He II 304 and He II 256 is caused primarily by non-equilibrium helium ionisation. Conclusion: The analysis shows that the long standing problem of the high helium EUV line intensities disappears when taking into account optically thick radiative transfer and non-equilibrium ionisation effects.