Non-equilibrium calcium ionisation in the solar atmosphere

TL;DR

This study investigates the non-equilibrium ionisation processes of calcium in the solar chromosphere using advanced numerical simulations, revealing that ionisation timescales are short but significant enough to affect spectral line modeling.

Contribution

The paper provides the first detailed analysis of calcium ionisation timescales in the solar chromosphere considering non-equilibrium effects and their dependence on shock dynamics and electron density.

Findings

Ionisation timescales are a few seconds at the top of the photosphere.

Recombination is dominated by radiative processes involving Ca III.

Non-equilibrium effects have negligible impact on Ca II spectral line modeling.

Abstract

Our aim is to determine the dominant processes and timescales for the ionisation equilibrium of calcium under solar chromospheric conditions. The study is based on numerical simulations with the RADYN code, which includes hydrodynamics, radiative transfer, and a detailed non-equilibrium treatment of hydrogen, calcium, and helium. The simulations are characterised by upwards propagating shock waves, which cause strong temperature fluctuations and variations of the ionisation degree of calcium. The passage of a hot shock front leads to a strong net ionisation of Ca II, rapidly followed by net recombination. The relaxation timescale of the Ca ionisation state is found to be of the order of a few seconds at the top of the photosphere and 10 to 30 s in the upper chromosphere. Generally, the timescales are significantly reduced in the wakes of hot shock fronts. The timescales can be reliably determined from a simple analysis of the eigenvalues of the transition rate matrix. The timescales are dominated by the radiative recombination from Ca III into the metastable Ca II energy levels of the 4d 2D term. These transitions depend strongly on the density of free electrons and therefore on the (non-equilibrium) ionisation degree of hydrogen, which is the main electron donor. The ionisation/recombination timescales derived here are too long for the assumption of an instantaneous ionisation equilibrium to be valid and, on the other hand, are not long enough to warrant an assumption of a constant ionisation fraction. Fortunately, the ionisation degree of Ca II remains small in the height range, where the cores of the H, K, and the infrared triplet lines are formed. We conclude that the difference due to a detailed treatment of Ca ionisation has only negligible impact on the modelling of spectral lines of Ca II and the plasma properties under the conditions in the quiet solar chromosphere.