Modelling low charge ions in the solar atmosphere

Abstract

Extensions have been made recently to the coronal approximation for the purpose of modelling line emission from carbon and oxygen in the lower solar atmosphere. The same modelling is used here for other elements routinely observed in the solar transition region: N, Ne, Mg, Si and S. The modelling includes the effects of higher densities suppressing dielectronic recombination and populating long-lived, metastable levels; the presence of metastable levels typically causes effective ionisation rates to increase and recombination rates to decrease. Processes induced by the radiation field, namely photo-ionisation and photo-excitation, have been included, along with charge transfer, which occurs when electrons are exchanged during atom-ion and ion-ion collisions. The resulting ion balances are shown, and indicate significant changes compared to the frequently-employed coronal approximation. The effect on level populations within ions caused by photo-excitation is also assessed. To give an illustration of how line emission could be altered by these processes, selected line contribution functions are presented at the end.

Accepted in MNRAS, 15 pages, 13 figures

References in corpus (6)

• CHIANTI - an atomic database for emission lines - Paper XV: Version 9, improvements for the X-ray satellite lines
• Radiative recombination data for modelling dynamic finite-density plasmas
• Helium line emissivities in the solar corona
• Modelling ion populations in astrophysical plasmas: carbon in the solar transition region
• Effects of density on the oxygen ionisation equilibrium in collisional plasmas
• The influence of photo-induced processes and charge transfer on carbon and oxygen in the lower solar atmosphere

Cited by in corpus (2)

• The Center-to-Limb Variation of Non-Thermal Velocities using IRIS Si IV
• CHIANTI -- an atomic database for emission lines -- Paper XVIII. Version 11, advanced ionization equilibrium models: density and charge transfer effects