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To predict line emission in the solar atmosphere requires models which arefundamentally different depending on whether the emission is from thechromosphere or the corona. At some point between the two regions, there mustbe a change between the two modelling regimes. Recent extensions to the coronalmodelling for carbon and oxygen lines in the solar transition region have shownimprovements in the emission of singly- and doubly-charged ions, along withLi-like ions. However, discrepancies still remain, particularly forsingly-charged ions and intercombination lines. The aim of this work is toexplore additional atomic processes that could further alter the charge statedistribution and the level populations within ions, in order to resolve some ofthe discrepancies. To this end, excitation and ionisation caused by both theradiation field and by atom-ion collisions have been included, along withrecombination through charge transfer. The modelling is carried out usingconditions which would be present in the quiet Sun, which allows an assessmentof the part atomic processes play in changing coronal modelling, separatelyfrom dynamic and transient events taking place in the plasma. The effect theprocesses have on the fractional ion populations are presented, as well as thechange in level populations brought about by the new excitation mechanisms.Contribution functions of selected lines from low charge states are also shown,to demonstrate the extent to which line emission in the lower atmosphere couldbe affected by the new modelling.

The influence of photo-induced processes and charge transfer on carbon and oxygen in the lower solar atmosphere