The influence of photo-induced processes and charge transfer on carbon and oxygen in the lower solar atmosphere
The influence of photo-induced processes and charge transfer on carbon and oxygen in the lower solar atmosphere
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DOI：
10.1093/mnras/stab514
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发表时间：
2021-02
期刊：
影响因子：
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通讯作者：
R. Dufresne;G. Del Zanna-G.-Del Zanna-146786635;N. Badnell
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文献类型：
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作者：
R. Dufresne;G. Del Zanna-G.-Del Zanna-146786635;N. Badnell
为了预测太阳大气中的线发射，需要根据发射是来自色球层还是日冕而有根本不同的模型。在两个区域之间的某个时刻，两种模拟制度之间必须有变化。最近对太阳过渡区碳和氧谱线的日冕模拟的扩展表明，单电荷和双电荷离子的发射以及类锂离子的发射沿着有所改善。然而，仍然存在差异，特别是对于单电荷离子和互组合线。这项工作的目的是探索额外的原子过程，可以进一步改变离子内的电荷态分布和能级分布，以解决一些差异。为此，包括了由辐射场和原子-离子碰撞引起的激发和电离，沿着电荷转移的复合。建模进行使用的条件，将存在于安静的太阳，这使得原子过程的一部分，在不断变化的日冕建模，独立于动态和瞬态事件发生在等离子体中发挥评估。的分数离子布居的过程中的效果，以及在水平人口所带来的新的激发机制的变化。还显示了低电荷状态的选定谱线的贡献函数，以展示低层大气中谱线发射可能受到新模型影响的程度。
To predict line emission in the solar atmosphere requires models which are fundamentally different depending on whether the emission is from the chromosphere or the corona. At some point between the two regions, there must be a change between the two modelling regimes. Recent extensions to the coronal modelling for carbon and oxygen lines in the solar transition region have shown improvements in the emission of singlyand doubly-charged ions, along with Li-like ions. However, discrepancies still remain, particularly for singly-charged ions and intercombination lines. The aim of this work is to explore additional atomic processes that could further alter the charge state distribution and the level populations within ions, in order to resolve some of the discrepancies. To this end, excitation and ionisation caused by both the radiation field and by atom-ion collisions have been included, along with recombination through charge transfer. The modelling is carried out using conditions which would be present in the quiet Sun, which allows an assessment of the part atomic processes play in changing coronal modelling, separately from dynamic and transient events taking place in the plasma. The effect the processes have on the fractional ion populations are presented, as well as the change 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 could be affected by the new modelling.