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首页> 美国卫生研究院文献>Springer Open Choice >The Influence of the Solar Coronal Radiation on Coronal Plasma Structures I: Determination of the Incident Coronal Radiation
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The Influence of the Solar Coronal Radiation on Coronal Plasma Structures I: Determination of the Incident Coronal Radiation

机译：太阳日冕辐射对日冕血浆结构的影响I：日冕辐射的确定

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摘要

Coronal structures receive radiation not only from the solar disc, but also from the corona. This height-dependent incident radiation plays a crucial role in the excitation and the ionisation of the illuminated plasma. The aim of this article is to present a method for computing the detailed incident radiation coming from the solar corona, which is perceived at a point located at an arbitrary height. The coronal radiation is calculated by integrating the radiation received at a point in the corona over all of the corona visible from this point. The emission from the corona at all wavelengths of interest is computed using atomic data provided by CHIANTI. We obtain the spectrum illuminating points located at varying heights in the corona at wavelengths between 100 and 912 Å when photons can ionise H or He atoms and ions in their ground states. As expected, individual spectral lines will contribute most at the height within the corona where the local temperature is closest to their formation temperature. As there are many spectral lines produced by many ions, the coronal intensity cannot be assumed to vary in the same way at all wavelengths and so must be calculated for each separate height that is to be considered. This code can be used to compute the spectrum from the corona illuminating a point at any given height above the solar surface. This brings a necessary improvement to models where an accurate determination of the excitation and ionisation states of coronal plasma structures is crucial.
机译：日冕结构不仅接收来自太阳圆盘的辐射，还接收来自日冕的辐射。这种与高度有关的入射辐射在被激发的等离子体的激发和电离中起着至关重要的作用。本文的目的是提出一种计算来自太阳日冕的详细入射辐射的方法，该太阳辐射是在任意高度的一点上感知到的。日冕辐射是通过将在电晕中某个点接收的辐射与从该点可见的所有日冕进行积分而计算得出的。使用CHIANTI提供的原子数据可以计算所有感兴趣波长的日冕的发射。当光子可以将处于基态的H或He原子和离子电离时，我们获得位于日冕中不同高度的光谱照明点，波长在100到912Å之间。不出所料，在局部温度最接近其地层温度的日冕内，各个光谱线将发挥最大作用。由于许多离子产生了许多谱线，因此不能假定冠冕强度在所有波长下都以相同的方式变化，因此必须针对要考虑的每个单独的高度进行计算。该代码可用于从日冕照亮太阳表面上方任意给定高度的点计算光谱。这给模型带来了必要的改进，在这些模型中，精确确定冠状等离子体结构的激发态和电离态至关重要。

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