将原子数据中的无偏性引入太阳和恒星观测的分析：Fe XIII的个例研究
Incorporating Uncertainties in Atomic Data Into the Analysis of Solar and Stellar Observations: A Case Study in Fe XIII
摘要：
关于天体物理学物体的物理特性的信息不能直接测量，而是通过在原子物理学计算的背景下解释光谱观测来推断。例如，发射谱线的比率可用于推断发射等离子体的电子密度。类似地，在宽的温度范围内形成的发射线的相对强度产生关于温度结构的信息。这种分析的一个关键组成部分是了解基础原子物理学中的不确定性如何传播到推断的等离子体参数中的不确定性。然而，目前，原子物理学数据库不包括原子参数的不确定性，即使它们包括，也没有建立使用它们的方法。在本文中，我们开发了简单的模型的不确定性的碰撞强度和衰变率的Fe XIII和应用它们的密度敏感线的解释与EUV成像光谱仪（EIS）的日出。我们将这些不确定性的贝叶斯框架。我们认为这是一个务实的贝叶斯方法的原子物理学的信息是不受观察到的数据，和一个完全的贝叶斯方法的数据可以用来探测的物理。与仅包含统计不确定性的模型相比，前者通常将推断密度的不确定性增加约5倍。后者减少了推断密度的不确定性，但确定了可能的系统问题与原子物理学或观测强度的领域。
英文摘要：
Information about the physical properties of astrophysical objects cannot be measured directly but is inferred by interpreting spectroscopic observations in the context of atomic physics calculations. Ratios of emission lines, for example, can be used to infer the electron density of the emitting plasma. Similarly, the relative intensities of emission lines formed over a wide range of temperatures yield information on the temperature structure. A critical component of this analysis is understanding how uncertainties in the underlying atomic physics propagates to the uncertainties in the inferred plasma parameters. At present, however, atomic physics databases do not include uncertainties on the atomic parameters and there is no established methodology for using them even if they did. In this paper we develop simple models for the uncertainties in the collision strengths and decay rates for Fe XIII and apply them to the interpretation of density sensitive lines observed with the EUV Imagining spectrometer (EIS) on Hinode. We incorporate these uncertainties in a Bayesian framework. We consider both a pragmatic Bayesian method where the atomic physics information is unaffected by the observed data, and a fully Bayesian method where the data can be used to probe the physics. The former generally increases the uncertainty in the inferred density by about a factor of 5 compared with models that incorporate only statistical uncertainties. The latter reduces the uncertainties on the inferred densities, but identifies areas of possible systematic problems with either the atomic physics or the observed intensities.
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