从模拟到冷等离子体观测：我们能从合成光谱中学到什么
From simulations to observations of cool plasma: What we can learn from synthetic spectra
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中文总结 AI 辅助
研究太阳日冕中冷等离子体，通过应用Promweaver框架从MHD模拟创建合成光谱，与IRIS观测对比，用四分位数分析探索可观测物演变及参数关系，发现模拟与耀斑驱动日冕雨观测匹配良好，还明确了强度与密度等的关联。
中文摘要 AI 辅助
日冕雨、日珥和细丝中的冷等离子体在太阳日冕中普遍存在。我们详细探索了MgII h&k线的合成光谱，并通过将合成光谱与观测光谱进行比较，分析日冕中凝聚的非绝热磁流体动力学（MHD）模拟与观测的匹配程度。我们应用用Python实现的非局部热力学平衡（non-LTE）辐射传输框架Promweaver，从用MPI-AMRVAC创建的二维MHD模拟中创建合成光谱。模拟展示了一个由众多冷的、密集的丝状结构组成的动态系统，我们将其与界面区域成像光谱仪（IRIS）的观测结果进行比较，重点是耀斑驱动的日冕雨。我们从合成光谱的角度对模拟进行了详细描述，展示了特定光谱如何形成以及为何形成。单条细丝就已显示出极大的复杂性。我们还使用四分位数分析系统地探索了观测光谱和合成光谱中可观测物的演变，概述了参数如何随时间变化以及模拟中看到的变化与观测中看到的变化相匹配。结果表明，该模拟在某些方面与耀斑驱动的日冕雨观测结果特别匹配。此外，我们探索了模拟参数与可观测物之间的关系。我们发现强度与密度之间存在显著相关性，但与温度（在所研究的5至20 kK温度范围内）无关。因此，强度与压力之间也存在相关性。这种关系使我们能够进一步将强度与洛伦兹力的垂直分量联系起来。这使我们更接近更好地理解观测光谱与其起源大气之间的联系。
英文摘要
Cool plasma of coronal rain or prominences and filaments is ubiquitous in the solar corona. We explored the synthetic spectra of MgII h&k lines in detail and analyse how well a non-adiabatic magnetohydrodynamic (MHD) simulation of condensations in the corona matches observations when comparing the synthetic with the observed spectra. We applied, a Python implemented, non-local thermodynamic equilibrium (non-LTE) radiative-transfer framework, Promweaver to create synthetic spectra from a 2.5D MHD simulation created with MPI-AMRVAC. The simulation shows a dynamic system of numerous cold, dense thread-like structures that we compare to observations of the $\textit{Interface Region Imaging Spectrograph}$ (IRIS), with a focus on flare-driven coronal rain. We give a detailed description of the simulation from the aspect of the synthetic spectra. We show how and why the particular spectra form. A single thread already demonstrates great complexity. We further used the quartile analysis to systematically explore the evolution of observables in the observed and the synthetic spectra. This gives an overview of how the parameters change in time and that the changes seen in the simulation fit with the changes seen in observations. The results show that the simulation, in some aspects, matches particularly well to the observations of flare-driven coronal rain. Furthermore, we explored relations of parameters of the simulation and the observables. We find significant correlation between intensity and density, but not with temperature (in the studied temperature range of 5 to 20 kK). As a result, there is also a correlation of intensity and pressure. This relation allows us to further relate intensity and the vertical component of the Lorentz force. This brings us a step closer to a better understanding of the connection between the observed spectra and the atmosphere from which it originates.
