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arXiv 2212.06261astro-ph.SRphysics.space-ph
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用IRIS观测2询问太阳耀斑环模型：等离子体特性、能量传输和未来方向

Interrogating Solar Flare Loop Models with IRIS Observations 2: Plasma Properties, Energy Transport, and Future Directions

Graham S. Kerr

备注：
Accepted for publication in Frontiers in Astronomy and Space Sciences (Research Topic: Flare Observations in the IRIS Era: What Have we Learned, and What's Next?
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摘要：

在太阳耀斑期间，大量的磁能被释放出来，并通过太阳的大气层进入日光层。尽管经过一个多世纪的研究，围绕太阳耀斑的许多未解决的问题仍然存在。其中包括太阳等离子体如何对耀斑能量沉积作出反应，以及将能量从日冕释放点通过过渡区和色球层传输的重要物理过程是什么？解决这些问题需要先进的数值模拟和高空间、时间和光谱分辨率观测的配合.耀斑是一种三维现象，三维模拟NLTE耀斑色球层并进行三维模型的参数研究在很大程度上与我们目前的计算能力不符。相反，我们依靠最先进的1D场对准模拟来研究控制耀斑的物理过程。在过去的十年中，来自界面区成像光谱仪（IRIS）的数据提供了至关重要的观测结果，我们可以批判性地询问这些耀斑环模型的预测。在本文中，我讨论了前向模拟耀斑如何帮助我们理解IRIS的观测结果，以及IRIS如何揭示我们的模型在哪里做得很好，我们可能错过了重要的过程，特别关注等离子体特性，能量传输机制和耀斑建模的未来方向。

英文摘要：

During solar flares a tremendous amount of magnetic energy is released and transported through the Sun's atmosphere and out into the heliosphere. Despite over a century of study, many unresolved questions surrounding solar flares are still present. Among those are how does the solar plasma respond to flare energy deposition, and what are the important physical processes that transport that energy from the release site in the corona through the transition region and chromosphere? Attacking these questions requires the concert of advanced numerical simulations and high spatial-, temporal-, and spectral- resolution observations. While flares are 3D phenomenon, simulating the NLTE flaring chromosphere in 3D and performing parameter studies of 3D models is largely outwith our current computational capabilities. We instead rely on state-of-the-art 1D field-aligned simulations to study the physical processes that govern flares. Over the last decade, data from the Interface Region Imaging Spectrograph (IRIS) have provided the crucial observations with which we can critically interrogate the predictions of those flare loop models. Here in Paper 2 of a two-part review of IRIS and flare loop models, I discuss how forward modelling flares can help us understand the observations from IRIS, and how IRIS can reveal where our models do well and where we are likely missing important processes, focussing in particular on the plasma properties, energy transport mechanisms, and future directions of flare modelling.

机构、总结、中文摘要均由AI分析而来，可能存在错误，请以论文正文为准。

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