日冕发光对总电离率和太阳莱曼阿尔法辐射变化的敏感性
Sensitivity of the helioglow to variation of the total ionization rate and solar Lyman-alpha emission
AI总结：
本研究通过数值实验分析了日冕发光对星际氢电离率和太阳莱曼阿尔法辐射变化的敏感性，发现两者在响应延迟和相关性上表现不同，为IMAP任务反演太阳风纬度结构提供了理论依据。
摘要：
对太阳风的直接观测大多局限于黄道面附近。基于星际中性氢后向散射发光的观测间接反演太阳风的纬度结构十分复杂，需要理论模型的支持。计划在IMAP任务中运行的GLOWS仪器，将以约75度的角距离沿日心环扫描日冕发光。其目标是反演星际氢电离率的纬度结构，并借此获取太阳风的结构。为未来的分析做准备，我们研究了光曲线对星际氢电离率以及太阳莱曼阿尔法照明的随时间和纬度变化的敏感性。基于精心设计的数值实验，我们分析了系统对电离率和太阳照明在日面纬度及时间上变化的响应延迟和弛豫时间。我们发现，太阳照明的变化会无延迟地反映在日冕发光中，但弛豫时间比变化上升时间更长。相比之下，电离率的变化与日冕发光亮度呈反相关关系，并存在数月的延迟。我们还发现，日冕发光对太阳极区电离率的变化不敏感，因此反演极区的电离率和太阳风需要使用适当的参数函数对电离率剖面进行近似。
英文摘要：
Direct observations of solar wind are mostly limited to the vicinity of the ecliptic plane. Retrieving the latitudinal structure of solar wind indirectly based on observations of the backscatter glow of interstellar neutral hydrogen is complex and requires support from theoretical models. The GLOWS instrument, to operate on the planned IMAP mission, will scan the helioglow along circumsolar rings with an angular distance of ~75 degrees. Its objective is to retrieve the latitudinal structure of the ionization rate of interstellar hydrogen and with this, the structure of the solar wind. In preparation for future analysis, we studied the sensitivity of the light curves to temporal and latitudinal variation of the ionization rate of interstellar hydrogen and the solar Lyman-alpha illumination. Based on carefully planned numerical experiments, we analyze the time delay and relaxation time of the system for variations of the ionization rate and solar illumination in heliolatitude and with time. We found that variations in the solar illumination are reflected in the helioglow without delay, but relaxation takes longer than the variation rise time. By contrast, variations in the ionization rate are anti-correlated with the helioglow brightness with a delay of several months. We also found that the helioglow is not sensitive to variations in the ionization rate at the solar poles, so retrieving the ionization rate and solar wind at the poles requires an approximation of the ionization rate profiles with appropriate parametric functions.
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