INFRARED [FE II] EMISSION LINES FROM RADIATIVE ATOMIC SHOCKS
INFRARED [FE II] EMISSION LINES FROM RADIATIVE ATOMIC SHOCKS
复制标题
辐射原子激波的红外 [FE II] 发射线
DOI：
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发表时间：
2016
期刊：
影响因子：
--
通讯作者：
Hyun
中科院分区：
文献类型：
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作者：
B. Koo;J. Raymond;Hyun
[Fe II]发射线在红外(IR)中很突出，是辐射原子冲击的重要诊断工具。我们用Raymond(1979)发展的具有更新原子参数的激波程序研究了[Fe II]线的发射特性。我们首先回顾了由激波气体产生的IR[Fe II]发射线的一般特征，并推导出它们随激波速度和环境密度的变化关系。我们汇编了星际激波的现有IR[Fe II]线观测，并将它们与从我们的模型预测的比率进行了比较。样本包括银河系和大麦哲伦星云中的年轻和古老的超新星遗迹以及几个赫比格-哈罗天体。我们发现，IR[Fe II]谱线的比例一般落在我们的激波模型网格上，但一些中IR谱线的比例，如[Fe II]35.35μm=[Fe II]25.99m，[Fe II]5.340μm=[Fe II]25.99μm，和[Fe II]5.340μm=[Fe II]17.94m，明显偏离了我们的模型网格。我们讨论了可能的解释，并得出结论，尽管激波模型和观测中的不确定性肯定存在，但原子速率的不确定性似乎是差异的主要来源。
[Fe II] emission lines are prominent in the infrared (IR) and important as diagnostic tools for radiative atomic shocks. We investigate the emission characteristics of [Fe II] lines using a shock code developed by Raymond (1979) with updated atomic parameters. We rst review general characteristics of the IR [Fe II] emission lines from shocked gas, and derive their uxes as a function of shock speed and ambient density. We have compiled available IR [Fe II] line observations of interstellar shocks and compare them to the ratios predicted from our model. The sample includes both young and old supernova remnants in the Galaxy and the Large Magellanic Cloud and several Herbig-Haro objects. We nd that the observed ratios of the IR [Fe II] lines generally fall on our grid of shock models, but the ratios of some mid-IR lines, e.g., [Fe II] 35.35 μm=[Fe II] 25.99 m, [Fe II] 5.340 μm=[Fe II] 25.99 μm, and [Fe II] 5.340 μm=[Fe II] 17.94 m, are signicantly oset from our model grid. We discuss possible explanations and conclude that while uncertainties in the shock modeling and the observations certainly exist, the uncertainty in atomic rates appears to be the major source of discrepancy.
Fe II 禁线的辐射跃迁率
影响因子：
6.5
作者：
Deb N
通讯作者：
Deb N