The observation of chemiluminescent NiO emissions in the laboratory and in the night airglow
The observation of chemiluminescent NiO emissions in the laboratory and in the night airglow
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实验室和夜间气辉化学发光氧化镍发射的观察
DOI：
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发表时间：
2011
期刊：
影响因子：
--
通讯作者：
E. Llewellyn
中科院分区：
文献类型：
--
作者：
W. Evans;R. Gattinger;A. L. Broadfoot;E. Llewellyn
抽象。最近在OSIRIS/Odin光谱中发现的87公里附近的夜间气辉的橙子光谱特征引起了人们对发射起源的兴趣。这一特征被确定为FeO* 发光，其中的铁是来自流星。由于中间层中的陨石来源的原子金属含有铁和镍，镍通常是铁的6%，预计在夜间气辉中也应该存在涉及镍的微弱发射。本研究总结了实验室观测的荧光NiO* 的排放量，并包括一个搜索的NiO* 签名在夜间气辉。一个非常微弱的以前未确定的“连续”扩展长波440纳米已被检测到的夜间气辉光谱与两个空间携带的临边观察仪器。通过与实验室光谱的比较，该连续谱被确定为来自NiO* 发射。还测量了新气辉发射的高度分布。FeO* 和NiO* 排放的高度分布的相似性也表明排放是NiO，因为两者都可以源自金属原子与中间层臭氧的反应。所观察到的NiO* FeO* 的比例表现出相当大的变化，这种观察到的变化的可能原因进行了简要讨论。
Abstract. The recent finding of an orange spectral feature in OSIRIS/Odin spectra of the night airglow near 87 km has raised interest in the origin of the emission. The feature was positively identified as the chemiluminescent FeO* emission where the iron is of meteoric origin. Since the meteorite source of atomic metals in the mesosphere contains both iron and nickel, with Ni being typically 6 % of Fe, it is expected that faint emissions involving Ni should also be present in the night airglow. The present study summarizes the laboratory observations of chemiluminescent NiO* emissions and includes a search for the NiO* signature in the night airglow. A very faint previously unidentified "continuum" extending longwave of 440 nm has been detected in the night airglow spectra obtained with two space-borne limb viewing instruments. Through a comparison with laboratory spectra this continuum is identified as arising from the NiO* emission. The altitude profile of the new airglow emission has also been measured. The similarity of the altitude profiles of the FeO* and NiO* emissions also suggests the emission is NiO as both can originate from reaction of the metal atoms with mesospheric ozone. The observed NiO* to FeO* ratio exhibits considerable variability; possible causes of this observed variation are briefly discussed.
流星烧蚀的化学模型
影响因子：
6.3
作者：
Vondrak T
通讯作者：
Vondrak T