CO prompt emission as a CO₂ marker in comets and planetary atmospheres

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• 作者：Konstantinos S. Kalogerakis^a ; ^ksk@sri.com ; Constantin Romanescu^a ; ¹ ; Musahid Ahmed^b ; Kevin R. Wilson^b ; Tom G. Slanger^a
• 关键词：Mars ; Atmosphere ; Venus ; Atmosphere ; Spectroscopy ; Photochemistry ; Comets
• 刊名：Icarus
• 出版年：2012
• 期刊代码：90_00191035
• 类别：ph
• 出版时间：July, 2012
• 卷：220
• 期：1
• 页码：205-210
• 文件大小：350 K

摘要

Observations of CO emissions in the visible and near-infrared (NIR) have been rare for comets, and no measurements from orbiters are currently available in the visible for the dayglows of Mars or Venus. Analysis of the ultraviolet CO(a-X) Cameron bands from Mars Express dayglow observations supports the conclusion that these bands have very high rotational temperatures, some thousands of kelvins. The most plausible source for the CO rotational excitation is its generation by CO₂ photodissociation. Recent laboratory measurements investigating the photodissociation of CO₂ in the extreme ultraviolet (EUV) reveal strong emissions in the visible and NIR region by the triplet CO(a鈥? d, e) states, which we take to be a primary source for the UV CO(a-X) Cameron bands. Thus, detection of visible emissions from the triplet CO states in planetary dayglows and comets provides an upper limit to the CO₂ density. The presence of CO high rotational excitation along with the intense visible and NIR band emissions should be considered as a practical way by which planetary dayglow and cometary spectra provide information on the presence of CO₂. Finally, we report on existing observations of cometary atmospheres and estimate the altitude for the emitting layer of the CO triplet states in Mars and Venus.