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A dynamic upper atmosphere of Venus as revealed by VIRUS on Venus Express

机译：维纳斯在维纳斯快车上揭示的金星动态高层大气

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摘要

The upper atmosphere of a planet is a transition region in which energy is transferred between the deeper atmosphere and outer space. Molecular emissions from the upper atmosphere (90-120 km altitude) of Venus can be used to investigate the energetics and to trace the circulation of this hitherto little-studied region. Previous spacecraft' and ground-based observations of infrared emission from CO_2, O_2 and NO have established that photochemical and dynamic activity controls the structure of the upper atmosphere of Venus. These data, however, have left unresolved the precise altitude of the emission owing to a lack of data and of an adequate observing geometry. Here we report measurements of day-side CO_2 non-local thermodynamic equilibrium emission at 4.3 urn, extending from 90 to 120 km altitude, and of night-side O_2 emission extending from 95 to 100 km. The CO_2 emission peak occurs at ～115 km and varies with solar zenith angle over a range of ～10km. This confirms previous modelling, and permits the beginning of a systematic study of the variability of the emission. The O_2 peak emission happens at 96 km ± 1 km, which is consistent with three-body recombination of oxygen atoms transported from the day side by a global fhermospheric sub-solar to anti-solar circulation, as previously predicted.
机译：行星的上层大气是过渡区域，在该过渡区域中，能量在深层大气与外层空间之间传递。来自金星的高层大气（海拔90-120 km）的分子发射可用于研究能量学，并追踪迄今研究较少的区域的环流。先前的航天器和地面对CO_2，O_2和NO的红外发射的观测已经确定，光化学和动态活动控制着金星的高层大气的结构。然而，由于缺乏数据和足够的观测几何形状，这些数据尚未确定发射的精确高度。在这里，我们报告了从90到120 km高度延伸的4.3 um的白天侧CO_2非局部热力学平衡排放以及从95到100 km延伸的夜间O_2排放的测量。 CO_2的排放峰值出现在〜115 km处，并随太阳天顶角在〜10 km范围内变化。这证实了先前的建模，并允许开始对排放变化的系统研究。 O_2的峰值发射发生在96 km±1 km处，这与先前由全球大气层次太阳能从天侧传输到反太阳循环的氧原子的三体重组相一致。

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