Structure of the Venusian atmosphere from surface up to 100 km
Structure of the Venusian atmosphere from surface up to 100 km
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DOI：
10.1134/s0010952506040095
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发表时间：
2006-07-01
期刊：
影响因子：
0.6
通讯作者：
Maiorov, B. S.
中科院分区：
文献类型：
--
作者：
Zasova, L. V.;Moroz, V. I.;Maiorov, B. S.
本文的目的是总结自1985年VIRA（Venus International Reference Atmosphere）或COSPAR模式发表以来获得的金星大气实验数据。自那时以来出现的最重要的成果如下：织女星航天器以高精度和高高度分辨率测量垂直温度分布;织女星航天器气球进行的测量;麦哲伦、金星-15和金星-16的无线电掩星测量;以及从金星-15获得的红外光谱数据得出的温度分布。与VIRA相比，新的结果是在55至100公里的高度范围内创建一个大气模型，取决于当地时间。该模型在我们的论文中以表格形式呈现。
The goal of this paper is to summarize the experimental data on the atmosphere of Venus obtained after 1985, when the VIRA (Venus International Reference Atmosphere) or COSPAR model was published. Among the most important results that have appeared since then are the following: measurements of the vertical temperature profile by the VEGA spacecraft with high precision and high altitude resolution; measurements made with balloons of the VEGA spacecraft; radio occultation measurements of Magellan, Venera-15, and Venera-16; and temperature profiles derived from the data of infrared spectrometry obtained by Venera-15. The new result as compared to VIRA is the creation of a model of the atmosphere in the altitude range 55 to 100 kin dependent on local time. This model is presented in our paper in tabulated form.