Structure of the Venusian Atmosphere from Surface up to 100 km

L. V. Zasova; V. I. Moroz; V. M. Linkin; I. V. Khatuntsev; B. S. Maiorov

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Structure of the Venusian Atmosphere from Surface up to 100 km

机译：从表面到100 km的金星大气结构

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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 Ven-era-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 km dependent on local time. This model is presented in our paper in tabulated form.

机译：本文的目的是总结1985年之后发布的关于金星大气的实验数据，当时VIRA（金星国际参考大气）或COSPAR模型发布了。此后出现的最重要的结果包括：VEGA航天器以高精度和高海拔分辨率测量垂直温度分布；用VEGA航天器的气球进行的测量；麦哲伦，Venera-15和Ven-era-16的无线电掩星测量；和温度曲线是从Venera-15获得的红外光谱数据得出的。与VIRA相比，新结果是根据当地时间创建了55至100 km高度范围内的大气模型。该模型以表格形式呈现在我们的论文中。

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来源
《Cosmic research》 |2006年第4期|p.364-383|共20页
作者
L. V. Zasova; V. I. Moroz; V. M. Linkin; I. V. Khatuntsev; B. S. Maiorov;
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作者单位

Space Research Institute, Russian Academy of Sciences, Profsoyuznaya ul. 84/32, Moscow 117997, Russia;

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原文格式 PDF
正文语种 eng
中图分类航天（宇宙航行）;
关键词
venus;

机译：金星;

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Structure of the Venusian Atmosphere from Surface up to 100 km

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