Measurements of pure CO2 absorption at high densities near 2.3 μm
Measurements of pure CO2 absorption at high densities near 2.3 μm
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2.3 μm 附近高密度下的纯 CO2 吸收测量
DOI：
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发表时间：
1991
期刊：
影响因子：
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通讯作者：
C. Bergh
中科院分区：
文献类型：
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作者：
C. Brodbeck;Nguyen Van;J. Bouanich;C. Boulet;A. Jean‐Louis;B. Bézard;C. Bergh
在金星背面约2.3 μm处可以探测到金星深层大气的热发射。对这种辐射的分析需要对远翼附近允许的CO2波段的吸收和碰撞引起的吸收有可靠的了解。我们测量了297.5 K下，在3910-4570 cm−1频率范围内，压力从30到60 bar的纯CO2的吸收系数。在金星夜侧辐射发生的4100-4500 cm−1区间内，其值在1.0到1.6 × 10−7 cm−1 amagat−2之间。实验结果与线对线代码计算的合成光谱的比较表明，洛伦兹线形状严重高估了观测到的吸收，而使用从3800-4000 cm−1区域外推的χ因子不能提供足够的不透明度。
Thermal emission from the deep atmosphere of Venus can be detected on the nightside around 2.3 μm. The analysis of this radiation requires a reliable knowledge of the absorption in the far wings of the nearby allowed CO2 bands and of the absorption due to collision-induced bands. We measured absorption coefficients for pure CO2 at pressures varying from 30 to 60 bars in the frequency range 3910–4570 cm−1 at 297.5 K. Values between 1.0 and 1.6 × 10−7 cm−1 amagat−2 are found in the 4100–4500 cm−1 interval where emission from the Venus nightside occurs. The comparison of experimental results with synthetic spectra calculated from a line by line code demonstrates that the Lorentzian line shape strongly overestimates the observed absorption, whereas the use of a χ factor extrapolated from the 3800–4000 cm−1 region does not provide enough opacity.