Wave signature in the Venus cloud layer at 58-64 km observed by ground-based dayside infrared spectroscopy
Wave signature in the Venus cloud layer at 58-64 km observed by ground-based dayside infrared spectroscopy
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通过地面日侧红外光谱观测到的 58-64 公里处金星云层中的波特征
DOI：
10.1016/j.icarus.2012.04.027
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发表时间：
2012
期刊：
影响因子：
3.2
通讯作者：
S. Ohtsuki and M. Takagi
中科院分区：
文献类型：
--
作者：
Hosouchi;M.;T. Kouyama;N. Iwagami;S. Ohtsuki and M. Takagi
我们对金星昼面进行了红外光谱测量，通过定量二氧化碳的吸收，找出了云层中58- 64公里处的大气波动结构。这是首次对该高度区域的大气波动进行研究。这一有效吸收高度介于紫外测量的70 km和红外热发射测量的50 km之间。在2007年5月、2007年11月和2010年8月，假设波数为1的结构占主导地位，所发现的类波信号的视旋转周期分别为3.5、4.9和8.4天。这些视周期可以解释为平均纬向流和波（如开尔文波和罗斯比波）的叠加。
We performed infrared spectroscopic measurements of the Venus’ dayside to find out atmospheric wave structures at 58–64km in the cloud layer by quantifying carbon dioxide absorption. This is the first investigation of atmospheric waves at this altitude region. This effective absorption altitude lies in between that of 70km by the ultraviolet measurements and of 50km by the infrared thermal emission measurements. The apparent rotation periods of wave-like signature found are 3.5, 4.9 and 8.4days, respectively, in May 2007, November 2007 and August 2010 assuming dominance of wavenumber one structure. Those apparent periods may be interpreted as superposition of the mean zonal flow and waves such as the Kelvin and the Rossby.