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Atmosphere of Titan
The atmosphere of Titan is the layer of gases surrounding Titan. It is the only thick atmosphere of a natural satellite in the Solar System.
==History==
The presence of a significant atmosphere was first suspected by Catalan astronomer Josep Comas i Solà, who observed distinct limb darkening on Titan, a moon of the planet Saturn, in 1903, and confirmed by Gerard P. Kuiper in 1944 using a spectroscopic technique that yielded an estimate of an atmospheric partial pressure of methane of the order of 100 millibars (10 kPa).〔
〕 Subsequent observations in the 1970s showed that Kuiper's figures had been significant underestimates; methane abundances in Titan's atmosphere were ten times higher, and the surface pressure was at least double what he had predicted. The high surface pressure meant that methane could only form a small fraction of Titan's atmosphere.〔Coustenis, pp. 13–15〕 In 1980, ''Voyager 1'' made the first detailed observations of Titan's atmosphere, revealing that its surface pressure was higher than Earth's, at 1.5 bars.〔Coustenis, p. 22〕 On June 23, 2014, NASA claimed to have strong evidence that nitrogen in the atmosphere of Titan came from materials in the Oort cloud, associated with comets, and not from the materials that formed Saturn in earlier times.
抄文引用元・出典: フリー百科事典『 ウィキペディア（Wikipedia）』
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