| タイトル | D to H ratio and the origin and evolution of Titan's atmosphere |
| 著者（英） | Yung, Y. L.; Kim, S.-J.; Lunine, J. I.; Pinto, J. P. |
| 著者所属（英） | Harvard Univ.|Arizona Univ.|California Inst. of Tech.|NASA Goddard Space Flight Center |
| 発行日 | 1986-01-30 |
| 言語 | eng |
| 内容記述 | Potential causative factors for the unusually large ratio of CH3D to CH4 reported in the stratosphere of Titan (6 x 10 to the -4th) compared to that of Saturn (8.7 x 10 to the -5th) or Jupiter (6.7 x 10 to the -5th) are examined. With uncertainty in the observations and data reduction taken into account, an atmospheric enrichment factor of three or more is calculated for Titan relative to the planets. This enrichment factor is seen to be accounted for by condensation to form tropospheric methane clouds, fractionation occurring over a hypothetical CH4-C2H6 ocean and between the ocean and the clathrate crust beneath, fractionation which occurred during the formation of Titan, and fractionation as a result of the evolution of Titan's atmosphere. It is concluded that the greater part of the observed fractionation is probably derived from the last two of these mechanisms. The mechanisms studied do not account for the observed CH3D/CH4 value of 1.7 x 10 to the -3rd obtained by Kim and Caldwell (1982). |
| NASA分類 | LUNAR AND PLANETARY EXPLORATION |
| レポートNO | 86A26480 |
| 権利 | Copyright |
| URI | https://repository.exst.jaxa.jp/dspace/handle/a-is/386064 |
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