笼形水合物作为土卫六大气中稀有气体的汇
Clathrate hydrates as a sink of noble gases in Titan's atmosphere
摘要：
我们使用统计热力学方法来确定笼形水合物的组成，这可能是从一个多个化合物的气体，其组成类似于土卫六的大气。假设惰性气体最初存在于这个气相中，我们计算的比例氙，氪和氩的笼形水合物中捕获的物种。我们发现，这些比率计算氙和氪是几个数量级高于共存气体的温度和压力条件接近土卫六目前的大气在地面水平。此外，我们表明，相比之下，氩被困在这些冰。这种捕获机制意味着，气相是逐步耗尽氙和氪时，共存的笼形水合物的形式，而氩的初始丰度几乎保持不变。因此，我们的研究结果与{ \it惠更斯}探测器在2005年1月14日下降时测量到的泰坦大气中氙和氪的不足是一致的。然而，为了解释{ \it Huygens}也揭示的太阳下原始Ar丰度，还必须调用泰坦形成期间或其演化期间发生的其他过程。
英文摘要：
We use a statistical thermodynamic approach to determine the composition of clathrate hydrates which may form from a multiple compound gas whose composition is similar to that of Titan's atmosphere. Assuming that noble gases are initially present in this gas phase, we calculate the ratios of xenon, krypton and argon to species trapped in clathrate hydrates. We find that these ratios calculated for xenon and krypton are several orders of magnitude higher than in the coexisting gas at temperature and pressure conditions close to those of Titan's present atmosphere at ground level. Furthermore we show that, by contrast, argon is poorly trapped in these ices. This trapping mechanism implies that the gas-phase is progressively depleted in xenon and krypton when the coexisting clathrate hydrates form whereas the initial abundance of argon remains almost constant. Our results are thus compatible with the deficiency of Titan's atmosphere in xenon and krypton measured by the {\it Huygens} probe during its descent on January 14, 2005. However, in order to interpret the subsolar abundance of primordial Ar also revealed by {\it Huygens}, other processes that occurred either during the formation of Titan or during its evolution must be also invoked.
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