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- W33775107 abstract "Clathrate hydrates have unique physical and chemical properties because their crystalline structure contains voids that are filled by gas molecules. Their occurrence in many natural environments on Earth (deep-sea sediments, ice sheets) suggests their potential formation elsewhere in the Solar System where suitable pressure – temperature – gas composition conditions occur. This raises the question of their putative role in the storage and release of volatiles. This chapter first reviews the structure of clathrate hydrates, compares their thermo–physical properties with those of water ice, and addresses their stability and methods for estimating equilibria. Then we discuss their likely occurrence in Solar System objects and focus on the geophysical implications of their presence, from the perspectives of both the internal structure of and thermal transfer in icy Solar System bodies, as well as outgassing processes. A particular emphasis is placed on Titan and Enceladus, respectively the largest and the most geologically active satellites of Saturn, where the dissociation of clathrate hydrates could participate in atmospheric formation (Titan) and plume activity (Enceladus)." @default.
- W33775107 created "2016-06-24" @default.
- W33775107 creator A5074401675 @default.
- W33775107 creator A5083984859 @default.
- W33775107 creator A5089765375 @default.
- W33775107 creator A5091548308 @default.
- W33775107 date "2012-04-28" @default.
- W33775107 modified "2023-10-16" @default.
- W33775107 title "Clathrate Hydrates: Implications for Exchange Processes in the Outer Solar System" @default.
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