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• W1493675263 abstract "Introduction: Gas hydrate clathrates are cage-like structures of water molecules surrounding a gas molecule such as carbon dioxide or methane. CO2 clathrate is structure I, indicating 5.75 H2O molecules : 1 CO2. Clathrates have properties similar to water ice, save their exceptional thermal expansivity and conductivity. Hydrates are stable at low temperature, modest pressure conditions making them likely to form in many environments throughout the solar system. Clathrates have been suggested sources of methane in the Martian atmosphere [1,2,3,4], and subsurface water and carbon reservoirs [5]. However, experimental data is needed to better understand reaction mechanisms and constrain the rates of the hydrate formation and dissociation processes. This will lead to predictions of gas fluxes between subsurface aquifers, hydrate reservoirs, and planetary atmospheres within models of carbon reservoirs on Mars and other planets. Methods: A device has been constructed at the University of Oklahoma to measure the rate of clathrate formation and dissociation by monitoring pressure and temperature conditions inside a reactor cooled within a commercial freezer. A small gas reservoir was also cooled within the freezer so that gas entering the reactor chamber is at thermal equilibrium with the ice in the reactor. The amount of gas present throughout the experiment was calculated using the Van der Waal’s equation to account for intermolecular attraction. Pressure and temperature measurements were taken every 15 seconds and recorded in Labview. A container of water, open only at the top was placed inside the reactor chamber and frozen before pressurization, leaving the top of the ice cylinder open and free to react with the gas in the headspace. In this arrangement the gas is reacting with a known surface area of ice, allowing surface area normalized rates to be measured. This geometry will also facilitate future work on diffusion rates during hydrate formation. Parallel experiments below atmospheric pressure were conducted in the Mars environment chamber (Andromeda chamber) at the University of Arkansas. This chamber has been previously described [6], and the results are reported in detail in another abstract [7]. Results: A comparison of rates above and below atmospheric pressure suggest that the rate of dissociation changes significantly with pressure (Table 1). However, the relative humidity of the headspace may also play a role in the hydrate dissociation mechanism. At low-pressure conditions within the Andromeda chamber, the headspace is significantly undersaturated with respect to water vapor, which may lead to sublimation of the hydrate, rather than dissociation and release of only the gas component, as observed at higher pressures." @default.
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• W1493675263 date "2010-03-01" @default.
• W1493675263 modified "2023-09-23" @default.
• W1493675263 title "CO2 Clathrate Dissociation Rates Below the Freezing Point of Water" @default.
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