Thermodynamics of Solid Solubility in Cryogenic Solvents

Preston, G.T.; Prausnitz, J. M.

doi:10.1021/i260034a017

Cited by 53 publications

(29 citation statements)

References 7 publications

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“…The assumed temperature is T = 90 K. The notation x.y(−n) = x.y × 10 −n has been used. One can notice that ideal solubility of CO 2 is comparable to the values reported by Preston and Prausnitz (1970) and Preston et al (1971) for somewhat higher temperatures around 130-140 K. We stress that an identical value of the enrichment ∆ is the consequence of a saturation of solutes that occurs at the very end of the evaporation. Of course, a solvent of a different composition (e.g., a methane rich one) leads strictly to the same result because here we are making the calculations by adopting the ideal solution hypothesis.…”

Section: Evaporites Upper Layer Composition Calculationsupporting

confidence: 74%

On the chemical composition of Titan’s dry lakebed evaporites

Cordier

Barnes

Ferreira

2013

Icarus

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Titan, the main satellite of Saturn, has an active cycle of methane in its troposphere. Among other evidence for a mechanism of evaporation at work on the ground, dry lakebeds have been discovered. Recent Cassini infrared observations of these empty lakes have revealed a surface composition poor in water ice compared to that of the surrounding terrains -suggesting the existence of organic evaporites deposits. The chemical composition of these possible evaporites is unknown. In this paper, we study evaporite composition using a model that treats both organic solids dissolution and solvent evaporation. Our results suggest the possibility of large abundances of butane and acetylene in the lake evaporites. However, due to uncertainties of the employed theory, these determinations have to be confirmed by laboratory experiments.

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Section: Evaporites Upper Layer Composition Calculationsupporting

confidence: 74%

On the chemical composition of Titan’s dry lakebed evaporites

Cordier

Barnes

Ferreira

2013

Icarus

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“…(1) Tan et al (2013); (2) this work, by fitting data from Gabis (1991) provided by Glein & Shock (2013); (3) this work, by fitting data from Neumann & Mann (1969); (4) Gross & Sadowski (2001); (5) this work, by fitting Cheung & Zander (1968) and previously used by Preston & Prausnitz (1970); (6) this work, by fitting data from Diez-y- Riega et al (2014);(X) set to zero, as dissolution data were not found in the literature. (Etters & Kuchta, 1989;Simon, 1980) C 6 H 6 7.384 9.416 6.757 90 (Craven et al, 1993)…”

Section: Namementioning

confidence: 99%

Structure of Titan’s evaporites

Cordier

Cornet

Barnes

et al. 2016

Icarus

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Numerous geological features that could be evaporitic in origin have been identified on the surface of Titan. Although they seem to be water-ice poor, their main properties -chemical composition, thickness, stratification-are essentially unknown. In this paper, which follows on a previous one focusing on the surface composition (Cordier et al., 2013b), we provide some answers to these questions derived from a new model. This model, based on the up-to-date thermodynamic theory known as "PC-SAFT", has been validated with available laboratory measurements and specifically developed for our purpose. 1-D models confirm the possibility of an acetylene and/or butane enriched central layer of evaporitic deposit. The estimated thickness of this acetylene-butane layer could explain the strong RADAR brightness of the evaporites. The 2-D computations indicate an accumulation of poorly soluble species at the deposit's margin. Among these species, HCN or aerosols similar to tholins could play a dominant role. Our model predicts the existence of chemically trimodal "bathtub rings" which is consistent with what it is observed at the south polar lake Ontario Lacus. This work also provides plausible explanations to the lack of evaporites in the south polar region and to the high radar reflectivity of dry lakebeds.

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“…We consider the case of the Ideal Solutions Theory (IST), for which X i,sat is calculated by assuming Γ i = 1 (all the molecules share the same affinity with each other), and the case of the Regular Solutions Theory (RST) of Preston and Prausnitz (1970) for which Γ i = 1 (molecules have preferential affinity with one or the other). The latter approach has already been used in several publications dealing with the lakes and seas composition (Raulin, 1987;Dubouloz et al, 1989;Cordier et al, 2009Cordier et al, , 2013b.…”

Section: B2 Solubility Of Titan's Solidsmentioning

confidence: 99%

“…Preston and Prausnitz (1970) and Szczepaniec-Cieciak et al (1978)), φ 1 is the volume fraction of the liquid, computed as follows:…”

Section: B2 Solubility Of Titan's Solidsmentioning

confidence: 99%

Dissolution on Titan and on Earth: Toward the age of Titan's karstic landscapes

et al. 2015

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Titan's polar surface is dotted with hundreds of lacustrine depressions. Based on the hypothesis that they are karstic in origin, we aim at determining the efficiency of surface dissolution as a landshaping process on Titan, in a comparative planetology perspective with the Earth as reference. Our approach is based on the calculation of solutional denudation rates and allow inference of formation timescales for topographic depressions developed by chemical erosion on both planetary bodies. The model depends on the solubility of solids in liquids, the density of solids and liquids, and the average annual net rainfall rates. We compute and compare the denudation rates of pure solid organics in liquid hydrocarbons and of minerals in liquid water over Titan and Earth timescales. We then investigate the denudation rates of a superficial organic layer in liquid methane over one Titan year. At this timescale, such a layer on Titan would behave like salts or carbonates on Earth depending on its composition, which means that dissolution processes would likely occur, but would be 30 times slower on Titan compared to the Earth due to the seasonality of precipitation. Assuming an average depth of 100 m for Titan's lacustrine depressions, these could have developed in a few tens of millions of years at polar latitudes higher than 70 • N and S, and a few hundreds of million years at lower polar latitudes. The ages determined are consistent with the youth of the surface (< 1 Gyr) and the repartition of dissolution-related landforms on Titan.

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Thermodynamics of Solid Solubility in Cryogenic Solvents

Cited by 53 publications

References 7 publications

On the chemical composition of Titan’s dry lakebed evaporites

On the chemical composition of Titan’s dry lakebed evaporites

Structure of Titan’s evaporites

Dissolution on Titan and on Earth: Toward the age of Titan's karstic landscapes

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