A geochemical model of non-ideal solutions in the methane–ethane–propane–nitrogen–acetylene system on Titan

Glein, Christopher R.; Shock, Everett L.

doi:10.1016/j.gca.2013.03.030

Cited by 58 publications

(45 citation statements)

References 110 publications

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“…Nitrogen tends to decrease the solubility of solids in liquids while ethane and propane tend to increase it. It should be noted that the solubility of hydrocarbons is quite in agreement between our study and others (Raulin, 1987;Dubouloz et al, 1989;Glein and Shock , 2013) but the solubility of nitriles appears lower in our simulations than in previous ones (Raulin, 1987;Dubouloz et al, 1989;Cordier et al, 2013a), for which they lie between our IST and RST estimates.…”

Section: B2 Solubility Of Titan's Solidssupporting

confidence: 91%

“…Methane, rather than water as on Earth, probably dominates the cycle on Titan and thus constitutes one of the main components of the surface liquid bodies observed in the polar regions (Glein and Shock , 2013;Tan et al, 2013). Ethane, the main photodissociation product of methane (Atreya, 2007), is also implied in Titan's lakes chemistry, as predicted by several thermodynamical models (Lunine et al, 1983;Raulin, 1987;Dubouloz et al, 1989;Cordier et al, 2009;Tan et al, 2013;Cordier et al, 2013a;Glein and Shock , 2013), or as identified in Ontario Lacus thanks to the Cassini/VIMS instrument (Brown et al, 2008).…”

Section: Introductionmentioning

confidence: 99%

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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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Section: B2 Solubility Of Titan's Solidssupporting

confidence: 91%

Section: Introductionmentioning

confidence: 99%

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

et al. 2015

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“…Our laboratory measured values allow a comparison between the properties of karst-forming materials on Earth, and materials on Titan under their respective environmental conditions and subsurface fluids (Glein and Shock, 2013a;Malaska et al, 2011). These values are presented in Fig.…”

Section: Karst On Titanmentioning

confidence: 99%

“…Theoretical estimates of the equilibrium solubilities of many proposed Titan materials in hydrocarbon liquids at 94 K are comparable to common terrestrial karst-forming materials in water at 298 K (Glein and Shock, 2013a;Malaska et al, 2011;Raulin, 1987). However, the solubilities and kinetics of dissolution in hydrocarbon liquids at 94 K have not been measured for many relevant organic materials.…”

Section: Introductionmentioning

confidence: 96%

Dissolution of benzene, naphthalene, and biphenyl in a simulated Titan lake

Malaska

Hodyss

2014

Icarus

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“…C 2 H 2 is highly soluble in Titan's liquid methane and ethane (Glein & Shock 2013;Cordier et al 2015;Singh et al 2015b), intermediate to the solubility of calcite and gypsum in water on Earth's surface. This property implies the existence dynamic surface processes: (1) erosion, through carving of fluvial channels and the formation of karstic lakes at high latitudes on Titan; (2) transport from the surface of continents after a rainstorm by surface runoff; and (3) sedimentation to the bottom of lakes and oceans.…”

Section: Discussionmentioning

confidence: 99%

Acetylene on Titan’s Surface

Singh

McCord

Combe

et al. 2016

ApJ

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Titan's atmosphere is opaque in the near-infrared due to gaseous absorptions, mainly by methane, and scattering by aerosols, except in a few "transparency windows." Thus, the composition of Titan's surface remains difficult to access from space and is still poorly constrained. Photochemical models suggest that most of the organic compounds formed in the atmosphere are heavy enough to condense and build up at the surface in liquid and solid states over geological timescales. Acetylene (C 2 H 2 ) net production in the atmosphere is predicted to be larger than any other compound and C 2 H 2 has been speculated to exist on the surface of Titan. C 2 H 2 was detected as a trace gas sublimated/evaporated from the surface using the Gas Chromatograph Mass Spectrometer after the landing of the Huygens probe. Here we show evidence of C 2 H 2 on the surface of Titan by detecting absorption bands at 1.55 and 4.93 μm using the Cassini Visual and Infrared Mapping Spectrometer at three different equatorial areas-Tui Regio, eastern Shangri La, and Fensal-Aztlan/Quivira. We found that C 2 H 2 is preferentially detected in lowalbedo areas, such as sand dunes and near the Huygens landing site. The specific location of the C 2 H 2 detections suggests that C 2 H 2 is mobilized by surface processes, such as surface weathering by liquids through dissolution/ evaporation processes.

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A geochemical model of non-ideal solutions in the methane–ethane–propane–nitrogen–acetylene system on Titan

Cited by 58 publications

References 110 publications

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

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

Dissolution of benzene, naphthalene, and biphenyl in a simulated Titan lake

Acetylene on Titan’s Surface

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