A facility for simulating Titan’s environment

Wasiak, F. C.; Luspay‐Kuti, A.; Welivitiya, W. D. D. P.; Roe, L.; Chevrier, V. F.; Blackburn, D. G.; Cornet, T.

doi:10.1016/j.asr.2012.10.020

Cited by 11 publications

(5 citation statements)

References 28 publications

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“…Based on these measurements, we maintain a CH 4 mole fraction of ∼2 × 10 −2 , which is slightly lower than 4.92 × 10 −2 , as measured at the Huygens landing site [ Niemann et al , 2005]. For a detailed description on the chamber see Wasiak et al [2012].…”

Section: Methodsmentioning

confidence: 99%

Experimental simulations of CH₄ evaporation on Titan

Luspay‐Kuti¹,

Chevrier²,

Wasiak³

et al. 2012

Geophysical Research Letters

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.[1] We present the first experimental results on the evaporation of liquid CH 4 under simulated Titan surface conditions similar to those observed at the Huygens landing site. An average evaporation rate of (3.1 AE 0.6) Â 10 À4 kg s À1 m À2 at 94 K and 1.5 bar was measured. While our results are generally higher than previous models based on energy balance, they show an excellent match with a theoretical mass transfer approach. Indeed, we find that evaporation in the Titan environmental chamber is predominantly diffusion driven and affected by the buoyancy of lighter CH 4 in the heavier N 2 atmosphere. After correcting for the difference in gravity of Earth and Titan, the resulting evaporation rate is (1.6 AE 0.3) Â 10 À4 kg s À1 m À2 (or 1.13 AE 0.3 mm hr À1 ). Using our experimental evaporation rates, we determine that the low-latitude storm recently observed by Cassini ISS would have resulted in a maximum evaporated mass of (5.4 AE 1.2) Â 10 10 kg of CH 4 equivalent to a 2.4 AE 0.5 m thick layer over 80 days. Based on our results, a sufficient amount of CH 4 can accumulate in the otherwise arid equatorial regions to produce transient ponds and liquid flows.

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Section: Methodsmentioning

confidence: 99%

Experimental simulations of CH₄ evaporation on Titan

Luspay‐Kuti¹,

Chevrier²,

Wasiak³

et al. 2012

Geophysical Research Letters

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“…Experiments were conducted at the University of Arkansas’ Titan Surface Simulation Chamber (i.e., Andromeda chamber) where liquid methane and ethane samples (10–200 g; CP grade) are studied under Titan-relevant surface temperatures (89–104 K) and a constant atmospheric pressure (1.5 bar nitrogen; N 2 ; purity >99.9%). The environmental chamber consists of an outer sealed and pressurized 2 m tall steel cylinder, that houses the Titan module, and an electronic balance (Figure ).…”

Section: Experimental Methodsmentioning

confidence: 99%

Floating Liquid Droplets on the Surface of Cryogenic Liquids: Implications for Titan Rain

Farnsworth

Soto

Chevrier

et al. 2023

ACS Earth Space Chem.

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Saturn's moon, Titan, has a hydrocarbon-based hydrologic cycle with methane and ethane rainfall. Because of Titan's low gravity, "floating liquid droplets" (coherent droplets of liquid hydrocarbons that float upon a liquid surface) may form on the surface of Titan's hydrocarbon lakes and seas during rainfall. Floating liquid droplets, however, have not been investigated in the laboratory under conditions appropriate for the surface of Titan (cryogenic, hydrocarbon, liquids). We conducted a set of experiments to simulate methane and ethane rainfall under Titan surface conditions (89−94 K, 1.5 bar nitrogen atmosphere) and find that floating ethane droplets form in a wide range of bulk liquid compositions, yet floating methane droplets only form in a narrow compositional range and impact velocity. We find droplet formation is independent of the liquid density and hypothesize that dissolved atmospheric nitrogen in the bulk liquid may repel liquid ethane droplets at the surface. We propose that liquid droplets will form in Titan's methane-rich lakes and seas during ethane rainfall with a droplet radius of ≤3 mm and an impact velocity of ≤0.7 m/s. The presence of these droplets on Titan's lakes may result in a liquid surface layer that is dominated in rainfall composition.

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“…To investigate the nitrogen exsolution process and conditions necessary for nitrogen bubble formation in Titan's lakes, we conducted a series of laboratory experiments in the University of Arkansas' Titan Surface Simulation Chamber (TSSC; Wasiak et al, ). The TSSC allows us to create and study hydrocarbon ponds (10–100 g) at Titan surface conditions (1.5‐bar nitrogen atmosphere, 89–94 K; Fulgichoni et al, ; Jennings et al, ; Cottini et al, ).…”

Section: Methodsmentioning

confidence: 99%

Nitrogen Exsolution and Bubble Formation in Titan's Lakes

Farnsworth

Chevrier

Steckloff

et al. 2019

Geophysical Research Letters

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Titan's surface liquids are composed primarily of methane, ethane, and dissolved atmospheric nitrogen. The nitrogen content depends on the alkane composition and temperature, and exsolves as bubbles when these parameters are sufficiently perturbed. Herein, we present an experimental study of nitrogen bubbles in methane-ethane liquids, and propose that both methane and ethane are required for bubbles to form under Titan conditions. Bubbles occur when methane composes 40-95 mol% of the alkanes within the liquid. We identify two mechanisms that produce bubbles: ethane mediated titration and temperature-induced stratification. Both of these mechanisms produce a metastable nitrogen supersaturation within the liquid; equilibration triggers rapid nitrogen exsolution in the form of bubbles. Such equilibration could cause bubble events in Titan's lakes, possibly explaining the transient "Magic Island" features seen by Cassini RADAR (bubbles within the liquid column), and the presence of deltas in Ontario Lacus.Plain Language Summary Saturn's largest moon, Titan, has stable lakes on its surface composed of liquid methane, ethane, and dissolved atmospheric nitrogen. While nitrogen can dissolve into the liquid (dissolution), it can also be forced out of the liquid (exsolution). Nitrogen bubbles in Titan's lakes have been hypothesized, but not experimentally measured under Titan surface conditions. Here we create bubbles in a laboratory under Titan conditions using two methods: ethane slowly added to methane (titration) and temperature-induced methane-ethane liquid layering (cooling then warming). Both mechanisms create a metastable supersaturation of nitrogen. Once the metastable limit is reached, bubble nucleation occurs, triggering rapid bubble formation. Transient bright structures observed in Titan's lakes by the Cassini RADAR, known as "Magic Islands," may in fact be bubbles within the liquid column. Bubbles can also form in rivers as they flow into lakes and seas, potentially influencing geologic structures, such as the delta seen in one of Titan's largest lakes, Ontario Lacus. Key Points:• Nitrogen bubbles were created in the laboratory under Titan surface conditions • Liquid methane and ethane must be present for bubbles to form (40-95 mol% methane-alkane ratio) • Identified two mechanisms for bubble formation: ethane titration (>86 K) and temperature-induced stratification (<86 K)Supporting Information:• Supporting information S1• Movie S1• Movie S2• Movie S3• Movie S4

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A facility for simulating Titan’s environment

Cited by 11 publications

References 28 publications

Experimental simulations of CH₄ evaporation on Titan

Experimental simulations of CH₄ evaporation on Titan

Floating Liquid Droplets on the Surface of Cryogenic Liquids: Implications for Titan Rain

Nitrogen Exsolution and Bubble Formation in Titan's Lakes

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A facility for simulating Titan’s environment

Cited by 11 publications

References 28 publications

Experimental simulations of CH4 evaporation on Titan

Experimental simulations of CH4 evaporation on Titan

Floating Liquid Droplets on the Surface of Cryogenic Liquids: Implications for Titan Rain

Nitrogen Exsolution and Bubble Formation in Titan's Lakes

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Experimental simulations of CH₄ evaporation on Titan

Experimental simulations of CH₄ evaporation on Titan