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

Farnsworth, K.; Soto, Alejandro; Chevrier, V. F.; Steckloff, Jordan K.; Soderblom, Jason M.

doi:10.1021/acsearthspacechem.2c00311

Cited by 3 publications

(1 citation statement)

References 53 publications

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“…For instance, the hypotheses of floating "pumices," made of very porous organic material to ensure buoyancy, has been proposed (Yu et al, 2024). Laboratory experiments have shown (Farnsworth et al, 2023) that non-coalescing liquid droplets may exist at the surface of methane-rich seas after hydrocarbon rainfalls. Interestingly, this phenomenon may appear to be independent of the liquid density.…”

Section: The Case Of Titanmentioning

confidence: 99%

Capillary Processes in Extraterrestrial Contexts

Cordier,

Liger‐Belair,

Bonhommeau

et al. 2024

JGR Planets

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The Earth is no longer the only known celestial body containing one or more liquid phases. The Cassini spacecraft has discovered seas of hydrocarbons at the surface of Titan, while a series of corroborating evidences argue in favor of the existence of an aqueous ocean beneath the icy crust of several moons. Capillarity embraces a family of physical processes occurring at the free surface of a liquid. These phenomena depend on the liquid properties and on the local planetary conditions. Capillarity may have important direct or indirect implications on the geoscientific and astrobiological points of view. In this paper, we discuss capillarity physics among solar system objects and expected consequences for planetary science.

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Section: The Case Of Titanmentioning

confidence: 99%

Capillary Processes in Extraterrestrial Contexts

Cordier,

Liger‐Belair,

Bonhommeau

et al. 2024

JGR Planets

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The Fate of Simple Organics on Titan's Surface: A Theoretical Perspective

Yu,

Garver

et al. 2024

Geophysical Research Letters

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Atmospheric photochemistry on Titan continuously transforms methane and nitrogen gases into various organic compounds. This study explores the fate of these molecules when they land on Titan's surface. Our analytical exploration reveals that most simple organics found in Titan's atmosphere, including all nitriles, triple‐bonded hydrocarbons, and benzene, land as solids. Only a few compounds are in the liquid phase, while only ethylene remains gaseous. For the simple organics that land as solids, we further examine their interactions with Titan's lake liquids. Utilizing principles of buoyancy, we found that flotation can be achieved via porosity‐induced (25%–60% porosity) or capillary force‐induced buoyancy for hydrogen cyanide ices on ethane‐rich lakes. Otherwise, these ices would sink and become lakebed sediments. By evaluating the timescale of flotation, our findings suggest that porosity‐induced flotation of millimeter‐sized and larger sediments is the only plausible mechanism for floating solids to explain the transient “magic islands” phenomena on Titan's lakes.

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Ice Formation, Exsolution, and Multiphase Equilibria in the Methane–Ethane–Nitrogen System at Titan Surface Conditions

Engle,

Hanley,

Tan

et al. 2024

Planet. Sci. J.

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Titan is unique among the icy satellites in that it has a thick atmosphere, stable surficial bodies of liquid, and a precipitation system that promotes interactions between the two. Although Titan’s surface conditions are typically assumed to be above the freezing point temperatures of the major constituent species of the climate system (methane, ethane, and nitrogen), conditions may be sufficiently cool across parts of Titan to allow for ice formation alongside known liquid-vapor phases. In this study, we used Raman spectroscopy, visual inspection, and the CRYOCHEM 2.0 equation of state to map the appearance of first ice and to quantify the amount of nitrogen dissolution into liquid in the methane–ethane–nitrogen system along a 1.5 bar isobaric cooling path in the temperature range 80–95 K. This was with the intent of (1) determining the effects nitrogen has on the phase behaviors of the methane–ethane binary system, and (2) establishing the temperatures and ternary mixing ratios needed for ice formation on Titan’s surface. We found that ethane-rich mixtures enter a three-phase solid–liquid–vapor equilibrium and are characterized by nitrogen-rich exsolution upon freezing and ice that form at the bottom of the sample. With sufficient methane content, the mixtures cross a univariant four-phase solid–liquid–liquid–vapor boundary, which contributes to a distinct isothermal freezing point profile and ice that forms starting at the liquid–liquid interface. Our results generally agree with findings from previous studies of the methane–ethane–nitrogen system and are intended to add to our current understanding of Titan’s geochemical processes.

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

Cited by 3 publications

References 53 publications

Capillary Processes in Extraterrestrial Contexts

Capillary Processes in Extraterrestrial Contexts

The Fate of Simple Organics on Titan's Surface: A Theoretical Perspective

Ice Formation, Exsolution, and Multiphase Equilibria in the Methane–Ethane–Nitrogen System at Titan Surface Conditions

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