Models of titan with water-ice shell, rock-ice mantle, and constraints on the rock-iron component composition

Dunaeva, A. N.; Kronrod, V. A.; Kuskov, O. L.

doi:10.1134/s1028334x14010188

Cited by 7 publications

(3 citation statements)

References 10 publications

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“…For models of Titan that include an outer Ice-Ih shell roughly 100 km thick and a subsurface ocean atop an inner high-pressure Ice-V or Ice-VI layer, such as Fortes (2012) and Dunaeva et al (2014), this would correspond to the pressure in the ocean at a depth of roughly 120 km below the Ice-Ih shell. For models of Titan that include an outer Ice-Ih shell roughly 100 km thick and a subsurface ocean atop an inner high-pressure Ice-V or Ice-VI layer, such as Fortes (2012) and Dunaeva et al (2014), this would correspond to the pressure in the ocean at a depth of roughly 120 km below the Ice-Ih shell.…”

Section: Methodsmentioning

confidence: 99%

“…The range of pressures was limited by the maximum pressure able to be maintained with the apparatus, generally about 350 MPa. For models of Titan that include an outer Ice Ih shell roughly 100 km thick and a subsurface ocean atop an inner high-pressure Ice V or Ice VI layer, such as Fortes [2012] and Dunaeva et al [2014], this would correspond to the pressure in the ocean at a depth of roughly 120 km below the Ice Ih shell.…”

Section: Methodsmentioning

confidence: 99%

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The Liquidus Temperature for Methanol‐Water Mixtures at High Pressure and Low Temperature, With Application to Titan

et al. 2018

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Methanol is a potentially important impurity in subsurface oceans on Titan and Enceladus. We report measurements of the freezing of methanol‐water samples at pressures up to 350 MPa using a volumetric cell with sapphire windows. For low concentrations of methanol, the liquidus temperature is typically a few degrees below the corresponding ice freezing point, while at high concentrations it follows the pure methanol trend. In the Ice‐III regime, we observe several long‐lived metastable states. The results suggest that methanol is a more effective antifreeze than previously estimated and might have played an important role in the development of Titan's subsurface ocean.

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Section: Methodsmentioning

confidence: 99%

Section: Methodsmentioning

confidence: 99%

The Liquidus Temperature for Methanol‐Water Mixtures at High Pressure and Low Temperature, With Application to Titan

et al. 2018

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“…Titan's crust is thought to be composed primarily of water-ice (e.g. Dunaeva et al, 2014), and since impact craters expose subsurface material, one would expect impact craters to be more enriched in water-ice than other geologic units. However, an initial survey of impact craters by found a wide range of compositions in the VIMS data set.…”

Section: Introductionmentioning

confidence: 99%

Compositional variations of Titan's impact craters indicates active surface erosion

Werynski

Neish

Gall

et al. 2019

Icarus

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Impact craters on Titan are relatively scarce but provide ample information about the subsurface properties and modification processes present there. This study utilizes impact craters to examine compositional variations across Titan's surface and their subsequent modification. Fifteen craters and their ejecta blankets were studied. Subsurface composition was inferred from emissivity data from Cassini's RADAR instrument, and surficial composition from Cassini's Visible and Infrared Mapping Spectrometer (VIMS). Results show subsurface composition of these craters is controlled by their degradation state and local environment. Older craters are more infilled with organics than younger, and dunes craters show more organic enrichment than plains craters. Surficial composition is only controlled by the local environment (i.e. dunes or plains regions). Since degraded craters show organic rich subsurfaces, but varying surface compositions, it is likely there is an active surface process clearing the surface of sediments and infilling the craters' subsurface fractures.

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Capture of material by the protosatellite disks of Jupiter and Saturn

Kronrod

Makalkin

2019

J. Phys.: Conf. Ser.

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The problem of passing planetesimals through the accretion disks of Jupiter and Saturn and capture of their material into the disks is considered taking into account processes of aerodynamic braking, fragmentation, and ablation of the bodies in the disk’s gas medium. We have obtained limitations on planetesimal sizes at which the body remains in the protosatellite disk. Estimates are made for the mass of material captured into the disk for the case of power-law mass (and size) distribution of planetesimals. The narrower size range for the captured bodies and longer duration of satellite formation could yield the low differentiation of Callisto as compared with Ganymede. Only minor planetesimals with radii less than 12 m could be captured into the disk of Saturn in the formation region of Titan. This feature promoted significant lengthening of the process of Titan formation.

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Models of titan with water-ice shell, rock-ice mantle, and constraints on the rock-iron component composition

Cited by 7 publications

References 10 publications

The Liquidus Temperature for Methanol‐Water Mixtures at High Pressure and Low Temperature, With Application to Titan

The Liquidus Temperature for Methanol‐Water Mixtures at High Pressure and Low Temperature, With Application to Titan

Compositional variations of Titan's impact craters indicates active surface erosion

Capture of material by the protosatellite disks of Jupiter and Saturn

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