Modeling serpentinization: Applied to the early evolution of Enceladus and Mimas

Malamud, Uri; Prialnik, Dina

doi:10.1016/j.icarus.2013.04.024

Cited by 50 publications

(48 citation statements)

References 32 publications

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“…This model is further discussed below. Finally, time‐evolution models developed by Malamud and Prialnik [] and applied to Enceladus, Mimas, and Kuiper belt objects include the rock swelling and heating effects due to serpentinization, the flow of water liquid and vapor, and a detailed treatment of rock and ice porosity by means of equations of state. These models therefore offer an opportunity for comparison with those presented here.…”

Section: Introductionmentioning

confidence: 99%

“…We then explain how this model is incorporated as a cracking subroutine into the thermal evolution code of Desch et al [], along with the inclusion of silicate hydration and dehydration, and hydrothermal circulation in the porous layer. The level of detail in the resulting code is similar to that of Malamud and Prialnik [], albeit with a different approach in the treatment of differentiation, porosity, and hydrothermal heat transfer. We apply the model to Ceres and investigate the influence of fracturing and physical water‐rock processes on its evolution.…”

Section: Introductionmentioning

confidence: 99%

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Core cracking and hydrothermal circulation can profoundly affect Ceres' geophysical evolution

2015

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Observations and models of Ceres suggest that its evolution was shaped by interactions between liquid water and silicate rock. Hydrothermal processes in a heated core require both fractured rock and liquid. Using a new core cracking model coupled to a thermal evolution code, we find volumes of fractured rock always large enough for significant interaction to occur. Therefore, liquid persistence is key. It is favored by antifreezes such as ammonia, by silicate dehydration which releases liquid, and by hydrothermal circulation itself, which enhances heat transport into the hydrosphere. The effect of heating from silicate hydration seems minor. Hydrothermal circulation can profoundly affect Ceres' evolution: it prevents core dehydration via "temperature resets, " core cooling events lasting ∼50 Myr during which Ceres' interior temperature profile becomes very shallow and its hydrosphere is largely liquid. Whether Ceres has experienced such extensive hydrothermalism may be determined through examination of its present-day structure. A large, fully hydrated core (radius 420 km) would suggest that extensive hydrothermal circulation prevented core dehydration. A small, dry core (radius 350 km) suggests early dehydration from short-lived radionuclides, with shallow hydrothermalism at best. Intermediate structures with a partially dehydrated core seem ambiguous, compatible both with late partial dehydration without hydrothermal circulation, and with early dehydration with extensive hydrothermal circulation. Thus, gravity measurements by the Dawn orbiter, whose arrival at Ceres is imminent, could help discriminate between scenarios for Ceres' evolution.

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Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Core cracking and hydrothermal circulation can profoundly affect Ceres' geophysical evolution

2015

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“…Initial studies 7,9 suggested that Notum might act as a phospholipase enzyme, cleaving the link between membranebound glycoproteins called GPI anchors and glypicans -large poly saccharides that form complexes with extra cellular molecules such as Wnt. Cleavage releases glypicans into the extracellular space, decreasing their ability to restrain Wnt activity.…”

Section: Disarming Wntmentioning

confidence: 99%

“…As with many components of the Wnt signalling pathway, Notum was originally discovered in fruit flies, in screens for genes that interact with the Wnt protein Wingless 7,8 . Loss of Notum in flies leads to abnormal wing growth, indicating that Wnt signalling (which drives wing growth and patterning) becomes un restrained in its absence.…”

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confidence: 99%

Enceladus' hot springs

Tobie

2015

Nature

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“…Several theoretical models have been proposed to understand the evolution of icy planetary bodies (Prialnik and Bar‐Nun ; Cohen and Coker ; Prialnik et al ; Schubert et al. ; Barr and Canup ; Prialnik and Merk ; Sahijpal and Gupta ; Wakita and Sekiya ; Sahijpal ; Malamud and Prialnik , ). Some of these theoretical models have indicated that the short‐lived radionuclide, 26 Al (τ~1 Ma; million years), could have played a major role in the heating and differentiation of planetary bodies in the early solar system.…”

Section: Introductionmentioning

confidence: 99%

Thermal evolution of trans‐Neptunian objects, icy satellites, and minor icy planets in the early solar system

Bhatia

Sahijpal

2017

Meteorit & Planetary Scien

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Numerical simulations are performed to understand the early thermal evolution and planetary scale differentiation of icy bodies with the radii in the range of 100–2500 km. These icy bodies include trans‐Neptunian objects, minor icy planets (e.g., Ceres, Pluto); the icy satellites of Jupiter, Saturn, Uranus, and Neptune; and probably the icy‐rocky cores of these planets. The decay energy of the radionuclides, 26Al, 60Fe, 40K, 235U, 238U, and 232Th, along with the impact‐induced heating during the accretion of icy bodies were taken into account to thermally evolve these planetary bodies. The simulations were performed for a wide range of initial ice and rock (dust) mass fractions of the icy bodies. Three distinct accretion scenarios were used. The sinking of the rock mass fraction in primitive water oceans produced by the substantial melting of ice could lead to planetary scale differentiation with the formation of a rocky core that is surrounded by a water ocean and an icy crust within the initial tens of millions of years of the solar system in case the planetary bodies accreted prior to the substantial decay of 26Al. However, over the course of billions of years, the heat produced due to 40K, 235U, 238U, and 232Th could have raised the temperature of the interiors of the icy bodies to the melting point of iron and silicates, thereby leading to the formation of an iron core. Our simulations indicate the presence of an iron core even at the center of icy bodies with radii ≥500 km for different ice mass fractions.

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Modeling serpentinization: Applied to the early evolution of Enceladus and Mimas

Cited by 50 publications

References 32 publications

Core cracking and hydrothermal circulation can profoundly affect Ceres' geophysical evolution

Core cracking and hydrothermal circulation can profoundly affect Ceres' geophysical evolution

Enceladus' hot springs

Thermal evolution of trans‐Neptunian objects, icy satellites, and minor icy planets in the early solar system

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