Relict Ocean Worlds: Ceres

Sanctis, Maria Cristina DeÂ; Mitri, G.; Castillo‐Rogez, Julie; House, Christopher H.; Marchi, S.; Raymond, C. A.; Sekine, Yasuhito

doi:10.1007/s11214-020-00683-w

Cited by 19 publications

(18 citation statements)

References 172 publications

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“…The evaporative concentrations and consequent carbonate precipitations within Orog, Olgoy, and Boon Tsagaan Lakes could be analogous to the concentrations of dissolved components upon the freezing of subsurface oceans of Ceres and Pluto (e.g., [2,6]). Similar concentrations of dissolved components may occur within subsurface oceans of icy moons, such as Enceladus, due to decreases in the oceanic volume upon the orbital evolution (e.g., [39,40]).…”

Section: Implications For the Water Chemistry Of Enceladus' Oceanmentioning

confidence: 99%

“…The multiple ocean worlds in the outer solar system are icy bodies with subsurface liquid oceans beneath their icy crusts [1,2]. The water chemistries of subsurface oceans on icy bodies that formed from ultramafic (e.g., chondritic) rocks beyond the CO 2 snowline [3] should be saline, carbonate-rich, and have high pH [4][5][6][7][8], suggesting Na ± , Cl − , CO 3 2− , and HCO 3 − as major dissolved species.…”

Section: Introductionmentioning

confidence: 99%

“…The water chemistries of subsurface oceans on icy bodies that formed from ultramafic (e.g., chondritic) rocks beyond the CO 2 snowline [3] should be saline, carbonate-rich, and have high pH [4][5][6][7][8], suggesting Na ± , Cl − , CO 3 2− , and HCO 3 − as major dissolved species. Such icy bodies include Saturn's moon Enceladus in the present day, icy dwarf planets (e.g., Ceres and Pluto), and the parent bodies of D-type asteroids in the past [1,2]. The ubiquity of dissolved Na 2 CO 3 or NaHCO 3 in alkaline lakes on Earth suggests that these lakes can serve as terrestrial analogues for studying the aqueous chemistry and mineral precipitations possibly occurring within ocean worlds.…”

Section: Introductionmentioning

confidence: 99%

“…Previously, the authigenic carbonate mineral species formed during evaporation in alkaline lakes were believed to be calcite or aragonite, common stable calcium carbonates [9][10][11]. In fact, geochemical modeling has assumed the formation of calcite and magnesite to reconstruct the water chemistries of Enceladus, Ceres, and icy planetesimals [4][5][6][7][8], because these carbonates are indeed found in carbonaceous chondrites, and possibly on Ceres [2,12]. However, Fukushi and Matsumiya [13] reviewed the water chemistries of a wide range of terrestrial alkaline lakes, and found that the solution chemistries of alkaline lakes are commonly and significantly oversaturated with respect to the common stable carbonate minerals.…”

Section: Introductionmentioning

confidence: 99%

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In Situ Formation of Monohydrocalcite in Alkaline Saline Lakes of the Valley of Gobi Lakes: Prediction for Mg, Ca, and Total Dissolved Carbonate Concentrations in Enceladus’ Ocean and Alkaline-Carbonate Ocean Worlds

et al. 2020

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The nature of mineral precipitations in terrestrial alkaline soda lakes provides insights into the water chemistry of subsurface oceans on icy bodies in the outer solar system. Saturation analyses of terrestrial alkaline lakes have shown that the solution chemistries of lake waters are generally controlled by the presence of monohydrocalcite (MHC) and amorphous Mg-carbonate (AMC). However, direct observations of the formation of these metastable carbonates in natural alkaline lakes have been limited. This study provides evidence of in situ MHC formation in alkaline lakes, based on the water chemistry and mineralogy of suspended matter in Olgoy, Boon Tsagaan, and Orog Lakes (Valley of Gobi Lakes, Mongolia). The solution chemistries were close to saturation with respect to MHC and AMC, consistent with other alkaline lakes worldwide. Suspended matter was separated by the ultracentrifugation of lake water following freeze-drying. Our results show that MHC is the common mineral phase in the suspended matter. These observations confirm that MHC is the direct authigenic product of evaporation in alkaline lakes. The carbonate fraction in suspended matter from Olgoy Lake has a Mg/Ca ratio of 0.4, suggesting the formation of AMC in association with MHC. Based on the dissolution equilibria of AMC and MHC, we predict the Mg2+, Ca2+, and total dissolved carbonate concentrations in Enceladus’ ocean to be ~1 mmol/kg, ~10 μmol/kg, and 0.06–0.2 mol/kg, respectively, in the presence of AMC and MHC. We propose that the measurements of Mg contents in plumes will be key to constraining the total dissolved carbonate concentrations and chemical affinities of subsurface oceans on Enceladus and other alkaline-carbonate ocean worlds.

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Section: Implications For the Water Chemistry Of Enceladus' Oceanmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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In Situ Formation of Monohydrocalcite in Alkaline Saline Lakes of the Valley of Gobi Lakes: Prediction for Mg, Ca, and Total Dissolved Carbonate Concentrations in Enceladus’ Ocean and Alkaline-Carbonate Ocean Worlds

et al. 2020

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“…Recently, studies [3] confirmed the presence of ammonium phyllosilicate materials using the visible and infrared (VIR)spectrometer on the Dawn mission [4]. De Sanctis et al [5] reports that the bright spots on the Ceres surface (Occator…”

Section: Introductionmentioning

confidence: 99%

Reflectance Spectroscopy of Ammonium Salts: Implications for Planetary Surface Composition

et al. 2020

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Recent discoveries have demonstrated that the surfaces of Mars, Ceres and other celestial bodies, as well as asteroids and comets, are characterized by the presence of ammonium-bearing minerals. A careful study of remote data compared with the analyses of more accurate laboratory data might allow a better remote characterization of planetary bodies. In this paper, the reflectance spectra of some ammoniated hydrous and anhydrous salts, namely sal-ammoniac NH4Cl, larderellite (NH4)B5O7(OH)2·H2O, mascagnite (NH4)SO4, struvite (NH4)MgPO4·6H2O and tschermigite (NH4)Al(SO4)2·12H2O, were collected at 293 and at 193 K. The aim is to detect how the NH4 vibrational features are affected by the chemical and structural environment. All samples were recovered after cooling cycles and were characterized by X-ray powder diffraction. Reflectance spectra of the studied minerals show absorption features around 1.3, 1.6, 2.06, 2.14, 3.23, 5.8 and 7.27 μm, related to the ammonium group. Between them, the 2ν3 at ~1.56 μm and the ν3 + ν4 at ~2.13 μm are the most affected modes by crystal structure type, with their position being strictly related to both anionic group and the strength of the hydrogen bonds. The reflectance spectra of water-rich samples [struvite (NH4)MgPO4·6(H2O) and tschermigite (NH4)Al(SO4)2·12(H2O)] show only H2O fundamental absorption features in the area from 2 to 2.8 μm and a band from hygroscopic water at 3 μm. Thermal analyses (TA), thermal gravimetry (TG) and differential scanning calorimetry (DSC) allowed to evaluate the dehydration temperatures and the occurring phase transitions and decompositions in the analyzed samples. In almost all samples, endothermic peaks at distinct temperatures were registered associated to loss of water molecules, differently linked to the structures. Moreover, an endothermic peak at 465 K in sal-ammoniac was associated to the phase transition from CsCl to NaCl structure type.

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Compositions and Interior Structures of the Large Moons of Uranus and Implications for Future Spacecraft Observations

Castillo‐Rogez

Weiss

Beddingfield

et al. 2022

Preprint

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The five large moons of Uranus are important targets for future spacecraft missions. To motivate and inform the exploration of these moons, we model their internal evolution, present-day physical structures, and geochemical and geophysical signatures that may be measured by spacecraft. We predict that if the moons preserved liquid until present, it is likely in the form of residual oceans less than 30 km thick in Ariel, Umbriel, Titania, and Oberon. The preservation of liquid strongly depends on material properties and, potentially, on dynamical circumstances that are unknown. Miranda is unlikely to preserve liquid until present unless it experienced tidal heating a few tens of million years ago. The triaxial shapes estimated from Voyager 2 data for Miranda and Ariel further support the prospect that these moons are internally differentiated with a rocky core and icy shell. We find that since the thin residual layers may be hypersaline, their induced magnetic fields could be detectable by future spacecraft-based magnetometers. However, if the ocean is maintained primarily by ammonia, and thus well below the water freezing point, then its electrical conductivity may be too small to be detectable by spacecraft. Lastly, our calculated tidal Love number (k 2 ) and dissipation factor (Q) are consistent with the Q/k 2 values previously inferred from dynamical evolution models. In particular, we find that the low Q/k 2 estimated for Titania supports the hypothesis that Titania currently holds an ocean.

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Relict Ocean Worlds: Ceres

Cited by 19 publications

References 172 publications

In Situ Formation of Monohydrocalcite in Alkaline Saline Lakes of the Valley of Gobi Lakes: Prediction for Mg, Ca, and Total Dissolved Carbonate Concentrations in Enceladus’ Ocean and Alkaline-Carbonate Ocean Worlds

In Situ Formation of Monohydrocalcite in Alkaline Saline Lakes of the Valley of Gobi Lakes: Prediction for Mg, Ca, and Total Dissolved Carbonate Concentrations in Enceladus’ Ocean and Alkaline-Carbonate Ocean Worlds

Reflectance Spectroscopy of Ammonium Salts: Implications for Planetary Surface Composition

Compositions and Interior Structures of the Large Moons of Uranus and Implications for Future Spacecraft Observations

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