Nature, formation, and distribution of carbonates on Ceres

Carrozzo, F. G.; Sanctis, M. C. De; Raponi, A.; Ammannito, E.; Castillo‐Rogez, Julie; Ehlmann, B. L.; Marchi, S.; Stein, N.; Ciarniello, M.; Tosi, F.; Capaccioni, F.; Capria, M. T.; Fonte, S.; Formisano, M.; Frigeri, Alessandro; Giardino, Marco; Longobardo, A.; Magni, G.; Palomba, E.; Zambon, F.; Raymond, C. A.; Russell, C. T.

doi:10.1126/sciadv.1701645

Cited by 92 publications

(97 citation statements)

References 34 publications

(76 reference statements)

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“…No similar faculae are observed on any other mountains independent of rim/wall faculae in impact craters. Mons contain some Na carbonate associated with bright material Carrozzo et al, 2017 ). The rim/wall faculae are compositionally similar to many floor faculae, but the dominant carbonate tends to be Mg-Ca carbonate whereas floor faculae and the most extensive rim/wall faculae (e.g.…”

Section: Ahuna Monsmentioning

confidence: 99%

The Formation and Evolution of Bright Spots on Ceres

Stein¹,

Ehlmann²,

Palomba³

et al. 2017

Geological Society of America Abstracts With Programs

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a b s t r a c tThe otherwise homogeneous surface of Ceres is dotted with hundreds of anomalously bright, predominantly carbonate-bearing areas, termed "faculae," with Bond albedos ranging from ∼0.02 to > 0.5. Here, we classify and map faculae globally to characterize their geological setting, assess potential mechanisms for their formation and destruction, and gain insight into the processes affecting the Ceres surface and near-surface. Faculae were found to occur in four distinct geological settings, associated predominantly with impact craters: (1) crater pits, peaks, or floor fractures (floor faculae), (2) crater rims or walls (rim/wall faculae), (3) bright ejecta blankets, and (4) the mountain Ahuna Mons. Floor faculae were identified in eight large, deep, and geologically young (asteroid-derived model (ADM) ages of < 420 ± 60 Ma) craters: Occator, Haulani, Dantu, Ikapati, Urvara, Gaue, Ernutet, and Azacca. The geometry and geomorphic features of the eight craters with floor faculae are consistent with facula formation via impact-induced heating and upwelling of volatile-rich materials, upwelling/excavation of heterogeneously distributed subsurface brines or their precipitation products, or a combination of both processes. Rim/wall faculae and bright ejecta occur in and around hundreds of relatively young craters of all sizes, and the geometry of exposures is consistent with facula formation via the excavation of subsurface bright material, possibly from floor faculae that were previously emplaced and buried. A negative correlation between rim/wall facula albedo and crater age indicates that faculae darken over time. Models using the Ceres crater production function suggest initial production or exposure of faculae by large impacts, subsequent dissemination of facula materials to form additional small faculae, and then burial by impact-induced lateral mixing, which destroys faculae over timescales of less than 1.25 Gyr. Cumulatively, these models and the observation of faculae limited to geologically young craters indicate relatively modern formation or exposure of faculae, indicating that Ceres' surface remains active and that the near surface may support brines in the present day.

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Section: Ahuna Monsmentioning

confidence: 99%

The Formation and Evolution of Bright Spots on Ceres

Stein¹,

Ehlmann²,

Palomba³

et al. 2017

Geological Society of America Abstracts With Programs

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“…Previous studies (e.g. Carrozzo et al, 2018) showed that occurrence of carbonate content increases the reflectance while the opaque causes darkening. Albedo was calculated by applying a Hapke photometric correction to the entire dataset as described by Ciarniello et al, 2017.…”

Section: Albedo Maps At 12 μMmentioning

confidence: 91%

“…Unlike the two bands described in the previous section, the absorption at 4 µm shows a band center variability. It moves toward longer wavelengths indicating a compositional variation (Carrozzo et al, 2018). Generally, the 4 µm bands is centered at 3.95 µm, showing the presence of Mgcarbonates, even if in specific regions, it shifts to 3.99 µm, suggesting the presence of Na-carbonates (De Sanctis et al, 2016, Carrozzo et al 2018, Fig.…”

Section: Vir Band Center and Depth At 4 μMmentioning

confidence: 92%

“…9). These Na-carbonates deposits are mainly located in Dantu and Azacca ejecta, and in Consus crater (see also Stephan et al, On Ceres, a strong anti-correlation between phyllosilicates and Na-carbonates content is observed (De Sanctis et al, 2015;De Sanctis et al, 2016;Zambon et al, 2017a;Carrozzo et al 2018). Sodium carbonates rich areas are related with low spectral slope values (bluish material, Stephan et al, 2017), both in the visible and in the infrared range.…”

Section: Vir Band Center and Depth At 4 μMmentioning

confidence: 96%

“…In general on Ceres, an albedo increasing is related with the occurrence of Na-carbonate deposits (e.g. Carrozzo et al, 2018).…”

Section: Vir Reflectance At 12 µMmentioning

confidence: 99%

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The mineralogy of Ceres’ Nawish quadrangle

Carrozzo

Zambon

Sanctis

et al. 2019

Icarus

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Quadrangle Ac-H-08 Nawish is located in the equatorial region of Ceres (Lat 22°S-22°N, Lon 144°E-216°E), and it has variable mineralogy and geology. Here, we report on the mineralogy using spectra from the Visible and InfraRed (VIR) mapping spectrometer onboard the NASA Dawn mission. This quadrangle has two generally different regions: the cratered highlands of the central and eastern sector, and the eastern lowlands. We find this dichotomy is also associated with differences in the NH 4 -phyllosilicates distribution. The highlands, in the eastern part of the quadrangle, appear depleted in NH 4 -phyllosilicates, conversely to the lowlands, in the north-western side. The Mg-phyllosilicates distribution is quite homogeneous across Nawish quadrangle, except for few areas. The 2.7-µm band depth is lower in the south-eastern part, e.g. in the Azacca ejecta and Consus crater ejecta, and the band depth is greatest for the Nawish crater ejecta, and indicates the highest content of Mg-phyllosilicates of the entire quadrangle. Our analysis finds an interesting relationship between geology, mineralogy, ACCEPTED MANUSCRIPT A C C E P T E D M A N U S C R I P T 3 topography, and the age in this quadrangle. The cratered terrains in the highlands, poor in NH 4 phyllosilicates r r Ga). Conversely, the smooth terrain, such as with Vindimia Planitia, is richer in ammonia-bearing phy s t s s y u r Ga). At the local scale, Ac-H-8 Nawish, displays several interesting mineralogical features, such as at Nawish crater, Consus crater, Dantu and Azzacca ejecta, which exhibit localized Na-carbonates deposits. This material is superimposed on the cratered terrains and smooth terrains and shows the typical depletion of phyllosilicates, already observed on Ceres in the presence of Na-carbonates.

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Replenishment of near-surface water ice by impacts into Ceres' volatile-rich crust: Observations by Dawn's Gamma Ray and Neutron Detector

Prettyman

Yamashita

Landis

et al. 2021

Preprint

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Nature, formation, and distribution of carbonates on Ceres

Abstract: Hydrated carbonates indicate that the surface of Ceres is recent and dehydration is ongoing, implying a still-evolving body.

Cited by 92 publications

References 34 publications

The Formation and Evolution of Bright Spots on Ceres

The Formation and Evolution of Bright Spots on Ceres

The mineralogy of Ceres’ Nawish quadrangle

Replenishment of near-surface water ice by impacts into Ceres' volatile-rich crust: Observations by Dawn's Gamma Ray and Neutron Detector

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