Occator crater in color at highest spatial resolution

Nathues, A.; Platz, Thomas; Thangjam, G.; Hoffmann, M.; Scully, J. E. C.; Stein, N.; Ruesch, O.; Mengel, K.

doi:10.1016/j.icarus.2017.12.021

Cited by 23 publications

(20 citation statements)

References 23 publications

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“…This plains‐type flow appears channelized, typical of T2 and T3 flows, and is found within the ejecta blanket from Occator crater but overprinting the ejecta, suggesting that the flow is associated with ejecta but occurred after the ejecta was emplaced. Occator is known to be young (~20 Ma) and have a recently active crater floor (e.g., Nathues, Platz, Thangjam, et al, ). However, unlike the flows described above and shown in Figure , the ejecta in this region does not appear to be fluidized—it is absent any other lobate structures typically associated with fluidized ejecta.…”

Section: Landslides In Broader Geologic Contextmentioning

confidence: 99%

Landslides on Ceres: Diversity and Geologic Context

et al. 2019

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Landslides are among the most widespread geologic features on Ceres. Using data from Dawn's Framing Camera, landslides were previously classified based upon geomorphologic characteristics into one of three archetypal categories, Type 1(T1), Type 2 (T2), and Type 3 (T3). Due to their geologic context, variation in age, and physical characteristics, most landslides on Ceres are, however, intermediate in their morphology and physical properties between the archetypes of each landslide class. Here we describe the varied morphology of individual intermediate landslides, identify geologic controls that contribute to this variation, and provide first‐order quantification of the physical properties of the continuum of Ceres's surface flows. These intermediate flows appear in varied settings and show a range of characteristics, including those found at contacts between craters, those having multiple trunks or lobes; showing characteristics of both T2 and T3 landslides; material slumping on crater rims; very small, ejecta‐like flows; and those appearing inside of catenae. We suggest that while their morphologies can vary, the distribution and mechanical properties of intermediate landslides do not differ significantly from that of archetypal landslides, confirming a link between landslides and subsurface ice. We also find that most intermediate landslides are similar to Type 2 landslides and formed by shallow failure. Clusters of these features suggest ice enhancement near Juling, Kupalo and Urvara craters. Since the majority of Ceres's landslides fall in the intermediate landslide category, placing their attributes in context contributes to a better understanding of Ceres's shallow subsurface and the nature of ground ice.

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Section: Landslides In Broader Geologic Contextmentioning

confidence: 99%

Landslides on Ceres: Diversity and Geologic Context

et al. 2019

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“…, ; Nathues et al. , , ) despite their association with impact craters. Therefore, a systematic study of bright material requires consideration of the geologic context and formation combined with spectral information.…”

Section: Ceres Bright and Dark Materialsmentioning

confidence: 99%

“…Their origin by post‐impact endogenic processes (Nathues et al. , ) of ascending subsurface brine is likely. Cerealia Facula is a central pit hosting a dome in its center while Vinalia Faculae is a cluster of bright spots to the northeast of Cerealia Facula (Nathues et al.…”

Section: Ceres Bright and Dark Materialsmentioning

confidence: 99%

“…Cerealia Facula is a central pit hosting a dome in its center while Vinalia Faculae is a cluster of bright spots to the northeast of Cerealia Facula (Nathues et al. , , ). The bright material at the dome of Cerealia Facula shows overall red sloped spectra in FC wavelengths (Nathues et al.…”

Section: Ceres Bright and Dark Materialsmentioning

confidence: 99%

“…The dark carbonaceous chondritic‐like surface of Ceres was subjected to aqueous and thermal alteration processes and mixed with bright and compositionally diverse subsurface material (e.g., Nathues et al. , , ; McCord and Castillo‐Rogez ; McSween et al. ).…”

Section: Introductionmentioning

confidence: 99%

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Spectral properties and geology of bright and dark material on dwarf planet Ceres

Thangjam

Nathues

Platz

et al. 2018

Meteorit & Planetary Scien

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Variations and spatial distributions of bright and dark material on dwarf planet Ceres play a key role in understanding the processes that have led to its present surface composition. We define limits for "bright" and "dark" material in order to distinguish them consistently, based on the reflectance of the average surface using Dawn Framing Camera data. A systematic classification of four types of bright material is presented based on their spectral properties, composition, spatial distribution, and association with specific geomorphological features. We found obvious correlations of reflectance with spectral shape (slopes) and age; however, this is not unique throughout the bright spots. Although impact features show generally more extreme reflectance variations, several areas can only be understood in terms of inhomogeneous distribution of composition as inferred from Dawn Visible and Infrared Spectrometer data. Additional material with anomalous composition and spectral properties are rare. The identification of the composition and origin of the dark, particularly the darkest material, remains to be explored. The spectral properties and the morphology of the dark sites suggest an endogenic origin, but it is not clear whether they are more or less primitive surficial exposures or excavated subsurface but localized material. The reflectance, spectral properties, inferred composition, and geologic context collectively suggest that the bright and dark material tends to gradually change toward the average surface over time. This could be because of multiple processes, i.e., impact gardening/space weathering, and lateral mixing, including thermal and aqueous alteration, accompanied by changes in composition and physical properties such as grain size, surface temperature, and porosity (compaction).

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GAUSS - genesis of asteroids and evolution of the solar system

et al. 2021

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The goal of Project GAUSS (Genesis of Asteroids and evolUtion of the Solar System) is to return samples from the dwarf planet Ceres. Ceres is the most accessible candidate of ocean worlds and the largest reservoir of water in the inner Solar System. It shows active volcanism and hydrothermal activities in recent history. Recent evidence for the existence of a subsurface ocean on Ceres and the complex geochemistry suggest past habitability and even the potential for ongoing habitability. GAUSS will return samples from Ceres with the aim of answering the following top-level scientific questions: What is the origin of Ceres and what does this imply for the origin of water and other volatiles in the inner Solar System? What are the physical properties and internal structure of Ceres? What do they tell us about the evolutionary and aqueous alteration history of dwarf planets? What are the astrobiological implications of Ceres? Is it still habitable today? What are the mineralogical connections between Ceres and our current collections of carbonaceous meteorites?

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Occator crater in color at highest spatial resolution

Cited by 23 publications

References 23 publications

Landslides on Ceres: Diversity and Geologic Context

Landslides on Ceres: Diversity and Geologic Context

Spectral properties and geology of bright and dark material on dwarf planet Ceres

GAUSS - genesis of asteroids and evolution of the solar system

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