Cryogenic flow features on Ceres: Implications for crater‐related cryovolcanism

Craters on Ceres, such as Haulani, Kupalo, Ikapati, and Occator show postimpact modification by the deposition of extended plains material with pits, multiple lobate flows, and widely dispersed deposits that form a diffuse veneer on the preexisting surface. Bright material units in these features ha...

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Published inGeophysical research letters Vol. 43; no. 23; pp. 11,994 - 12,003
Main Authors Krohn, K., Jaumann, R., Stephan, K., Otto, K. A., Schmedemann, N., Wagner, R. J., Matz, K.‐D., Tosi, F., Zambon, F., Gathen, I., Schulzeck, F., Schröder, S. E., Buczkowski, D. L., Hiesinger, H., McSween, H. Y., Pieters, C. M., Preusker, F., Roatsch, T., Raymond, C. A., Russell, C. T., Williams, D. A.
Format Journal Article
LanguageEnglish
Published Washington John Wiley & Sons, Inc 16.12.2016
Subjects
Asteroids
Coefficient of friction
Computing time
Craters
cryovolcanism
Deposits
Dispersion
dwarf planet Ceres
Efficiency
Enrichment
flow features
Friction
Geomorphology
Geophysics
Gravitation
Gravity
Height
impact melt
Impact melts
Length
Marine
Pits
Plains
Planets
Slopes
Spectra
subsurface materials
Viscosity
Volcanology
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Summary:Craters on Ceres, such as Haulani, Kupalo, Ikapati, and Occator show postimpact modification by the deposition of extended plains material with pits, multiple lobate flows, and widely dispersed deposits that form a diffuse veneer on the preexisting surface. Bright material units in these features have a negative spectral slope in the visible range, making it appear bluish with respect to the grey‐toned overall surface of Ceres. We calculate the drop height‐to‐runout length ratio of several flow features and obtain a coefficient of friction of < 0.1: The results imply higher flow efficiency for flow features on Ceres than for similar features on other planetary bodies with similar gravity, suggesting low‐viscosity material. The special association of flow features with impact craters could either point to an impact melt origin or to an exogenic triggering of cryovolcanic processes. Key Points We analyzed the geomorphology several flows of craters to prove if they were formed by impact melt or cryovolcanic processes The low coefficient of friction implies higher flow efficiency for flows on Ceres than for similar features on other planetary bodies The formation of the flows could be due to the mobility of crustal subsurface reservoirs enriched with hydrated salts by impacts
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ISSN:0094-8276
1944-8007
DOI:10.1002/2016GL070370