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 in | Geophysical research letters Vol. 43; no. 23; pp. 11,994 - 12,003 |
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| Main Authors | , , , , , , , , , , , , , , , , , , , , |
| Format | Journal Article |
| Language | English |
| Published |
Washington
John Wiley & Sons, Inc
16.12.2016
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| Subjects | |
| Online Access | Get full text |
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| Abstract | 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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| AbstractList | Abstract
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 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. 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 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 |
| Author | Stephan, K. Tosi, F. Hiesinger, H. Preusker, F. Wagner, R. J. Matz, K.‐D. Raymond, C. A. Krohn, K. Jaumann, R. Gathen, I. Schröder, S. E. Roatsch, T. Schulzeck, F. Williams, D. A. Buczkowski, D. L. Otto, K. A. Pieters, C. M. Zambon, F. Russell, C. T. McSween, H. Y. Schmedemann, N. |
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| Snippet | Craters on Ceres, such as Haulani, Kupalo, Ikapati, and Occator show postimpact modification by the deposition of extended plains material with pits, multiple... Abstract Craters on Ceres, such as Haulani, Kupalo, Ikapati, and Occator show postimpact modification by the deposition of extended plains material with pits,... |
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| SubjectTerms | 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 |
| Title | Cryogenic flow features on Ceres: Implications for crater‐related cryovolcanism |
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