dc.contributor.author |
Marchi, Simone |
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dc.contributor.author |
Ermakov, A. I. |
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dc.contributor.author |
Raymond, Carol A. |
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dc.contributor.author |
Fu, Roger R. (Roger Rennan) |
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dc.contributor.author |
O'Brien, D. P. |
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dc.contributor.author |
Bland, M. T. |
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dc.contributor.author |
Ammannito, E. |
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dc.contributor.author |
De Sanctis, M. Cristina |
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dc.contributor.author |
Bowling, T. |
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dc.contributor.author |
Schenk, Paul M. |
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dc.contributor.author |
Scully, J. E. C. |
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dc.contributor.author |
Buczkowski, Debra L. |
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dc.contributor.author |
Williams, David A. (Planetary geologist) |
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dc.contributor.author |
Hiesinger, H. (Harald) |
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dc.contributor.author |
Russell, C. T. (Christopher T.) |
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dc.coverage.spatial |
Ceres (Dwarf planet) |
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dc.date.accessioned |
2020-02-21T21:51:00Z |
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dc.date.available |
2020-02-21T21:51:00Z |
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dc.date.issued |
2016-07-26 |
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dc.identifier.citation |
Marchi, S. et al. The missing large impact craters on Ceres. Nat. Commun. 7:12257 doi: 10.1038/ncomms12257 (2016). |
en |
dc.identifier.other |
PMID: 27459197 |
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dc.identifier.other |
PMCID: PMC4963536 |
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dc.identifier.other |
DOI: 10.1038/ncomms12257 |
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dc.identifier.uri |
https://hdl.handle.net/20.500.11753/1432 |
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dc.description.abstract |
Asteroids provide fundamental clues to the formation and evolution of planetesimals. Collisional models based on the depletion of the primordial main belt of asteroids predict 10–15 craters 4400 km should have formed on Ceres, the largest object between Mars and Jupiter, over the last 4.55 Gyr. Likewise, an extrapolation from the asteroid Vesta would require at least 6–7 such basins. However, Ceres' surface appears devoid of impact craters 4B280 km. Here, we show a significant depletion of cerean craters down to 100–150 km in diameter. The overall scarcity of recognizable large craters is incompatible with collisional models, even in the case of a late implantation of Ceres in the main belt, a possibility raised by the presence of ammoniated phyllosilicates. Our results indicate that a significant population of large craters has been obliterated, implying that long-wavelength topography viscously relaxed or that Ceres experienced protracted widespread resurfacing. |
en |
dc.description.statementofresponsibility |
S. Marchi, A.I. Ermakov, C.A. Raymond, R.R. Fu, D.P. O'Brien, M.T. Bland, E. Ammannito, M.C. De Sanctis, T. Bowling, P. Schenk, J.E.C. Scully, D.L. Buczkowski, D.A. Williams, H. Hiesinger & C.T. Russell |
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dc.format.mimetype |
application/pdf |
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dc.language.iso |
en |
en |
dc.publisher |
Nature |
en |
dc.relation.ispartofseries |
LPI contribution ; no. 2273 |
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dc.subject |
Ceres (Dwarf planet) |
en |
dc.subject |
Impact craters |
en |
dc.title |
The missing large impact craters on Ceres |
en |
dc.type |
Article |
en |
dc.rights.license |
This work is licensed under a Creative Commons Attribution 4.0 International License. The images or other third party material in this article are included in the article's Creative Commons license, unless indicated otherwise in the credit line |
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