T166 Ceres' Surface Composition as an Indication of Interior Evolution (Posters)
Monday, 26 September 2016
9:00 AM - 6:30 PM
Exhibit Hall E/F
COMPOSITION OF THE URVARA-YALODE REGION ON CERES
Paper number: T166-11
Program: Technical Sessions
Time: 9:00 AM – 6:30 PM
Authors
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Federico TosiIAPS - Istituto di Astrofisica e Planetologia Spaziali, Rome
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Sergio FonteIAPS - Istituto di Astrofisica e Planetologia Spaziali, Rome
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Marco GiardinoIAPS - Istituto di Astrofisica e Planetologia Spaziali, Rome
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Lucy A. McFaddenGSFC, Greenbelt, MD
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Ernesto PalombaIAPS - Istituto di Astrofisica e Planetologia Spaziali, Rome
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Katrin StephanInstitute of Planetary Research, Berlin
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Carol A. RaymondCalifornia Institute of Technology, Pasadena, CA
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Christopher T. RussellUniversity of California, Los Angeles, Los Angeles, CA
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Maria Cristina De SanctisIAPS - Istituto di Astrofisica e Planetologia Spaziali, Rome
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Filippo Giacomo CarrozzoINAF - Istituto Nazionale di Astrofisica, Rome
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Francesca ZambonIAPS - Istituto di Astrofisica e Planetologia Spaziali, Rome
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Mauro CiarnielloIAPS - Istituto di Astrofisica e Planetologia Spaziali, Rome
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Jean-Philippe CombeBear Fight Institute, Winthrop, WA
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Alessandro FrigeriIAPS - Istituto di Astrofisica e Planetologia Spaziali, Rome
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Andrea LongobardoINAF - Istituto Nazionale di Astrofisica, Rome
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Andrea RaponiIAPS - Istituto di Astrofisica e Planetologia Spaziali, Rome
Abstract
The morphology of this region is dominated by the two impact craters Urvara (45°S and 249°E, diam: 170Km) and Yalode (42°S and 292°E, diam: 260Km). The catenae here present (Gerber, Pongal and Baltay) seem to be associated with the formation these impacts. The northern part is dominated by smooth material while the southern is more cratered.
As noted for the global maps [2], also in this region the chemical composition of phyllosilicate is uniform while their abundance varies. The element that seems to be of particular interest is a positive anomaly in the presence of NH4 phyllosilicates within Urvara which, together with Dantu, has the highest concentration of ammoniated clays on the surface of Ceres. We discuss here the correlation of the composition with the morphology, topography to understand the origin of this NH4 rich location.
[1] De Sanctis M.C. et al. (2011) Space Sci. Rev., 163, 329–369. [2] Ammannito E. et al. (2016), Science.
Geological Society of America Abstracts with Programs. Vol. 48, No. 7
doi: 10.1130/abs/2016AM-286845
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