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Geologic Mapping of the Ac-H-13 Urvara Quadrangle of Ceres from Nasa’S Dawn Mission

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Geologic Mapping of the Ac-H-13 Urvara Quadrangle of Ceres from Nasa’S Dawn Mission 47th Lunar and Planetary Science Conference (2016) 1599.pdf GEOLOGIC MAPPING OF THE AC-H-13 URVARA QUADRANGLE OF CERES FROM NASA’S DAWN MISSION. H. G. Sizemore1, D. A. Williams2, T. Platz1,3, S. C. Mest1, R. A. Yingst1, D. A. Crown1, D. O’Brien1, D. L. Buczkowski4, P. M. Schenk5, J. E. C. Scully6, R. Jaumann7, T. Roatsch7, F. Preusker7, A. Nathues3, M. C. De- Sanctis8, C. T. Russell9, C. A. Raymond6, 1Planetary Science Institute, Tucson, Arizona ([email protected]), 2Arizona State University, Tempe, AZ USA,3MPI for Solar System Research, Göttingen, Germany, 4JHU-APL, Laurel, Maryland, USA, 5LPI, Houston, Texas, USA, 6NASA JPL, California Institute of Technology, Pasadena, California, USA, 7DLR, Berlin, Germany, 8National Institute of Astrophysics, Rome, Italy, 9UCLA, Los Angeles, California, USA. Introduction: NASA’s Dawn spacecraft arrived at southwest portion of the quadrant have complete rims, Ceres on March 5, 2015, and has been studying the but strongly asymmetric ejecta. A third unnamed crater dwarf planet through a series of successively lower in the northeast portion of the quadrangle is also orbits, obtaining morphological, topographical, miner- asymmetric; the western rim of this crater has col- alogical, elemental, and gravity data. The Dawn Sci- lapsed and mapped ejecta extend to the west. All three ence Team is conducting a geologic mapping cam- small asymmetric craters are associated with hum- paign for Ceres similar to that done for Vesta [1,2], mocky and lobate materials. These observations sug- including production of a Survey- and High Altitude gest that there may be substantial heterogeneity in the Mapping Orbit (HAMO)-based global map, and a se- material properties and volatile content of the subsur- face. ries of 15 Low Altitude Mapping Orbit (LAMO)-based Like the smaller impact craters, the Urvara basin quadrangle maps. In this abstract we discuss the geo- exhibits a distinct morphological and textural dichoto- logic evolution of the Ac-H-13 Urvara Quadrangle. my. The northern rim is sharply defined. The southern Mapping Data: At the time of this writing LAMO rim is less distinct, due to the presence of rugged inte- images (35 m/pixel) are just becoming available. Thus, rior wall terraces and hummocky ejecta to the south. A our geologic maps are based on HAMO images (140 portion of the Urvara rim bounding the Yalode basin to m/pixel) and Survey (400 m/pixel) digital terrain mod- the east is heavily degraded. Smooth material covers els (for topographic information). Dawn Framing much of the Urvara floor, as well as the northern inte- Camera (FC) color images are also used to provide rior wall, and an extended region to the north of the context for map unit identification. The maps to be basin. The distribution of this material suggests that presented as posters will be updated from analyses of much of it was deposited as fluidized ejecta, and via LAMO images. wall collapse. Additionally, some smooth basin floor Mapping Results: The Urvara Quadrangle is dom- materials maybe sourced from a system of grooves or inated by the 170-km diameter impact basin Urvara lineaments on the Urvara floor via post-impact extru- (46.4°S, 248.6°E) and includes cratered terrain to the sion of volatile rich material. Embayment relationships west. Named features include the impact craters Me- with the surrounding terraced wall material, and possi- anderi (40.9°S, 193.7°E, 103 km diameter), Sekhet ble flow margins (mapped as undefined linear features) (66.4°S, 254.9°E, 41 km diameter), and Fluusa are consistent with this interpretation. Pitted textures (31.5°S, 277.9°E), as well as the crater chains Gerber near the base of the central peak complex and at the Catena (38.1°S, 214.8°E) and Samhain Catena (19.6°S, eastern margin of the groove system may indicate 210.3°E). Preliminary geologic mapping defined three volatile loss, again consistent with impact emplace- major units (cratered terrain, smooth material, and ment or possible extrusion of a volatile rich material. undivided cratered material) that dominate the quad- Smooth floor materials and associated linear features rangle. Additional mapped units include hummocky will be mapped in detail as LAMO images of the re- material, lobate material, crater central peak material, gion become available. crater terrace material, crater rim material, and pitted Both Samhain Catena and Gerber Catena run west terrain (Fig. 1) [3,4]. Mapped features include crater by northwest across the western portion of the quad- rims, crater central peaks, crater chains, ridges, rangle. Because these features run parallel to four simi- troughs, domes, grooves, and lineaments. lar catenae in the Occator quadrangle to the north, and Impact structures in the Urvara Quadrangle range because individual craters in Samhain divert around a from degraded features in the north whose rims are degraded crater, they likely did not originate via sec- only apparent in topography data, to realtively pristine ondary impacts. We interpret them to be pit crater features (including Urvara itself) with distinct rims and chains. In contrast, a pair of large curvilinear depres- ejecta deposits that are apparent in both color and sions extending eastward from Urvara toward Yalode greyscale imagery. Four craters, again including Urva- mirror the curvature of three secondary crater chains to ra, exhibit strong asymmetries in the texture and/or the south in the Zadeni Quadrangle. Both curvilinear extent of ejecta materials. Two unnamed craters in the depressions in the Urvara Quadrangle narrow and sep- 47th Lunar and Planetary Science Conference (2016) 1599.pdf arate into crater chains at their distal ends, suggesting morphological asymmetries in crater materials that they originated as secondary impact chains. Indi- throughout the quadrangle indicate heterogeneities in vidual craters may have expanded and merged to pro- subsurface composition and volatile content. Features duce the extant depressions. Sublimation is a possible on the Urvara basin floor are consistent with impact mechanism for this expansion. The presence of an ex- fluidization of target materials; post impact extrusion panded secondary chain in the northeastern portion of of volatile rich material may have also played a minor the quadrangle is consistent with our interpretation of role. the smooth material as volatile rich. Summary: The Urvara Quadrangle is dominated References: [1] Williams D.A. et al. (2014) Icarus, by impact structures, large and small. We interpret two 244, 1-12. [2] Yingst R.A. et al. (2014) PSS, 103, 2-23. prominent catenae as pit craters associated with large [3] Sizemore et al. (2015) GSA Abstracts with Pro- scale tectonism rather than secondary impacts. We gram, Abstract 308-13. [4] Sizemore et al. (2015) AGU interpret two large curvilinear depressions near the Fall Meeting, P53E-2180. eastern quadrangle boundary as secondary crater chains resulting from the Urvara impact. Textural and Figure 1: Geologic map of the Ac-H-13 Urvara Quadrangle of dwarf planet Ceres. Mapping base is Dawn FC HAMO mosaic (courtesy DLR). This work was supported by the Dawn at Ceres Guest Investigator Program. .
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