GSA Annual Meeting in Indianapolis, Indiana, USA - 2018

Paper No. 238-5
Presentation Time: 9:05 AM

GEOLOGICAL MAPPING OF DWARF PLANET CERES FROM NASA’S DAWN MISSION


WILLIAMS, David A.1, MEST, Scott C.2, BUCZKOWSKI, Debra L.3, SCULLY, Jennifer E.C.4, RAYMOND, Carol A.4 and RUSSELL, Christopher T.5, (1)School of Earth and Space Exploration, Arizona State University, Tempe, AZ 85287, (2)Planetary Science Institute, 1700 E. Fort Lowell Rd., Suite 106, Tucson, AZ 85719, (3)Johns Hopkins University Applied Physics Laboratory, 11100 Johns Hopkins Rd, Laurel, MD 20723, (4)NASA Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, CA 91109, (5)Earth and Space Sciences, University of California, Los Angeles, 595 Charles Young Drive East, Los Angeles, CA 90095

A geologic mapping campaign was conducted during NASA’s Dawn Mission at dwarf planet Ceres, including production of a global geologic map and a series of 15 quadrangle maps to determine the variety of process-related geologic materials and the geologic history of Ceres. Mapping results demonstrate that all major planetary geologic processes (impact cratering, volcanism, tectonism, and gradation (weathering-erosion-deposition)) have occurred on Ceres. Ceres crust, dominated by altered and NH3-bearing silicates, carbonates, salts and <30% water ice, preserves impact craters at all sizes and degradation states, and is interpreted to represent the remains of the bottom of an ancient ocean. Volcanism is manifested by cryovolcanic domes, such as Ahuna Mons and Cerealia Facula, and by explosive cryovolcanic plume deposits such as the Vinalia Faculae. It is possible that the volcanism of the faculae is impact-induced, as it occurs within the 92-km diameter Occator impact crater. Tectonism is represented by several catenae extending from Ceres impact basins Urvara and Yalode, terracing in many larger craters, and many localized fractures around smaller craters. Gradation is manifested in a variety of flow-like features caused by mass wasting (landslides), ground ice flows, as well as impact ejecta lobes and melts. Our working chronostratigraphy and geologic timescale for Ceres is centered around major impact events. Ceres geologic periods include Pre-Kerwanan, Kerwanan, Yalodean/Urvaran, and Azaccan (the time of rayed craters, similar to the lunar Copernican). The presence of geologically young cryovolcanic deposits on Ceres surface suggests that there could be warm melt pockets within Ceres shallow crust and the dwarf planet remain geologically active.