Ninth International Conference on Mars 2019 (LPI Contrib. No. 2089) 6354.pdf CONTINUOUS EJECTA DEPOSITS OBSERVED BEYOND LAYERED EJECTA RAMPARTS ON MARS. L. L. Tornabene1, J. L. Piatek2, N. G. Barlow3, J. Boyce4, R. Sopocco1, R. Capitan1, A. S. McEwen5, G. R. Osinski1, S. J. Robbins6, W. Watters7, 1Centre for Planetary Science and Exploration and Dept. of Earth Sci- ences, University of Western Ontario, 1151 Richmond Street, London, ON N6A 5B, (
[email protected]), 2Dept. of Geological Sciences, Central Connecticut State Univ., New Britain, CT, 3Dept. Physics and Astronomy, Northern Arizona Univ., Flagstaff, AZ, 4 Hawaii Institute of Geophysics and Planetology, University of Hawai'i, Honolulu, HI, 5LPL, University of Arizona, Tucson, AZ, 6Southwest Research Institute, Boulder, CO, 7Dept. Astronomy, Whitin Observatory, Wellesley College, Wellesley, MA. Introduction: Continuous ejecta deposits on inations of these craters are actively underway, Mars are generally divided into two main morpholog- inlcuding initial measurements of the extent of their ic types: “radial” and “layered”. While radial ejecta “Beyond-Rampart Continuous Ejecta” (BRaCE) faci- represents the most common morphologic type on the es, which is forthcoming. Moon and Mercury [1], layered ejecta is the dominant Beyond-Rampart Continuous EjectA (BRaCE) morphology for well-preserved craters on Mars facies: HiRISE observations show abundant flows (>90% for craters ≥ 5 km in diameter) [2,3]. Volatile emanating from what are interpreted to be volatile- or ice content within (or on) the target [e.g., 4], and/or rich impact melt-bearing deposits that lie atop well- effects from interactions between the ejection process preserved layered ejecta (LE) blankets [14; see Fig.