Mesoscale raised rim depressions (MRRDs) on Earth: A review of the characteristics,processes, and spatial distributions of analogs for Mars |
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| Authors: | Devon M. Burr Barbara C. Bruno Peter D. Lanagan Lori S. Glaze Windy L. Jaeger Richard J. Soare Jean-Michel Wan Bun Tseung James A. Skinner Stephen M. Baloga |
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| Affiliation: | 1. Earth and Planetary Science Department, University of Tennessee, 1412 Circle Drive, Knoxville, TN 37996-1410, USA;2. SETI Institute, 515 North Whisman Road, Mountain View, CA 94043, USA;3. School of Ocean and Earth Science and Technology (SOEST), University of Hawaii, 1000 Pope Road, MSB 205, Honolulu, HI 96822, USA;4. Proxemy Research, 20528 Farcroft Lane, Gaithersburg, MD, 20882, USA;5. 700 College Dr., Mail Code H3C, College of Southern Nevada, Henderson, NV 89002, USA;6. Goddard Space Flight Center, Greenbelt, MD 20771, USA;7. Geological Survey, Astrogeology Team, 2255 N. Gemini Dr., Flagstaff, AZ 86001, USA;8. Department of Geography, Planning and Environment, Concordia University, 1455 De Maisoneuve W., Montreal, Quebec, Canada H3G 1M8;9. Department of Geography, University of Calgary, 2500 University Drive NW, Calgary, Alberta, Canada T2N 1N4;10. Department of Earth Sciences & Physics and Astronomy, University of Western Ontario, 1151 Richmond Street, London, Canada, N6A 5B7;11. Department of Geography, Dawson College, 3040 Sherbrooke St. W., Montreal, Canada, H3Z 1A4;1. ASI, Rome, Italy;2. University of Annunzio, Pescara, Italy;3. ESA/ESTEC, Noordwijk, The Netherlands;4. University of Western Ontario, London, Canada;1. Dept. of Space Studies, Southwest Research Institute, 1050 Walnut St. #300, Boulder, CO 80302, USA;2. Carl Sagan Center, SETI Institute, 189 Bernardo Ave, Suite 100, Mountain View, CA 94043, USA;3. Lowell Observatory, 1400 W. Mars Hill Rd., Flagstaff, AZ 86001, USA;1. Lunar and Planetary Laboratory, University of Arizona, Tucson, AZ 85721-0063, USA;2. Department of Earth and Planetary Sciences, University of Tennessee, Knoxville, TN 37996-1410, USA;1. Lunar and Planetary Laboratory, University of Arizona, Tucson, AZ 85721, USA;2. Department of Earth and Planetary Sciences, University of Tennessee, Knoxville, TN 37996, USA;3. School of Earth and Atmospheric Sciences, Georgia Institute of Technology, GA 30332, USA |
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| Abstract: | Fields of mesoscale raised rim depressions (MRRDs) of various origins are found on Earth and Mars. Examples include rootless cones, mud volcanoes, collapsed pingos, rimmed kettle holes, and basaltic ring structures. Correct identification of MRRDs on Mars is valuable because different MRRD types have different geologic and/or climatic implications and are often associated with volcanism and/or water, which may provide locales for biotic or prebiotic activity. In order to facilitate correct identification of fields of MRRDs on Mars and their implications, this work provides a review of common terrestrial MRRD types that occur in fields. In this review, MRRDs by formation mechanism, including hydrovolcanic (phreatomagmatic cones, basaltic ring structures), sedimentological (mud volcanoes), and ice-related (pingos, volatile ice-block forms) mechanisms. For each broad mechanism, we present a comparative synopsis of (i) morphology and observations, (ii) physical formation processes, and (iii) published hypothesized locations on Mars. Because the morphology for MRRDs may be ambiguous, an additional tool is provided for distinguishing fields of MRRDs by origin on Mars, namely, spatial distribution analyses for MRRDs within fields on Earth. We find that MRRDs have both distinguishing and similar characteristics, and observation that applies both to their mesoscale morphology and to their spatial distribution statistics. Thus, this review provides tools for distinguishing between various MRRDs, while highlighting the utility of the multiple working hypotheses approach. |
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