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    A depth versus diameter scaling relationship for the best-preserved melt-bearing complex craters on Mars

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    Name:
    Tornabene_et_al_ICARUS_2016_50 ...
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    Description:
    Final Accepted Manuscript
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    Author
    Tornabene, Livio L.
    Watters, Wesley A.
    Osinski, Gordon R.
    Boyce, Joseph M.
    Harrison, Tanya N.
    Ling, Victor
    McEwen, Alfred S.
    Affiliation
    Univ Arizona, Lunar & Planetary Lab
    Issue Date
    2018-01-01
    
    Metadata
    Show full item record
    Publisher
    ACADEMIC PRESS INC ELSEVIER SCIENCE
    Citation
    Tornabene, L. L., Watters, W. A., Osinski, G. R., Boyce, J. M., Harrison, T. N., Ling, V., & McEwen, A. S. (2018). A depth versus diameter scaling relationship for the best-preserved melt-bearing complex craters on Mars. Icarus, 299, 68-83.
    Journal
    ICARUS
    Rights
    © 2017 Elsevier Inc. All rights reserved.
    Collection Information
    This item from the UA Faculty Publications collection is made available by the University of Arizona with support from the University of Arizona Libraries. If you have questions, please contact us at repository@u.library.arizona.edu.
    Abstract
    We use topographic data to show that impact craters with pitted floor deposits are among the deepest on Mars. This is consistent with the interpretation of pitted materials as primary crater-fill impactite deposits emplaced during crater formation. Our database consists of 224 pitted material craters ranging in size from similar to 1 to 150 km in diameter. Our measurements are based on topographic data from the Mars Orbiter Laser Altimeter (MOLA) and the High-Resolution Stereo Camera (HRSC). We have used these craters to measure the relationship between crater diameter and the initial post-formation depth. Depth was measured as maximum rim-to-floor depth, (d(r)), but we also report the depth measured using other definitions. The database was down-selected by refining or removing elevation measurements from problematic craters affected by processes and conditions that influenced their d(r)/D, such as pre-impact slopes/topography and later overprinting craters. We report a maximum (deepest) and mean scaling relationship of d(r) = (0.347 +/- 0.021)D-0.537 +/- (0.017) and d(r) = (0.323 +/- 0.017)D-0.538 +/- (0.016), respectively. Our results suggest that significant variations between previously-reported MOLA-based d(r) vs. D relationships may result from the inclusion of craters that: 1) are influenced by atypical processes (e.g., highly oblique impact), 2) are significantly degraded, 3) reside within high-strength regions, and 4) are transitional (partially collapsed). By taking such issues into consideration and only measuring craters with primary floor materials, we present the best estimate to date of a MOLA-based relationship of dr vs. D for the least-degraded complex craters on Mars. This can be applied to crater degradation studies and provides a useful constraint for models of complex crater formation. (C) 2017 Elsevier Inc. All rights reserved.
    Note
    24 month embargo; published online: 14 July 2017
    ISSN
    00191035
    DOI
    10.1016/j.icarus.2017.07.003
    Version
    Final accepted manuscript
    Additional Links
    https://linkinghub.elsevier.com/retrieve/pii/S0019103516308363
    ae974a485f413a2113503eed53cd6c53
    10.1016/j.icarus.2017.07.003
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