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    New Craters on Mars: An Updated Catalog

    Access Status
    Fulltext not available
    Authors
    Daubar, I.J.
    Dundas, C.M.
    McEwen, A.S.
    Gao, A.
    Wexler, D.
    Piqueux, S.
    Collins, G.S.
    Miljković, Katarina
    Neidhart, Tanja
    Eschenfelder, J.
    Bart, G.D.
    Wagstaff, K.L.
    Doran, G.
    Posiolova, L.
    Malin, M.
    Speth, G.
    Susko, D.
    Werynski, A.
    Date
    2022
    Type
    Journal Article
    
    Metadata
    Show full item record
    Citation
    Daubar, I.J. and Dundas, C.M. and McEwen, A.S. and Gao, A. and Wexler, D. and Piqueux, S. and Collins, G.S. et al. 2022. New Craters on Mars: An Updated Catalog. Journal of Geophysical Research: Planets. 127 (7): ARTN e2021JE007145.
    Source Title
    Journal of Geophysical Research: Planets
    DOI
    10.1029/2021JE007145
    ISSN
    2169-9097
    Faculty
    Faculty of Science and Engineering
    School
    School of Earth and Planetary Sciences (EPS)
    Funding and Sponsorship
    http://purl.org/au-research/grants/arc/DP180100661
    http://purl.org/au-research/grants/arc/DE180100584
    URI
    http://hdl.handle.net/20.500.11937/90184
    Collection
    • Curtin Research Publications
    Abstract

    We present a catalog of new impacts on Mars. These craters formed in the last few decades, constrained with repeat orbital imaging. Crater diameters range from 58 m down to <1 m. For each impact, we report whether it formed a single crater or a cluster (58% clusters); albedo features of the blast zone (88% halos; 64% linear rays; 10% arcuate rays; majority dark-toned; 4% light-toned; 14% dual-toned); and exposures of ice (4% definite; 2% possible). We find no trends in the occurrences of clusters with latitude, elevation, or impact size. Albedo features do not depend on atmospheric fragmentation. Halos are more prevalent at lower elevations, indicating an atmospheric pressure dependence; and around smaller impacts, which could be an observational bias. Linear rays are more likely to form from larger impacts into more consolidated material and may be enhanced by lower atmospheric pressure at higher elevations. Light- and dual-toned blast zones occur in specific regions and more commonly around larger impacts, indicating excavation of compositionally distinct material. Surfaces covered with bright dust lacking cohesion are favored to form detectable surface features. The slope of the cumulative size frequency distribution for this data set is 2.2 for diameters >8 m (differential slope 2.9), significantly shallower than the slope of new lunar craters. We believe that no systematic biases exist in the Martian data set sufficient to explain the discrepancy. This catalog is complete at the time of writing, although observational biases exist, and new discoveries continue.

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