The rayed crater Zunil and interpretations of small impact craters on Mars

By Alfred S. McEwena, Brandon S. Preblicha, Elizabeth P. Turtlea, Natalia A. Artemievab, Matthew P. Golombekc, Michelle Hurstd, Randolph L. Kirke, Devon M. Burre, Philip R. Christensenf. 2005

351 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Atmospheric Science

View Paper: https://www.semanticscholar.org/paper/4c7e925660f27e545cf8856b7d95317e5ede981f

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Citations in the corpus

The current martian cratering rate (2010, background): “…there has been much debate over the relative contributions of secondary versus primary craters at small crater sizes (e.g. Shoemaker, 1965; McEwen et al., 2005; McEwen and Bierhaus, 2006; Hartmann, 2007; Werner et al., 2009; Robbins and Hynek, 2011; Xiao and Strom, 2012), but we now have…”
THE IMPORTANCE OF SECONDARY CRATERING TO AGE CONSTRAINTS ON PLANETARY SURFACES (2006, background): “…appear; for secondaries within a few crater radii of their parent primary, the maximum diameter is closer to 0.05 Dp, whereas for secondaries that first appear at greater ranges from their parent primary [e.g., Zunil on Mars (McEwen et al. 2005)], the value is less, approximately 0.025 Dp.”
Geologic history of Mars (2010, background): “Dating younger (b1 Gyr) terrains, where small craters must be used, is more uncertain because of the non-uniform distribution of secondary craters (McEwen et al., 2005) and the possibility of a long”
Very recent and wide‐spread basaltic volcanism on Mars (2011, result): “…to minimize complications from the inclusion of small secondary craters in the analyzed crater population, although Werner et al. [2009] and Hartmann et al. [2010] showed that this issue does not compromise absolute age dating as severely as predicted by earlier assertions [McEwen et al., 2005].”
Emplacement of the youngest flood lava on Mars: A short, turbulent story (2010, background): “2), suggesting that the mantling deposit was aerially extensive but relatively thin (because secondaries penetrate through to the lava substrate) at the time of the Zunil impact event.”
Context Camera Investigation on board the Mars Reconnaissance Orbiter (2007, background): “…them are secondaries from a single impact in the region, suggests to some that the terrain is geologically quite young [Hartmann and Berman, 2000; McEwen et al., 2005], while others point out that exhumation from beneath yardangforming materials has also occurred, and may limit the utility of…”
THE YARKOVSKY AND YORP EFFECTS: Implications for Asteroid Dynamics (2006, background): “…the size-frequency distribution of kilometer-sized NEOs is shallower than one would expect from a population dominated by fresh ejecta (Morbidelli & Vokrouhlický 2003, Stuart & Binzel 2004, Bottke et al. 2005b, McEwen et al. 2005). www.annualreviews.org • The Yarkovsky and YORP Effects 159 A nn u.”
Mars Reconnaissance Orbiter's High Resolution Imaging Science Experiment (HiRISE) (2007, background): “tion function for small primary craters is poorly known [McEwen et al., 2005; McEwen and Bierhaus, 2006].”
Global Catastrophic Risks (2008, background): “A rain of perhaps 10 million boulders, metre sized and upwards, would be expected over at least continental dimensions if analogy with the Martian impact crater distribution holds (McEwen et al., 2005).”
Linking the collisional history of the main asteroid belt to its dynamical excitation and depletion (2005, background): “Others claim this change occurred over the last 400–800 Ma (McEwen et al., 2005; Culler et al., 2000), though this is considered controversial (Hörz, 2000; Grier et al., 2001; see B05 for details).”
Selection of the InSight Landing Site (2017, background): “1 (e.g., Pike and Wilhelms 1978; Schultz and Singer 1980; McEwen et al. 2005), about half as deep as primary craters (Pike 1980; Wood and Andersson 1978).”
The global martian volcanic evolutionary history (2009, background): “Plescia and Saunders (1979) based their reference crater production function on counts in the Lunae Planum region, although Neukum and Wise (1976) and Wise et al. (1979a) demonstrated resurfacing activity that obscured the crater size-frequency distribution of this region. Such calibration curves re”