Crater Cluster (Atmospheric Breakup)
Reference work entry
Group of separated (sometimes overlapping) impact craters that formed simultaneously, likely by the breakup of an impacting body in the atmosphere.
A given cluster’s size depends on atmospheric density, strength and density of the impactor, and speed and angle of atmospheric entry. Individual craters in Martian clusters have diameters of a few tens of meters down to the limit of detection, and the clusters can be spread over areas from 10s of meters to a few 100 m across (Popova et al. 2003; 2007; Daubar et al. 2013). On Venus, irregular craters are a tight cluster of 1–10 km-sized impact craters characterized by irregular and/or discontinuous rims and hummocky or multiple floors (Fig. 1).
- Cochrane CG, Ghail RC (2006) Topographic constraints on impact crater morphology on Venus from high-resolution stereo synthetic aperture radar digital elevation models. J Geophys Res 111:e04007. doi:10.1029/2005je002570Google Scholar
- Hartmann WK, Engel S, Chyba C, Sagan C (1994) Mars cratering record as a probe of ancient pressure variations. Bull Am Astron Soc 26:1116Google Scholar
- McGill GE (2004) Geologic map of the Bereghinya Planitia Quadrangle (V–8), Venus. Geologic investigations series I–2794. U.S. Geological Survey, Flagstaff, AZGoogle Scholar
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