Encyclopedia of Planetary Landforms

2015 Edition
| Editors: Henrik Hargitai, Ákos Kereszturi

Secondary Crater Cluster

Reference work entry
DOI: https://doi.org/10.1007/978-1-4614-3134-3_330


Isolated groups of small craters, generally consisting of 10 or more craters from 10 m to a few km diameter (Figs. 1, 2). They often overlap, are presumed to have formed simultaneously, and are interpreted as craters formed by the impact of ejecta from a large impact.
This is a preview of subscription content, log in to check access.


  1. Hawke BR et al (2006) The comparison and origin of Copernicus rays: implications for the Copernican-Eratosthenian boundary. In: Abstracts of the annual meeting of planetary geologic mappers, Nampa, Idaho. USGSGoogle Scholar
  2. Kumar PS, Kumar AS, Keerthi V, Goswami JN, Krishna BG, Kumar ASK (2011) Chandrayaan-1 observation of distant secondary craters of Copernicus exhibiting central mound morphology: evidence for low velocity clustered impacts on the Moon. Planet Space Sci 59(9):870–879CrossRefGoogle Scholar
  3. Masursky H, Colton GW, El-Baz F (1978) Apollo over the moon: a view from orbit. scientific and technical information office NASA, Washington. NASA SP-362Google Scholar
  4. McEwen AS, Preblich BS, Turtle EP, Artemieva NA, Golombek MP, Hurst M, Kirk RL, Burr DM, Christensen PR (2005) The rayed crater Zunil and interpretations of small impact craters on Mars. Icarus 176:351–381CrossRefGoogle Scholar
  5. Oberbeck VR, Morrison RH (1973) On the formation of the lunar herringbone pattern. Lunar Planet Sci Conf Proc 4:107Google Scholar
  6. Pike RJ, Wilhelms DE (1978) Secondary-impact craters on the Moon: topographic form and geologic process. Lunar Planet Sci IX:907–909, HoustonGoogle Scholar
  7. Popova OP, Hartmann WK, Nemtchinov IV, Richardson DC, Berman DC (2007) Crater clusters on Mars: shedding light on Martian ejecta launch conditions. Icarus 190(1):50–73CrossRefGoogle Scholar
  8. Tornabene LL, Moersch JE, McSween HY Jr, McEwen AS, Piatek JL, Milam KA, Christensen PR (2006) Identification of large (2–10 km) rayed craters on Mars in THEMIS thermal infrared images: implications for possible Martian meteorite source regions. J Geophys Res 111, E10006. doi:10.1029/2005JE002600CrossRefGoogle Scholar

Copyright information

© Springer Science+Business Media New York 2015

Authors and Affiliations

  1. 1.University of ArizonaTucsonUSA