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Bernard (crater)








Bernard (crater)


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Not to be confused with Barnard (Martian crater).










Bernard

Martian crater Bernard based on day THEMIS.png
Bernard crater based on day-time THEMIS image

Planet
Mars
Coordinates
23°36′S 154°18′W / 23.6°S 154.3°W / -23.6; -154.3Coordinates: 23°36′S 154°18′W / 23.6°S 154.3°W / -23.6; -154.3
Diameter
131.0 km
Eponym
P. Bernard, a French atmospheric scientist

Bernard is a large crater in the Memnonia quadrangle of Mars, located at 23.6° south latitude and 154.3° west longitude. It is 131.0 km in diameter and was named after P. Bernard, a French atmospheric scientist.[1]


Nearby prominent craters include Cross to the southwest, Comas Sola to the northwest, Kovalsky to the east-southeast and Dejnev to the west. Northeast of Bernard crater is Mangala Valles.





  • Map showing the relative positions of Bernard Crater and other nearby craters in Memnonia quadrangle




The floor of the crater contains large cracks, which may be due to erosion.





  • West side of Bernard Crater, as seen by CTX camera (on Mars Reconnaissance Orbiter).







  • Close-up of part of floor of Bernard Crater, as seen by CTX camera (on Mars Reconnaissance Orbiter).







  • Close-up of part of floor of Bernard Crater showing troughs and dust devil tracks, as seen by CTX camera (on Mars Reconnaissance Orbiter).







  • Bernard Crater Floor, as seen by HiRISE. Large cracks are visible on floor.







  • Troughs on the floor of Bernard Crater showing many boulders, as seen by HiRISE under HiWish program







  • Troughs on the floor of Bernard Crater, as seen by HiRISE under HiWish program






Impact craters generally have a rim with ejecta around them, in contrast volcanic craters usually do not have a rim or ejecta deposits. As craters get larger (greater than 10 km in diameter) they usually have a central peak.[2] The peak is caused by a rebound of the crater floor following the impact.[3] If one measures the diameter of a crater, the original depth can be estimated with various ratios. Because of this relationship, researchers have found that many Martian craters contain a great deal of material; much of it is believed to be ice deposited when the climate was different.[4] Sometimes craters expose layers that were buried. Rocks from deep underground are tossed onto the surface. Hence, craters can show us what lies deep under the surface.



See also[edit]


  • Dust devil tracks

  • Impact crater

  • Impact event

  • HiRISE

  • HiWish program

  • List of craters on Mars

  • Water on Mars

  • Climate of Mars

  • Ore resources on Mars


References[edit]




  1. ^ "Bernard (crater)". Gazetteer of Planetary Nomenclature. USGS Astrogeology Research Program.


  2. ^ http://www.lpi.usra.edu/publications/slidesets/stones/


  3. ^ Hugh H. Kieffer (1992). Mars. University of Arizona Press. ISBN 978-0-8165-1257-7. Retrieved 7 March 2011. 


  4. ^ Garvin, J., et al. 2002. Global geometric properities of martian impact craters. Lunar Planet Sci. 33. Abstract @1255.












Retrieved from "https://en.wikipedia.org/w/index.php?title=Bernard_(crater)&oldid=847740141"





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