Mare Orientale

"Oriental Sea" redirects here. For other uses, see East Sea (disambiguation).
Mare Orientale

1967 Lunar Orbiter 4 image
Coordinates 19°24′S 92°48′W / 19.4°S 92.8°W / -19.4; -92.8Coordinates: 19°24′S 92°48′W / 19.4°S 92.8°W / -19.4; -92.8
Diameter 327 km (203 mi)[1]
Eponym Eastern Sea

Mare Orientale ("eastern sea" in Latin) is a lunar mare. It is located on the western border of the Moon's nearside and is difficult to see from an Earthbound perspective. Images from spacecraft have revealed it to be one of the most striking large scale lunar features, resembling a target ring bullseye.

Geology

During the 1960s, rectified images of Mare Orientale by Gerard Kuiper at the Lunar and Planetary Laboratory gave rise to the notion of it being an impact crater.[2][3] The structure, with the flat plain of the mare in the center, is about 900 kilometres (560 mi) across and was formed by the impact of an asteroid-sized object.[4][5] Compared with most other lunar basins, Mare Orientale is less flooded by mare basalts, so that a lot of the basin structure is visible. The basalt in the central portion of the Orientale basin is probably less than 1 km (0.62 mi) in thickness which is much less than mare basins on the earth-facing side of the moon.[4] The collision caused ripples in the lunar crust, resulting in the three concentric circular features. The innermost rings of this vast, multi-ringed crater are the inner and outer Montes Rook, and the outermost ring are the Montes Cordillera, 930 km (580 mi) in diameter. Outward from here, ejecta extend some 500 km (310 mi) from the foot of the mountains and form a rough surface with hummocks and with features radially aligned towards the center.[4]

The Apollo program did not sample rocks from Mare Orientale so its precise age is not known. However, it is the Moon's most recent impact basin, probably rather younger than the Imbrium Basin, which is about 3.85 billion years old.[4] The surrounding basin material is of the Lower Imbrian epoch with the mare material being of the Upper Imbrian epoch.[6]

Located at the antipode of Mare Orientale is Mare Marginis.

A mass concentration (mascon), or gravitational high, was identified in the center of Mare Orientale from Doppler tracking of the five Lunar Orbiter spacecraft in 1968.[7] The mascon was confirmed and mapped at higher resolution with later orbiters such as Lunar Prospector and GRAIL.

Discovery and name

Mare Orientale is difficult to observe from Earth, as it lies at the extreme western edge of the near side. All that can be seen are the rough mountain ranges—the Montes Rook and the Montes Cordillera—and some glimpses of the dark mare material beyond them.[8] However, the Moon's libration means that on rare occasions Mare Orientale is turned slightly more toward the Earth, and becomes a little more discernible.[9]

Although various astronomers had observed hints of the mare, it was first fully described by the German astronomer Julius Franz in his 1906 book Der Mond ("The Moon"). Franz also gave the mare its name. At the time, it was located on what by convention was considered the eastern side of the Moon, hence Franz named it the "Eastern Sea".[10] This paradox is known from the reversed moon images which were seen on the astronomer telescopes lenses for many years. In 1961, however, the International Astronomical Union adopted the astronautic convention for East and West on the Moon and this limb became the western edge.[9]

The first detailed study of the Mare Orientale was by Hugh Percy Wilkins, who called it "Lunar Mare X".[11] Franz's discoveries were not well known,[11] and in the 1976 edition of his book Guide to the Moon, Patrick Moore claims that he and Wilkins discovered and named Mare Orientale in 1946. However, Moore credits Franz as discoverer in his 2009 Yearbook of Astronomy (p. 133-135).

Gallery

  1. ^ Ulrich & Saunders 1968, pp. 47-48.

References

  1. ↑ "Nomenclature Search Results: Moon Mare/Maria". Gazetteer of Planetary Nomenclature. United States Geological Survey. Retrieved 2010-08-20.
  2. ↑ Beals & Tanner 1975, p. 299-306.
  3. ↑ Hartmann & Kuiper 1962, pp. 51-66.
  4. 1 2 3 4 Kiefer, Walter S. "Lunar Orbiter: Impact Basin Geology". Lunar and Planetary Institute. Retrieved 29 October 2013.
  5. ↑ Benningfield, Damond (17 June 2008). "Mare Orientale". StarDate.org. McDonald Observatory. Retrieved 29 October 2013.
  6. ↑ "The Isabel Williamson Lunar Observing Program" (PDF). Royal Astronomical Society of Canada. March 2013. Retrieved 29 October 2013.
  7. ↑ P. M. Muller, W. L. Sjogren (1968). "Mascons: Lunar Mass Concentrations". Science. 161 (3842): 680–684. doi:10.1126/science.161.3842.680.
  8. ↑ Consolmagno & Davis 2011.
  9. 1 2 Baum & Whitaker 2007, p. 129.
  10. ↑ Baum & Whitaker 2007, p. 132.
  11. 1 2 Baum & Whitaker 2007, p. 133.

Bibliography

  • Beals, C. S.; Tanner, R. W. (December 1975). "On the Age of Mare Orientale". Journal of the Royal Astronomical Society of Canada 69: 299–306. Bibcode:1975JRASC..69..299B. 
  • Baum, R.; Whitaker, E. A. (June 2007). "Mare Orientale: The Eastern Sea in the west - Discovery and nomenclature". Journal of the British Astronomical Association 117 (3): 129–135. Bibcode:2007JBAA..117..129B. 
  • Consolmagno, G.; Davis, D. M. (2011). Turn Left at Orion (4th ed.). Cambridge University Press. p. 39. ISBN 9780521153973. 
  • Hartmann, W. K.; Kuiper, G. P. (1962). "Concentric Structures Surrounding Lunar Basins". Communications of the Lunar and Planetary Laboratory 1 (1): 51–66. Bibcode:1962CoLPL...1...51H. 
  • Ulrich, G. E.; Saunders, R. S. (July 1968). "Advanced Systems Traverse Research Project Report" (PDF). Astrogeology (7). United States Geological Survey: 47–48. OCLC 51798143. Retrieved 29 October 2013. 
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