Mare Nectaris

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Mare Nectaris
Mare Nectaris.jpg
Mare Nectaris
Coordinates15°12′S 34°36′E / 15.2°S 34.6°E / -15.2; 34.6Coordinates: 15°12′S 34°36′E / 15.2°S 34.6°E / -15.2; 34.6
Diameter340 km (210 mi)[1]
EponymSea of Nectar
View from Apollo 8

Mare Nectaris /ˈnɛktərɪs/ (Latin nectaris, the "Sea of Nectar") is a small lunar mare or sea (a volcanic lava plain noticeably darker than the rest of the Moon's surface) located south of Mare Tranquillitatis southwest of Mare Fecunditatis, on the near side of the moon. Montes Pyrenaeus borders the mare to the east and Sinus Asperitatis fuses to its northwestern edge. It is 84,000 square kilometers in size.[2]

Several large craters are situated at the borders of Mare Nectaris. The biggest one is lava-filled Fracastorius (124 km), which fuses with southern coast of the Sea. A prominent trio of 100-km craters Theophilus, Cyrillus and Catharina is located near northwestern coast. Other notable feature is a "ghost crater" Daguerre, almost entirely covered with lava, in the northern part of Mare Nectaris.[3]

Mare Nectaris is located in the central part of 860-km-diameter impact basin, which was formed 3.8–3.9 billions year ago. This event marks the beginning of Nectarian period of the lunar geologic timescale.[4] The best-preserved part of the rim of this basin is called Rupes Altai, in the southwest part of the basin.

Lava filling of Mare Nectaris is younger than the basin itself. The mare material is approximately 1000m in depth, and mainly of the Nectarian period and the Lower Imbrian epoch, with the mare material of the Upper Imbrian epoch. The crater Theophilus on the northeastern side of the mare is of the Eratosthenian period. Thus, the crater is younger than the mare to its southeast. Enough subsidence has occurred to open a few arcuate grabens on the western margin of the mare.[5]

A mass concentration (mascon), or gravitational high, was identified in the center of Mare Nectaris from Doppler tracking of the five Lunar Orbiter spacecraft in 1968.[6] The mascon was confirmed and mapped at higher resolution with later orbiters such as Lunar Prospector and GRAIL.

See also[edit]


  1. ^ "Mare Nectaris". Gazetteer of Planetary Nomenclature. International Astronomical Union (IAU) Working Group for Planetary System Nomenclature (WGPSN). 2010-10-18. Retrieved 2014-12-11.
  2. ^ Whitford-Stark J. L. (May 1982). "A preliminary analysis of lunar extra-mare basalts: Distribution, compositions, ages, volumes, and eruption styles" (PDF). The Moon and the Planets. 23 (3): 323–338. Bibcode:1982M&P....26..323W. doi:10.1007/BF00928015. S2CID 121034438.
  3. ^ Grego P. (2006). The Moon and How to Observe It. Springer Science & Business Media. pp. 27, 205, 220. ISBN 978-1-846-28243-0.
  4. ^ Tanaka K.L.; Hartmann W.K. (2012). "Chapter 15 – The Planetary Time Scale". In F. M. Gradstein; J. G. Ogg; M. D. Schmitz; G. M. Ogg (eds.). The Geologic Time Scale. Elsevier Science Limited. pp. 275–298. doi:10.1016/B978-0-444-59425-9.00015-9. ISBN 978-0-444-59425-9.
  5. ^ "Mare Nectaris". Archived from the original on June 16, 2002. Retrieved October 16, 2007.
  6. ^ P. M. Muller; W. L. Sjogren (1968). "Mascons: Lunar Mass Concentrations". Science. 161 (3842): 680–684. Bibcode:1968Sci...161..680M. doi:10.1126/science.161.3842.680. PMID 17801458. S2CID 40110502.