Lunar mare volcanism - Stratigraphy, eruption conditions, and the evolution of secondary crusts

Details Lunar mare volcanism - Stratigraphy, eruption conditions, and the evolution of secondary crusts Lunar mare volcanism - Stratigraphy, eruption conditions, and the evolution of secondary crusts

Jun 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992gecoa..56.2155h&link_type=abstract

(Geological Society of America, Workshop on Mare Volcanism and Basalt Petrogenesis, Dallas, TX, Oct. 27, 28, 1992) Geochimica et

Mathematics

Logic

93

Lunar Crust, Lunar Maria, Remote Sensing, Stratigraphy, Volcanology, Landforms, Lunar Craters

Scientific paper

Recent developments in the geological analysis of lunar mare volcanism are reviewed. Analysis of returned samples and photogeological and remote sensing studies shows that mare volcanism began prior to the end of heavy bombardment (the period of cryptomare formation), in pre-Nectarian times, and continued until the Copernical Period, the total duration approaching 3.5-4 Ga. Stratigraphic analysis shows that the flux was not constant, but peaked in early lunar history, during the Imbrian Period. Average volcanic output rate during this period was about 0.01 cu cm/a. Volcanic landforms indicate that many eruptions were of high volume and long duration. Some eruptions associated with sinuous rills may have lasted a year and emplaced 1000 cu km of lava, representing the equivalent in one year of about 70,000 yr at the average flux. The occurrence of farside maria within craters whose diameter is generally near to or less than the thickness of the crust may be accounted for by the difference between local and regional compensation.

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