The depths of the mare basalt source region

Details The depths of the mare basalt source region The depths of the mare basalt source region

Feb 1985

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985lpsc...15..396b&link_type=abstract

(Lunar and Planetary Institute, NASA, American Geophysical Union, et al., Lunar and Planetary Science Conference, 15th, Houston,

Physics

3

Basalt, Glass, Lunar Maria, Lunar Rocks, Magma, Melting, Metal Oxides, Mineralogy, Olivine, Pyroxenes, Moon, Samples, Lunar, Maria, Basalts, Source, Depth, Chemistry, Magma, Parent Materials, Mineralogy, Melting, Formation, Composition, Olivine

Scientific paper

Chemical data for the parental magmas of the nine known VLT Array I pyroclastic glasses show statistically significant trends due to olivine (approximately Fo83) control during their formation by partial melting. The compositional scatter is largely due to compositional variations in the source regions on the + or - 1 percent level. This compositional scatter is small when one considers that the scale of the source region is up to 1000 km, but is sufficient to make positive identification of the residual phase(s) in the source regions difficult. Nevertheless, when the effects of the scatter are properly modeled, it is relatively clear that olivine is the residual phase in the source region. Hence these data and additional constraints indicate that the source regions are at shallow depths in the moon.

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