The origin and evolution of lunar high-Ti basalts - Periodic melting of a single source at Mare Tranquillitatis

Details The origin and evolution of lunar high-Ti basalts - Periodic melting of a single source at Mare Tranquillitatis The origin and evolution of lunar high-Ti basalts - Periodic melting of a single source at Mare Tranquillitatis

Jan 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994gecoa..58..515j&link_type=abstract

Geochimica et Cosmochimica Acta, vol. 58, p. 515

Computer Science

9

Basalt, Lunar Rocks, Titanium, Melting, Apollo 11 Flight, Lunar Composition, Rare Earth Elements, Potassium, Potassium Oxides

Scientific paper

Five groups of basalts (A, B1, B2, B3, D) with three principal ages exist at the Apollo 11 site. These range from the low-K, low-REE Groups B1, B2, and B3 to the low-K, high-REE Group D basalts, to the high-K, high-REE Group A basalts. The Group A basalts are the only high-K basalts and are youngest, with an age of 3.59 +/- 0.02 Ga; Groups B3 and B1 are 3.71 +/- 0.02 and 3.67 +/- 0.02 Ga, respectively; Group B2 basalts are the oldest at 3.85 +/- 0.02 Ga. Group D basalts have not been dated. Fractionation modeling for major and trace elements indicates that the B1 basalts could have formed from a B3-like parent liquid. The B2 and D basalts can also be related to liquids similar to the B3-B composition through the presence of varying amounts of modal whitlockite. Thus the entirety of low-K high-Ti basalts at Apollo 11 may have formed through melting of the same source region. The Group A basalt compositions are consistent with formation from a different parent liquid, with the composition of Apollo 11 orange glass.

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