Use this URL to cite or link to this record in EThOS: https://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.522298
Title: The geology of the Moon : geochemistry and petrology of lunar basalts
Author: Hallis, Lydia
ISNI:       0000 0004 0123 487X
Awarding Body: Open University
Current Institution: Open University
Date of Award: 2010
Availability of Full Text:
Access from EThOS:
Access from Institution:
Abstract:
The aim of this research is to determine any genetic relationships between high- and lowTi lunar basalts in terms of petrology, mineralogy, geochemistry and geochronology, using a set of Apollo samples. SEM images, mineral compositions, and major- and trace-element data indicate that the high and low-Ti mare-basalts form two distinct groups, both mineralogically and chemically. Apollo 12 and 15 low-Ti basalts were produced from similar source regions, whereas the Apollo 11 and 17 basalts show greater source region compositional variation. Pb-Pb age dating of low-Ti and high-Ti samples confirm previous observations indicating the former are generally younger than the latter. Geochemical modelling suggests that the low-Ti basalts formed from < 10 % partial melting of a depleted Moon source, followed by olivine fractionation. The high-Ti basalts were probably formed as a result of < 15 % partial melting of relatively incompatible-elementenriched source regions, followed by multi-phase crystal fractionation. The REE content of Apollo 14 low-Ti, high-AI basalt 14053 can be reconstructed by ~ 10 % partial melting of a depleted Moon source, followed by olivine fractionation and 1.5 % simultaneous assimilation of a KREEPy/granitic crustal component. The REE contents of Apollo 11 high-Ti, high-K basalts match well with 10 % KREEP assimilation, along with multi-phase fractionation from a parental melt similar to Apollo 11 orange glass. Setting aside the different parental melt evolutions, bulk-rock elemental evidence clearly indicates that the high- and low-Ti mare-basalts were produced by compositionally different source regions. This conclusion is supported by different oxygen isotope compositions of the high- and low-Ti basalts. However, oxygen isotope data implies that rather than a bi-modal system, a mare-basalt compositional continuum exists. This continuum fits well with the heterogeneous cumulate source model for mare-basalt formation. Our oxygen isotope data reveal no detectable difference between the 0 of the Earth and Moon, with implications for the viability of the giant impact origin of the Moon.
Supervisor: Not available Sponsor: Not available
Qualification Name: Thesis (Ph.D.) Qualification Level: Doctoral
EThOS ID: uk.bl.ethos.522298  DOI:
Share: