The titanium contents of lunar mare basalts

Giguere, T. A.; Taylor, G. J.; Hawke, B. R.; Lucey, P. G.

doi:10.1111/j.1945-5100.2000.tb01985.x

Cited by 187 publications

(160 citation statements)

References 35 publications

(41 reference statements)

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“…S7). The high-TiO 2 peak is similar to the in situ APXS analyses and the remote sensing results (27,28). The low-TiO 2 tail of the smallest craters is due to excavating the underlying low-Ti basalt unit, as indicated by the low-TiO 2 peak for the larger craters (1-4 km in diameter) and the presence of old low-Ti basalt about 10 km north to the landing site.…”

Section: Underlying Basalt Unitssupporting

confidence: 62%

Volcanic history of the Imbrium basin: A close-up view from the lunar rover Yutu

Zhang

Yang

et al. 2015

Proc. Natl. Acad. Sci. U.S.A.

116

117

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We report the surface exploration by the lunar rover Yutu that landed on the young lava flow in the northeastern part of the Mare Imbrium, which is the largest basin on the nearside of the Moon and is filled with several basalt units estimated to date from 3.5 to 2.0 Ga. The onboard lunar penetrating radar conducted a 114-m-long profile, which measured a thickness of ∼5 m of the lunar regolith layer and detected three underlying basalt units at depths of 195, 215, and 345 m. The radar measurements suggest underestimation of the global lunar regolith thickness by other methods and reveal a vast volume of the last volcano eruption. The in situ spectral reflectance and elemental analysis of the lunar soil at the landing site suggest that the young basalt could be derived from an ilmenite-rich mantle reservoir and then assimilated by 10-20% of the last residual melt of the lunar magma ocean.volcanic history | Imbrium basin | lunar rover Yutu | lunar penetrating radar | Chang'e-3 mission

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Section: Underlying Basalt Unitssupporting

confidence: 62%

Volcanic history of the Imbrium basin: A close-up view from the lunar rover Yutu

Zhang

Yang

et al. 2015

Proc. Natl. Acad. Sci. U.S.A.

116

117

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“…Later studies of multispectral data from Earth-based observations and various remote-sensing missions (mostly Galileo, Clementine, and Prospector), instead have found a continuous gradation from very low-Ti to high-Ti mare basalts (e.g., Giguere et al 2000).…”

Section: Tio 2 Resultsmentioning

confidence: 99%

“…7). These values should be shifted upward (∼20%, according to Giguere et al 2000) because of admixing and "contamination" of the maria regolith with materials excavated or ejected from underlying and neighboring highland rocks. Taking these adjustments into account, our figures are still comparable with samples of low-Ti basalts and the inferred unimodal trend.…”

Section: Tio 2 Resultsmentioning

confidence: 99%

Stratigraphy and composition of lava flows in Mare Nubium and Mare Cognitum

Bugiolacchi

Spudis

Guest

2006

Meteorit & Planetary Scien

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Abstract-Three major periods of basaltic activity characterize the infill of the basins. Each of these periods was itself punctuated by discrete phases of widespread magma eruptions: three during both the Late Imbrian Epoch and the early Eratosthenian Period and then two in the late Eratosthenian Period. We found the youngest lavas off the eastern border of the Fra Mauro peninsula and, mantling a much larger area, over most of the central western Nubium basin. Our results place the Nubium/Cognitum basalts in the low-Ti category (1-5 wt% TiO 2 ).The data indicate that the majority (~90%) of the mare terrain has iron content between 18 and 22 wt%. In particular, FeO contents tend to concentrate toward two compositional poles, each of ∼20 wt%, and a much smaller one of ∼15 wt%. These values are typical of nearside lunar maria.To complement our compositional data, we present a census of craters larger than 500 m using Orbiter IV images. The result was a crater count average with frequency 5.6 × 10 −2 km −2 , translating into an inferred mean age of 3300 Ma for the exposed lava flows.By combining lava chemistry with age, we find a possible correlation between the ages of the most prominent flow units and their estimated titanium content, with younger basalts becoming progressively Ti-richer with time (from 2-3 to 4-5 wt% TiO 2 ).

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“…Additionally, low-Ti mare basalts are the predominant form of basalt exposed on the lunar surface (approx. 90%; [112]), and their prevalence over high-Ti mare basalts is consistent with magma ocean crystallization models that indicate that more than 78% of the lunar mantle would be dominated by olivine and orthopyroxene, whereas ilmenite-rich cumulates formed after 95% crystallization [113]. If localized eruption processes were the cause of Zn isotopic variations in lunar mare basalts, correlations might be expected between crystallization history or mantle source composition, yet the δ 66 Zn values seem invariant to these parameters.…”

Section: (D) Local Eruption Processes?mentioning

confidence: 99%

Evaporative fractionation of volatile stable isotopes and their bearing on the origin of the Moon

Day

Moynier

2014

Phil. Trans. R. Soc. A.

108

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The Moon is depleted in volatile elements relative to the Earth and Mars. Low abundances of volatile elements, fractionated stable isotope ratios of S, Cl, K and Zn, high μ ( 238 U/ 204 Pb) and long-term Rb/Sr depletion are distinguishing features of the Moon, relative to the Earth. These geochemical characteristics indicate both inheritance of volatile-depleted materials that formed the Moon and planets and subsequent evaporative loss of volatile elements that occurred during lunar formation and differentiation. Models of volatile loss through localized eruptive degassing are not consistent with the available S, Cl, Zn and K isotopes and abundance data for the Moon. The most probable cause of volatile depletion is global-scale evaporation resulting from a giant impact or a magma ocean phase where inefficient volatile loss during magmatic convection led to the present distribution of volatile elements within mantle and crustal reservoirs. Problems exist for models of planetary volatile depletion following giant impact. Most critically, in this model, the volatile loss requires preferential delivery and retention of late-accreted volatiles to the Earth compared with the Moon. Different proportions of late-accreted mass are computed to explain present-day distributions of volatile and moderately volatile elements (e.g. Pb, Zn; 5 to >10%) relative to highly siderophile elements (approx. 0.5%) for the Earth. Models of early magma ocean phases may be more effective in explaining the volatile loss. Basaltic materials (e.g. eucrites and angrites) from highly differentiated airless asteroids are volatile-depleted, like the Moon, whereas the Earth and Mars have proportionally greater volatile contents. Parent-body size and the existence of early atmospheres are therefore likely to represent fundamental controls on planetary volatile retention or loss.

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The titanium contents of lunar mare basalts

Cited by 187 publications

References 35 publications

Volcanic history of the Imbrium basin: A close-up view from the lunar rover Yutu

Volcanic history of the Imbrium basin: A close-up view from the lunar rover Yutu

Stratigraphy and composition of lava flows in Mare Nubium and Mare Cognitum

Evaporative fractionation of volatile stable isotopes and their bearing on the origin of the Moon

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