Search NASA⌕ Search

DOE OSTI · 3363743

Trivalent titanium in high-titanium lunar ilmenite

Vira, Advik D. [Georgia Institute of Technology, Atlanta, GA (United States)] (ORCID:0000000308694951)·Burgess, Katherine D. [US Naval Research Lab. (NRL), Washington, DC (United States)] (ORCID:000000032028447X)·First, Emily C. [Macalester College, Saint Paul, MN (United States)] (ORCID:0000000267951228)·Tian, Mengkun [Georgia Institute of Technology, Atlanta, GA (United States)] (ORCID:0000000327907799)·Eames, Keyes M. [Georgia Institute of Technology, Atlanta, GA (United States)] (ORCID:0009000854797330)·Trivedi, Roshan S. [Georgia Institute of Technology, Atlanta, GA (United States)] (ORCID:0009000229753340)·Dotson, Gabriella K. [Georgia Institute of Technology, Atlanta, GA (United States)]·Kim, Dean M. [Georgia Institute of Technology, Atlanta, GA (United States)]·Farr, Tyler P. [Georgia Institute of Technology, Atlanta, GA (United States); Lawrence Berkeley National Laboratory (LBNL), Berkeley, CA (United States)]·Lisabeth, Harrison [Lawrence Berkeley National Laboratory (LBNL), Berkeley, CA (United States)] (ORCID:000000034491013X)·Tamura, Nobumichi [Lawrence Berkeley National Laboratory (LBNL), Berkeley, CA (United States)] (ORCID:0000000236982611)·Livernois, Emma R. [Georgia Institute of Technology, Atlanta, GA (United States)]·Jones, Brant M. [Georgia Institute of Technology, Atlanta, GA (United States)]·Orlando, Thomas M. [Georgia Institute of Technology, Atlanta, GA (United States)] (ORCID:0000000224224506)·Jiang, Zhigang [Georgia Institute of Technology, Atlanta, GA (United States)] (ORCID:0000000198843337)·First, Phillip N. [Georgia Institute of Technology, Atlanta, GA (United States)] (ORCID:0000000308199598)

Abstract

Lunar mare basalts are often rich in titanium, hosted predominantly within the mineral ilmenite (Fe 2+ Ti 4+ O 3 ). Here, we examine ilmenite in a ~3.8 billion-year-old mare basalt (Apollo rock 75035) using high-resolution electron microscopy and electron energy loss spectroscopy. A key finding is that 75035 ilmenite is itself enriched in Ti, beyond the end member of the conventional solid solution series. Using energy loss near-edge spectroscopy, we determine that the excess Ti is trivalent, with Ti 3+ accounting for 13% of the total Ti content. This discovery confirms the presence of trivalent Ti in lunar ilmenite, long hypothesized based on the Moon’s reducing environment. Accounting for the change in implied stoichiometry, a review of literature data suggests that Ti 3+ may be present in ilmenite across a wide range of lunar samples. We extrapolate known relationships from the literature to connect Ti 3+ to redox conditions, estimating the oxygen fugacity during crystallization of 75035 to be below the iron-wüstite buffer, ΔIW≤ − 1.6. Further quantifying the relationship between Ti valence state and oxygen fugacity would allow Ti 3+ -bearing ilmenite to serve as an oxybarometer able to access the reducing conditions found on many planetary bodies.

Explore related subjects

Keep this discovery

Explore connections, maps & timelines

BibTeXRIS

Vira, Advik D. [Georgia Institute of Technology, Atlanta, GA (United States)] (ORCID:0000000308694951), Burgess, Katherine D. [US Naval Research Lab. (NRL), Washington, DC (United States)] (ORCID:000000032028447X), First, Emily C. [Macalester College, Saint Paul, MN (United States)] (ORCID:0000000267951228), Tian, Mengkun [Georgia Institute of Technology, Atlanta, GA (United States)] (ORCID:0000000327907799), Eames, Keyes M. [Georgia Institute of Technology, Atlanta, GA (United States)] (ORCID:0009000854797330), Trivedi, Roshan S. [Georgia Institute of Technology, Atlanta, GA (United States)] (ORCID:0009000229753340), Dotson, Gabriella K. [Georgia Institute of Technology, Atlanta, GA (United States)], Kim, Dean M. [Georgia Institute of Technology, Atlanta, GA (United States)], Farr, Tyler P. [Georgia Institute of Technology, Atlanta, GA (United States); Lawrence Berkeley National Laboratory (LBNL), Berkeley, CA (United States)], Lisabeth, Harrison [Lawrence Berkeley National Laboratory (LBNL), Berkeley, CA (United States)] (ORCID:000000034491013X), Tamura, Nobumichi [Lawrence Berkeley National Laboratory (LBNL), Berkeley, CA (United States)] (ORCID:0000000236982611), Livernois, Emma R. [Georgia Institute of Technology, Atlanta, GA (United States)], Jones, Brant M. [Georgia Institute of Technology, Atlanta, GA (United States)], Orlando, Thomas M. [Georgia Institute of Technology, Atlanta, GA (United States)] (ORCID:0000000224224506), Jiang, Zhigang [Georgia Institute of Technology, Atlanta, GA (United States)] (ORCID:0000000198843337), First, Phillip N. [Georgia Institute of Technology, Atlanta, GA (United States)] (ORCID:0000000308199598). 2026-03-27. Trivalent titanium in high-titanium lunar ilmenite. https://doi.org/10.1038/s41467-026-69770-w

Cite the original work for its findings. Save a collection to share your selection of sources.

KEEP EXPLORING

Related reports

A Diversity of Temperature and Pressure Conditions Recorded by Zircon within Suevite from Ries Crater, Germany

The temperature and pressure conditions experienced by rocks during an impact event can be constrained using petrologic and microstructural analysis and is crucial to providing ground truth to the impact cratering process. Suevite is a polymict, impact melt-bearing breccia, specific to Ries crater in Germany. There are competing models for suevite formation and emplacement, such as clastic flows pushed out of the crater rim or ejecta plume fallback. Knowledge of the temperature and pressure pathways recorded by grains within the suevite can help distinguish between these and other models. The accessory phase zircon (ZrSiO4) and its high-pressure polymorph reidite are particularly useful in such circumstances as they are highly refractory minerals that can record the high-temperature and/or high-pressure conditions of an impact event. Here we present evidence for a wide array of temperature and pressure conditions recorded in zircon grains within a single thin section of suevite. Zircons in this study range from unshocked to highly shocked (>53 GPa), and record temperatures more than 1673 °C. These findings confirm previous studies concluding that suevites contain material exposed to very diverse pressure and temperature conditions during initial shock compression and excavation but do not, as a whole, experience extreme temperatures (>1673 °C) or pressures (>30 GPa).

mineralogy↗

Distribution of Aliphatic Amines in CO, CV, and CK Carbonaceous Chondrites and Relation to Mineralogy and Processing History

The analysis of water-soluble organic compounds in meteorites provides valuable insights into the prebiotic synthesis of organic matter and the processes that occurred during the formation of the solar system. We investigated the concentration of aliphatic monoamines present in hot acid water extracts of the unaltered Antarctic carbonaceous chondrites, Dominion Range (DOM) 08006 (CO3) and Miller Range (MIL) 05013 (CO3), and the thermally altered meteorites, Allende (CV3), LAP 02206 (CV3), GRA 06101 (CV3), Allan Hills (ALH) 85002 (CK4), and EET 92002 (CK5). We have also reviewed and assessed the petrologic characteristics of the meteorites studied here to evaluate the effects of asteroidal processing on the abundance and molecular distributions of monoamines. The CO3, CV3, CK4, and CK5 meteorites studied here contain total concentrations of amines ranging from 1.2 to 4.0 nmol/g of meteorite; these amounts are 1-3 orders of magnitude below those observed in carbonaceous chondrites from the CI, CM, and CR groups. The low-amine abundances for CV and CK chondrites may be related to their extensive degree of thermal metamorphism and/or to their low original amine content. Although the CO3 meteorites, DOM 08006 and MIL 05013, do not show signs of thermal and aqueous alteration, their monoamine contents are comparable to those observed in moderately/extensively thermally altered CV3, CK4, and CK5 carbonaceous chondrites. The low content of monoamines in pristine CO carbonaceous chondrites suggests that the initial amounts, and not asteroidal processes, play a dominant role in the content of monoamines in carbonaceous chondrites. The primary monoamines, methylamine, ethylamine, and n-propylamine constitute the most abundant amines in the CO3, CV3, CK4, and CK5 meteorites studied here. Contrary to the predominance of n-x-amino acid isomers in CO3 and thermally altered meteorites, there appears to be no preference for the larger n-amines.

mineralogy↗

Apatite Nanoresponse to Acidic Dissolution

Phosphorus uptake by plants and organisms is one of the most important life-sustaining processes occurring in the critical zone (CZ). Because 95% of Earth’s reserves is relatively immobile in the form of apatite, plants and organisms rely on molecular scale solubilization process to extract available P. As the world experiences a global P shortage, influencing food production, it becomes increasingly important to understand apatite dissolution. The detailed study of chemically weathered apatite surfaces at the μm to nm-scale is key to understanding P solubilization and uptake in the CZ, allowing for better crop management and efficient fertilization. Apatite weathering is generally viewed in terms of a pH-dependent process where protons weaken atomic bonds, this leading to the disintegration of the apatite structure. A general feature of apatite weathering in acid and near neutral pH conditions is an apparent non-stoichiometric dissolution characterized by [Ca/P]aq > 1.66 in both fluorapatites (FAP) and hydroxyapatites (HAP). This process leads to the formation of a surface altered layer (SAL) with a different composition from the bulk, which many have argued is a Ca-depleted “leached layer.” We investigated apatite weathering at the nanoscale using FIB-prepared TEM-foils. Our preliminary results based on laboratory-altered FAP at ambient T and pH 3 show the formation of amorphous SALs with a maximum thickness of ~10 nm. High resolution chemical mapping and profiling using STEM-EELS and STEM-EDXS indicate that the SALs are generally, but not always, depleted in Ca and enriched in P. These results provide an alternate view of the mechanism of apatite dissolution with stoichiometric breakdown of the apatite structure, followed by the reprecipitation of an amorphous surface layer depleted in Ca. This mechanism can be described in terms of coupled interfacial dissolution-reprecipitation (CIDR), which is increasingly viewed as a universal mechanism of silicate mineral and glass dissolution. Our observation that apatite may dissolve similarly to silicates implies not only that apatite weathering may be more complex than originally thought, but also that the CIDR mechanism may extend beyond silicates.

mineralogy↗