¹M.C. Benner, ^1,5 V.R. Manga, ¹B.S. Prince, ^2,3,4L.M. Ziurys, ^1,5T.J. Zega
Geochimica et Cosmochimica Acta (in Press) Link to Article [https://doi.org/10.1016/j.gca.2025.01.012]
¹Lunar and Planetary Laboratory, University of Arizona, 1629 E. University Blvd., Tucson, AZ 85721, USA
²Department of Chemistry and Biochemistry, University of Arizona, Tucson, AZ 85721, USA
³Department of Astronomy, Steward Observatory, University of Arizona, 933 North Cherry Ave., Tucson, AZ 85721, USA
⁴Arizona Radio Observatory, Steward Observatory, University of Arizona, 933 North Cherry Ave., Tucson, AZ 85721, USA
⁵Department of Materials Science and Engineering, 1235 E. James E. Rogers Way, University of Arizona, Tucson, AZ 85721, USA
Copyright Elsevier

As the limiting element in the development of living systems, it is crucial to understand the history of phosphorus (P), from its stellar origins to its arrival on planet surfaces. A key component in this cycle is understanding the forms of P delivered to the presolar nebula and their subsequent evolution on planetary bodies, including meteorites. Here, we report on the P distribution in the Bishunpur (LL3.15), Queen Alexandra Range (QUE) 97,008 (L3.05), and Allan Hills (ALHA) 77,307 (CO3.0) chondrites to determine its origins and secondary processing in the solar protoplanetary disk and on meteorite parent bodies using a coordinated analytical approach. In support of the microstructural characterization, we used density functional theory (DFT) to calculate the Gibbs free energy of the Fe3P – Ni3P binary under non-ideal mixing conditions in its entire range of composition and temperature space and performed equilibrium condensation modeling. We identified 106P-bearing regions in these petrologic type-3 chondrites and find that the major P-bearing minerals are schreibersite ((Fe, Ni)3P) and merrillite (Ca9NaMg(PO4)7). Bishunpur predominately contains merrillite, which occurs in rims on chondrules and as hopper crystals. QUE 97008 primarily contains merrillite in association with metal and sulfides. Microstructural evaluation of merrillite in Bishunpur suggests igneous origins within the chondrule-forming region, whereas merrillite in QUE 97008 formed via condensation. In comparison, the dominant P-bearing phase in ALHA 77307 is P-bearing metal, including several Ni-rich schreibersite grains that are composed of 45 and 52.5 at. % Ni, far higher than predicted by equilibrium condensation. The equilibrium thermodynamic model, including our newly described non-ideal schreibersite solid solution, predicts the formation of a miscibility gap where (Fe0.63, Ni0.37)3P and Ni3P form via nebular condensation. We therefore suggest that Ni-rich schreibersite formed through non-equilibrium condensation.

^1,2,3Meike Fischer,^1,4Stefan T. M. Peters,^6,7Daniel Herwartz,²Paul Hartogh,¹Tommaso Di Rocco,¹Andreas Pack
Proceedings of the National Academy of Sciences (PNAS) 121, e2321070121 Open Access Link to Article [https://doi.org/10.1073/pnas.2321070121]
¹Geowissenschaftliches Zentrum, Abteilung für Geochemie und Isotopengeologie, Georg-August-Universität Göttingen, Göttingen 37077, Germany
²Max-Planck-Institut für Sonnensystemfoschung, Abteilung Planeten und Kometen, Göttingen 37077, Germany
³Thermo Fisher Scientific (Bremen) GmbH, Bremen 28199, Germany
⁴Zentrum für Biodiversitätsmonitoring & Naturschutzforschung, Leibniz-Institut zur Analyse des
⁵Biodiversitätswandels–Standort Hamburg, Hamburg 20146, Germany
⁶Institut für Mineralogie und Petrologie, Universität Köln, Köln 50674, Germany
⁷Ruhr-Universtät Bochum, Institut für Geologie, Mineralogie und Geophysik, Bochum 44801, Germany

The Moon formed 4.5 Ga ago through a collision between proto-Earth and a planetesimal known as Theia. The compositional similarity of Earth and Moon puts tight limits on the isotopic contrast between Theia and proto-Earth, or it requires intense homogenization of Theia and proto-Earth material during and in the aftermath of the Moon-forming impact, or a combination of both. We conducted precise measurements of oxygen isotope ratios of lunar and terrestrial rocks. The absence of an isotopic difference between the Moon and Earth on the sub-ppm level, as well as the absence of isotope heterogeneity in Earth’s upper mantle and the Moon, is discussed in relation to published Moon formation scenarios and the collisional erosion of Theia’s silicate mantles prior to colliding with proto-Earth. The data provide valuable insights into the origin of volatiles in the Earth and Moon as they suggest that the water on the Earth may not have been delivered by the late veneer. The study also highlights the scientific value of samples returned by space missions, when compared to analyses of meteorite material, which may have interacted with terrestrial water.