¹Ralph E. Milliken et al. (>10)
Meteoritics & Planetary Science (in Press) Open Access Link to Article [https://doi.org/10.1111/maps.70179]
¹Department of Earth, Environmental and Planetary Sciences, Brown University, Providence, Rhode Island, USA
Published by arrangement with John Wiley & Sons

Near-Earth rubble-pile asteroids Bennu and Ryugu are part of the carbonaceous taxonomic complex (C-complex), and samples returned from both bodies resemble the most aqueously altered carbonaceous chondrites. However, telescopic and spacecraft visible–near infrared (VIS–NIR) reflectance spectra of Ryugu exhibit a red (positive) spectral slope, whereas Bennu has a blue (negative) spectral slope characteristic of the rare B-type subclass of asteroids. The asteroid spectra also suggest different levels of hydration, with Ryugu dominated by OH and Bennu containing spectral evidence of more H2O. To understand what causes these differences, we acquired VIS–NIR reflectance data (~0.3–5 μm) from a variety of Bennu samples over spatial scales of 100 μm to several millimeters. No single sample reproduces the average spectral properties of Bennu, but by evaluating samples of different petrology and physical states—groups of particles, isolated particles, and larger stones—we demonstrate that primary composition, and highly hydrated Mg-rich phosphate in particular, plays a strong role in controlling the spectral slope and average hydration absorption strength of Bennu materials. Bennu and Ryugu may be dominated by different lithologies originating from different regions of a common planetesimal, thus explaining their different spectral evolution. The spectral characteristics of B-type asteroids, particularly those with blue slopes at near-infrared wavelengths and broad hydration features at ~3 μm, may indicate the presence of Mg phosphate and thus a history of complex fluid–rock interactions relevant to prebiotic chemistry.

^1,2,3Rachael Lappan,^3,4Rachel S. Kirby,⁴Andrew G. Tomkins
Meteoritics & Planetary Science (in Press) Open Access Link to Article [https://doi.org/10.1111/maps.70178]
¹Department of Microbiology, Biomedicine Discovery Institute, Monash University, Melbourne, Victoria, Australia
²Securing Antarctica’s Environmental Future, Monash University, Melbourne, Victoria, Australia
³School of Earth, Atmosphere and Environment, Monash University, Melbourne, Victoria, Australia
⁴Space Science and Technology Centre, School of Earth and Planetary Science, Curtin University, Perth, Western Australia,Australia
Published by arrangement with John Wiley & Sons

Since the discovery of nine meteorites near the Yamato mountains in 1969, Antarctica has been recognized as a superb location for meteorite recovery. While Antarctic recovery expeditions prioritize meteorite preservation for mineralogical and planetary studies, meteorites are not typically collected for biological applications. The LifeMet expedition was the first Australian Antarctic meteorite recovery expedition, conducted in the 2024–2025 austral summer in the Wohlthat and Orvin Mountains in Dronning Maud Land, Antarctica. The expedition had two primary objectives: (1) to examine whether Antarctic microorganisms colonize and consume nutrients from meteorites, providing insights into microbial ecosystem formation, interactions with uncommon minerals and extremophile survival strategies in Antarctica; and (2) to evaluate the practical and logistical factors influencing meteorite recovery in these regions, and the suitability of recovery approaches for biological sampling. A total of 13 stones, including one confirmed meteorite, were recovered. Adjacent environments (air, sediment, snow, ice, and terrestrial rocks) were sampled to characterize microbial sources. We found that low-altitude blue ice zones were poorly suited to meteorite recovery; however, microbe–meteorite interactions may be enhanced in these areas due to warmer temperatures and periodic ice melting. Our observations suggest that the low albedo of meteorites may promote the formation of periodically water-filled potholes and cryoconite, which may support microbial proliferation. In contrast, meteorites stranded on nunataks are minimally oxidized. Based on our observations at ~71°S, blue ice fields at altitudes above ~2000 m are better suited to meteorite recovery at current climatic conditions.

¹Kanako Yoshihara,²Akira Yoshiasa,³Huimin Shao,⁴Makoto Tokuda,⁵Ginga Kitahara,²Hiroshi Isobe
Meteoritics & Planetary Science (in Press) Open Access Link To Article [https://doi.org/10.1111/maps.70180]
¹Graduate School of Science and Technology, Kumamoto University, Kumamoto, Japan
²Department of Earth and Environmental Sciences, Faculty of Advanced Science and Technology, Kumamoto University,Kumamoto, Japan
³Chinese National Space Science Center, Beijing, China
⁴Institute of Industrial Nanomaterials, Kumamoto University, Kumamoto, Japan
⁵Institute of Materials Structure Science, High Energy Accelerator Research Organization, Tokai, Ibaraki, Japan
Published by arrangement with John Wiley & Sons

Ni, Co, and Fe K-edge X-ray absorption fine structure (XAFS) measurements were performed, revealing an unexpected local structure around Co in well-known iron and stony-iron meteorites. Cobalt is enriched in kamacite but remains in taenite at concentrations of at least 0.3 atom%. The Co K-edge X-ray absorption near-edge structure (XANES) spectra of taenite with a face-centered cubic (FCC) structure in all examined iron meteorites exhibited an unexpected body-centered cubic (BCC)-type local coordination, with Co showing a coordination number of 8 + 6. The local FCC and BCC structures can be clearly distinguished based on their XANES patterns. In taenite, up to 20% of the local structure is inferred to be BCC in regions where three-dimensional periodicity is maintained. Moreover, local BCC structures are likely to predominate in subregions that do not contribute to three-dimensional periodicity. Co transforms into a locally ordered BCC structure within the high-temperature parent FCC phase of iron meteorites. In this phase, Co appears to have a stronger affinity for Fe than for Ni, leading to the formation of Co-Fe clusters with a regular BCC arrangement.

^1,2,3,5Hongmei Yang, ^1,2,3Xiaoju Lin, ^1,2,3Xiao Wu, ^1,2,3,4Haiyang Xian, ^1,2,3,4Jianxi Zhu, ^1,2,3,4Shan Li, ^1,2,3Jiaxin Xi, ^1,2,3Yiping Yang, ^1,2,3,4Hongping He
Icarus (in Press) Link to Article [https://doi.org/10.1016/j.icarus.2026.117209]
¹State Key Laboratory of Deep Earth Processes and Resources, Guangzhou Institute of Geochemistry, Chinese Academy of Sciences, Guangzhou 510640, China
²Center for Advanced Planetary Science, Guangzhou Institute of Geochemistry, Chinese Academy of Sciences, Guangzhou 510640, China
³Guangdong Provincial Key Laboratory of Mineral Physics and Materials, Guangzhou Institute of Geochemistry, Chinese Academy of Sciences, Guangzhou 510640, China
⁴University of Chinese Academy of Sciences, Beijing 100049, China
⁵Guangzhou Institute of Energy Conversion, Chinese Academy of Sciences, Guangzhou 510640, China
Copyright Elsevier

Impact is one of the most crucial geological processes on the lunar surface. As the main mafic mineral in lunar mare basalts, pyroxene can be transformed into an amorphous phase under the high-temperature and high-pressure conditions triggered by impact events. However, the formation mechanism of impact-induced pyroxene glass and its implications for the impact history of the lunar surface have yet to be elicited. In this study, we investigated the formation mechanism of augite glass from a Chang’e-5 breccia using the electron pair distribution function and molecular dynamics simulations. The results show that the augite transformed into dense melt under the high-temperature and high-pressure conditions induced by impact, with subsequent quenching leading to glass formation. Atomic structural analysis indicates that the augite dense melt solidified at a temperature of approximately 4100 K and a residual pressure of about 10 GPa. The mosaicization of this augite glass in the breccia clasts indicates that it had experienced a later impact event with a shock intensity of M-S2 after its formation. By establishing the link between the atomic structure of augite glass and its formation pressure-temperature conditions, this study provides a robust method for inverting impact parameters from natural lunar glass samples. It also offers a new perspective for deciphering the multi-stage impact history of the lunar surface and the evolutionary processes of lunar regolith, and holds universal reference value for studies of impact processes on the Moon and other terrestrial planets.

¹Guillaume Leseigneur, ²Manuel Reinhardt, ¹Fatma Yesil Sahan, ³Uwe Meierhenrich
Earth and Planetary Science Letters 690, 120141 Open Access Link to Article [https://doi.org/10.1016/j.epsl.2026.120141]
¹Max-Planck-Institute for Solar System Research; Justus-von-Liebig-Weg 3, 37077 Göttingen, Germany
²University of Göttingen, Geoscience Center, Department of Geobiology; Goldschmidtstraße 3, 37077 Göttingen, Germany
³Institut de Chimie de Nice (ICN), UMR 7272 CNRS, Université Côte d’Azur; 28 Avenue Valrose, 06108 Nice, France
Copright Elsevier

The isoprenoid alkanes pristane and phytane are widely detected in meteorites. As isoprenoids are considered markers of Earth’s biosphere, their presence in meteorites has led to a prevailing consensus that they represent terrestrial contamination, thereby calling into question the indigeneity of the entire meteoritic hydrocarbon inventory. Indeed, these chiral molecules are ubiquitous in biological systems, where their stereogenic centers are fixed and of the same absolute configuration. In this study we separate, for the first time, the different relevant chiral configurations of pristane and phytane in a meteorite sample, and we show that the isoprenoid alkanes detected in the Murchison meteorite are racemic. On Earth, racemization of these molecules has only been observed in oil shales and crude oils subjected to a certain degree of thermal maturation. In light of previous findings, these results strongly suggest that the Murchison meteorite was contaminated exclusively by petroleum pollutants present in Earth’s atmosphere, and categorically exclude any contribution from the biosphere at the fall site. Consequently, this work establishes a foundation for systematic investigations into the chirality of isoprenoids in other meteorite samples and the different sources of atmospheric petroleum pollution.

¹Line Colin, ¹Stéphane Labrosse, ¹Chloé Michaut, ²Adrien Morison
Earth and Planetary Science Letters 690, 120164 Open Access Link to Article [https://doi.org/10.1016/j.epsl.2026.120164]
¹Laboratoire de Géologie de Lyon: Terre, Planète, Environnement, Ecole Normale Supérieure de Lyon, Université de Lyon, Université Claude Bernard Lyon 1, Lyon,France
²Research Software Engineering, MVLS SRF, University of Glasgow, Glasgow,United Kingdom
Copyright Elsevier

The Moon presents a striking asymmetry between the nearside, which concentrates the lunar mare and shows a thin crust, and the farside, composed of thick anorthosite terranes. One proposed explanation for this asymmetry is a mantle overturn, driven by the instability of a dense, ilmenite-rich layer at the top of cumulates near the end of lunar magma ocean solidification. However, thermal instabilities may arise before the crystallization of this dense layer. In particular, material exchange by melting and crystallization at the magma ocean-cumulates boundary facilitates flow through the boundary and hence the onset of convection in the cumulates. Accounting for this flow-through interface, we investigate the onset and duration of a thermal overturn using linear stability analysis and direct numerical simulations. Our results show that a thermal overturn can initiate well before the end of magma ocean solidification, lasting from ten thousand years to tens of millions of years. The dominant convective mode corresponds to a spherical harmonic of degree one and could affect crustal growth and stabilization if the top interface is sufficiently flow-through and the Rayleigh number not too large. Taking into account the thermal evolution of the core, this early overturn could generate an early lunar dynamo.

^1,2Xiaofeng Lu, ³Olivier Namur, ¹Yongjiang Xu, ⁴Bernard Charlier, ¹Yanhao Lin
Earh and Planetary Science Letters 690, 120123 Open Access Link to Article [https://doi.org/10.1016/j.epsl.2026.120123]
¹Lin Earth and Planetary Laboratory, Center for High pressure Science and Technology Advanced Research, Beijing, 100193, China
²School of Earth Sciences and Resources, China University of Geosciences, Beijing, 100083, China
³Earth and Environmental Sciences, KU Leuven, 3001, Leuven, Belgium
⁴Department of Geology, University of Liège, 4000, Sart Tilman, Belgium
Copyright Elsevier

Chemical data from the MESSENGER spacecraft reveal that Mercury’s lavas are unusually sulfur-rich, suggesting highly reduced conditions during their formation. As a major volatile, sulfur profoundly affects the physical and chemical properties of silicate melts, potentially impacting key processes such as magma ocean crystallization and mantle melting. Here we conducted near-liquidus experiments (1650–2000 °C and 3–5 GPa) to quantify the effect of sulfur on phase relations in olivine- and orthopyroxene-saturated mafic compositions representative of Mercury’s mantle. Our results show that elevated sulfur contents (up to 6 wt.% S) can depress the liquidus of Mercurian mantle by up to 200 °C. The liquidus depression of silicate melt is positively correlated with sulfur concentrations, negatively correlated with pressure, and compositionally-sensitive with a larger S-effect on higher Mg/Si melt. Using a newly developed parameterization for sulfur-bearing melting, we show that the mantle potential temperatures required to produce the volcanic provinces are lower than previously estimated. Furthermore, modeling of magma ocean cooling and crystallization dynamics indicates that sulfur-induced liquidus depression can extend solidification timescales by tens to hundreds to thousands of years, especially beneath an insulating graphite crust (>100 m). Using viscosity models, we find that sulfur also reduces the critical crystal size for settling, thus promoting fractional crystallization and formation of a chemically stratified mantle. These findings provide critical constraints on Mercury’s interior structure and show that sulfur lowers the solidus and liquidus, enhances melt production, and helps to explain Mercury’s fertile mantle, extensive crustal formation, and diverse surface lavas.

¹Ioana-Bogdana Radu, ¹Cécile Deligny, ¹Henrik Skogby, ²Roland Stalder, ¹Jeremy J. Bellucci, ¹Martin J. Whitehouse
Geochimica et Cosmochimica Acta (in Press) Open Access Link to Article [10.1016/j.gca.2026.06.002]
¹Department of Geosciences, Swedish Museum of Natural History, Box 50007, SE-104 05 Stockholm, Sweden
²Institut für Mineralogie und Petrographie, Universität Innsbruck, Innsbruck 6020, Austria
Copyright Elsevier

Water on Mars has traditionally been estimated from hydrogen contents in melt inclusions and apatite, yet these may not account for magma degassing or post-crystallization dehydration. Pyroxenes offer an alternative approach, as they incorporate trace amounts of water during crystallisation via charge-balancing structural defects, that are retained after dehydration enabling experimentally reversing water loss and constraining magmatic water contents. Here we report the first hydrothermal rehydration experiments on pyroxene from both nakhlites and shergottites. The treated nakhlite augites contain 140‒185 ppm H2O, consistent with previous values for Nakhla (130 ± 26 ppm) and within the range of terrestrial basaltic pyroxene. Using clinopyroxene-melt partition coefficients, this corresponds to 1.59 ± 0.03‒1.83 ± 0.10 wt% average H2O in the nakhlite magma, slightly higher than previous estimates (0.69‒1.42 wt% H2O). The complex hydrothermal history of nakhlites, including evidence for magmatic degassing and interaction with H2O-poor, Cl-rich fluids, suggests these estimates may represent minimum values of the nakhlite magmatic water content. Assuming a low degree of partial melting, the nakhlite mantle source is expected to contain 80‒91 ppm H2O, overlapping previous estimates (59‒184 ppm), and comparable to Earth’s MORB mantle (54‒330 ppm). This is consistent with a common magmatic source for all nakhlites, and broadly consistent with water estimates for the chassignite mantle source (39‒252 ppm), suggesting that any exogenous fluid assimilation had a negligible effect on the net water budget. In contrast, shergottite pigeonites show no detectable water by Fourier Transform Infrared Spectroscopy, consistent with expected water contents of ∼ 2‒11 ppm H2O derived from published source compositions for depleted and enriched shergottites. Together, these results refine our understanding of Martian magmatic water content, consistent with a common, more water-rich mantle source for nakhlites, distinct from the more heterogeneous and generally drier shergottite mantle reservoirs

¹S. A. Singerling
Meteoritics & Planetary Science (in Press) Open Access Link to Article [https://doi.org/10.1111/maps.70177]
¹Schwiete Cosmochemistry Laboratory, Goethe University, Frankfurt, Germany
Published by arrangement with John Wiley & Sons

This study documents micro- to nanoscale observations of primary nebular and secondary parent body iron sulfides in the CR1 GRO 95577. Despite the extensive alteration of the bulk sample, some primary sulfides managed to avoid alteration, having originally formed in the solar nebula during chondrule formation by either fission-sulfidization or crystallization. Secondary sulfides formed by precipitation from a fluid during aqueous alteration on the parent body and show features such as lath-like or euhedral morphologies, fine-scale intergrowths with serpentine, and porosity in pyrrhotite. Microstructures in pentlandite are most consistent with formation via impact-induced shock. Experiments have the potential to better constrain the effects of shock on pentlandite. Given pentlandite’s ubiquity in both minimally and heavily altered meteorites, it has the potential to be used as a shock indicator for samples otherwise ill-suited to shock determination (i.e., heavily aqueously altered materials).

^1,2Jennifer T. Mitchell,^3,4Natasha R. Stephen,¹Zsuzsanna P. Allerton,¹Weiming Ding, Xin-Yuan Zhe
Meteoritics & Planetary Science (in Press) Open Access Link to Article [https://doi.org/10.1111/maps.70181]
¹N.H. Winchell School of Earth & Environmental Sciences, University of Minnesota, 116 Church St SE, Minneapolis,Minnesota, 55455, USA
²Characterization Facility, University of Minnesota, 100 Union St, Minneapolis, Minnesota, 55455, USA
³The Geological Society of London, Burlington House, Picadilly, London, W1J 0BG, UK
⁴Department of Earth Science & Engineering, Imperial College London, Exhibition Road, London, SW7 2AZ, UK
Published by arrangement with John Wiley & Sons

This study provides an initial characterization of Stardust Mine, a fresh gabbroic enriched shergottite collected in Arizona, USA, in September 2024 and is the first Martian meteorite to be unequivocably collected on US soil. Analysis was conducted on the type specimen and finds that Stardust Mine is composed of equal proportions of pyroxene and maskelynite, with large Fe-Ti oxides and phosphates. Ti/Al ratios and two-pyroxene thermometry of the most primitive pyroxenes (Mg# >57), inferred to represent preplagioclase pyroxene crystallization, give an estimated minimum initial crystallization depth of ~40 km at ~1140°C. Sector zoning is restricted to these pyroxenes and may have developed through magmatic undercooling in response to magma ascent before storage in a staging chamber in the volcanic system. Pyroxene and plagioclase cocrystallized for almost the entirety of the crystallization sequence with evolving melt compositions, followed by phosphates and Fe-Ti oxides. Ilmenite-titanomagnetite pairs and D(Cr)pyroxene suggest the magma was relatively oxidized (fO2 ΔQFM −1.3) compared with other shergottites. Accumulation and crystal settling in a sill, dyke, or intracrustal magma chamber allowed the development of a shape-preferred orientation and decomposition of metastable pyroxenes to three-phase symplectites. Stardust Mine represents a highly fractionated lithology that extends the range of high-Al basaltic shergottites to ~8 wt% Al. Our analysis does not find a clear pairing with shergottites in literature in lieu of radiogenic isotope data, and Stardust Mine may therefore represent a previously unsampled lithology.