^1,2Martin Bizzarro,^1,3Anders Johansen,⁴Caroline Dorn
Nature Reviews Chemistry 9, 378–396 Link to Article [DOI https://doi.org/10.1038/s41570-025-00711-9]
¹Centre for Star and Planet Formation, Globe Institute, University of Copenhagen, Copenhagen, Denmark
²Institut de Physique du Globe de Paris, Université de Paris, Paris, France
³Lund Observatory, Department of Astronomy and Theoretical Physics, Lund University, Lund, Sweden
⁴ETH Zurich, Institute for Particle Physics and Astrophysics, Zurich, Switzerland

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^1,2Ritesh Kumar Mishra,³Kuljeet Kaur Marhas,⁴Justin Ibrahim Simon,⁵Yves Marrocchi,⁵Johan Villeneuve
Meteoritics & Planetary Science (in Press) Link to Article [https://doi.org/10.1111/maps.70062]
¹Independent Researcher, Dhawalpur, India
²Veer Kunwar Singh University, Ara, India
³Planetary Sciences Division, Physical Research Laboratory, Ahmedabad, India
⁴Astromaterials Research and Exploration Science Division, NASA-Johnson Space Center, Houston, Texas, USA
⁵Centre de Recherches Pétrographiques et Géochimiques, Nancy, France
Published by arrangement with John Wiley & Sons

Ordinary, enstatite, and Rumuruti type have the lowest abundance of refractory inclusions amongst chondritic meteorites. Calcium-aluminum-rich inclusions (CAIs) within these are hallmarked by a relatively small average diameter of ~45 μm (size range 4–382 μm). One CAI, one amoeboid olivine aggregate (AOA), one spinel-bearing chondrule, and two aluminum-rich chondrules from Semarkona (LL3.00) along with one CAI each from Allan Hills (ALHA) 81251 (LL3.2) and Chainpur (LL3.4) were identified following an extensive search. These objects were studied for their petrography, mineral chemistry, relative (26Al) chronology, and three oxygen isotopic compositions. The initial 26Al/27Al ratio of (4.96 ± 0.14) × 10−5 (2σ) in a type A CAI in Chainpur, the largest size (1500 × 1200 μm) found so far in the noncarbonaceous (ordinary) chondrites, forming in an 16O-rich early solar system reservoir (Δ17O = −24‰) is consistent with previous studies. The Chainpur CAI 1 has a Wark–Lovering rim, the first reported case within the noncarbonaceous chondrites. The hibonite–pyroxene spherule in ALHA81251 (CAI 1) is the first reported case of a hibonite–pyroxene spherule in the ordinary chondrites of these rare objects (~12 known so far) within meteorites. The hibonite–pyroxene spherule in ALHA81251 has a low abundance of 26Al/27Al ratio of (1.2 ± 0.6) × 10−5 with Δ17O of ~ −14.5‰ ± 2.0‰. An olivine-phyric Al-rich chondrule in Semarkona (Ch 54) formed at ~0.9 Ma with Δ17O of ~0‰, while Semarkona (Ch 44) formed in a relatively 16O-rich reservoir with Δ17O of ~ −2.0‰. The spinel-bearing chondrule in Semarkona (Ch 205) shows no resolved excess in Δ26Mg and has a planetary-like oxygen isotopic composition. Oxygen isotope composition and 26Al-26Mg relative chronology of these objects confirm their origin and evolution under cosmochemical conditions similar to their “typical” carbonaceous kindred and extend the knowledge of the cosmochemical environment in the early solar system.

¹Takumi Miura,²Hidenori Terasaki,^2,3Hyu Takaki,²Kotaro Kobayashi,⁴Geoffrey David Bromiley,²Takashi Yoshino
Meteoritics & Planetary Science (in Press) Open Access Link to Article [https://doi.org/10.1111/maps.70068]
¹Department of Earth and Space Science, Osaka University, Osaka, Japan
²Department of Earth Sciences, Okayama University, Okayama, Japan
³Institute for Planetary Materials, Okayama University, Tottori, Japan
⁴School of Geosciences, The University of Edinburgh, Edinburgh, UK
Published by Arrangement with John Wiley & Sons

During precursor stages of planet formation, many planetesimals and planetary embryos are considered to have differentiated, forming an iron-alloy core and silicate mantle. Percolation of liquid iron-alloy in solid silicates is one of the major possible differentiation processes in these small bodies. Based on the dihedral angles between Fe-S melts and olivine, a criterion for determining whether melt can percolate through a solid, it has been reported that Fe-S melt can percolate through olivine matrices below 3 GPa in an oxidized environment. However, the dihedral angle between Fe-S melts and orthopyroxene (opx), the second most abundant mineral in the mantles of small bodies, has not yet been determined. In this study, high-pressure and high-temperature experiments were conducted under the conditions of planetesimal and planetary embryo interiors, 0.5–5.0 GPa, to determine the effect of pressure on the dihedral angle between Fe-S melts and opx. Dihedral angles tend to increase with pressure, although the pressure dependence is markedly reduced above 4 GPa. The dihedral angle is below the percolation threshold of 60° at pressures below 1.0–1.5 GPa, indicating that percolative core formation is possible in opx-rich interiors of bodies where internal pressures are lower than 1.0–1.5 GPa. The oxygen content of Fe-S melt decreases with increasing pressure. High oxygen contents in Fe-S melt reduce interfacial tension between Fe-S melt and opx, resulting in reduced dihedral angles at low pressure. Combined with previous results for dihedral angle variation of the olivine/Fe-S system, percolative core formation possibly occurs throughout bodies up to a radius of 1340 km for an olivine-dominated mantle, and up to 770 km for an opx-dominated mantle, in the case of S-rich cores segregating under relatively oxidizing conditions. For mantles of small bodies in which abundant olivine and opx coexist, the mineral with the largest volume fraction and/or smallest grain size will allow formation of interconnected mineral channels, and, therefore, the wetting property of this mineral determines the wettability of the melt, that is, controls core formation.

¹A.R.Russell et al. (>10)
Journal of Geophysical Reserac (Planets)(in Press) Open Access Link to Article [https://doi.org/10.1029/2025JE009244]
¹Arizona State University, Tempe, AZ, USA
Published by arrangement with John Wiley & Sons

The Martian surface preserves evidence of a global climate transition from wetter to drier conditions, but the nature of the fluids involved in this evolution remains poorly constrained. In Gale crater, the clay-sulfate transition and presence of evaporite mineral assemblages can provide insights into the properties of these fluids and the timing of environmental change. While traversing through the Chenapau member of the sulfate-bearing unit in Gale crater, the Curiosity rover encountered a set of dark-toned veins enriched in Na and Cl, suggestive of halite. However, previous halite detections in Gale crater have been limited to occurrences along the edges of Ca-sulfate veins or nodules, suggesting a unique origin for this set of veins. Here, we hypothesize that these veins formed through the infiltration of saline fluids along pre-existing hydraulically induced fractures. These fluids permeated into the host rock beyond the primary fractures, precipitating halite and cementing the fractures. Using Mastcam and ChemCam spectra, we found that the veins displayed a downturn in the near-infrared wavelengths, consistent with the presence of ferrous iron. Furthermore, textural analysis of the veins reveals host rock material preserved within the veins. ChemCam laser-induced breakdown spectroscopy observations also support the presence of a minor Fe component in the veins and halite concentrated along the center of the fractures. Our results demonstrate that these veins represent a distinct class of diagenetic features in Curiosity’s mission that record an important transition in near-surface fluid chemistry consistent with a transition to a drier environment.

¹Lars E. Borg, ¹Thomas S. Kruijer, ¹Ming-Chang Liu, ^1,2Autumn G. Roberts, ¹Josh Wimpenny, ¹Ouyanatu N.Z. Maina, ¹Joseph Boro, ¹Charles K. Shearer, ^1,4Kyle M. Samperton
Geochimica et Cosmochimica Acta (in Press) Link to Article [https://doi.org/10.1016/j.gca.2025.10.028]
¹Cosmochemical & Isotopic Signatures Group, Lawrence Livermore National Laboratory, 7000 East Avenue L-231, Livermore, CA 94550, USA
²Geological Sciences, University of Colorado, Boulder, CO 80309, USA
³Department of Earth and Planetary Science, Institute of Meteoritics, University of New Mexico, Albuquerque, NM 87131, USA
⁴Trace Nuclear Measurement Technology Group, Savannah River National Laboratory, Aiken SC 29802 USA
Copyright Elsevier

Temporal relationships among the three most common suites of lunar crustal rocks have been investigated by obtaining new high precision ages on Felsic/Alkali-suite Quartz monzodiorite Clast B from breccia 15405 and Magnesian-suite norite 78235/6/8/55/56 and comparing them to previously dated ferroan anorthosite sample 60025. The weighted average age of 4337.19 ± 0.49 Ma of 15405 Clast B is defined by zircon U-Pb and Pb-Pb ages as well as mineral isochron Sm-Nd and Nd-Nd ages. It is identical to the weighted average age for Apollo 17 norite 78235/6/8/55/56 of 4334.1 ± 3.5 Ma which is defined by Pb-Pb ages measured on baddeleyites in this investigation and less precise Pb-Pb and Sm-Nd ages reported in the literature. Both ages are ∼ 25 Ma younger than the weighted average of Sm-Nd and Pb-Pb ages reported in the literature on ferroan anorthosite 60025 of 4359.3 ± 2.3 Ma. The fact that ages of all three samples are defined by multiple U-Pb, Pb-Pb, Sm-Nd, and 142Nd-143Nd chronometers provide confidence that they record the igneous crystallization history of the samples and do not represent disturbances or mixing lines with no temporal significance.
The extent to which these three ages represent broader scale magmatism is difficult to evaluate. Nevertheless, the age defined for 15405 Clast B, 78235/6/8/55/56, and 60025 are contemporaneous with the peak of ages observed in detrital zircons from the Apollo 12, 14, 15, and 17 landing sites (4340 ± 20 Ma), a Mg-suite Sm-Nd whole rock isochron defined by samples from Apollo 14, 15, 16, and 17 landing sites (4348 ± 25 Ma), and a Ferroan Anorthosite-suite Sm-Nd whole rock isochron defined by samples from the Apollo 15 and 16 landing sites (4354 ± 29 Ma). This implies that Ferroan Anorthosite-suite magmatism is temporally distinct and earlier than magmatism associated with the Mg-suite and the Felsic/Alkali-suite, as predicted by the lunar magma ocean model of lunar differentiation. The short 35 ± 10 Ma interval between primary ferroan anorthosite magmatism and secondary magmatism suggests that the lunar crust formed over a limited period of time. Although heat from decay of long-lived isotopes, large impacts, tidal heating associated with interactions between the Earth and Moon, and density driven overturn of the magma ocean have all been invoked to explain production of ancient secondary crustal magmatism, only tidal heating and cumulate overturn are consistent with the apparent short duration of secondary crustal magmatism and the great depth of crystallization implied for some Mg-suite samples.
The initial ε143Nd values derived from the 15405 Clast B and 78238 Mg-suite norite isochrons, as well as a Mg-suite whole rock isochron are −0.23 ± 0.11, −0.27 ± 0.74, and −0.25 ± 0.09, respectively. They are identical within uncertainty indicating that Mg-suite and Felsic/Alkali-suite magmas were derived from materials that had the same time averaged Sm/Nd ratios since the formation of the solar system. This, combined with the contemporaneous nature of 15405 Clast B and 78235/6/8/55/56 Mg-suite norite, is consistent with evolution of both samples, and likely both magma suites, from a common source through closed system fractional crystallization or partial melting processes.

¹Rainer Wieler,¹Donald S. Burnett
ACS Earth and Space Chemistry 9, 1142-1151 Link to Article [https://doi.org/10.1021/acsearthspacechem.5c00009]
¹Department of Earth and Planetary Sciences, ETH Zürich, 8092 Zürich, Switzerland
²Division of Geological and Planetary Sciences, California Institute of Technology, Pasadena, California 91125, United States

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¹Ashwani Raju, ²Saraah Imran, ¹Jiwantika Kumari, ¹Ankit Kumar, ³Ramesh P. Singh
Advances in Space Research 76, 1172-1195 Link to Article [https://doi.org/10.1016/j.asr.2025.04.079]
¹Remote Sensing & GIS Lab., Department of Geology, Institute of Science, Banaras Hindu University, Varanasi 221005 Uttar Pradesh, India
²Department of Earth Sciences, Indian Institute of Technology Roorkee, Roorkee 247667 Uttarakhand, India
³School of Life and Environmental Sciences, Schmid College of Science and Technology, Chapman University, Orange, United States

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¹Juulia-Gabrielle Moreau, ¹Argo Jõeleht, ^2,3Anna Losiak, ⁴Meng-Hua Zhu, ¹Jüri Plado
Icarus (in Press) Link to Article [https://doi.org/10.1016/j.icarus.2025.116856]
¹Department of Geology, University of Tartu, Ravila 14A, 50411 Tartu, Estonia
²Institute of Geological Sciences, Polish Academy of Sciences, Podwale 75, PL-50449 Wroclaw, Poland
³Lunar and Planetary Institute, Houston, USA
⁴State Kay Laboratory of Lunar and Planetary Sciences, Macau University of Science and Technology, Taipa, Macau, China
Copyright Elsevier

Sedimentary rocks often form the upper layers or the entire target rocks in impact events. Thermodynamic properties of sedimentary rocks related to porosity and water saturation affect the process of impact crater formation. The heterogeneous distribution of sedimentary facies can complicate the development and distribution of shock effects, especially in numerical modeling. This work focuses on the shock thermodynamic properties of carbonate rocks with differing porosity textures (e.g., isolated pores, interstitial porosity, elongated pores) and water saturation levels. Using mesoscale numerical modeling, we found that water saturation reduces shock temperatures compared to those in dry, porous carbonate rocks. The orientation of elongated pores and porosity lineations influences the shock temperature distribution and rock deformation at angles of 50–90° to the shock front. Additionally, due to complex shock wave interactions, interstitial porosity is key in creating temperature zonations around larger grains.

¹Rui Tahara et al. (>10)
Meteoritics & Planetary Science (in Press) Open Access Link to Article [https://doi.org/10.1111/maps.70066]
¹Japan Aerospace Exploration Agency, Sagamihara, Japan
Published by arrangement with John Wiley & Sons

NASA’s OSIRIS-REx mission successfully collected and returned ~121.6 g of bulk samples from the B-type, near-Earth asteroid (101955) Bennu to Earth in September 2023. Upon returning to Earth, the samples were transported to the NASA Johnson Space Center where most of the samples have been stored and processed. On August 22, 2024, 0.5 wt% of Bennu samples (0.663 g) and a contact pad that collected particles from the surface of Bennu were permanently transferred to JAXA from NASA based on a Memorandum of Understanding and a letter of agreement between the two agencies. Following this, all the Bennu samples have been curated under nitrogen-purged gloveboxes, called clean chambers in a clean room at the Extraterrestrial Sample Curation Center in Sagamihara. While maintaining the pristinity of samples at the curation, we conduct a series of nondestructive analyses, including near-infrared spectroscopy within the clean chambers. Bennu curation was conceptualized primarily based on the Hayabusa2 curation, whereas lessons learned from the Hayabusa2 curation were integrated into designing Bennu curation. Here, we describe preparations for the Bennu curation, with an emphasis on the differences from the Hayabusa2 curation.

^1,2,3Xuhang Zhang et al. (>10)
Earth and Planetary Science Letters 671, 119666 Open Access Link to Article [https://doi.org/10.1016/j.epsl.2025.119666]
¹Key Laboratory of Earth and Planetary Physics, Institute of Geology and Geophysics, Chinese Academy of Sciences, Beijing 100029, China
²Key Laboratory of Earth and Planetary Physics, Institute of Geology and Geophysics, Chinese Academy of Sciences, Beijing 100029, China
³Institute of Geology and Geophysics, Chinese Academy of Sciences, Beijing 100029, China
Copyright Elsevier

Understanding the elemental and isotopic composition of the Sun is key to reconstructing planetary formation, atmospheric evolution and solar activity over time. Noble gases from solar wind implanted into lunar regolith provide a unique archive of solar history, but their interpretation is complicated by implantation uncertainties and secondary processes (e.g., diffusion, regolith gardening, solar and galactic cosmic ray exposure). Here we report the isotopic composition of the noble gases (helium, neon, and argon) in thirty six high-purity plagioclase grains from Chang’e-5 lunar soil to assess the preservation of implanted solar wind in lunar materials. Compared with plagioclase from several Apollo sites, the grains retain a more pristine solar wind record, revealing a dynamic equilibrium between solar wind and cosmic ray irradiation and intense diffusive loss driven by localized heating likely due to micro-impacts or temperature gradients at the lunar surface. These coupled mechanisms explain the observed inter-grain He/Ne/Ar variations. Our data further indicate that kinetic diffusion during solar wind implantation, rather than post-implantation alteration, is the primarily driver of elemental fractionation relative to original solar wind values in plagioclase. Collectively, these findings reveal pathways of solar wind-driven noble gas retention and loss in lunar materials and further accounts for the presence of solar wind-derived He and Ne in the lunar exosphere. They also underscore the need to correct for process-related modifications when reconstructing past solar wind compositions, thereby enabling improved inference of solar evolution, planetary volatiles origins, and the initial solar nebula composition.