¹L. E. McGraw, ¹C. A. Thomas, ¹J. P. Emery, ²A. S. Rivkin
The Planetary Science Journal, 7, 55 Open Source Link to Article [DOI: 10.3847/PSJ/ae3de0]
¹Department of Astronomy and Planetary Science, Northern Arizona University, PO Box 6010, Flagstaff, AZ 86011, USA
²JHU/APL, 211100 Johns Hopkins Road, Laurel, MD 20723, USA

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¹Helena C. Bates, ¹Ashley J. King, ²Kerri L. Donaldson Hanna, ^2,3Audrey C. Martin, ⁴Joshua P. Emery, ⁵Neil E. Bowles, ¹Sara S. Russell
The Planetary Science Journal, 7, 90 Open Source Link to Article [DOI: 10.3847/PSJ/ae5931]
¹Natural History Museum, Cromwell Road, London, SW7 5BD, UK
²University of Central Florida, Orlando, FL 32816, USA
³California Institute of Technology, Pasadena, CA 91125, USA
⁴Northern Arizona University, Flagstaff, AZ 86011, USA
⁵Oxford University, Oxford, OX1 3PU, UK

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^1,2Max Mahlke (>10)
The Planetary Science Journal, 7, 114 Open Source Link to Article [DOI: 10.3847/PSJ/ae6643]
¹Institut d’Astrophysique Spatiale, Université Paris-Saclay, CNRS, F-91405 Orsay, France
²Université Marie et Louis Pasteur, CNRS, Institut UTINAM (UMR 6213), F-25000 Besançon, France

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^1,2Nicole M. Ozdowski, ¹Ian J. Marrs, ^1,2Max A. Hood, ¹Mark R. Salvatore, ¹Cristina A. Thomas, ^1,3Mark J. Loeffler
The Planetary Science Journal, 7, 158 Open Source Link to Article [DOI: 10.3847/PSJ/ae6faa]
¹Department of Astronomy and Planetary Science, Northern Arizona University, Box 6010, Flagstaff, AZ 86011, USA
²Department of Astronomy, University of Maryland, 4296 Stadium Dr., Physical Sciences Complex (Building 415), Room 1113, College Park, MD 20742, USA
³Center for Materials Interfaces in Research and Applications, Northern Arizona University, Flagstaff, AZ 86011, USA

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¹David C. Cantillo, ^1,2Neil C. Pearson, ¹Kaycee I. Ridenhour, ¹Vrinda McBride, ¹Miren Miranda, ¹Adam Battle, ¹Thomas Joyce, ²Juan A. Sanchez, ¹Vishnu Reddy
The Planetary Science Journal, 7, 151 Open Source Link to Article [DOI: 10.3847/PSJ/ae6db2]
¹Lunar and Planetary Laboratory, University of Arizona, 1629 East University Boulevard, Tucson, AZ 85721, USA
²Planetary Science Institute, 1700 East Fort Lowell Road, Tucson, AZ 85719, USA

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¹Roshan S. Trivedi (>10)
The Planetary Science Journal, 7, 147 Open Source Link to Article [DOI: 10.3847/PSJ/ae6074]
¹School of Physics, Georgia Institute of Technology, USA

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¹Romy D. Hanna, ¹Richard A. Ketcham, ¹Dave R. Edey, ²Guillaume Avice, ³Kelly Miller, ⁴Alan Whittington
The Planetary Science Journal, 7, 138 Open Source Link to Article [DOI: 10.3847/PSJ/ae63c9]
¹Jackson School of Geosciences, The University of Texas at Austin, 2275 Speedway Stop C9000, Austin, TX 78712, USA
²Université Paris Cité, Institut de physique du globe de Paris, CNRS, Paris, F-75005, France
³Southwest Research Institute, San Antonio, TX 78238, USA
⁴The University of Texas at San Antonio, San Antonio, TX 78249, USA

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¹E. Dobrică, ²J.P. Greenwood, ¹A.N. Krot, ³A.J. Brearley, ⁴E.P. Vicenzi, ⁵S. Itoh, ⁶N. Sakamoto, ⁷H. Yurimoto
Geochimica et Cosmochimica Acta (in Press) Link to Article [DOI: 10.1016/j.gca.2026.08.009]
¹Hawai‘i Institute of Geophysics and Planetology, University of Hawai‘i at Mānoa, HI, USA
²Department of Earth and Environmental Sciences, Wesleyan University, Middletown, CT, USA
³Department of Earth and Planetary Sciences, University of New Mexico, NM, USA
⁴Smithsonian Institution, Museum Conservation Institute, Suitland, MD, USA
⁵Division of Earth and Planetary Sciences, Kyoto University, Kyoto, Japan
⁶Isotope Imaging Laboratory, Creative Research Institution, Hokkaido University, Sapporo, Japan
⁷Department of Natural History Sciences, Hokkaido University, Sapporo, Japan
Copyright Elsevier

Hydrogen isotopes in apatite are widely used to constrain the origin and evolution of water in Martian magmas and crustal reservoirs. However, the extent to which shock metamorphism modifies hydrogen-isotope compositions in apatites is poorly understood. In this study, we combine scanning electron microscopy (SEM), cathodoluminescence (CL), transmission electron microscopy (TEM) observations, and secondary ion mass spectrometry (SIMS) measurements of hydrogen isotopes and water contents in apatites from the Martian meteorite Los Angeles. Panchromatic CL imaging reveals distinct bright and dark domains within individual apatite grains. These domains correlate with variations in hydrogen-isotope composition, chlorine abundance, and shock metamorphic microstructures (dislocations, planar fractures, and shock-induced melting) observed at the nanoscale. Bright CL regions show higher defect densities, more abundant melt pockets, lower chlorine contents, and elevated δD values relative to dark CL regions. Defect density correlates positively with δD and melt pocket abundance but shows no systematic relationship with bulk H₂O content. These observations demonstrate that hydrogen-isotope modification can occur in heavily deformed apatite without requiring complete melting or recrystallization. Shock-induced defects therefore provide pathways for hydrogen redistribution and isotopic exchange at the micron scale. The results indicate that shock metamorphism can locally modify primary hydrogen isotope signatures in Martian meteorites while preserving bulk water contents within the typical Martian apatite range. Cathodoluminescence imaging provides a rapid and non-destructive method for identifying apatite domains that can correlate with deformation-enhanced and isotopically-modified regions. These findings have important implications for interpreting Martian volatile reservoirs and for future sample-return missions such as Martian Moons eXploration (MMX).

¹Shiori Inada, ^1,2Shogo Tachibana
Geochimica et Cosmochimica Acta (in Press) Open Source Link to Article [DOI: 10.1016/j.gca.2026.07.046]
¹Department of Earth and Planetary Science, The University of Tokyo, 7-3-1 Hongo, Tokyo 113-0033, Japan
²UTokyo Organization for Planetary and Space Science, The University of Tokyo, 7-3-1 Hongo, Tokyo 113-0033, Japan
Copyright Elsevier

Effects of ambient gas are important for understanding evaporation of planetary materials in the protosolar disk. In this study, we experimentally investigated the evaporation kinetics of forsterite in H₂-H₂O gas mixtures to elucidate the dependences on H₂O abundance at  of 10⁻⁴–10⁻², temperatures of 1400–1600 K, and a total pressure of 1 Pa. We found that the evaporation rate decreases with increasing  with a reaction order of −1.02 ± 0.12 only above certain  (10⁻³–10⁻² depending on temperature). The activation energy increased when the evaporation is suppressed by H₂O (497 ± 11 kJ mol⁻¹, while 359 ± 1 kJ mol⁻¹ without the effect of H₂O). The  dependence of the evaporation rate is consistent with the previously proposed model based on the chemical equilibrium consideration and the Hertz-Knudsen equation. This consistency can be explained in terms of a reaction mechanism. Based on the experimentally determined evaporation kinetics, we evaluated conditions of the protosolar disk where H₂O affects evaporation of forsterite dust. This showed that H₂O suppresses the evaporation at 1300 K at  of the Solar abundance and 1600 K under H₂O-enriched conditions, which possibly affected moderate-temperature thermal processing of silicate dust and evaporation of chondrule melt under oxidizing conditions.

¹Leire Coloma, ¹Fernando Alberquilla, ¹Julene Aramendia, ¹Gorka Arana, ²Ed Cloutis, ¹Juan Manuel Madariaga
Journal of Geophysical Research: Planets (in Press) Open Source Link to Article [DOI: 10.1029/2026JE009954]
¹Faculty of Science and Technology, Department of Analytical Chemistry, University of the Basque Country, Leioa, Spain
²Department of Geography, University of Winnipeg, Winnipeg, MB, Canada
Published by arrangement with John Wiley & Sons

The presence of minor minerals is a key factor distinguishing meteorite types, as they provide valuable insights into the formation processes, surface conditions, and evolutionary history of their parent bodies. In Martian nakhlites, one of the most distinctive minor phases is iron-titanium oxides forming characteristic skeletal textures. However, their mineralogical nature remains debated, with most studies identifying them as titanomagnetite, whereas others suggest ilmenite skeletal textures. This study uses Raman imaging to investigate the mineralogical distribution of these skeletal textures. Additionally, scanning electron microscopy-energy dispersive spectroscopy (SEM-EDS) was used to assess titanium concentration gradients from the exterior to the core of the structures. Chemometric methods were applied to differentiate and represent the mineralogical distribution. Furthermore, similar skeletal textures observed in terrestrial analogs from the Timanfaya and Maciot volcanoes (Lanzarote, Canary Islands, Spain) were analyzed using Raman imaging to evaluate potential similarities or differences in composition and formation processes with those found in the paired meteorites studied. The results show that the skeletal textures in the MIL nakhlites consist of ilmenite surrounded by titanomagnetite and magnetite. In contrast, in the analogs, two types of skeletal textures were identified: some composed of ilmenite and others of magnetite. These findings indicate that skeletal oxide textures in Martian and terrestrial samples from two field sites formed through distinct processes and constitute sensitive recorders of the evolution of mafic magmatic systems. These differences reflect restricted redox conditions and limited subsolidus re-equilibration in the MIL nakhlites, versus oxidation and faster cooling histories in the terrestrial analogs.