¹M. Jakubowska, ²A. Grabias, ³M. Woźniak, ¹J. Gałązka-Friedman, ⁴K. Szopa
Interactions (in Press) Link to Article [DOI: 10.1007/s10751-026-02385-1]
¹Faculty of Physics, Warsaw University of Technology, Koszykowa 75, Warsaw, 00-662, Poland
²Łukasiewicz Research Network – Institute of Microelectronics and Photonics, Warsaw, Poland
³Faculty of Biology, University of Warsaw, Miecznikowa 1, Warszawa, 02-096, Poland
⁴Faculty of Natural Sciences, University of Silesia, Będzińska 60, Sosnowiec, 41-200, Poland

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¹Hanna Pentikäinen, ¹Eric M. MacLennan, ¹Antti Penttilä, ¹Karri Muinonen, ²Dagmara A. Oszkiewicz, ³Alberto Cellino, ⁴Paolo Tanga, ⁵Xiaobin Wang, ⁶Lauri Siltala
Astronomy & Astrophysics, 707, A132
Open Access Link to Article [DOI: 10.1051/0004-6361/202556127]
¹Department of Physics, PO Box 64, 00014 University of Helsinki, Finland
²Astronomical Observatory Institute, Faculty of Physics, A. Mickiewicz University, Słoneczna 36, 60-286 Poznań, Poland
³INAF – Osservatorio Astrofisico di Torino, 10025 Pino Torinese, Italy
⁴Université Côte d’Azur, Observatoire de la Côte d’Azur, CNRS, Laboratoire Lagrange, France
⁵Yunnan Observatories, Chinese Academy of Sciences, Kunming, China
⁶Karman+, 11365 Main St, Broomfield, CO 80020, USA

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¹P. Matlovič et al. (>10)
Astronomy & Astrophysics, 706, A247
Open Access Link to Article [DOI: 10.1051/0004-6361/202558248]
¹Faculty of Mathematics, Physics and Informatics, Comenius University Bratislava, Mlynská dolina, 84248 Bratislava, Slovakia

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^1,2T. V. Kizovski, ³L. F. White, ⁴A. Černok, ^1,5K. T. Tait, ¹V. E. Di Cecco, ⁵X. Chu, ^1,5J. M. Tomacic, ¹R. I. Nicklin, ⁶J. R. Darling
Geochemical Perspectives Letters (in Press)
Link to Article [DOI: 10.7185/geochemlet.2619]
¹Department of Natural History, Royal Ontario Museum, Toronto, ON M5S 2C6, Canada
²Department of Earth Sciences, Brock University, St. Catharines, ON L2S 3A1, Canada
³Planetary and Space Sciences, School of Physical Sciences, The Open University, Milton Keynes MK7 6AA, United Kingdom
⁴Dipartimento di Matematica, Informatica e Geoscienze, Università di Trieste, 34128 Trieste, Italy
⁵Department of Earth Sciences, University of Toronto, Toronto, ON M5S 3B1, Canada
⁶Institute of the Earth and Environment, University of Portsmouth, Portsmouth PO1 3QL, United Kingdom

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¹Anish M. Amarsi, ^2,3Nicolas Grevesse
Astronomy and Astrophysics Review, 34, 5
Open Access Link to Article [DOI: 10.1007/s00159-026-00172-z]
¹Theoretical Astrophysics, Department of Physics and Astronomy, Uppsala University, Box 524, 75120 Uppsala, Sweden
²Centre Spatial de Liège, Université de Liège, avenue Pré Aily, 4031 Angleur-Liège, Belgium
³Space sciences, Technologies and Astrophysics Research (STAR) Institute, Université de Liège, Allée du 6 août, 17, B5C, 4000 Liège, Belgium

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^1,2Viktor Bertrandsson Erlandsson, ²Gerd Rantitsch, ²Timothy Mitterdorfer, ²Monika Feichter, ³Aleš Šoster
Geochemistry (in Press)
Open Access Link to Article [DOI: 10.1016/j.chemer.2026.126468]
¹Division of Geosciences and Environmental Engineering, Luleå University of Technology, Luleå, 971 87, Sweden
²Department of Applied Geosciences and Geophysics, Technical University of Leoben, Peter-Tunner Strasse 5, Leoben, AT-8700, Austria
³Faculty of Natural Sciences and Engineering, Aškerčeva c. 12, Ljubljana, SI-1000, Slovenia

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¹Rody C. Erftemeijer, ²Thomas Müller, ¹Christian J. Renggli
Journal of Geophysical Research: Planets, 131, e2026JE010018
Open Source Link to Article [DOI: 10.1029/2026JE010018]

¹Max Planck Institute for Solar System Research, Göttingen, Germany
²Department of Mineralogy, Geoscience Center, Georg-August-Universität Göttingen, Göttingen, Germany

Published by arrangement with John Wiley & Sons

The surface of Mercury contains elevated amounts of sulfur of up to 4 wt.%. Volcanic degassing of S from the interior of the planet could have initiated sulfidation reactions between the degassed S and surface materials in the planet’s past, leading to the observed surface S enrichment. Mercury’s highly reducing conditions cause nominally lithophile elements, such as Mg and Ca, to become chalcophile and to form sulfides such as oldhamite (CaS) and niningerite (MgS) when reacting with S. Reactions of silicate minerals, serving as an analog for Mercury’s surface, and gaseous S under highly reducing conditions (at the graphite-CO buffer) have been investigated before, but the underlying mechanisms and kinetics of the sulfidation reaction are not well understood. In this study, olivine and diopside were exposed to temperatures between 800 and 1,300°C and experimental durations between 1 hr and 4 weeks in the presence of reduced S gas. Results show that the reaction in both minerals is initially interface-controlled, but mineralogical changes in the substrates cause a shift toward a transport-controlled kinetic regime. Moreover, the results are a combination of products from the primary sulfidation reactions as well as secondary processes, such as reduction in olivine and chemical re-equilibration in diopside. These findings highlight potential processes that formed oldhamite and niningerite as well as silicate byproducts, both in enstatite chondrites and on the surface of Mercury. This is especially relevant in the light of upcoming observations by the ESA/JAXA BepiColombo mission arriving at Mercury in late 2026.

^1,2A. Mojarro (>10)
Journal of Geophysical Research: Planets, (in Press), (in Press)
Open Source Link to Article [DOI: 10.1029/2026JE009985]
¹University of Maryland Baltimore County and Center for Research and Exploration in Space Science and Technology, NASA GSFC, Greenbelt, MD, USA
²Solar System Exploration Division, NASA Goddard Space Flight Center, Greenbelt, MD, USA

Published by arrangement with John Wiley & Sons

The Viking missions landed two spacecraft on Mars each equipped with a pyrolysis‐gaschromatograph‐mass spectrometer system capable of detecting signs of life. Although working as intended,detections of chloromethane and dichloromethane were initially attributed to terrestrial contamination. Decadeslater, the Phoenix Mars Lander identified perchlorate salts in the Martian regolith that are known to catalyze theoxidation and chlorination reactions of organics. Subsequent analyses by the Sample Analysis at Mars (SAM)instrument suite aboard the Curiosity rover have since confirmed a variety of syngenetic chlorinatedhydrocarbons in Gale crater samples. However, the nature of the parent organic matter (exogenous, abioticendogenous, or biological) remains unresolved. Here we evaluate the Murchison (CM2) carbonaceous chondriteas a proxy for organic matter delivered to the surface of Mars by meteoritic and interplanetary dust particle infallover geologic timescales. We characterize the generation of chlorinated hydrocarbons during the pyrolysis ofMurchison in the presence of 1 and 5 wt.% calcium perchlorate. Experiments produced a suite of C1‐C7chlorinated hydrocarbons dominated by aromatic species, including compounds detected by both Viking andSAM. Increasing the perchlorate content from 1 to 5 wt.% did not amplify the relative abundances or diversity ofchlorinated products but rather preferentially oxidized parent organics. Results suggest that organics detected atGale crater represent a fraction of molecules liberated from a macromolecular source that is compositionallyconsistent with meteoritic organic matter. Unambiguously resolving the origin and diversity of Martian organicmatter may ultimately require the coordinated laboratory analysis of samples returned to Earth.

¹James M.D. Day, ¹Jasmeet K. Dhaliwal
Earth and Planetary Science Letters, 698, 120451
Open Source Link to Article [DOI: 10.1016/j.epsl.2026.120451]
¹Scripps Institution of Oceanography, UC San Diego, La Jolla, CA, 92093, USA

Copyright Elsevier

Highly siderophile element (HSE: Re, Os, Ir, Ru, Pt, Pd) abundances are reported for eucrites, diogenites and howardites from Vesta. The four orders of magnitude variation (1 × 10^–3 to 1 × 10^–6 × CI chondrite) and measured ¹⁸⁷Os/¹⁸⁸Os (0.103 to 3.07) ranges in eucrites primarily reflect post-crystallization impactor additions and constrain meteorites previously identified as pristine (<1 μg/g Ni) as having limited (<0.1%) chondritic HSE additions. Pristine eucrites have fractionated inter-element HSE ratios with respect to chondrites, with a wide range of ¹⁸⁷Os/¹⁸⁸Os, making them distinct and more HSE-rich than lunar mare basalts. These eucrites define the crustal Vesta HSE composition as broadly similar to modern terrestrial basaltic oceanic crust. Models assuming either residual metal in the mantle, or its complete exhaustion, during eucrite melt extraction predict an HSE enriched bulk silicate Vesta compared to bulk silicate Earth or bulk silicate Mars, requiring between 0.4 to 1.9% post-core formation accretion (PCFA). A preferred alternative model using regression of the HSE to MgO contents of eucrites and diogenites derives a composition between bulk silicate Earth and bulk silicate Moon, requiring ∼0.12% PCFA. Such a composition is like the HSE contents measured for peridotites considered to come from Vesta. The estimates of PCFA from this large dataset of vestan meteorites are all higher than previously determined estimates, requiring a proportional increase in mass from leftover planetesimal and asteroidal sources to the inner Solar System planets.

¹Felipe Abrahão Monteiro, ²Maria Elizabeth Zucolotto, ¹Amanda Araujo Tosi
Anuário do Instituto de Geociências (in Press)
Open Access Link to Article [DOI: 10.11137/1982-3908_2026_49_71839]
¹Universidade Federal do Rio de Janeiro, Instituto de Geociências, Departamento de Geologia, RJ, Rio de Janeiro, Brazil
²Universidade Federal do Rio de Janeiro, Museu Nacional, Departamento de Geologia e Paleontologia, Setor de Meteoritos, RJ, Rio de Janeiro, Brazil

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