¹George L. Carson,¹Lindsay J. McHenry,²Brian M. Hynek,¹Barry I. Cameron, ¹Chase T. Glenister
American Mineralogist 108, 409-429 Link to Article [http://www.minsocam.org/msa/ammin/toc/2023/Abstracts/AM108P0409.pdf]
¹Wisconsin-Milwaukee, 3209 N. Maryland Avenue, Milwaukee, Wisconsin 53211, U.S.A.
²Laboratory for Atmospheric and Space Physics, University of Colorado Boulder, 1234 Innovation Drive, Boulder, Colorado 80303, U.S.A
Copyright: The Mineralogical Society of America

Iceland’s Námafjall geothermal area exhibits a range of alteration environments. Geochemical and
mineralogical analyses of fumaroles and hot springs interacting with Holocene basaltic lavas at Hverir,
and with Pleistocene hyaloclastites atop nearby Námaskar∂, reveal different patterns of alteration
depending on the water/rock ratio, degree of oxidation, and substrate composition and age. The focus
of this study is a transect of a Hverir fumarole that has formed a bullseye pattern of alteration of a
Holocene basaltic lava flow. Surface samples and samples collected from shallow pits were analyzed
by X-ray diffraction (XRD), X-ray fluorescence (XRF), and scanning electron microscopy (SEM) to
constrain changes in mineral assemblage and major elemental composition with both distance and
depth. Elemental sulfur is concentrated near the vent, with leached deposits with amorphous silica
and anatase nearby and kaolinite, hematite, and jarosite/alunite-group sulfate minerals farther out,
with smectites and less altered material at the margins, though smaller-scale mineralogical diversity
complicates this pattern.
Silica phases include amorphous silica (most samples), cristobalite (some samples in the leached
part of the apron), and quartz (minor constituent of a few samples). The silica was concentrated through
residual enrichment caused by leaching and is accompanied by a significant enrichment in TiO2 (in
anatase). The presence of abundant cristobalite in a surface fumarole-altered Holocene basaltic lava
flow most likely reflects cristobalite formed during the devitrification of volcanic glass or precipitation
from fumarolic vapors, rather than high-temperature processes. Minor, localized quartz likely reflects
diagenetic maturation of earlier-formed amorphous silica, under surface hydrothermal conditions.
Natroalunite, natrojarosite, and jarosite are all present and even exhibit compositional zonation within
individual crystals, showing that under surface hydrothermal conditions, these minerals can form a
significant solid solution.
The high iron content of the substrate basalt and the prevalence of Fe-sulfates and Fe-oxide spherules
among the alteration products makes this geothermal area an especially useful analog for potential
martian hydrothermal environments. The residual enrichment of silica in the leached deposits of the
Hverir fumarole apron could serve as an acid-sulfate leaching model in which amorphous silica forms
without appreciable sulfur-bearing phases in many samples, a possible analog for silica-rich soils in
the Columbia Hills on Mars. The coexistence of hematite spherules and jarosite-group minerals serves
as an intriguing analog for a volcanic/hydrothermal model for hematite and jarosite occurrences at
Meridiani Planum.

¹Tutolo,²Benjamin M.
Science Advances Open Access Link to Article [DOI10.1126/sciadv.add8472]
¹University of Calgary, Department of Geoscience, Calgary, AB, Canada
²University of Cambridge, Department of Earth Sciences, Cambridge, United Kingdom

We currently do not have a copyright agreement with this publisher and cannot display the abstract here

¹Marco Morelli,^2,3Annarita Franza,¹Daniela Faggi,¹Giovanni Pratesi
Meteoritics & Planetary Science (in Press) Open Access Link to Article [https://doi.org/10.1111/maps.13974]
¹Parsec Foundation, Via di Galceti 74, 59100 Prato, Italy
²Department of Earth Sciences, University of Firenze, Via G. La Pira, 4, 50121 Firenze, Italy
³INAF-IAPS, Istituto di Astrofisica e Planetologia Spaziali, Via Fosso del Cavaliere 100, 00133 Roma, Italy
Published by arrangement with John Wiley & Sons

For the first time, this paper presents to the planetary scientists’ community the catalog of the meteorite collection preserved at the Italian Museum of Planetary Sciences (Museo Italiano di Scienze Planetarie, henceforth MISP) in Prato (Italy). Founded in 2005, MISP is a type specimen official repository approved by the Nomenclature Committee of the Meteoritical Society. It represents one of the few museums worldwide entirely devoted to planetary sciences. The catalog of its meteorite collection encompasses 430 meteorites for a total of 1536 specimens, including 291 thin sections, 184 thick sections, and 278 specimens that MISP has classified. Furthermore, MISP is currently classifying 57 other meteorites. Some samples were found during meteorite recovery expeditions in hot deserts, promoted by MISP in collaboration with diverse Italian universities and national research institutions. MISP also keeps an impact rocks collection comprising 257 samples. In a country like Italy, where most of the collected meteorites are housed in museums whose catalogs are not available online, the publication of the MISP meteorite collection catalog, together with the catalog of the impact rocks collection, represents not only a significant scientific primary source but also a remarkable tool for disseminating meteoritics to nonresearch audiences in educational activities and citizen science projects.

^1,2L. V. Forman,^2,3,4L. Daly,¹P. A. Bland,^1,2,5G. K. Benedix,⁶C. Corrigan
Meteoritics & Planetary Science (in Press) Open Access Link to Article [https://doi.org/10.1111/maps.13970]
¹Space Science & Technology Centre, School of Earth & Planetary Sciences, Curtin University, Bentley, Western Australia, Australia
²Department of Earth & Planetary Sciences, Western Australian Museum, Perth, Western Australia, Australia
³School of Geographical & Earth Sciences, University of Glasgow, Glasgow, UK
⁴Australian Centre for Microscopy and Microanalysis, University of Sydney, Sydney, New South Wales, Australia
⁵Planetary Science Institute, Tucson, Arizona, USA
⁶Department of Mineral Science, National Museum of Natural History (NMNH), Washington, DC, USA
Published by arrangement with John Wiley & Sons

Evidence of impact-induced compaction in the carbonaceous chondrites, specifically CMs and CVs, has been widely investigated utilizing microscopy techniques and impact experiments. Here, we use high-resolution photography and large area and high-resolution electron backscattered diffraction (EBSD) mapping analyses in tandem, to explore the effects of impact-induced compaction at both the meso- and micro-scales in the Allende CV3.6 carbonaceous chondrite. Macro-scale photography images of a ~25 cm slab of Allende captured meso-scale features including calcium-aluminum inclusions (CAIs) and chondrules. CAIs have a long-axis shape-preferred orientation (SPO). Examination of such meso-scale features in thin section revealed the same trend. Matrix grains from this section display a large amount of heterogeneity in petrofabric orientation; microscale, high-resolution, large area EBSD mapping of ~300,000 olivine matrix grains; high-resolution large area EBSD map across an elongate CAI; and a series of high-resolution EBSD maps around two chondrules and around the CAI revealed crystallographic preferred orientations (CPOs) in different directions. Finally, internal grains of the CAI were found to demonstrate a weak lineation CPO, the first crystallographic detection of possible CAI “flow.” All results are consistent with multiple, gentle impacts on the Allende parent body causing hemispheric compaction. The larger, more resistant components are likely to have been compressed and oriented by earlier impacts, and the matrix region petrofabrics and CAI “flow” likely occurred during subsequent impacts. Meteoritic components respond differently to impact events, and consequently, it is likely that different components would retain evidence of different impact events and angles.

¹M. E. Newcombe,²S. G. Nielsen,¹L. D. Peterson,³J. Wang,³C. M. O’D. Alexander,⁴A. R. Sarafian,⁵K. Shimizu,^6,3L. R. Nittler,⁷A. J. Irving
Nature 615, 854-857 Link to Article [DOI https://doi.org/10.1038/s41586-023-05721-5]
¹University of Maryland, College Park, MD, USA
²NIRVANA Laboratories, Woods Hole Oceanographic Institution, Woods Hole, MA, USA
³Earth and Planets Laboratory, Carnegie Institution for Science, Washington, DC, USA
⁴Corning Incorporated, Corning, NY, USA
⁵University of Wisconsin, Madison, WI, USA
⁶School Of Earth and Space Exploration, Arizona State University, Tempe, AZ, USA
⁷University of Washington, Seattle, WA, USA

We currently do not have a copyright agreement with this publisher and cannot display the abstract here

^1,2Johanna Marin-Carbonne,¹Kevin D. McKeegan,^3,4Andrew M. Davis,⁵Glenn J. MacPherson,⁵Ruslan A. Mendybaev,⁵Frank M. Richter
Meteoritics & Planetary Science (in Press) Open Access Link to Article [https://doi.org/10.1111/maps.13971]
¹Department of Earth, Planetary, and Space Sciences, University of California—Los Angeles, Los Angeles, California, USA
²Institut des Sciences de la Terre, Université de Lausanne, Lausanne, Switzerland
³Department of the Geophysical Sciences, University of Chicago, Illinois, USA
⁴Enrico Fermi Institute, University of Chicago, Chicago, Illinois, USA
⁵Department of Mineral Sciences, National Museum of Natural History, Smithsonian Institution, Washington, DC, USA
Published by arrangement with John Wiley & Sons

Oxygen, magnesium, and silicon isotopic abundances in Vigarano 1623-5 were studied using secondary ion mass spectrometry to investigate correlations between isotopic and petrologic properties of this unique forsterite-bearing FUN inclusion. Vigarano 1623-5 displays large, correlated mass-dependent fractionation effects, tightly linked to mineralogy within distinct petrologic units of the inclusion. The pyroxene-rich and melilite-rich interior parts of the inclusion display highly mass-fractionated isotopic compositions of oxygen, magnesium, and silicon, consistent with Rayleigh distillation during evaporation of a melt with initial oxygen composition close to a solar composition. However, the chemical composition, enriched in magnesium and silicon, suggests a precursor already fractionated by prior melt evaporation. A discontinuous igneous rim was produced by a flash-melting event followed by isotopic exchange in the rim melilite with planetary-like oxygen, mechanical fragmentation, and reassembly with an accretionary rim of heterogeneous materials. Al-rich minerals in 1623-5 show evidence for having crystallized with live 26Al but at less than the “canonical” level of most CV calcium-aluminum-rich inclusions. However, well-defined 26Al-26Mg isochrons are not found and temporal implications are ambiguous.

^1,2,3Ying-Kui Xu,^1,4Zhi Li,^1,2Shi-Jie Li,³Ze-Zhou Wang,^1,4De-Liang Wang,^1,5Yan Fan,^1,2Xiong-Yao Li,^1,2Jian-Zhong Liu,^6,2Dan Zhu
Geochimica et Cosmochimica Acta (in Press) Link to Article [https://doi.org/10.1016/j.gca.2023.03.031]
¹Center for Lunar and Planetary Sciences, Institute of Geochemistry, Chinese Academy of Sciences, Guiyang, 550081, China
²CAS Center for Excellence in Comparative Planetology, Hefei, 230022, China
³Isotope Laboratory, Department of Earth and Space Sciences, University of Washington, Seattle, WA 98195, USA
⁴University of Chinese Academy of Sciences, Beijing, 100049, China
⁵Department of Geology, Northwest University, Xi’an, 710069, China
⁶State Key Laboratory of Ore Deposit Geochemistry, Institute of Geochemistry, Chinese Academy of Sciences, Guiyang, 550081, China
Copyright Elsevier

To constrain how impacts influence the behavior of moderately volatile elements (MVEs), we report potassium (K) and zinc (Zn) contents and isotopic compositions of shock melt pockets (SMPs) and unmelted parts of three heavily shocked ordinary chondrites and bulk rocks of Chelyabinsk meteorite. All SMPs are enriched in K content and have lower isotopic values (δ41K = -1.99‰, -1.22‰ and -1.40‰) while the adjacent unmelted parts are enriched in heavy K isotopes (δ41K = -0.41‰, -0.01‰ and 0.04‰) compared to the bulk rocks of Chelyabinsk meteorite (δ41K = -0.77‰ and -0.73‰). By contrast, Zn is depleted in SMPs and the isotopic compositions are heavier (δ66Zn = -0.19‰, 2.42‰, 1.74‰) in SMPs than that in unmelted parts (δ66Zn = -0.65‰, 1.76‰, -0.97‰). Our results indicate a decoupling between the two MVEs that Zn is lost from shock melts while K is dramatically enriched in shock melts during impacts. The isotope fractionation of Zn is probably caused by evaporation of shock melts, while K isotope fractionation is most likely caused by solid-melt diffusion which is controlled by its incompatibility. The isotopic decoupling of K from Zn during major impacts further enhances our understanding of high temperature elemental and isotopic behavior of MVEs and may shed new light on the variously heterogeneous distribution of MVEs in solar system.

¹A. Tavernier,^2,3G. A. Pinto,^4,5,6M. Valenzuela,¹A. Garcia,¹C. Ulloa,⁷R. Oses,^8,9,10,11B. H. Foing
Meteoritics & Planetary Science (in Press) Link to Article [https://doi.org/10.1111/maps.13972]
¹Instituto de Investigaciones Científicas y Tecnológicas, IDICTEC, Laboratorio de Investigacion de la Criosfera y Aguas, Universidad de Atacama, UDA, Copiapó, Chile
²Instituto de Investigación en Astronomía y Ciencias Planetarias, INCT, Universidad de Atacama, UDA, Copiapó, Chile
³Centre de Recherches Pétrographiques et Géochimiques, CRPG, Université de Lorraine, Nancy, France
⁴Departamento de Ciencias Geológicas, Universidad Católica del Norte, UCN, Antofagasta, Chile
⁵Millennium Institute of Astrophysics, MAS, Santiago, Chile
⁶Center for Excellence in Astrophysics and Associated Technologies, CATA, Santiago, Chile
⁷Centro Regional de Investigacion y Desarrollo Sustentable de Atacama, CRIDESAT, Universidad de Atacama, UDA, Copiapó, Chile
⁸Instituto de Investigación en Astronomía y Ciencias Planetarias, INCT, Universidad de Atacama, UDA, Copiapó, Chile
⁹International Lunar Exploration Working Group, ILEWG, EuroMoonMars, Noordwijk, The Netherlands
¹⁰Vrije Universiteit Amsterdam, VUA, Amsterdam, The Netherlands
¹¹Universiteit Leiden, Leiden, The Netherlands
Published by arrangement with John Wiley & Sons

In 2019, while launching a multidisciplinary research project aimed at developing the Puna de Atacama region as a natural laboratory, investigators at the University of Atacama (Chile) conducted a bibliographic search identifying previously studied geographic points of the region and of potential interest for planetary science and astrobiology research. This preliminary work highlighted a significant absence of local institutional involvement in international publications. In light of this, a follow-up study was conducted to confirm or refute these first impressions, by comparing the search in two bibliographic databases: Web of Science and Scopus. The results show that almost 60% of the publications based directly on data from the Puna, the Altiplano, or the Atacama Desert with objectives related to planetary science or astrobiology do not include any local institutional partner (Argentina, Bolivia, Chile, and Peru). Indeed, and beyond the ethical questioning of international collaborations, Latin-American planetary science deserves a strategic structuring, networking, as well as a road map at national and continental scales, not only to enhance research, development, and innovation, but also to protect an exceptional natural heritage sampling extreme environmental niches on Earth. Examples of successful international collaborations such as the field of meteorites, terrestrial analogs, and space exploration in Chile or astrobiology in Mexico are given as illustrations and possible directions to follow to develop planetary science in South America. To promote appropriate scientific practices involving local researchers, possible responses at academic and institutional levels will eventually be discussed.

¹I. Kouvatsis,¹J.A. Cartwright,²M.J. Whitehouse
Geochimica et Cosmochimica Acta (in Press) Link to Article [https://doi.org/10.1016/j.gca.2023.03.026]
¹Department of Geological Sciences, University of Alabama, Tuscaloosa, AL 35487, USA
²Department of Geosciences, Swedish Museum of Natural History, SE-104 05 Stockholm, Sweden
Copyright Elsevier

Asteroid 4 Vesta is the largest known differentiated body in the asteroid belt, and is thought to be the likely parent body of howardite, eucrite, and diogenite (HED) meteorites. Howardites likely represent the vestan surface, eucrites likely crystallized as lavas in the upper crust, and diogenites likely originated from a plutonic layer deep in the crust. HEDs are potentially linked to another group of meteorites: the stony-iron mesosiderite group, due to mineralogical, geochemical, and isotopic similarities. Collision and disruption processes in the asteroid belt are key to understanding the evolution of asteroids, with impact events generating significant volumes of melt, which, if dated, can provide information on the timing and nature of such events. We performed in situ lead-lead (Pb-Pb) dating using Secondary Ionization Mass Spectrometry (SIMS) on melt clasts (mainly comprised of pyroxene, plagioclase, ± iron-nickel metal and/or glass) in two eucrites (Serra Pelada and Northwest Africa (NWA) 2696) and phosphates targeted within three mesosiderites (Vaca Muerta, Hainholz, and Estherville), respectively. The eucrite melt clasts yielded ages of 4520 ± 11 Ma and 4528.6 ± 6.3 Ma, in Serra Pelada and NWA 2696, respectively, and are likely indicative of a major heating event, such as an impact, metamorphism due to burial, or prolonged magmatism on the parent body. Our results from targeted mesosiderite phosphate analysis yielded a younger age range of ∼3968 – 4112 Ma, similar to ages reported previously for phosphate analysis in eucrites, as well as the broad range observed previously for many HEDs, and towards the upper end of the age range observed in lunar materials. These data may suggest a period of increased impact flux or possibly several higher-magnitude impacts on the mesosiderite parent body within that timeframe. Our results add further support to the likelihood of the existence of (at least) two different parent bodies for the HEDs (Vesta) and mesosiderites (Mesosiderite Parent Body – MPB).

¹Keelan T. O’Neill,¹Einar Fridjonsson,¹Declan Smeed,²Timothy Hopper,¹Michael Johns
Icarus (in Press) Link to Article [https://doi.org/10.1016/j.icarus.2023.115544]
¹Department of Chemical Engineering, University of Western Australia, Crawley, WA 6009, Australia
²Orebody Intelligence, Orica, 37 Kewdale Rd, Welshpool, WA 6106, Australia
Copyright Elsevier

Water is critical in the future of space exploration and development of planetary bodies. Benchtop nuclear magnetic resonance (NMR) is a geophysical measurement technique with the potential to be used for identification and characterisation of water resources on planetary bodies, such as the Moon and Mars. In this work, we explore the potential of NMR for space exploration by conducting measurements on Lunar and Martian regolith simulants using two main NMR pulse sequences. The first sequence is a decay due to internal fields (DDIF) pulse sequence which probes the pore size of the porous structure created by the regolith simulants. We then use a simple pore-to-particle size model to estimate the particle size distribution of the simulants and validate this against laser particle size analysis (LPSA) data. The DDIF type sequence can also be used to resolve the material surface relaxivity: which is useful in understanding the concentration of paramagnetic species as well as for correlating the length scales of various water volumes. The second pulse sequence utilised is a multi-echo sequence used to quantify fluid volumes as well as total moisture content within the porous media. The fluid volumes observed include adsorbed or hydrated water bound to clay minerals, as well as interparticle water between the regolith simulant grains. The NMR measured moisture content showed reasonably good agreement to corresponding gravimetric measurements used for validation. Finally, we discuss the implications of the current measurements and provide suggested focal points for potential future developments of NMR systems for space exploration.