cometadata/datacite-titles-descriptions-related-identifiers huggingface dataset:
DOI: 10.17169/refubium-39223
title: Replication Data for: Lunar megaregolith mixing by impacts: Spatial diffusion of basin melt and its implications for sample interpretation.

description: The formation ages of lunar impact basins are critical to understanding the late accretion history of the inner solar system. Furthermore, the correct interpretation of the provenance and isotopic dates of basin-derived impact melt (‘basin melt’) is essential for the calibration of lunar chronology function. However, abundances of basin melt in the lunar near-surface are not well understood. Basin melt has been gardened by a long sequence of subsequent impact events, altering its abundance and size distribution. We developed a numerical model to investigate this process by means of the Monte Carlo method in a spatially resolved model. The fraction of melt in ejecta was tracked globally and at the Apollo 14–17 and Luna 20 sampling sites and was compared with K-Ar age distributions of lunar impact melt breccias. It was found that melt produced by the very large SPA basin as well as the relatively late-forming Imbrium basin should be dominant in the near-surface (top one meter). The simulation shows that the melt component at the Apollo 14–17 and Luna 20 sites is strongly affected by nearby mid- to late-forming basins. Imbrium melt should be abundant in Apollo 14–17 samples; Crisium melt is the most significant component of basin-sourced melt in Luna 20 samples; all the Apollo 14–17 and Luna 20 samples could include melt from Serenitatis and the SPA basin; Nectaris melt should occur in Apollo 16, Apollo 17 and Luna 20 samples; and Orientale melt has no significant mixing in the Apollo 14–17 and Luna 20 sampling sites. In general, besides a prominent age peak at 3.9 Ga (related to the Imbrium basin), the model predicts pronounced abundance peaks of older basin melt (&gt;3.9 Ga) which tend to be absent from distributions of K-Ar ages of impactites from landing sites. The diffusion characteristics of basin melt suggest that for future sampling aimed at collecting early basin melt, the re-excavation zones of late impact craters larger than tens of kilometer in diameter inside basins may provide the highest abundances of melt from early basins.
DOI: 10.17169/refubium-39401
title: Replication Data for: Impact-related crystallization and modification of small zircons in Apollo 15 and 16 impactites at 4.2 Ga

description: Because of their robustness against resetting, in situ U-Pb ages of zircons in lunar impactites have the potential to provide constraints on the lunar bombardment history that may complement the more common K-Ar ages. Most previous work has focused on relatively large zircons that show growth zoning and ages were mostly interpreted as early igneous crystallization ages. Here we combine high-resolution mineralogical imaging and in situ U-Pb dating by ion microprobe to identify, characterize and date &lt;20 μm size zircons in thin sections of lunar impact breccias. Several tens of grains of zircons of this size range were identified in thin sections of impactites from the Apollo 15 and 16 landing sites. Small zircons are more abundant in both noritic and evolved clinopyroxene, SiO2 or K-feldspar bearing lithologies compared to anorthositic bulk compositions. Both granular zircon aggregates and overgrowth on existing zircon or baddeleyite (in breccias 15455 and 67915) are interpreted to reflect high-temperature recrystallization of zircons or its high-temperature-pressure precursor phases, following shock heating events by impact. In contrast, conchoidal or poikilitic zircons &lt;10 μm in Fe-Ni metal bearing noritic clasts or matrix (67915, 67955) crystallized in situ from impact melt. Most U-Pb ages of the 24 analyzed grains are either concordant or reverse discordant with 207Pb-206Pb ages ranging from 4.15 to 4.25 Ga. The small age range, combined with a large textural spectrum and the frequent presence of Fe-Ni metal suggest zircon crystallization from impact melt and recrystallization of pre-existing zirconium-bearing minerals by impact heating. Such ‘impact’ zircons with 4.2 Ga ages have now been reported from most Apollo landing sites, suggesting widespread formation and modification of zircons by basin-forming impacts at this time. The contrast between U-Pb zircon (predominantly 4.2 Ga) and K-Ar feldspar ages (predominantly 3.9 Ga) likely reflects resetting of the latter chronometer by impact heating.
DOI: 10.17169/refubium-39160
title: Replication Data for: Nano- and microstructures in lunar zircon from Apollo 15 and 16 impactites: implications for age interpretations.

description: Meteorite impact processes are ubiquitous on the surfaces of rocky and icy bodies in the Solar System, including the Moon. One of the most common accessory minerals, zircon, when shocked, produces specific micro-structures that may become indicative of the age and shock conditions of these impact processes. To better understand the shock mechanisms in zircon from Apollo 15 and 16 impact breccias, we applied transmission electron microscopy (TEM) and studied nano-structures in eight lunar zircons displaying four different morphologies from breccias 15455, 67915, and 67955. Our observations revealed a range of shock-related features in zircon: (1) planar and non-planar fractures, (2) “columnar” zircon rims around baddeleyite cores, (3) granular textured zircon, in most cases with sub-µm-size inclusions of monoclinic ZrO2 (baddeleyite) and cubic ZrO2 (zirconia), (4) silica-rich glass and metal inclusions of FeS and FeNi present at triple junctions in granular zircon and in baddeleyite, (5) inclusions of rutile in shocked baddeleyite, (6) amorphous domains, (7) recrystallized domains. In many grain aggregates, shock-related micro-structures overprint each other, indicating either different stages of a single impact process or multiple impact events. During shock, some zircons were transformed to diaplectic glass (6), and others (7) were completely decomposed into SiO2 and Zr-oxide, evident from the observed round shapes of cubic zirconia and silica-rich glass filling triple junctions of zircon granules. Despite the highly variable effect on textures and Zr phases, shock-related features show no correlation with relatively homogeneous U–Pb or 207Pb/206Pb ages of zircons. Either the shock events occurred very soon after the solidification or recrystallization of the different Zr phases, or the shock events were too brief to result in noticeable Pb loss during shock metamorphism.
DOI: 10.17169/refubium-39219
title: Replication Data for: Nano- and micro-structures in lunar zircon from Apollo 15 and 16 impactites: implications for age interpretations

description: Abstract: Meteorite impact processes are ubiquitous on the surfaces of rocky and icy bodies in the Solar System, including the Moon. One of the most common accessory minerals, zircon, when shocked, produces specific micro-structures that may become indicative of the age and shock conditions of these impact processes. To better understand the shock mechanisms in zircon from Apollo 15 and 16 impact breccias, we applied transmission electron microscopy (TEM) and studied nano-structures in eight lunar zircons displaying four different morphologies from breccias 15455, 67915, and 67955. Our observations revealed a range of shock-related features in zircon: (1) planar and non-planar fractures, (2) “columnar” zircon rims around baddeleyite cores, (3) granular textured zircon, in most cases with sub-µm-size inclusions of monoclinic ZrO2 (baddeleyite) and cubic ZrO2 (zirconia), (4) silica-rich glass and metal inclusions of FeS and FeNi present at triple junctions in granular zircon and in baddeleyite, (5) inclusions of rutile in shocked baddeleyite, (6) amorphous domains, (7) recrystallized domains. In many grain aggregates, shock-related micro-structures overprint each other, indicating either different stages of a single impact process or multiple impact events. During shock, some zircons were transformed to diaplectic glass (6), and others (7) were completely decomposed into SiO2 and Zr-oxide, evident from the observed round shapes of cubic zirconia and silica-rich glass filling triple junctions of zircon granules. Despite the highly variable effect on textures and Zr phases, shock-related features show no correlation with relatively homogeneous U–Pb or 207Pb/206Pb ages of zircons. Either the shock events occurred very soon after the solidification or recrystallization of the different Zr phases, or the shock events were too brief to result in noticeable Pb loss during shock metamorphism.
DOI: 10.17169/refubium-39158
title: Replication Data for: The role of impact bombardment history in lunar evolution

description: • We present 3D evolution models of the Moon coupled to its early bombardment history. • Thermal anomalies induced by impacts on the Moon decay within 100–200 Myrs. • Ejecta deposits modify surface heat flux even on long timescales. • Surface insulation may maintain bombardment-induced anomalies until present. • Impact bombardment may alter lunar contraction history.
DOI: 10.17169/refubium-41374
title: Public Attitudes towards the Liberal Script (PALS) Survey
title: Wave 2

description: The survey covers the following countries: France, Germany, Hungary, Israel, Latvia, Poland, Serbia, Thailand, Turkey, and United States of America. Most but not all items of the wave 1 questionnaire are included in wave 2.
description: The comparative public opinion survey “Public Attitudes towards the Liberal Script” (PALS) is part of the Cluster of Excellence "Contestations of the Liberal Script (SCRIPTS)". The goal of PALS is to measure citizen attitudes towards what we call the liberal script, a specific understanding of how society should be organized around liberal principles. After having conducted a first wave in 26 countries from December 2021 to July 2022, conducting a second wave in some countries served the following purposes: 1. Re-running the survey with as many respondents from wave 1 as possible in selected countries to explore whether individual attitudes toward the liberal script have changed over time (panel data), 2. interviewing additional respondents from selected countries of wave 1 to be able to make statements about the change of public opinion in these countries (cross-sectional data at two points in time), 3. adding additional questions to address, in particular, the changing global situation with regard to Russia’s war against Ukraine, and 4. extending the geographical coverage to four new countries, namely, Thailand, Israel, Serbia, and Hungary which can be described as battlegrounds concerning the liberal script.
DOI: 10.17169/refubium-43210
title: Reproduction Data for: Moderately volatile elements in chondrites record chondrule formation, two component mixing and redistribution on parent bodies

description: Abstract: Most chondrites are depleted in moderately volatile elements (MVE) relative to the bulk solar system composition represented by CI chondrites. Here we present high-precision isotope dilution data for 11 moderately volatile elements (S, Cu, Zn, Ga, Se, Ag, Cd, In, Sn, Te and Tl) together with Cd and Zn stable isotope compositions for carbonaceous, ordinary, enstatite and Rumuruti chondrites complemented by a literature compilation of MVE stable isotope results. Together these data allow new insights into the processes that led to MVE depletion in chondrites and their redistribution within parent bodies.<br> Moderately volatile element abundances in carbonaceous, ordinary and Rumuruti chondrites are best explained by two-component mixing between a CI-like MVE-rich matrix and a MVE-poor refractory component dominated by chondrules. The refractory component is enriched in light MVE isotopes due to kinetic recondensation of a small vapor fraction initially lost from chondrules and chondrule precursor dust. Later, thermal metamorphism redistributed some MVE within chondrite parent bodies which is associated with stable isotope fractionation.<br> Compared to other chondrite classes enstatite chondrites show more complex MVE abundance patterns when the elements are plotted as a function of condensation temperatures. Type 3 and 4 enstatite chondrites are more MVE-rich than expected from their low matrix fractions. Most likely type 3 and 4 enstatite chondrites are MVE-rich, because a larger MVE vapor fraction recondensed after chondrule formation than observed for other chondrite classes and presumably at comparatively high H2 pressures.<br> Because MVE abundances and isotope compositions are fully consistent with chondrule formation, two-component mixing and MVE redistribution on parent bodies, we refute partial condensation from a hot solar nebula as the cause for MVE depletion in chondrite formation regions of the protoplanetary disk.
DOI: 10.15468/dl.cur4v6
title: Occurrence Download

description: A dataset containing 5707 species occurrences available in GBIF matching the query:
{
 "and" : [
 "HasGeospatialIssue is false",
 "HasCoordinate is true",
 "OccurrenceStatus is Present",
 "BasisOfRecord is one of (Human Observation, Machine Observation, Occurrence evidence, Observation)",
 "TaxonKey is one of (Calidris canutus (Linnaeus, 1758))",
 "Country is one of (Algeria, Angola, Benin, Botswana, British Indian Ocean Territory, Burkina Faso, Burundi, Cabo Verde, Cameroon, Central African Republic, Chad, Comoros, Congo, Congo, Democratic Republic of the, Côte d’Ivoire, Djibouti, Egypt, Equatorial Guinea, Eritrea, Eswatini, Ethiopia, French Southern Territories, Gabon, Gambia, Ghana, Guinea, Guinea-Bissau, Kenya, Lesotho, Liberia, Libya, Madagascar, Malawi, Mali, Mauritania, Mauritius, Mayotte, Morocco, Mozambique, Namibia, Niger, Nigeria, Réunion, Rwanda, Saint Helena, Ascension and Tristan da Cunha, Sao Tome and Principe, Senegal, Seychelles, Sierra Leone, Somalia, South Africa, South Sudan, Sudan, Tanzania, United Republic of, Togo, Tunisia, Uganda, Western Sahara, Zambia, Zimbabwe)"
 ]
}

 The dataset includes 5707 records from 24 constituent datasets; see https://api.gbif.org/v1/occurrence/download/0020835-250525065834625/datasets/export for details.
 
Data from some individual datasets included in this download may be licensed under less restrictive terms.
DOI: 10.17169/refubium-44795
title: Replication Data for: Formation of simple impact craters in layered targets: Implications for lunar crater morphology and regolith thickness.

description: Key Points - Impact velocity and target properties largely affect simple crater morphology in layered targets - Lunar regolith thicknesses inferred from crater morphometry deviate up to 80% from previous estimates - The morphological transition from normal to flat-bottomed craters is the most robust indicator for the thickness of the uppermost layer
DOI: 10.17169/refubium-44804
title: Replication Data for: Classification of CM chondrite breccias – Implications for the evaluation of samples from the OSIRIS REx and Hayabusa 2 missions.

description: Key Points: • <b>CM Chondrites as Breccias</b>: CM chondrites are complex impact breccias, primarily consisting of different lithic clasts exhibiting various degrees of aqueous alteration. • <b> Investigation of Clasts</b>: The study analyzed the degree of alteration in individual clasts within 19 CM chondrites and CM-like clasts in three achondrites, focusing on the chemical analysis of tochilinite-cronstedtite intergrowths (TCIs). • <b>Methodology</b>: Identification of TCIs in various chondritic lithologies was performed using backscattered electron (BSE) images of polished thin sections, followed by electron microprobe measurements for classification. • <b>Subclassifying CM Chondrites</b>: The study proposes an extended classification scheme based on Rubin's scale (CM2.0-CM2.9), with a focus on the "FeO"/SiO2 ratio in TCI chemistry, while considering brecciation and the degree of alteration of individual clasts. • <b>Implications for Future Missions</b>: The findings will be significant for interpreting samples returned from the OSIRIS-REx and Hayabusa 2 missions, given the range of aqueous alteration and mixing of clasts with different alteration histories in CM chondrites.
DOI: 10.17169/refubium-39159
title: Replication Data for: Controls on determining the bulk water content of the Moon.

description: The Moon is much wetter than previously thought. The estimated bulk H2O concentrations based on the analyses of H2O in lunar materials show a wide range from 5 to 1650 ppm. To better constrain bulk H2O in the lunar magma ocean (LMO), we model LMO crystallization and vary DH (concentration of H2O in LMO mineral/concentration of H2O in melt), interstitial melt fraction, and initial LMO depth. We take the highest and lowest values of DH reported in the literature for the LMO minerals. We assess the bulk H2O content required in the initial magma ocean to satisfy two observational constraints: (1) H2O measured in plagioclase grains from ferroan anorthosites and (2) crustal mass from GRAIL. We find that the initial bulk LMO H2O that best explains the H2O content in crustal plagioclase is strongly dependent on DH rather than interstitial melt fractions or initial LMO depths, with a drier magma ocean (10 ppm H2O) being favored with higher DH and a wetter magma ocean (100–1000 ppm H2O) with lower DH. This underscores the importance of constraining DH specific to lunar conditions in future studies. We also demonstrate that crustal mass is not an effective hygrometer.
DOI: 10.17169/refubium-44799
title: Replication Data for: Common feedstocks of late accretion for the terrestrial planets

description: Abstract: Abundances of the highly siderophile elements (HSEs) in silicate portions of Earth and the Moon provide constraints on the impact flux to both bodies, but only since ~100 Myr after the beginning of the Solar System (hereafter tCAI). The earlier impact flux to the inner Solar System remains poorly constrained. The former dwarf planet Vesta offers the possibility to probe this early history, because it underwent rapid core formation ~1 Myr after tCAI and its silicate portions possess elevated chondritic HSE abundances. Here we quantify the material accreted into Vesta’s mantle and crust and find that the HSE abundances can only be explained by the bombardments of planetesimals from the terrestrial planet region. The Vestan mantle accreted HSEs within the first 60 Myr; its crust accreted HSEs throughout the Solar System history, with asteroid impacts dominating only since ~4.1 billion years ago. Our results indicate that all major bodies in the inner Solar System accreted planetesimals predominantly from the terrestrial planet region. The asteroid belt was either never significantly more massive than today, or it rapidly lost most of its mass early in the Solar System history.
DOI: 10.17169/refubium-44798
title: Replication Data for: Evaporation of Boron from Aluminoborosilicate Melt

description: <b>Key Points</b>: - Experiments on B2O3 evaporation from Ca- and Mg-bearing aluminoborosilicate melts were conducted at 1250 and 1350 °C for 60-1020 hours, under varying oxygen fugacities (FMQ-6 to FMQ+1.5) and in air. - Results indicate that B evaporation increases by an order of magnitude under higher oxygen fugacities compared to reducing conditions, with two possible gas-phase speciation reactions for B2O3 suggested by Gibbs free energy minimization. - B2O3 evaporation rate constants were calculated from the final glass compositions, showing slower evaporation rates than diffusion rates, indicating that evaporation is the rate-limiting process.
DOI: 10.17169/refubium-44800
title: Replication Data for: Geological mapping and chronology of lunar landing sites: Apollo 12

description: <b>Highlights</b> • Using recent data, a new geological map is produced for the Apollo 12 landing site region. • The N(1) values of the mapped geological units were compared with recently determined radiometric sample ages. • Updated calibration points are consistent with the lunar cratering chronology of Neukum (1983) and Neukum et al. (2001).
DOI: 10.17169/refubium-44801
title: Replication Data for: Formation of diamond and lonsdaleite in ureilites by impact shock processing of graphite

description: 1. <b>Investigation Methods</b>: Carbon phase assemblages (CPAs) in five ureilitic samples from asteroid 2008 TC3 were analyzed using transmission electron microscopy, Raman spectroscopy, synchrotron X-ray diffraction, and cathodoluminescence. 2. <b>Shock Degrees of Samples</b>: Samples MS-MU 006, MS-187, and MS-170 had low to moderate shock degrees (U-S2 and U-S3), while samples MS-MU 027 (U-S4) and MS-MU 045 (U-S5) experienced higher shock levels. 3. <b>Presence of Diamond Grains</b>: No diamond grains were found in samples MS-MU 006 and MS-187. Sample MS-170 contained diamond grains up to 12 μm, formed under relatively low shock pressures (5–15 GPa) with a catalytic process involving a Fe, Ni, Cr, S, P-rich melt. 4. <b>CPAs in Highly Shocked Samples</b>: MS-MU 027 and MS-MU 045, the highly shocked ureilites, displayed three types of CPAs: nanopolycrystalline diamond and defect-rich diamond/lonsdaleite, disordered and distorted graphite, and polycrystalline diamond with Fe-rich mineral inclusions. 5. <b>Formation Mechanisms</b>: CPAs with only diamond and planar defect-rich diamond (e.g., MS-MU 027) likely formed through martensitic transformation of graphite at &gt;15 GPa and &gt;2000 K. Assemblages of diamond, defect-rich diamond, and disordered graphite (e.g., MS-MU 045) underwent martensitic transformation followed by back-transformation to disordered graphite. No conclusive evidence supports diamond formation under high static pressure.
DOI: 10.17169/refubium-39191
title: Replication Data for: Geomorphological analysis of the southwestern margin of Xanadu, Titan: Insights on tectonics

description: Titan Southwestern Xanadu Geomorphological Map: ArcMap project, map Shapefiles, layer symbologies, SAR and ISS basemaps. Rose Diagram data: azimuthal analysis data tables and shapefiles. Related paper: https://doi.org/10.1029/2020JE006407
DOI: 10.17169/refubium-41913
title: Replication Data for: Geological mapping and chronology of lunar landing sites: Apollo 14

description: • We produced detailed geological map for the Apollo 14 landing site on Fra Mauro formation which is Imbrian basin ejecta. • The N(1) values of the Fra Mauro formation were compared with recently determined radiometric sample ages. • The newly obtained calibration points are consistent with the lunar cratering chronology of Neukum (1983).
DOI: 10.17169/refubium-39225
title: Replication Data for: Halogen and Cl isotopic systematics in Martian phosphates: Implications for the Cl cycle and surface halogen reservoirs on Mars.

description: • In situ investigation of the Cl and halogen concentrations in Martian meteorites. • Cl compositions in Martian meteorites controlled by interactions with the surface halogens and perchlorate. • Evidence for early and widespread interaction between Martian meteorites, Martian hydrosphere, and Martian atmosphere. • Similar bulk initial Cl isotope composition between the Earth, Moon, and Mars.