cometadata/datacite-titles-descriptions-related-identifiers huggingface dataset:
DOI: 10.17169/refubium-39143
title: Replication Data for: The H2O content of the ureilite parent body.

description: The fate of highly volatile elements (H, C, F, Cl and S) during planetary accretion and differentiation is debated. Recent analyses of water in non-carbonaceous chondrites (RC, OC, EC) and achondrites (angrites, eucrites) have been used to argue that inner solar system parent bodies accreted and retained their highly volatile element budgets from their primary feedstock without substantial loss during accretion, metamorphism and differentiation. An alternative model posits that differentiated inner solar system parent bodies (e.g., the angrite parent body, 4 Vesta, Earth) derived the majority of their water from a carbonaceous chondrite-like source, delivered during the final stages of accretion. In order to add new constraints to this debate, we have measured water in nominally anhydrous minerals, melt inclusions, and interstitial glass in ureilites, the largest group of primitive achondrites in the terrestrial meteorite collection. Primitive achondrites did not experience global melting and homogenization. Therefore, these meteorites capture part of the transition from chondritic to achondritic parent bodies, allowing us to constrain the fate of water during the earliest stages of differentiation. Our nano-scale secondary ion mass spectrometry (nanoSIMS) analyses allow us to assess the viability of ureilite-like material as a potential source of terrestrial water. Analyses of pigeonite in main group ureilites yield a range of 2.0 – 6.0 µg/g H2O, and analyses of high-Ca pyroxene and glass (glassy melt inclusions and interstitial glass) in the Almahata Sitta ureilitic trachyandesite yield ranges of 13 – 19 µg/g H2O and 44 – 216 µg/g H2O, respectively. Mass balance, incremental melting, and batch melting calculations yield a preferred ureilite parent body H2O content of 2 – 20 µg/g, similar to previous estimates of water in the eucrite parent body (4 Vesta), but lower than estimates of Earth’s water budget. With these data, we demonstrate that 1) the ureilite parent body is H2O-depleted relative to the Earth; 2) ureilite-like material is unlikely to be a primary source of H2O to the Earth; 3) C and H are not necessarily coupled elements during planetary accretion and thermal processing; and 4) accretion, heating, partial melting, and degassing of rocky planetesimals likely results in significant depletion of H2O.
DOI: 10.17169/refubium-39174
title: Replication Data for: Chlorine and hydrogen degassing in Vesta’s magma ocean

description: The hydrophilic nature of halogens makes these elements ideal for probing potential hydrous geologic processes. Generally, in magmatic settings the stable isotopes of Cl may fractionate when H is in low concentrations and little fractionation occurs when the H concentration is high. We determined the Cl isotope composition and halogen content (F, Cl, Br, and I) of apatite and merrillite in seven basaltic eucrites, which are meteorites linked to the asteroid 4-Vesta, by using secondary ion mass spectrometry. We compare our halogen results with H isotope data, existing bulk rock concentrations, and petrologic models. The inferred Cl isotope composition of eucrites from this study, expressed in standard notation, which ranges from −3.8 to 7.7‰, correlates with the bulk major- and trace-element content, e.g., the Cl isotope composition positively correlates with Mg and Sc, while Cl isotope composition negatively correlates with K, V, and Cr. Here we suggest that eucrites preserve evidence of a degassing magma ocean as evidenced by the decreasing bulk rock K content with increasing . If the eucrite parent body, 4-Vesta, accreted with a negative of ‰, at least some parts of the solar nebula would have been isotopically light compared to most estimates of the Earth, which on average is close to 0‰.
DOI: 10.17169/refubium-39168
title: Replication Data for: Lack of late-accreted material as the origin of 182W excesses in the Archean mantle: Evidence from the Pilbara Craton, Western Australia

description: • 182W and HSE indicate partial lack late-accreted material in Pilbara source. • Only of normal amount of late-accreted material present at 3.3 Ga. • Similar 182W characteristics of other mantle sources indicates common process. • 182W–HSE mismatch for other sources caused by dissimilar behaviors of HSE vs. W. • Moon and pre-late accretion BSE had similar 182W.
DOI: 10.17169/refubium-39173
title: Replication Data for: Formation of Small Craters in the Lunar Regolith: How Do They Influence the Preservation of Ancient Melt at the Surface?

description: • A numerical model is developed to investigate the effect of small impact gardening on ancient melt in the lunar near-surface • Gardening of craters &lt;100 m in diameter likely lead to the excess of datable impact melt &lt;0.5 Ga in lunar regolith samples • Distribution of radiometrically datable melt in the regolith and the megaregolith is analyzed
DOI: 10.17169/refubium-39165
title: Replication Data for: MAGMARS: A Melting Model for the Martian Mantle and FeO-Rich Peridotite

description: Martian basalts identified by rover in-situ analyses and the study of meteorites represent a direct link to the melting process in the planet's interior and can be used to reconstruct the composition of the mantle and estimate its temperature. Experimentally calibrated numerical models are powerful tools to systematically search for the mantle compositions and melting conditions that can produce melts similar to primary basalts. However, currently available models are not suitable for modeling the melting of FeO-rich peridotites. In this study, we present experiments performed at 1.0 and 2.4–2.6 GPa on a primitive Martian mantle with various P2O5 contents. We use the new experiments together with a comprehensive database of previous melting experiments to calibrate a new model called MAGMARS. This model can reproduce the experimental melt compositions more accurately than Gibbs free energy minimization software (e.g., pMELTS) and can simulate near-fractional polybaric melting of various mantle sources. In addition, we provide an updated thermobarometer that can estimate the P–T melting conditions of primary melts and can be used as a prior step to constrain the input parameters of the MAGMARS melting model. We apply MAGMARS to estimate the source composition of the Adirondack-class basalts and find that melting a depleted mantle, at 2.3–1.7 GPa (Tp = 1390 ± 40°C) can best explain their bulk composition and K2O/Na2O ratio. MAGMARS represents a fast and accurate alternative to calculate the composition of the Martian primary melts and can be used as a stand-alone package or integrated with geodynamical models or other independent modeling software.
DOI: 10.17169/refubium-39167
title: Replication Data for: Lateral variation in bulk density and porosity of the upper Lunar crust from high-resolution gravity and topography data: comparison of different analysis techniques.

description: We map lateral variations in bulk density of the upper lunar highland crust using the most recent GRAIL gravity field solution of degree and order 1500 in combination with LOLA topography data, both truncated to an upper limit of degree and order 700. Our maps have a spatial resolution of 0.75, where each grid point was calculated using circular analysis regions of 3 radius. We apply two methods, which yield similar results for most parts of the study area. The first method minimizes the correlation between topography and Bouguer anomalies, the second maximizes the smoothness of the Bouguer anomalies. Both approaches suffer in the case that terrain is flat and lacks topographic features; consequently, this is where results from the two methods differ. We also mapped porosity of the crust using grain densities derived from Lunar Prospector spectrometry and sample analysis. It appears that variations in bulk density are mostly related to differences in crustal porosity. We find that high porosity is often associated with areas of impact basins. This confirms earlier studies, that impacts changed the geophysical characteristics of the lithosphere sustainably and that the high porosity of the upper lunar crust is most likely impact induced.
DOI: 10.17169/refubium-39178
title: Replication Data for: Predicted Sources of Samples Returned from Chang’e-5 Landing Region

description: • A numerical model is applied to trace the evolving distribution of components over the Chang’e-5 landing region. • The local mare component should account for ~60% in the samples. • The samples could contain abundant Imbrium melt.
DOI: 10.17169/refubium-39215
title: Replication Data for: Tellurium isotope cosmochemistry: Implications for volatile fractionation in chondrite parent bodies and origin of the late veneer.

description: Tellurium stable isotope compositions and abundances (δ128/126Te relative to SRM 3156) are reported for 43 ordinary, enstatite, and Rumuruti chondrites, which together with results from a companion study on carbonaceous chondrites are used to assess the origin of volatile element fractionations in chondrites. Whereas Te isotope variations among carbonaceous chondrites predominantly reflect mixing between isotopically light chondrules/chondrule precursors and CI-like matrix, Te isotope variations among non-carbonaceous chondrites mainly result from Te redistribution during parent body thermal metamorphism. The enstatite chondrites in particular display increasingly heavy Te isotopic compositions and decreasing Te concentrations with increasing degree of metamorphism, indicating migration of isotopically light Te from the strongly metamorphosed inner parts towards the cooler outer regions of the parent bodies. By contrast, ordinary and Rumuruti chondrites display less systematic Te isotope variations, implying more localized redistribution of Te during parent body thermal metamorphism.
DOI: 10.17169/refubium-39152
title: Replication Data for: Melt production and ejection from lunar intermediate sized impact craters: Where is the molten material deposited?

description: Differently aged impact melt in lunar samples is key to unveiling the early bombardment history of the Moon. Due to the mixing of melt products ejected from distant craters, the interpretations of the origin of lunar samples are difficult. We use numerical modelling for a better quantitative understanding of the production of impact-induced melt and in particular its distribution in ejecta blankets for lunar craters with sizes ranging from 1.5 to 50 km. We approximate the lunar stratigraphy with a porosity gradient, which represents the gradual transition from upper regolith via megaregolith to solid crustal material. For this lunar setting, we quantify melt production relative to crater volume and derive parameters describing its increasing trend with increasing transient crater size. We found about 30%-40% of the produced melt is ejected from the crater. The melt concentration in the ejecta blanket increases almost linearly with distance from the crater center, whilst the thickness of the ejecta blanked decreases following a power-law. Our study demonstrates that if the concentration of distant-derived melt of a certain age in lunar samples is rather high (&gt;30%), it could originate from large craters (&gt;10 km) located hundreds of kilometers away.
DOI: 10.5281/zenodo.15595233
title: QBS wavefunctions
DOI: 10.5281/zenodo.15595234
title: QBS wavefunctions
DOI: 10.17169/refubium-39400
title: Replication Data for: The first main group ureilite with primary plagioclase: A missing link in the differentiation of the ureilite parent body

description: MS-MU-012, a 15.5 g clast from the Almahata Sitta polymict ureilite, is the first known plagioclase-bearing main group ureilite. It is a coarse-grained (up to 4 mm), equilibrated assemblage of 52% olivine (Fo 88), 13% orthopyroxene (Mg# 89.2, Wo 4.5), 11% augite (Mg# 90.2, Wo 37.3), and 14% plagioclase (An 68), plus minor metal and sulfide. The plagioclase grains have been secondarily remelted and internally recrystallized, but retain primary external morphologies. Melt inclusions occur in olivine. Rounded chadocrysts of olivine and orthopyroxene are enclosed in augite grains. In terms of texture, mineralogy, major and minor element mineral compositions, and oxygen isotopes, MS-MU-012 is virtually identical to the archetypal Hughes-type main group ureilites, with the significant addition of primary plagioclase. We conclude that MS-MU-012 formed as a cumulate in a common lithologic unit with the Hughes-type ureilites. Based on reconstructed compositions of melts trapped in olivine, orthopyroxene, and augite in the Hughes-type samples, we infer that the parent magma of the Hughes unit originated as a late melt in the incremental melting of the ureilite parent body (UPB), near the end of the melting sequence, but was not completely extracted from the mantle like earlier melts and was emplaced in an intrusive body. MELTS calculations indicate that olivine began to crystallize at ~1260 °C, followed shortly thereafter by co-crystallization of orthopyroxene and augite. Plagioclase began to crystallize at ~1170–1180 °C. Graphite was buoyant in the melt and became heterogeneously distributed in flotation cumulates. Residual silicate liquid was extracted from the cumulate pile and could have crystallized to form the “labradoritic melt lithology” (with plagioclase of An ~68-35), which is partially preserved as clasts in polymict ureilites. The final equilibration temperature recorded by the Hughes unit was ~1140–1170 °C, just before catastrophic disruption of the UPB. MS-MU-012 provides a critical missing link in the differentiation history of this asteroid.
DOI: 10.17169/refubium-39398
title: Replication Data for: Insights into the formation of silica-rich achondrites from impact melts in Rumuruti-type chondrites.

description: Abstract: Ancient, SiO2‐rich achondrites have previously been proposed to have formed by disequilibrium partial melting of chondrites. Here, we test the alternative hypothesis that these achondrites formed by fractional crystallization of impact melts of Rumuruti (R) chondrites. We identified two new melt clasts in R chondrites, one in Pecora Escarpment (PCA) 91241 and one in LaPaz Icefield (LAP) 031275. We analyzed major, minor, and trace element concentrations, as well as oxygen isotopes, of these two clasts and a third one that had been previously recognized (Bischoff et al. 2011) as an impact melt in Dar al Gani (DaG) 013. The melt clast in PCA 91241 is an R chondrite impact melt closely resembling the one previously recognized in DaG 013. The melt clast in LAP 031275 has an L chondrite provenance. We show that SiO2‐rich melts could form from the mesostases of R chondrite impact melts. However, their CI‐normalized rare earth element patterns are flat, whereas those of ancient SiO2‐rich achondrites (Day et al. 2012; Srinivasan et al. 2018) and those of disequilibrium partial melts of chondrites (Feldstein et al. 2001) have positive Eu anomalies from preferential melting of plagioclase. Thus, we conclude that ancient SiO2‐rich achondrites were probably formed by disequilibrium partial melting (due to an internal heat source on their parent bodies), rather than from impact melts. TRR 170 no. 79
DOI: 10.17169/refubium-46513
title: Mikroklimatische Messungen im Berliner Stadtgebiet vom Institut für Meteorologie der Freien Universität Berlin des Jahres 2024
title: Microclimatic measurements in Berlin from the Institute of Meteorology, Freie Universität Berlin from 2024

description: The dataset contains 5 minute data of the Berlin stations from the FU Microclimate network (FUMiNET). This measurement network has been continuously built up since 2017 and is used for scale-dependent research of the urban climate of Berlin, which was funded by the 'Urban Climate under Change' Project (https://www.uc2-program.org/), BMBF. The stations reflect the urban structure and are located at sites which are typical of the Berlin urban area. The stations measure at a height of 2m the temperature and humidity. The data package contains data for the year 2024. For each of the stations there is a file with packed data in CSV format. In a full description contained in a pdf file, the locations are explicitly described.
description: Der Datensatz enthält Messwerte im fünf Minuten Takt des 'FU- Microclimate network' (FUMiNET) aus dem Berliner Stadtgebiet. Dieses Messnetz wurde kontinuierlich seit dem Jahr 2017 aufgebaut und dient der skalenübergreifenden Erfoschung des Stadtklimas von Berlin, welches durch das BMBF 'Stadtklima im Wandel Projektes' (https://www.uc2-program.org/) gefördert wurde. Die Stationen sind so aufgebaut, dass die Stadtstruktur von Berlin gut abgebildet wird. Gemessen wird die 2m Temperatur und Feuchte. Im Datenpaket sind die Daten des Jahres 2024 enthalten. Zu jeder der Stationen gibt es eine Datei mit gepackten Daten im CSV Format. In einer Gesamtbeschreibung als eine pdf Datei sind die Standorte expliziert beschrieben.
DOI: 10.17169/refubium-39670
title: Replication data for: Planetary impacts: effects of the impact speed on the crater depth

description: Abstract: Planetary impacts have shaped the surfaces and interiors of planets. They were particularly decisive in the last stage of planetary accretion, as they have eventually formed terrestrial planets. During these large supersonic collisions, shock waves melted the impactor and the target, and formed silicate magma oceans. Because the propagation of shock waves and the melting is faster than the excavation of an impact crater, the cratering stage can be considered as a purely hydrodynamic process. Here, we use both laboratory impact experiments in water and numerical simulations to investigate the crater dimensions resulting from the impact of a liquid impactor onto a liquid target. We show that our numerical models reproduce the laboratory experiments at subsonic impact velocities. We then explore the effect of both the Froude number, which is the ratio of the impactor kinetic energy to gravity, and the Mach number, which is the ratio of the impact speed to the sound speed. We vary these two parameters independently in impact simulations, going from subsonic to supersonic conditions. We obtain a new scaling law for the crater dimensions that describes the transition from subsonic to supersonic impacts. Our results indicate that the transition between these two regimes results from a change in the partitioning of the impactor kinetic energy into potential energy in the crater and internal energy. Finally, our scaling suggests that, in the limit of large Mach numbers, the crater depth depends only on the sound velocity and gravity, and is independent of the impact speed. Dataset contains: - iSALE input files (asteroid & material files) - EoS parameters for the different materials tested - 2 outcome example files from iSALE simulations (E1_1 & E1_2) - a .xlsx version of the table of results in the manuscript
DOI: 10.17169/refubium-46820
title: Molecular domino toppling for directed self-erasing information transfer

description: In the pursuit of more secure information transfer, advanced nanoelectronic technologies and nanomaterials must be developed. Here, we present a material able to undergo an unprecedented light-pumped directional charge transfer process reminiscent of toppling dominoes. The material is based on ortho-fluorinated azobenzene molecules which are organized in molecular rows by the regular array of a metal-organic framework. The azobenzene molecules undergo light-induced transcis forward as well as electrocatalytic cistrans backward isomerization. Our findings reveal that electron hopping occurs in a sequential and propagating manner between the light-generated cis isomers along with an isomerization of the sample to the trans state. Thus, light can be used to locally write information, which subsequently can be read out by the transferred charge with simultaneous deletion of the information. This freely repeatable, self-erasing domino information transfer is a groundbreaking new mechanism to process information on the molecular level that may find application in encryption.
DOI: 10.17169/refubium-40243
title: Wikidata Revision History Dataset

description: The "Wikidata Revision History Dataset" is a sample created from the Wikidata edit history. It contains details about each edit, including the task performed, the user group responsible, the timestamp, and the specific item and class to which it pertains. By analyzing these details, we can gain insights into the behavior of user groups and their editing patterns.
DOI: 10.17169/refubium-43212
title: Replication Data for: Silicon and iron isotopes in components of enstatite chondrites: Implications for metal–silicate–sulfide fractionation in the solar nebula

description: - Silicon and iron isotope compositions were analyzed in various components of enstatite chondrites (EC) to understand isotopic fractionation during planet formation.<br> - Metal–sulfide nodules in EC showed significant enrichment in light silicon isotopes.<br> - Silicon isotopic values in different fractions of EC varied, becoming progressively heavier with increasing Mg#.<br> - White mineral phases, primarily SiO2 polymorphs, exhibited the heaviest silicon isotopic values.<br> - Metal–silicate partitioning played a crucial role in determining the silicon isotopic composition of EC.<br> - The overall lighter silicon isotopic composition of bulk EC compared to other planetary materials was attributed to the enrichment of light silicon isotopes in EC metals and loss of heavier silicates.<br> - Iron isotope composition (δ56Fe) in EC components varied, with metals enriched in heavy isotopes and sulfides in light isotopes.<br> - Combined silicon and iron isotope data showed an inverse correlation, indicating significant fractionation under reduced conditions.<br> - Silicon isotopic compositions of silicate fractions largely retained information from nebular processing, while iron isotopes might have undergone re-equilibration during metamorphism.<br> - Uniform δ56Fe among different chondrites and Earth suggests common origin and fractionation processes in nebular reservoirs during planet formation.
DOI: 10.17169/refubium-41265
title: Public Attitudes towards the Liberal Script (PALS) Survey
title: Wave 1

description: The survey covers the following countries: Australia, Brazil, Chile, France, Germany, Ghana, India, Indonesia, Italy, Japan, Latvia, Nigeria, Mexico, Peru, Poland, Russia, Senegal, Singapore, Spain, South African, South Korea, Sweden, Tunisia, Turkey, United Kingdom, and United States of America.
description: The norms and institutions of liberal democracy, market economy, and open society have become increasingly contested worldwide. Is the rise of illiberal and authoritarian contestations reflected in a decline of citizens’ acceptance of liberal ideas and values? Are these contestations a response to unfulfilled promises, inherent tensions, or other unresolved challenges? As part of the Cluster of Excellence "Contestations of the Liberal Script (SCRIPTS)", the comparative public opinion survey “Public Attitudes towards the Liberal Script (PALS)" provides data that lets scholars address these questions. The goal of PALS is first and foremost to measure attitudes towards what we call the liberal script. PALS was conducted in 26 countries (+50,000 respondents) using CAWI (quota sampling) and CAPI (random probability sampling) modes of data collection. The sample draws from a diverse set of countries to provide a global perspective.