cometadata/datacite-titles-descriptions-related-identifiers huggingface dataset:
DOI: 10.17169/refubium-41914
title: Replication Data for: In situ Si isotope and chemical constraints on formation and processing of chondrules in the Allende meteorite

description: Chondrules in undifferentiated meteorites are former silicate melt droplets of variable texture and composition. Although widely studied, the chondrule formation mechanisms and conditions that explain all properties of chondrules are yet to be identified. To further constrain the processes that affected chondrules in the solar nebula and on the meteorite parent body, we determined in situ Si isotope ratios and major and trace element compositions of minerals in chondrules of variable types and sizes from the Allende CV3 chondrite. The δ30Si in chondrule minerals ranges from −1.28 ± 0.19 to 0.55 ± 0.20‰ (2SE). The δ30Si in chondrules shows no direct relationship with chondrule sizes or with distance between core and rim. Barred olivine-rich chondrules record the highest δ30Si, likely because of faster cooling and less interaction with isotopically light nebular gas. Type I non-porphyritic and some porphyritic chondrules show overall higher δ30Si compared to type II porphyritic chondrules. Furthermore, Mg-rich olivine and Mg-rich pyroxene have systematically higher δ30Si compared to Fe-rich olivine and Fe-rich pyroxene. The variable δ30Si of type I chondrule silicates (Mg-rich) compared to type II chondrule silicates (Fe-rich) may be explained by variable interaction of chondrule silicates with the nebular gas in the solar nebula. We envision a combination of equilibrium and kinetic isotope fractionation of Si between nebular gas and Fe-poor silicates (such as forsterite, anorthite, enstatite and mesostasis) and Fe-rich olivine and orthopyroxene. Petrographic evidence suggests that the enrichment of Fe in some highly altered porphyritic chondrules and at chondrule rims was likely caused by hydrothermal alteration on the parent body. Therefore, the correlation of Fe and δ30Si of the chondrule minerals might serve as an indicator for the extent of further secondary processing of some chondrule minerals. The sum of these observations suggests that the formation and alteration of type II chondrules occurred by oxidation of originally reduced, metal-rich type I chondrules, both in the solar nebula and later on the meteorite parent body. Remaining 30Si depleted gas contributed to the isotopic composition of matrix silicates. The evidence favours the formation of chondrules and matrix of the Allende meteorite in nebular settings rather than by asteroid impacts.
DOI: 10.17169/refubium-39189
title: Replication Data for: Intrusive magmatism strongly contributed to the volatile release into the atmosphere of early Earth

description: The purpose of this data set is to reproduce the figures in Vulpius and Noack (2022) as well as to access the corresponding data. This data set can be compiled with MATLAB or GNU Octave.
DOI: 10.17169/refubium-39195
title: Replication Data for: Layering by double-diffusive convection in the subsurface oceans of mid-sized icy satellites

description: Datatype: Source code. <br> Source code for double diffusive convection with finite Prandtl number and the input file.
DOI: 10.17169/refubium-39153
title: Replication Data for: Ménec Fossae on Europa: a Strike-Slip Tectonics Origin above a possible Shallow Water Reservoir

description: Europa's Ménec Fossae Geomorphological Map and Digital Terrain Model: QGIS project, map Shapefiles, layer symbologies, Digital Terrain Model (DTM) of the area
DOI: 10.17169/refubium-44797
title: Replication Data for: Mass fractions of siderophile elements, Sm and Ba in lunar low-Ti mare basalts by ID-ICP-MS

description: The data set contains concentration data for highly siderophile (Ir, Ru, Pt, Pd), siderophile volatile (Cu, Se, Ag, S, Te, Cd, In, and Tl) and, for reference, refractory lithophile elements (Ba and Sm) analyzed from the same digestion aliquot by isotope dilution-inductively coupled plasma mass spectrometry, following the methods described in Wang et al. (2015). We analyzed 12 low-Ti mare basalt samples collected at the Apollo 12 and 15 landing sites. Additionally we report highly siderophile element data for samples analyzed in Gleißner et al. (2022) for siderophile volatile elements. All samples were allocated by NASA/JSC and analyzed in the Geochemistry Laboratories at Freie Universität Berlin, Germany. Analysis period: 2019-2022
DOI: 10.17169/refubium-39208
title: Replication Data for: Mineralogy of volatile-rich clasts in brecciated meteorites

description: Meteoritic breccias are valuable samples as they can contain rare materials from the early solar system as clasts. Volatile-rich, CI- and CM-like clasts may represent parent body lithologies, which cannot be found as individual meteorites in today's meteorite collections. In order to reveal a better knowledge about the presence and chemical characteristics and variability of volatile (water-bearing) materials in the early solar system these clasts play an important role. Such materials may have been available as the volatile component during the accretion of terrestrial planets. To understand the distribution of volatile-rich materials in the solar system, we studied CI- and CM-like clasts in brecciated meteorites including polymict ureilites, HEDs, CR, CB, CH, and ordinary chondrites. CI-like clasts occur throughout all of the mentioned meteorite groups, whereas the CM-like clasts have only been identified in HEDs and ordinary chondrites. The abundance of volatile-rich clasts in general decreases in the order CH &gt; CR &gt; ureilites &gt; HEDs &gt; CB &gt; OC &gt; R. The mineralogy of CI-like clasts is similar to CI chondrites, but their compositions of phyllosilicates differ. The mineralogy of CM-like clasts clearly links them to CM chondrites. They must have been delivered to the HED parent body by low-velocity impacts after differentiation and volcanism, as there is no evidence for high shock and heating processes. Additionally, we propose that CI-like clasts in the CR, CB, and CH chondrites are a primary component of the appropriate parent bodies (accretionary breccias). Conversely, the CI-like clasts in polymict ureilites and HEDs represent an infall as (micro)meteorites or as low-velocity impactors, which happened after the accretion and differentiation of the appropriate parent bodies.
DOI: 10.17169/refubium-39212
title: Replication Data for: No 182W evidence for early Moon formation

description: Abstract: The Moon-forming giant impact was probably the last major event in Earth’s accretion, so dating this event is critical to determine the timeline of terrestrial planet formation. Recently, Thiemens et al. ( https://doi.org/10.1038/s41561-019-0398-3) used the short-lived <sup>182</sup>Hf–<sup>182</sup>W system to argue that the Moon formed within the first 60 Myr of Solar System history. Here we demonstrate, however, that mixing processes during and after the giant impact modified the <sup>182</sup>W compositions of the Earth and Moon, which hampers the use of the Hf–W system to date the Moon. Our results show that the lunar <sup>182</sup>W record is fully consistent with a recently determined, younger age of the Moon of 142 ± 25 Myr after Solar System formation (Maurice et al., Adv. 6, eaba8949, 2020)
DOI: 10.17169/refubium-39188
title: Replication Data for: Numerical investigation of lunar basin formation constrained by gravity signature

description: • We provide relationships between impactor size, gravity signal and farside basin size as a function of cooling history and formation time; • Gravity anomalies serve as a measure of basin size as impacts altered morphology and crustal thickness models simplify subsurface structure; • Our basin formation models agree with the assumed formation time based on crater chronology and the estimated cooling history of the Moon.
DOI: 10.17169/refubium-43209
title: Replication Data for: Onset of plate motion in the presence of chemical heterogeneities in the mantle and the effect of mantle temperature

description: Various structures observed in Earth’s mantle are considered to have a high density and therefore affect the mantle flow and the plate motion. We analyze the onset time of surface motion for 2D basally heated models with and without dense material. We find that the first motion is delayed for more, deeper or denser chemical heterogeneities. Due to a temperature-dependent viscosity, the temperature difference between the cold surface and a hot mantle leads to a highly viscous surface region. In contrast, in a cold mantle, the temperature difference is too small to form rigid plates. The heat from the core first needs to be transported upwards by plumes. Therefore, it takes longer for highly viscous plates to form. In the period after the Earth’s mantle was (partially) molten, the mantle was hotter than today. Under these conditions, plate motion can occur within approximately the first 0.5 Gyr if no chemical structures are present or if they are initially located at the surface. For a system that additionally has deep chemical heterogeneities, the onset of plate motion will be delayed by at least one order of magnitude. The motion will have been less stable than today, probably showing short subduction events.
DOI: 10.17169/refubium-39197
title: Replication Data for: Origin of Isotopic Diversity among Carbonaceous Chondrites

description: Carbonaceous chondrites are some of the most primitive meteorites and derive from planetesimals that formed a few million years after the beginning of the solar system. Here, using new and previously published Cr, Ti, and Te isotopic data, we show that carbonaceous chondrites exhibit correlated isotopic variations that can be accounted for by mixing among three major constituents having distinct isotopic compositions, namely refractory inclusions, chondrules, and CI chondrite-like matrix. The abundances of refractory inclusions and chondrules are coupled and systematically decrease with increasing amount of matrix. We propose that these correlated abundance variations reflect trapping of chondrule precursors, including refractory inclusions, in a pressure maximum in the disk, which is likely related to the water ice line and the ultimate formation location of Jupiter. The variable abundance of refractory inclusions/chondrules relative to matrix is the result of their distinct aerodynamical properties resulting in differential delivery rates and their preferential incorporation into chondrite parent bodies during the streaming instability, consistent with the early formation of matrix-poor and the later accretion of matrix-rich carbonaceous chondrites. Our results suggest that chondrules formed locally from isotopically heterogeneous dust aggregates, which themselves derive from a wide area of the disk, implying that dust enrichment in a pressure trap was an important step to facilitate the accretion of carbonaceous chondrite parent bodies or, more generally, planetesimals in the outer solar system.
DOI: 10.17169/refubium-39156
title: Replication Data for: Origin of lunar fragmental matrix breccias—Highly siderophile element constraints

description: The dataset contains concentration data for highly siderophile elements (Ru, Rh, Pd, Re, Os, Ir, Pt, and Au) analyzed by isotope dilution inductively coupled plasma mass spectrometry. We analyzed 5 different impact breccias sampled from the rim of the North Ray Crater, during the Apollo 16 mission to the lunar highlands. All samples we allocated by NASA/JSC and analyzed in the Geochemistry Laboratories at Freie Universität Berlin, Germany. (2019-08-06), TRR 170 paper no. 71
DOI: 10.17169/refubium-39198
title: Replication Data for: Parameterising a Model of Clinopyroxene/Melt Partition Coefficients for Sodium to Higher Upper Mantle Pressure

description: This dataset encompasses two codes to replicate data published in Schmidt and Noack (2021): The code D_Na.m calculates clinopyroxene/melt partition coefficients for sodium thermodynamically. The code Param_variousF.ipynb uses a least square approximation to fit the calculated partition coefficients over various melt fractions to a scaling law.
DOI: 10.17169/refubium-39203
title: Replication Data for: Regolith mixing by impacts: Lateral diffusion of basin melt.

description: • Cumulative impact gardening on presence of melt laterally and with depth is modeled by means of a Monte Carlo approach. • The quantitative abundance of the melt from three mid- to late-forming basin is estimated. • Burying and transportation play more important roles than re-melting process in melt diffusion. • The simulated abundance of basin melt is consistent with the radiometric ages from Apollo and Luna highland samples.
DOI: 10.17169/refubium-44796
title: Replication Data for: Solar System evolution and terrestrial planet accretion determined by Zr isotopic signatures of meteorites

description: Highlights • We present new Zr isotope data for a comprehensive suite of meteorites. • The NC-CC dichotomy among Solar System materials exists in Zr isotopes. • Isotope variation was likely caused by time-varied infall from the molecular cloud. • Earth & Mars accreted little CC material, precluding a pebble accretion scenario.
DOI: 10.17169/refubium-39193
title: Replication Data for: Syneruptive incorporation of martian surface sulphur in the nakhlite lava flows revealed by S and Os isotopes and highly siderophile elements: implication for mantle sources in Mars.

description: The data set contains petrographic (BSE and X-ray maps), chemical (highly siderophile elements), and stable isotope (in situ ∆33S and δ34S for sulpide grains) data for five Martian meteorite samples (nakhlites). Samples were obtained from the Natural History Museum of London and NASA Johnson Space Center. Scanning Electron Microscopy was performed at the Imaging Spectroscopy and Analysis Centre of the University of Glasgow (Great Britain). Sulphur isotope compositions were measured at the Centre de Recherches Pétrographiques et Géochimiques in Nancy (France). Highly siderophile element data were obtained at the Durham Geochemistry Centre, Durham University (Great Britain) and at the Institute of Geological Sciences, Freie Universität Berlin (Germany).
DOI: 10.17169/refubium-44803
title: Replication Data for: The anomalous polymict ordinary chondrite breccia of Elmshorn (H3-6)—Late reaccretion after collision between two ordinary chondrite parent bodies, complete disruption, and mixing possibly about 2.8 Gyr ago

description: Abstract: Elmshorn fell April 25, 2023, about 30 km northwest of the city of Hamburg (Germany). Shortly after the fall, 21 pieces were recovered totaling a mass of 4277 g. Elmshorn is a polymict and anomalous H3-6 chondritic, fragmental breccia. The rock is a mixture of typical H chondrite lithologies and clasts of intermediate H/L (or L, based on magnetic properties) chondrite origin. In some of the 21 pieces, the H chondrite lithologies dominate, while in others the H/L (or L) chondrite components are prevalent. The H/L chondrite assignment of these components is based on the mean composition of their olivines in equilibrated type 4 fragments (~Fa21–22). The physical properties like density (3.34 g cm−3) and magnetic susceptibility (logχ &lt;5.0, with χ in 10−9 m3 kg−1) are typical for L chondrites, which is inconsistent with the oxygen isotope compositions: all eight O isotope analyses from two different fragments clearly fall into the H chondrite field. Thus, the fragments found in the strewn field vary in mineralogy, mineral chemistry, and physical properties but not in O isotope characteristics. The sample most intensively studied belongs to the stones dominated by H chondrite lithologies. The chemical composition and nucleosynthetic Cr and Ti isotope data are typical for ordinary chondrites. The noble gases in Elmshorn represent a mixture between cosmogenic, radiogenic, and primordially trapped noble gases, while a solar wind component can be excluded. Because the chondritic rock of Elmshorn contains (a) H chondrite parent body interior materials (of types 5 and 6), (b) chondrite parent body near-surface materials (of types 3 and 4), (c) fragments of an H/L chondrite (dominant in many stones), (d) shock-darkened fragments, and (e) clasts of various types of impact melts but no solar wind-implanted noble gases, the different components cannot have been part of a parent body regolith. The most straightforward explanation is that the fragmental breccia of Elmshorn represents a reaccreted rock after a catastrophic collision between an H chondrite parent body and another body with H/L (or L) chondrite characteristics but with deviating O isotope values (i.e. that of H chondrites), complete disruption of the bodies, mixing, and reassembly. This is the only straightforward way that the implantation of solar wind gases could have been avoided in this kind of complex breccia. The gas retention ages of about 2.8 Gyr possibly indicate the closure time after the catastrophic collision between H and H/L (or L) chondrite parent bodies, while the cosmic ray exposure age for Elmshorn, which had a preatmospheric radius of 25–40 cm, is ~17–20 Myr.
DOI: 10.17169/refubium-39396
title: Replication Data for: The stability of antigorite in subduction zones revisited: the effect of F on antigorite stability and its breakdown reactions at high pressures and high temperatures, with implications for the geochemical cycles of halogens

description: We present new experimental data on the effect of F on the stability of antigorite and its breakdown products at high pressures (2–6 GPa) and high temperatures (570–850 °C). The experiments show that F does not affect the stability of antigorite, but addition of F to the system affects which minerals are formed when antigorite breaks down. In a F-free system and in a system with intermediate F contents (2 wt% F), antigorite breaks down to olivine and orthopyroxene, but in a F-rich system (5 wt% F), antigorite breaks down to other hydrous and F-bearing mineral assemblages which include chlorite, clinohumite and humite-group minerals (HGM). Since the latter mineral phases are stable at higher pressures and temperatures, and contain more F than antigorite, significant amounts of F and potentially other halogens can be retained in the subducting slab and transported deep into the mantle and possibly even into the Earth’s transition zone.
DOI: 10.17169/refubium-44791
title: Replication Data for: The Fe(Ni)–C–N-phase diagram at 10 GPa—implications for nitrogen and carbon storage in the deep mantle

description: Abstract: Nitrogen is the most abundant element in the Earth's atmosphere, yet its geochemical behavior and distribution among the various reservoirs (atmosphere, crust, mantle, and core) remain poorly understood. Although estimates of N and C fluxes in the mantle vary, there is a consensus regarding the disparity between input and output, leading to an increase in N and C contents in the mantle. The low solubility of N in mantle minerals raises questions about possible N or C storage in the mantle. Evidence suggests that Fe–N–C phases, such as Fe<sub>3</sub>C, Fe<sub>7</sub>C<sub>3</sub>, ε-Fe<sub>3</sub>N, metals, and non-stoichiometric carbonitrides, may be accessory phases at mantle pressure and temperature conditions, and thus potential hosts of C and N in the deep mantle. To investigate the phase relations and melting behavior in the (Fe,Ni)–N–C system, 19 experiments were conducted with varying starting compositions at 10 GPa and 1000–1400 °C. The results indicate that carbides, nitrides, carbonitrides, nitrocarbides, Fe(Ni)-metal, Fe-oxides, and diamond are stable at deep upper mantle pressure conditions. However, the compositions of naturally occurring nitrocarbides with high C and N contents, as found in diamond inclusions, could not be reproduced in the experiments. The significant incorporation of Ni in the experimental phases, which is also not observed in natural carbonitrides and nitrocarbides, suggests their formation in Ni-poor regimes. The solidus temperatures of the N- and C-rich systems are well below the adiabatic temperatures of the surrounding mantle. Therefore, it is hypothesized that cold regions in subduction zones, such as within or at the edge of a C- and N-rich subducted plate, are the likely formation environment for solid Fe–C–N phases.
DOI: 10.17169/refubium-44802
title: Mass fractions of siderophile elements, Sm and Ba in lunar high-Ti mare basalts by ID-ICP-MS

description: The data set contains mass fraction data for siderophile volatile (Cu, Se, Ag, S, Te, Cd, In, and Tl), highly siderophile (Ir, Ru, Pt, Pd), and, for reference, refractory lithophile elements (Ba and Sm) analyzed from the same digestion aliquot by isotope dilution-inductively coupled plasma mass spectrometry, following the methods described in Wang et al. (2015, https://doi.org/10.1111/j.1751-908X.2014.00312.x). We analyzed 13 high-Ti mare basalt samples collected at the Apollo 11 and 17 landing sites. Additionally, we report highly siderophile element data for 3 high-Ti mare basalt samples analyzed in Gleißner et al. (2022, https://doi.org/10.1016/j.epsl.2022.117680). All samples were allocated by NASA/JSC and analyzed in the Geochemistry Laboratories at Freie Universität Berlin, Germany.
DOI: 10.17169/refubium-39216
title: Replication Data for: The storage capacity of fluorine in olivine and pyroxene under upper mantle conditions.

description: Abstract: We present new experimental results on the fluorine storage capacity of olivine and orthopyroxene in the Earth’s mantle. Experiments were performed in the system MgO-SiO2 + MgF2 at temperatures between 1350 °C and 1700 °C and pressures up to 17 GPa. Electron microprobe measurements show that fluorine concentrations in olivine reach up to 5100 µg/g. The storage capacity of fluorine in olivine shows only a small pressure dependence but a strong temperature dependence with a positive correlation between increasing temperature and fluorine storage capacity. Fluorine concentrations found in enstatite are one order of magnitude smaller and reach up to 670 µg/g. Our data show that concentrations of fluorine in fluorine-saturated olivine are in the same range as water concentrations in olivine. Nevertheless, fluorine and water solubility in olivine show opposing behavior with increasing pressure and temperature. The fluorine solubility in olivine increases with increasing temperature but is not much affected by pressure. In contrast, water solubility in olivine has previously been shown to decrease with increasing temperature and increase with increasing pressure. Our experiments show that nominally fluorine-free minerals like forsterite and enstatite are capable of storing the entire fluorine budget of the upper mantle, without the need to invoke accessory phases such as apatite or amphibole. TRR 170 no. 19
DOI: 10.17169/refubium-39166
title: Replication Data for: 3D-simulation of Lunar Megaregolith Evolution: Quantitative Constraints on Spatial Variation and Size of Fragment

description: • A 3D numerical model was built to quantitatively constrain the distribution of lunar megaregolith and its fragment size. • Megaregolith has a distinct spatial variation and the size of fragments in the top 2 km is generally four orders of magnitude smaller than that deeper than 10 km. • Basin-forming events controlled the megaregolith growth where the SPA impact shaped its structure.