cometadata/datacite-titles-descriptions-related-identifiers huggingface dataset:
DOI: 10.17169/refubium-39222
title: Replication Data for: A numerical study of thermal and chemical structures at the core-mantle boundary

description: The core-mantle boundary (CMB) represents the lower boundary layer of the actively convecting Earth's mantle and is structurally very complex. Thermal and chemical structures such as thermal plumes and thermochemical piles have been considered to explain the complexities. Both affect the dynamics of the Earth's mantle and its temporal evolution. But also the surface plates are an essential aspect of mantle convection that strongly influence the dynamics of the interior. We use numerical thermochemical models of mantle convection to study the structure and dynamics of the lowermost mantle. Our approach allows for the investigation of plumes and piles in combination with plate-like surface motion and deep subduction. The models show that the presence of a dense CMB layer generally reduces the mobility of the surface plates but that during plate evolution a variety of plume classes occur leaving a complex structure at the CMB. The CMB topography shows large elevated areas with sharp edges and a flat or slightly dented top for piles with plumes atop. Also, plume clusters can cause large elevated areas with sharp edges but a flat top with a few smaller peaks. Smaller-scale patterns, often close to the edges of the large structures cause smaller peaks in CMB topography and can be explained by either line-plumes or wind-driven thermals. The latter often arise when heat is trapped beneath subducted slabs that spread over the CMB.
DOI: 10.17169/refubium-39177
title: Replication Data for: An Improved Electron Microprobe Method for the Analysis of Halogens in Natural Silicate Glasses

description: We present a new analytical method, which allows the simultaneous analysis of fluorine (F), chlorine (Cl), bromine (Br), and iodine (I) in geological samples. To account for interferences of Fe on the spectral lines of F, of Al on Br-lines, and of Ca on I-lines, we prepared four new halogen-free calibration glasses. The new method is used to analyze various glass reference materials and crystal-hosted melt inclusions from the Azores. Our results show that our new method allows reliable and reproducible analyses of all four halogens in silicate glasses.
DOI: 10.17169/refubium-39155
title: Replication Data for: Ancient Bombardment of the Inner Solar System: Reinvestigation of the 'Fingerprints' of Different Impactor Populations on the Lunar Surface

description: Craterstats (.scc, .plt and .txt) files, GIS-ready .shp files based on Head et al. (2010) and Fassett et al. (2012)" Note: We reloaded all the CSFD measurements (GIS-ready files) into new shapefiles and recalculated the area and crater sizes in an updated CraterTools extension.
DOI: 10.17169/refubium-39162
title: Replication Data for: Chalcophile elements in Martian meteorites indicate low sulfur content in the Martian interior and a volatile element-depleted late veneer.

description: • Ratios of Cu, S, Se, Te, Re, Pt and Pd in Martian meteorites are relatively constant. • Martian meteorites show very limited eruptive losses of volatile Re, S, Se and Te. • The parent magmas of most Martian meteorites were sulfide-undersaturated. • Martian mantle and core have a low sulfur content. • Low Te/PGE ratios in Martian meteorites reflect a strongly volatile element-depleted Martian late veneer.
DOI: 10.17169/refubium-39171
title: Replication Data for: Clinopyroxene/Melt Partitioning: Models for Higher Upper Mantle Pressures Applied to Sodium and Potassium

description: This dataset encompasses five codes to replicate data published in Schmidt and Noack 2021 (accepted): 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. The same least square approximation method is used in Parameterization_drySolidus.ipynb and Parameterization_Liquidus.ipynb, but applied to dry solidus and liquidus conditions (+,-50 K) respectively. The code D_K.m calculates clinopyroxene/melt partition coefficients for potassium with both the help of the thermodynamic model and the fitted scaling laws.
DOI: 10.17169/refubium-39164
title: Replication Data for: Degradation of Small Simple and Large Complex Lunar Craters: Not a Simple Scale Dependence

description: • We model the surface evolution for a pre-Nectarian lunar surface unit• Relative to their size, large craters are less destructive to the surrounding terrain than small simple craters• A simple scale dependence from small to large craters does not explain the per-crater contribution to topographic diffusion of large craters
DOI: 10.17169/refubium-44793
title: Replication Data for: Early evolution of the solar accretion disk inferred from Cr-Ti-O isotopes in individual chondrules

description: <b>Highlights</b> • First combined Cr, Ti, O isotope data for individual chondrules. • Isotopic compositions of NC chondrules distinct from CC chondrules. • Isotopic variability not due to chondrule transport, but precursor heterogeneity. • Incomplete mixing of NC-like and CAI-like nebular components in the disk at all scales.
DOI: 10.17169/refubium-44789
title: Replication Data for: Effects of Faraday cup deterioration on Sr and Cr isotope analyses by thermal ionization mass spectrometry

description: Abstract By comparing data from an extensive set of Sr and Cr isotope measurements performed on two different thermal ionization mass spectrometers (TIMS), using three sets of Faraday cups with different usage histories, we assess the effects of Faraday cup deterioration on high-precision isotope measurements by TIMS. We find that dynamic <sup>84</sup>Sr/ <sup>86</sup>Sr and <sup>87</sup>Sr/ <sup>86</sup>Sr measurements provide stable and reproducible results over the entire 56 months of this study, regardless of which set of Faraday cups is used. By contrast, static <sup>84</sup>Sr/ <sup>86</sup>Sr and <sup>87</sup>Sr/ <sup>86</sup>Sr measurements lead to deviant results, drifts over time, and in general exhibit larger scatter. For the most part, these differences can be attributed to changing Faraday cup efficiencies. For the instruments of this study we find that the center cup is most affected, consistent with this cup often receiving the highest ion beam intensities during measurements conducted in our laboratory. For Cr isotopes, we find that the correlation between mass fractionation-corrected <sup>53Cr</sup>/ <sup>52</sup>Cr and <sup>54</sup>Cr/ <sup>52</sup>Cr ratios observed for static measurements in several prior studies also reflects different Faraday cup efficiencies. Again, the changing efficiency of predominantly the center cup can account for the observed drift and correlation in <sup>53</sup>Cr/ <sup>52</sup>Cr and <sup>54</sup>Cr/ <sup>52 </sup>Cr. Multi-static Cr isotope measurements reduce this drift, but still result in a residual correlation between the two ratios, suggesting this correlation in part also reflects unaccounted mass fractionation effects.
DOI: 10.17169/refubium-44794
title: Replication Data for: Effect of mantle oxidation state and escape upon the evolution of Earth’s magma ocean atmosphere.

description: Abstract <i>Context</i>. The magma ocean period was a critical phase determining how Earth’s atmosphere developed into habitability. However, there are major uncertainties in the role of key processes such as outgassing from the planetary interior and escape of species to space that play a major role in determining the atmosphere of early Earth. <i>Aims</i>. We investigate the effect of outgassing of various species and escape of H2 for different mantle redox states upon the composition and evolution of the atmosphere for the magma ocean period. <i>Methods</i>. We included an important new atmosphere-interior coupling mechanism: the redox evolution of the mantle, which strongly affects the outgassing of species. We simulated the volatile outgassing and chemical speciation at the surface for various redox states of the mantle by employing a C-H-O based chemical speciation model combined with an interior outgassing model. We then applied a line-by-line radiative transfer model to study the remote appearance of the planet in terms of the infrared emission and transmission. Finally, we used a parameterized diffusion-limited and XUV energy-driven atmospheric escape model to calculate the loss of H2 to space. <i>Results</i>. We have simulated the thermal emission and transmission spectra for reduced and oxidized atmospheres present during the magma ocean period of Earth. Reduced/thin atmospheres consisting of H2 in abundance emit more radiation to space and have a larger effective height than oxidized/thick atmospheres, which are abundant in H2O and CO2. We obtain that the outgassing rates of H2 from the mantle into the atmosphere are a factor of ten times higher than the rates of diffusion-limited escape to space. We estimate the timescale of total mass loss of outgassed H2 via escape to be few tens of million years, which is comparable to other studies. <i>Conclusions</i>. Our work presents useful insight into the development of the terrestrial atmosphere during the magma ocean period and provides input to guide future studies that discuss exoplanetary interior compositions and their possible links with atmospheric compositions that might be estimated from observed infrared spectra by future missions.
DOI: 10.17169/refubium-44792
title: Replication Data for: Graphite in ureilites, enstatite chondrites, and unique clasts in ordinary chondrites – Insights from the carbon-isotope composition

description: Abstract: Carbon is of fundamental interest for constraining the volatile element inventory of terrestrial planets. In some meteorites, like ureilites and enstatite chondrites, graphite is the major carbon-carrier. Here, we report the in-situ analyses of graphite in 19 ureilites, 11 enstatite chondrites, and 3 graphite-bearing clasts in ordinary chondrites by secondary ion mass spectrometry (SIMS). In coarse-grained ureilites the obtained carbon-compositions of graphite range from –9.2‰ to –0.1‰ (δ13C). The carbon-composition tends to be homogeneous within a sample and correlates with the Fa content in olivine. In contrast, fine-grained ureilites exhibit considerable intra-sample heterogeneity, and graphite tends towards 13C-enriched compositions (up to +10.4‰). Isotopic and petrographic differences are presumably a result of post-igneous shock processing, including annealing during impact smelting. Enstatite chondrites host a variety of graphite morphologies, occurring in two distinct assemblages: Silicate-associated graphite (SAG) and metal-associated graphite (MAG). These assemblages show diverging carbon-compositions: SAG consistently exhibits δ13C in a narrow range between –4‰ and +1‰, very similar to the bulk silicate Earth value. In contrast, diverse compositions from –19.7‰ to +13.7‰ were observed for MAG. These differences are likely pre-accretionary in origin and potentially point towards isotopically distinct precursors. If Earth accreted from enstatite-chondrite-like material, carbon potentially hosted by Earth's core may have an isotopically light signature when compared to the mantle. Although graphite-bearing clasts in unequilibrated ordinary chondrites (UOCs) are extraordinarily rare, these clasts are of particular interest as they might represent materials, not corresponding to known meteorites. Graphite from these clasts show coinciding carbon-compositions with a mean δ13C close to –1‰. Although the coinciding compositions might argue for a genetic relationship among the clasts, petrographic evidence suggests they have experienced distinct thermal histories.
DOI: 10.17169/refubium-39148
title: Replication Data for: Heterogeneous accretion of Earth inferred from Mo-Ru isotope systematics

description: • The Mo-Ru correlation only exists for non-carbonaceous meteorites. • Earth's mantle falls off the Mo-Ru correlation. • The Mo-Ru isotope systematics are consistent with heterogeneous accretion of Earth.
DOI: 10.17169/refubium-39169
title: Replication Data for: Hydrogen isotopic composition of CI- and CM-like clasts from meteorite breccias – Sampling unknown sources of carbonaceous chondrite materials

description: Volatile-rich, CI- and CM-like clasts occur in different brecciated achondrite and chondrite groups. The CI-like clasts in HEDs, polymict ureilites, as well as ordinary, CR, and CB chondrites have a similar mineralogy, indicating a similar alteration history. However, when viewed in detail, their mineral chemistry shows some minor differences between the clasts from different meteorite groups. For CM-like clasts found in HED meteorites, the clasts are, based on their mineralogy, clearly fragments of CM chondrites. To be able to decipher whether CI- (or CM-)like clasts from different meteorite groups are related to certain meteorite classes known to contain volatiles, we obtained D/H ratios of several clasts from the meteorite groups mentioned above and compared them with those of CI and CM chondrites as well as to unique carbonaceous chondrites such as Bells, Essebi, and Tagish Lake. Considering the δD-values, CM-like clasts in HEDs span a similar range compared to bulk values of CM chondrites, further indicating that CM-like clasts are fragments of CM chondrites. For CI-like clasts a clear distinction can be made: While CI-like clasts in HEDs and ordinary chondrites show a very similar range in their δD-signatures compared to “common” CI chondrites, meaning that these clasts are likely related to CI chondrites, the CI-like clasts in polymict ureilites are enriched in D up to 3000‰; a similarly high enrichment is found for the CI-like clasts in CR chondrites. Thus, although the CI-like clasts in ureilites and CR chondrites likely experienced similar alteration histories as the CI-like clasts found in the other meteorite types, these clasts probably formed in a different region than the CI chondrites and, thus, are more accurately referred to as C1 clasts. Overall, the existence and isotopic signatures of the C1 clasts in several meteorite groups proves the existence of additional primitive, volatile-rich material in the (early) Solar System besides the matter we study as the CI, CM, and CR chondrites. This material was distributed throughout the Solar System very early and might have played an important role for the volatile inventory of the terrestrial planets.
DOI: 10.17169/refubium-39149
title: Replication Data for: Low volcanic outgassing rates for a stagnant lid Archean earth with graphite-saturated magmas

description: • Stagnant lid C-O-H outgassing rates predicted across mantle oxidation states. • Fully-coupled convection model reveals limiting effect of mantle volatile budget. • Early Archean CO2 outgassing was not necessarily stronger than the modern rate.
DOI: 10.17169/refubium-44790
title: Replication Data for: Impactor Core Breakup During Impact Into a Magma Ocean: A Parameter Study

description: Abstract: The present day concentrations of highly siderophile elements in Earth's mantle cannot be sufficiently explained by planetary differentiation processes. Material from iron cores of large differentiated bodies, incorporated into a magma ocean due to impact during the late accretion phase, may offer an explanation for the increased abundance of highly siderophile elements, which are considered a measure of the late addition of material. For the chemical equilibration of metallic impactor core material with a silicate magma ocean it is important whether the core breaks up into fragments that mix with the magma ocean or penetrates the magma ocean as a coherent mass that does not equilibrate with the surrounding silicates. In order to quantify the fragmentation process between these two end-member cases we performed hydrocode simulations of differentiated impactors into magma oceans at different impactor sizes, impact velocities and magma ocean depths. For this, we developed and implemented a new disruption method into our simulation code, which allows for a more realistic and quantitative description then previously possible. We find that there is significant breakup of the impactor core, increasing with greater magma ocean depth, until the impactor core is completely fragmented at a depth of more than twice the impactor radius. If the magma ocean is shallower, large portions of the impactor core can reach the magma ocean bottom before fragmenting, hence avoiding chemical reequilibration with the surrounding silicates.
DOI: 10.17169/refubium-39175
title: Replication Data for: Quantification of impact-induced melt production in numerical modelling revisited

description: • We provide an improved method to quantify impact-induced melt production for rocks. • We quantify impact-induced melt production and separate between heating due to shock compression and plastic work. • Melting due to frictional heating (plastic work) dominates over shock melting for impact velocities below 7-13 km/s depending on strength.
DOI: 10.17169/refubium-39151
title: Replication Data for: Re-Os, highly siderophile (HSE) and chalcophile (S-Se-Te) element characterisation of the New Caledonia peridotites

description: This dataset includes a compilation of Os isotopes, HSE (PGE +Re-Au) and S-Se-Te data of the New Caledonia lherzolites and harzburgites.
DOI: 10.17169/refubium-39201
title: Replication Data for: Re‐examination of the Population, Stratigraphy, and Sequence of Mercurian Basins: Implications for Mercury's Early Impact History and Comparison With the Moon

description: This data set contains the derived data products for the published manuscript Orgel et al. (2020) "Re-examination of the population, stratigraphy, and sequence of mercurian basins: Implications for Mercury´s early impact history and comparison with the Moon" at Journal of Geophysical Research Planets. This data package includes GIS-ready shapefiles of Mercurian basins, crater counting measurements, and Craterstats files.
DOI: 10.17169/refubium-39180
title: Replication Data for: Studying the Global Spatial Randomness of Impact Craters on Mercury, Venus, and the Moon With Geodesic Neighborhood Relationship

description: • We improve approaches to quantify the spatial randomness of impact craters by applying geodesic methods • We apply these methods to analyze the global spatial randomness of impact crater populations on Mercury, Venus, and the Moon • We use the results to investigate known crater population variations and surface evolution scenarios on Mercury, Venus, and the Moon This is Version 2, Version 1 is stored in Mendeley, http://dx.doi.org/10.17632/mn2b542k5r.2
DOI: 10.17169/refubium-39220
title: Replication Data for: Ruthenium isotope fractionation in protoplanetary cores

description: Mass-dependent Ru isotope variations (δ102/99Ru) and Ru concentrations were determined for 35 magmatic iron meteorites from the five major chemical groups (IIAB, IID, IIIAB, IVA, IVB). In addition, four equilibrated ordinary chondrites were analyzed. The IIAB, IIIAB and IVB iron meteorites display increasingly heavier Ru isotopic compositions with decreasing Ru content. Modeling demonstrates that the trends for these three iron groups can be reproduced by the incremental extraction of isotopically lighter Ru into solids, which leads to progressively heavier δ102/99Ru in the remaining melt. The modeling further shows that the Ru isotopic variations of the IIAB and IIIAB irons are consistent with derivation from parental melts with an ordinary chondrite-like δ102/99Ru, whereas the IVB irons more likely derive from a melt with heavier δ102/99Ru. This heavy Ru isotopic composition of the IVB parental melt probably results from high-temperature processing of the IVB precursor material. The Ru isotope systematics of the IID and IVA irons are more complex and show no correlation between δ102/99Ru and Ru content. Although most samples exhibit heavy Ru isotopic compositions, especially the late-crystallized irons of these groups deviate from the expected fractional crystallization trends. This deviation most likely results from mixing and re-equilibration of early-crystallized solids and late-stage liquids, followed by further fractional crystallization. The mixing might be related to the migration of liquids through a complex network of dendrites or to the overturn of a cumulate inner core, and bears testimony to the complex solidification history of at least some protoplanetary cores.
DOI: 10.17169/refubium-44788
title: Replication Data for: The Temperature and Composition of the Mantle Sources of Martian Basalts

description: The composition of basaltic melts in equilibrium with the mantle can be determined for several Martian meteorites and in-situ rover analyses. We use the melting model MAGMARS to reproduce these primary melts and estimate the bulk composition and temperature of the mantle regions from which they originated. We find that most mantle sources are depleted in CaO and Al2O3 relative to models of the bulk silicate Mars and likely represent melting residues or magma ocean cumulates. The concentrations of Na2O, K2O, P2O5, and TiO2 are variable and often less depleted, pointing to the re-fertilization of the sources by fluids and low-degree melts, or the incorporation of residual trapped melts during the crystallization of the magma ocean. The mantle potential temperatures of the sources are 1400–1500°C, regardless of the time at which they melted and within the range of the most recent predictions from thermochemical evolution models.
DOI: 10.17169/refubium-39176
title: The Earth-Moon late-accretion conundrum

description: Nature Geoscience, News & Views, Published: 19 August 2019 // The Earth–Moon late-accretion conundrum: The distribution of iron-loving elements between the mantles of the Moon and Earth may differ from established belief, suggest two studies that determine the hafnium–tungsten ratio and sulfide–silicate melt partitioning of elements in the lunar mantle.// Nature Geoscience volume 12, pages 683–684(2019) (2019).
DOI: 10.17169/refubium-45033
title: Valleys and deltas in Jezero crater, Mars

description: The dataset contains shape-files of the valleys and deltas in the Jezero crater on Mars: 1) initial and last incision valleys for the western inlet, northern inlet and outlet; 2) minimum, medium and maximum extents of the western and northern deltas. The mapping was done in ArcGIS 10.8.2 using CTX and HiRISE data (Planetary Data System Imaging Node https://pds-874 imaging.jpl.nasa.gov/) and HRSC data (data archives of ESA and NASA and https://maps.planet.fu-berlin.de [Walter et al., 2018]). For the minimum extent of the western delta a GIS version of the map of [Stack et al., 2020] was used. Details of mapping are described in [Ovchinnikova A. et al. A modeling approach for water and sediment transport in Jezero crater on Mars based on new geomorphological evidence. Icarus (accepted)].