cometadata/datacite-titles-descriptions-related-identifiers huggingface dataset:
DOI: 10.17169/refubium-41920
title: Replication Data for: Modal abundances of coarse-grained (&gt;5 µm) components within CI-chondrites and their individual clasts – Mixing of various lithologies on the CI parent body(ies).

description: Abstract: For the bulk rocks of CI chondrites, various values are given for the modal abundance of matrix (95–100 vol%) and the accompanying mineral constituents. Here, we have determined the modal abundance of phases &gt;5 μm in the CI chondrites Orgueil, Ivuna, Alais, and Tonk. Considering this cut-off grain-size to distinguish between matrix and coarse-grained constituents, then, we find the modal abundance of the minor phases magnetite, pyrrhotite, carbonate, olivine, and pyroxene to be 6 vol% in total, and these phases are embedded within the fine-grained, phyllosilicate-rich matrix, making up 94 vol%. The values vary slightly from meteorite to meteorite. Considering all four chondrites, the most abundant phase is - by far - magnetite (4.3 vol%) followed by pyrrhotite (∼1.1 vol%). All four CI chondrites are complex breccias, and their degree of brecciation decreases in the sequence: Orgueil &gt; Ivuna &gt; Alais ∼ Tonk. Because these meteorites contain clasts with highly variable modal abundances, we therefore also studied individual clasts with high abundances of specific coarse-grained phases. In this respect, in Orgueil we found a fragment with a 21.5 vol% of magnetite as well as a clast having 31.8 vol% phosphate. In Ivuna, we detected an individual clast with a 21.5 vol% of carbonates. Thus, since the CI composition is used as a geochemical standard for comparison, one also should keep in mind that sufficiently large sample masses are required to reveal a homogeneous CI composition. Small aliquots with one dominating lithology may significantly deviate from the suggested standard CI composition. TRR 170 no. 70
DOI: 10.17169/refubium-41918
title: Replication Data for: Overturn of Ilmenite-Bearing Cumulates in a Rheologically Weak Lunar Mantle

description: The crystallization of the lunar magma ocean (LMO) determines the initial structure of the solid Moon. Near the end of the LMO crystallization, ilmenite-bearing cumulates (IBC) form beneath the plagioclase crust. Being denser than the underlying mantle, IBC are prone to overturn, a hypothesis that explains several aspects of the Moon's evolution. Yet the formation of stagnant lid due to the temperature dependence of viscosity can easily prevent IBC from sinking. To infer the rheological conditions allowing IBC to sink, we calculated the LMO crystallization sequence and performed high-resolution numerical simulations of the overturn dynamics. We assumed a diffusion creep rheology and tested the effects of reference viscosity, activation energy, and compositional viscosity contrast between IBC and mantle. The overturn strongly depends on reference viscosity and activation energy and is facilitated by a low IBC viscosity. For a reference viscosity of 1021 Pa s, characteristic of a dry rheology, IBC overturn cannot take place. For a reference viscosity of 1020 Pa s, the overturn is possible if the activation energy is a factor of 2–3 lower than the values typically assumed for dry olivine. These low activation energies suggest a role for dislocation creep. For lower-reference viscosities associated with the presence of water or trapped melt, more than 95% IBC can sink regardless of the activation energy. Scaling laws for Rayleigh-Taylor instability confirmed these results but also showed the need of numerical simulations to accurately quantify the overturn dynamics. Whenever IBC sink, the overturn occurs via small-scale diapirs.
DOI: 10.17169/refubium-41903
title: Replication Data for: Shock stage distribution of 2280 ordinary chondrites – Can bulk chondrites with a shock stage of S6 exist as individual rocks?

description: Abstract: The brecciation and shock classification of 2280 ordinary chondrites of the meteorite thin section collection at the Institut für Planetologie (Münster) has been determined. The shock degree of S3 is the most abundant shock stage for the H and LL chondrites (44% and 41%, respectively), while the L chondrites are on average more heavily shocked having more than 40% of rocks of shock stage S4. Among the H and LL chondrites, 40–50% are “unshocked” or “very weakly shocked.” Considering the petrologic types, in general, the shock degree is increasing with petrologic type. This is the case for all meteorite groups. The main criteria to define a rock as an S6 chondrite are the solid‐state recrystallization and staining of olivine and the melting of plagioclase often accompanied by the formation of high‐pressure phases like ringwoodite. These characteristics are typically restricted to local regions of a bulk chondrite in or near melt zones. In the past, the identification of high‐pressure minerals (e.g., ringwoodite) was often taken as an automatic and practical criterion for a S6 classification during chondrite bulk rock studies. The shock stage classification of many significantly shocked chondrites (&gt;S3) revealed that most ringwoodite‐bearing rocks still contain more than 25% plagioclase (74%). Thus, these bulk chondrites do not even fulfill the S5 criterion (e.g., 75% of plagioclase has to be transformed into maskelynite) and have to be classified as S4. Studying chondrites on typically large thin sections (several cm2) and/or using samples from different areas of the meteorites, bulk chondrites of shock stage S6 should be extremely rare. In this respect, the paper will discuss the probability of the existence of bulk rocks of S6. TRR 170 no. 51
DOI: 10.15468/dl.mpp74w
title: Occurrence Download

description: A dataset containing 16164 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 (Anguilla, Antigua and Barbuda, Argentina, Aruba, Bahamas, Barbados, Belize, Bolivia (Plurinational State of), Bonaire, Sint Eustatius and Saba, Bouvet Island, Brazil, Cayman Islands, Chile, Colombia, Costa Rica, Cuba, Curaçao, Dominica, Dominican Republic, Ecuador, El Salvador, Falkland Islands (Malvinas), French Guiana, Grenada, Guadeloupe, Guatemala, Guyana, Haiti, Honduras, Jamaica, Martinique, Mexico, Montserrat, Nicaragua, Panama, Paraguay, Peru, Puerto Rico, Saint Barthélemy, Saint Kitts and Nevis, Saint Lucia, Saint Martin (French part), Saint Vincent and the Grenadines, Sint Maarten (Dutch part), South Georgia and the South Sandwich Islands, Suriname, Trinidad and Tobago, Turks and Caicos Islands, Uruguay, Venezuela (Bolivarian Republic of), Virgin Islands (British), Virgin Islands (U.S.))"
 ]
}

 The dataset includes 16164 records from 31 constituent datasets; see https://api.gbif.org/v1/occurrence/download/0020830-250525065834625/datasets/export for details.
 
Data from some individual datasets included in this download may be licensed under less restrictive terms.
DOI: 10.17169/refubium-41905
title: Replication Data for: The effect of target properties on transient crater scaling for simple craters.

description: The effects of the coefficient of friction and porosity on impact cratering are not sufficiently considered in scaling laws that predict the crater size from a known impactor size, velocity, and mass. We carried out a systematic numerical study employing more than 1000 two-dimensional models of simple crater formation under lunar conditions in targets with varying properties. A simple numerical setup is used where targets are approximated as granular or brecciated materials, and any compression of porous materials results in permanent compaction. The results are found to be consistent with impact laboratory experiments for water, low-strength and low-porosity materials (e.g., wet sand), and sands. Using this assumption, we found that both the friction coefficient and porosity are important for estimating transient crater diameters as is the strength term in crater scaling laws, i.e., the effective strength. The effects of porosity and friction coefficient on impact cratering were parameterized and incorporated into π group scaling laws, and predict transient crater diameters within an accuracy of ±5% for targets with friction coefficients f ≥ 0.4 and porosities Φ = 0–30%. Moreover, 90 crater scaling relationships are made available and can be used to estimate transient crater diameters on various terrains and geological units with different coefficient of friction, porosity, and cohesion. The derived relationships are most robust for targets with Φ &gt; 10–15%, applicable for a lunar environment, and could therefore yield significant insights into the influence of target properties on cratering statistics.
DOI: 10.15468/dl.58tars
title: Occurrence Download

description: A dataset containing 9042 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 (Afghanistan, Armenia, Azerbaijan, Bahrain, Bangladesh, Bhutan, Brunei Darussalam, Cambodia, China, Cyprus, Georgia, Hong Kong, India, Indonesia, Iran (Islamic Republic of), Iraq, Israel, Japan, Jordan, Kazakhstan, Korea (Democratic People’s Republic of), Korea, Republic of, Kuwait, Kyrgyzstan, Lao People’s Democratic Republic, Lebanon, Macao, Malaysia, Maldives, Mongolia, Myanmar, Nepal, Oman, Pakistan, Palestine, State of, Philippines, Qatar, Saudi Arabia, Singapore, Sri Lanka, Syrian Arab Republic, Tajikistan, Thailand, Timor-Leste, Türkiye, Turkmenistan, United Arab Emirates, Uzbekistan, Viet Nam, Yemen)"
 ]
}

 The dataset includes 9042 records from 17 constituent datasets; see https://api.gbif.org/v1/occurrence/download/0020831-250525065834625/datasets/export for details.
 
Data from some individual datasets included in this download may be licensed under less restrictive terms.
DOI: 10.17169/refubium-41916
title: Replication Data for: Accretion of differentiated achondritic and aqueously altered chondritic materials in the early solar system - Significance of an igneous fragment in the CM chondrite NWA 12651

description: Abstract: One approach to decipher the dynamics of material transport and planetary accretion in the early solar system is to investigate xenolithic fragments in meteorites. In this work, we examined an igneous fragment from the NWA 12651 meteorite—the first igneous fragment found in any CM chondrite—by analyzing its mineralogy, rare earth elements (REEs), and O‐isotopes. The study shows that the exsolution lamellae of the igneous fragment consist of Fe‐rich and Ca‐rich pyroxene. Thus, the fragment was part of a progressive crystallization in a closed system, such as in a depleted magma reservoir or mantle. In this environment, the pyroxene co‐crystallized with plagioclase, resulting in a negative Eu anomaly and enrichment of the heavy REEs compared to the light REEs. The O‐isotopes of the fragment are more 16O‐enriched than the mafic minerals in the matrix or in other bulk CM chondrites; therefore, the fragment was formed in a different region than the NWA 12651 parent body. The iron meteorites Tucson and Deep Springs, the pallasite Milton, and the CB chondrites have similar O‐isotopes as the igneous fragment. However, no direct connection can be drawn and it is questionable if the fragment shares a same parent body with one of these meteorites. The close formation region to the CB chondrites may suggest a formation of the fragment in the carbonaceous chondrite region. Thus, a wide transport through the nebula of the early solar system may not have been necessary to move the fragment to the CM chondrite formation region. TRR 170 no. 76
DOI: 10.17169/refubium-45641.2
title: Meteorologisches Bürgermessnetz in Berlin 2023
title: Citizen Science Projekt des Open Urban Climate Observatory (OpenUCO) Berlin
title: Citizen Science Weather Station Network OpenUCO Berlin 2023

description: Citizen Science, zu Deutsch Bürgerwissenschaft, bezeichnet eine Form der wissenschaftlichen Forschung, bei der Bürgerinnen und Bürger aktiv an wissenschaftlichen Projekten teilnehmen. Eine Form der Teilnahme ist die aktive Unterstützung beim Sammeln von Daten. Die gesammelten Daten aus dem Citizen Science Projekt Open Urban Climate Observatory (OpenUCO), insbesondere aus einer Messkampagne im Sommer 2023 werden hier genauer beschrieben und zur Verfügung gestellt. OpenUCO ist ein Forschungsprojekt von Freier Universität Berlin und Technischer Universität Berlin, das von der Berlin University Alliance gefördert wird. Um räumlich stark ausdifferenzierte stadtklimatischen Variablen wie Lufttemperatur und Starkregen besser zu erfassen, setzt das Projekt auf Wetterbeobachtungen durch Bürger*innen. Diese ergänzen mit den von ihnen erfassten Wetterdaten das bestehende wissenschaftliche Messnetz des Urban Climate Observatory Berlin (UCO Berlin).
description: Der Datensatz enthält Minutenwerte der meteorologischen Messgrößen Luftdruck, Niederschlag, Luftfeuchtigkeit, Beleuchtungsstärke und Lufttemperatur (mittels verschiedener Sensoren gemessen und modelliert), die mit dem Messgerät MESSI erhoben wurden. Der MESSI (Mein eigenes Subskalen Messinstrument für atmosphärische Größen) ist eine kostengünstige Wetterstation für Citizen Science Projekte, die an der Freien Universität entworfen wurde. Zudem beinhaltet der Datensatz auch Messungen von Wetterstationen der Firma Pessl Instruments, die die Messgrößen Lufttemperatur, Luftfeuchtigkeit und Niederschlag beinhalten. Bei diesen Stationen ist die minimale Messfrequenz 5 Minuten. Alle 98 Messstationen wurden dabei vornehmlich in Kleingärten von teilnehmenden Bürger:innen platziert. Die Messungen fokussierten sich jeweils auf die Sommermonate 2023, wobei vereinzelte Stationen auch über einen längeren Zeitraum gemessen haben.
DOI: 10.6084/m9.figshare.29239607
title: Chapter_3_SupplementaryTables_V2.xlsx

description: Supplementary Table for Chapter 3 of my PhD Thesis.
DOI: 10.6084/m9.figshare.29239607.v1
title: Chapter_3_SupplementaryTables_V2.xlsx

description: Supplementary Table for Chapter 3 of my PhD Thesis.
DOI: 10.17169/refubium-46276
title: Thin films of a dinuclear Fe2+ complex on HOPG: Spin-crossover studies using X-ray absorption spectroscopy

description: The spin-crossover (SCO) properties of the dinuclear complex [{Fe(H2B(pz)2)2}2μ−(ac(bipy)2)] were studied as (sub)-monolayer and thin film deposited by an ultra-high vacuum liquid-jet deposition technique on highly oriented pyrolytic graphite (HOPG) by X-ray absorption spectroscopy. A comparison of the SCO properties of thin films and a dropcast sample indicates that the spin-switching probability of the thin films is limited due to substrate–molecule interactions. The maximum percentage of molecules in the low-spin (LS) state observed for 0.7 and 1.8 monolayers (ML) is approximately 43 % at a temperature of 80 K in comparison to the dropcast sample where ≈ 66 % of the complex is in the LS state. The similar switching properties of the dropcast sample as of a bulk powder sample confirm that the SCO properties are not affected by the presence of solvent necessary for deposition. The soft-X-ray-induced excited spin-state trapping (SOXIESST) effect is pronounced in all samples, although the light-induced high-spin (HS) fraction of the dropcast and the thin-film samples on HOPG is higher as compared to the HS fraction attained by SOXIESST, which confirms the sensitivity of the complex to light.
DOI: 10.17169/refubium-39187
title: Replication Data for: Multistage Core Formation in Planetesimals Revealed by Numerical Modeling and Hf-W Chronometry of Iron Meteorites

description: Iron meteorites provide some of the most direct insights into the processes and timescales of core formation in planetesimals. Of these, group IVB irons stand out by having one of the youngest 182Hf-182W model ages for metal segregation (2.9 ± 0.6 Ma after solar system formation), as well as the lowest bulk sulfur content and hence highest liquidus temperature. Here, using a new model for the internal evolution of the IVB parent body, we show that a single stage of metal-silicate separation cannot account for the complete melting of pure Fe metal at the relatively late time given by the Hf-W model age. Instead, a complex metal-silicate separation scenario is required that includes migration of partial silicate melts, formation of a shallow magma ocean, and core formation in two distinct stages of metal segregation. In the first stage, a protocore formed at ≈1.5 Ma via settling of metal particles in a mantle magma ocean, followed by metal segregation from a shallow magma ocean at ≈5.4 Ma. As these stages of metal segregation occurred at different times, the two metal fractions had different 182W compositions. Consequently, the final 182W composition of the IVB core does not correspond to a single differentiation event, but represents the average composition of early- and late-segregated core fractions. Our best fit model indicates an ≈100 km radius for the IVB parent body and provides an accretion age of ≈0.1–0.5 Ma after solar system formation. The computed solidification time is, furthermore, consistent with the Re-Os age for crystallization of the IVB core.
DOI: 10.17169/refubium-39204
title: Replication Data for: Nature of late accretion to Earth inferred from mass-dependent Ru isotopic compositions of chondrites and mantle peridotite

description: • Uniform mass-dependent Ru isotopic compositions of chondrites. • Chondritic mass-dependent Ru isotopic composition of Earth's mantle. • No fractionated metal component in late accretionary assemblage of Earth. • Bulk addition of impactor cores to Earth's mantle during late accretion.
DOI: 10.17169/refubium-39184
title: Replication Data for: Formation of Thermochemical Heterogeneities by Core-Mantle Interaction

description: The core-mantle boundary (CMB) shows a complex structure. Seismologists have observed features that are possibly denser than their surroundings. These structures form from a dense layer above the CMB. Therefore typical mantle convection models have assumed an initial dense basal layer. The thickness and density of this prescribed layer are crucial but hardly constrained. Here we investigate core-mantle interaction as one possible origin for this layer and employ 2D Cartesian models of mantle convection that consider a diffusive chemical gradient between the iron-rich core and the silicate mantle. Our simulations show that the diffusive influx is coupled to the convective mantle flow. Convection-assisted diffusion gives a larger influx beneath slabs spreading over the CMB. Additionally, as in the models with a prescribed layer, the rising plumes pull dense material up and form piles. In this study, however, the constant chemical influx leads to piles existing for longer times. The piles are typically smaller but can maybe in combination with a primordial layer explain different seismologically observed structures and the presence of core material in the mantle.
DOI: 10.17169/refubium-39192
title: Replication Data for: Crustal Porosity of Lunar Impact Basins

description: • The bulk density and porosity of the upper highland crust are revisited using a high-resolution GRAIL gravity field model (Park et al., 2015) in combination with LOLA topography (Smith et al., 2017) and independently estimated grain densities • Using the estimated bulk densities in combination with grain densities estimated from surface composition, the porosity of the upper crust was determined. Each grid point with a spacing of 0.75 deg was calculated using a circular analysis region of 3 deg radius. The grids are equally sampled following the sample theorem of Driscoll and Healy (1994). • For many impact basins, porosity is reduced within their peak ring and increased near and just exterior to the main rim • Large impact basins show a stronger pronounced porosity signature than smaller basins, and old impact basins reveal a muted porosity signature compared to younger basins
DOI: 10.17169/refubium-39183
title: Replication Data for: Treatment of non-sparse cratering in planetary surface dating.

description: • We present a new technique for the treatment of non-sparsely cratered surfaces. • Technique accounts for loss of small craters due to subsequent crater coverage. • Correction extends the crater diameter range usable for age extractions. • CSFDs on lunar highlands seem consistent with the lunar production function.
DOI: 10.17169/refubium-39213
title: Replication Data for: Lunar megaregolith mixing by impacts: Evaluation of the non-mare component of mare soils

description: The source of the non-mare component in the lunar mare soil samples is still an open question. A spatially resolved numerical model tracing the diffusion of non-mare material was developed by means of the Monte Carlo method to study this issue in more detail. The vertically- and laterally-transported non-mare components are recorded separately to assess their concentration on the surface. We find a general higher efficiency of lateral transport than of vertical transport, but the opposite may occur within small zones of interest. The overall (background) distribution of non-mare component is estimated by averaging out regional variations of material composition caused by local impact mixing. We find that almost all the mare surface is mixed with non-mare material. If most of the mare regions have filled basaltic material about 500 m in thickness since the formation of basins, the average non-mare fraction in the top 5 m is about 0.1. The abundance of the non-mare component decreases with increasing distance from the mare-highland boundary, but the slope of the distance-dependence is shallower within ~100 km of the boundary than further away.