cometadata/datacite-titles-descriptions-related-identifiers huggingface dataset:
DOI: 10.35003/m8i5lm
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: 10.5281/zenodo.7740874
title: A PETase enzyme synthesised in the chloroplast of the microalga Chlamydomonas reinhardtii is active against PET and polystyrene

description: The list contains: 1) raw data for chromatographies: HiprepSPHP and SEC 2) raw data for UV-vis Spectrum 3) raw data for all MS/MS spectra manuscript + supplementary 4) raw data for AFM 5) report data from HPLC
DOI: 10.5281/zenodo.7740875
title: A PETase enzyme synthesised in the chloroplast of the microalga Chlamydomonas reinhardtii is active against PET and polystyrene

description: The list contains: 1) raw data for chromatographies: HiprepSPHP and SEC 2) raw data for UV-vis Spectrum 3) raw data for all MS/MS spectra manuscript + supplementary 4) raw data for AFM
DOI: 10.5281/zenodo.7956450
title: A PETase enzyme synthesised in the chloroplast of the microalga Chlamydomonas reinhardtii is active against PET and polystyrene

description: The list contains: 1) raw data for chromatographies: HiprepSPHP and SEC 2) raw data for UV-vis Spectrum 3) raw data for all MS/MS spectra manuscript + supplementary 4) raw data for AFM 5) report data from HPLC
DOI: 10.6084/m9.figshare.23058431.v3
title: <strong>Supplementary data (ECOSER-S-23-00352): </strong>Appendix_B_Species_occurrence_data.xlsx

description: <strong>Supplementary data (ECOSER-S-23-00352): </strong>Appendix_B_Species_occurrence_data.xlsx
DOI: 10.35003/ba2o5g
title: Replication Data for: Controls on determining the bulk water content of the Moon.

description: The Moon is much wetter than previously thought. The estimated bulk H2O concentrations based on the analyses of H2O in lunar materials show a wide range from 5 to 1650 ppm. To better constrain bulk H2O in the lunar magma ocean (LMO), we model LMO crystallization and vary DH (concentration of H2O in LMO mineral/concentration of H2O in melt), interstitial melt fraction, and initial LMO depth. We take the highest and lowest values of DH reported in the literature for the LMO minerals. We assess the bulk H2O content required in the initial magma ocean to satisfy two observational constraints: (1) H2O measured in plagioclase grains from ferroan anorthosites and (2) crustal mass from GRAIL. We find that the initial bulk LMO H2O that best explains the H2O content in crustal plagioclase is strongly dependent on DH rather than interstitial melt fractions or initial LMO depths, with a drier magma ocean (10 ppm H2O) being favored with higher DH and a wetter magma ocean (100–1000 ppm H2O) with lower DH. This underscores the importance of constraining DH specific to lunar conditions in future studies. We also demonstrate that crustal mass is not an effective hygrometer.
DOI: 10.6084/m9.figshare.23058311.v3
title: <strong>Supplementary data (ECOSER-S-23-00352): </strong>Appendix_A_Data_parameters.xlsx

description: <strong>Supplementary data (ECOSER-S-23-00352): </strong>Appendix_A_Data_parameters.xlsx
DOI: 10.5281/zenodo.7441716
title: Data for "The use of a graph database is a complementary approach to a classical similarity search for identifying commercially available fragment merges"

description: The input and output data to the filtering pipeline described in "The use of a graph database is a complementary approach to a classical similarity search for identifying commercially available fragment merges"; code available from https://github.com/oxpig/fragment_network_merges.
DOI: 10.5281/zenodo.7441715
title: Data for "The use of a graph database is a complementary approach to a classical similarity search for identifying commercially available fragment merges"

description: The input and output data to the filtering pipeline described in "The use of a graph database is a complementary approach to a classical similarity search for identifying commercially available fragment merges"; code available from https://github.com/oxpig/fragment_network_merges.
DOI: 10.5281/zenodo.7957805
title: Data for "The use of a graph database is a complementary approach to a classical similarity search for identifying commercially available fragment merges"

description: The input and output data to the filtering pipeline described in "The use of a graph database is a complementary approach to a classical similarity search for identifying commercially available fragment merges"; code available from https://github.com/oxpig/fragment_network_merges.
DOI: 10.35003/9ggqml/c1sqpc
title: 1-s2.0-S0019103521003481-gr5.jpg

description: :unav
DOI: 10.35003/9ggqml/ea0sst
title: 1-s2.0-S0019103521003481-gr1.jpg

description: :unav
DOI: 10.35003/9ggqml/kebyn6
title: 1-s2.0-S0019103521003481-gr4.jpg

description: :unav
DOI: 10.35003/9ggqml/el0ih1
title: 1-s2.0-S0019103521003481-gr6.jpg

description: :unav
DOI: 10.35003/9ggqml/9z0fe3
title: table1-4.xlsx

description: :unav
DOI: 10.35003/9ggqml/suyksk
title: 1-s2.0-S0019103521003481-gr2.jpg

description: :unav
DOI: 10.35003/9ggqml/lcjmyq
title: 1-s2.0-S0019103521003481-fx1.jpg

description: :unav
DOI: 10.35003/9ggqml/onjqrf
title: figure_discription.xlsx

description: :unav
DOI: 10.35003/9ggqml/2bglwi
title: 1-s2.0-S0019103521003481-gr3.jpg

description: :unav
DOI: 10.35003/9ggqml
title: Replication Data for: The terrestrial planet formation paradox inferred from high-resolution N-body simulations

description: Recent improvements to GPU hardware and the symplectic N-body code GENGA allow for unprecedented resolution in simulations of planet formation. In this paper, we report results from high-resolution N-body simulations of terrestrial planet formation that are mostly direct continuation of our previous 10 Myr simulations (Woo et al., 2021a) until 150 Myr. By assuming that Jupiter and Saturn have always maintained their current eccentric orbits (EJS), we are able to achieve a reasonably good match to the current inner solar system architecture. However, due to the strong radial mixing that occurs in the EJS scenario, it has difficulties in explaining the known isotopic differences between bodies in the inner solar system, most notably between Earth and Mars. On the other hand, assuming initially circular orbits for Jupiter and Saturn (CJS) can reproduce the observed low degree of radial mixing in the inner solar system, while failing to reproduce the current architecture of the inner solar system. These outcomes suggest a possible paradox between dynamical structure and cosmochemical data for the terrestrial planets within the classical formation scenario. In addition, we use our high-resolution simulations to study the assembly of Earth in unprecedented detail, focusing on its collisional history. We find that more than 90% of giant impacts (GIs) on Earth occur within 80 Myr in the EJS simulations, matching the possible early timing of the Moon-forming GI based on the ages recorded by various meteoritic samples. However, the CJS and EJS scenarios both result in a leftover planetesimal mass that is 1–2 orders of magnitude greater than what currently exists in the solar system. Our overall results strongly suggest the need to consider alternative initial conditions for terrestrial planet formation in the solar system. For example, it may be necessary to assume a lower initial mass in the asteroid belt in order to lower the subsequent effect of radial mixing in the EJS scenario, as well as reduce the mass of leftover planetesimals. Similarly, in the CJS scenario, including an early giant planet instability within 80 Myr could make the scenario dynamically feasible.
DOI: 10.35003/bdofwa/j6srqs
title: 410_2022_1977_Fig2_HTML.webp

description: :unav
DOI: 10.35003/bdofwa/tfb1kw
title: 410_2022_1977_Fig7_HTML.webp

description: :unav
DOI: 10.35003/bdofwa/kel8rc
title: 410_2022_1977_Fig3_HTML.webp

description: :unav
DOI: 10.35003/bdofwa/5w9qbx
title: 410_2022_1977_Fig1_HTML.webp

description: :unav
DOI: 10.35003/bdofwa/6mtdwo
title: 410_2022_1977_Fig8_HTML.webp

description: :unav
DOI: 10.35003/bdofwa/p0s3rn
title: 410_2022_1977_Fig10_HTML.webp

description: :unav
DOI: 10.35003/bdofwa/gvqwug
title: 410_2022_1977_Fig9_HTML.webp

description: :unav
DOI: 10.35003/bdofwa/eao3h2
title: 410_2022_1977_MOESM1_ESM.pdf

description: :unav
DOI: 10.35003/bdofwa/xmohkt
title: 410_2022_1977_Fig5_HTML.webp

description: :unav
DOI: 10.35003/bdofwa/qkn1yn
title: 410_2022_1977_Fig4_HTML.webp

description: :unav
DOI: 10.35003/bdofwa/3et5vp
title: figure_text.txt

description: :unav
DOI: 10.35003/bdofwa/rtiesp
title: 410_2022_1977_Fig6_HTML.webp

description: :unav
DOI: 10.35003/bdofwa
title: Replication Data for: Nano- and microstructures in lunar zircon from Apollo 15 and 16 impactites: implications for age interpretations.

description: Meteorite impact processes are ubiquitous on the surfaces of rocky and icy bodies in the Solar System, including the Moon. One of the most common accessory minerals, zircon, when shocked, produces specific micro-structures that may become indicative of the age and shock conditions of these impact processes. To better understand the shock mechanisms in zircon from Apollo 15 and 16 impact breccias, we applied transmission electron microscopy (TEM) and studied nano-structures in eight lunar zircons displaying four different morphologies from breccias 15455, 67915, and 67955. Our observations revealed a range of shock-related features in zircon: (1) planar and non-planar fractures, (2) “columnar” zircon rims around baddeleyite cores, (3) granular textured zircon, in most cases with sub-µm-size inclusions of monoclinic ZrO2 (baddeleyite) and cubic ZrO2 (zirconia), (4) silica-rich glass and metal inclusions of FeS and FeNi present at triple junctions in granular zircon and in baddeleyite, (5) inclusions of rutile in shocked baddeleyite, (6) amorphous domains, (7) recrystallized domains. In many grain aggregates, shock-related micro-structures overprint each other, indicating either different stages of a single impact process or multiple impact events. During shock, some zircons were transformed to diaplectic glass (6), and others (7) were completely decomposed into SiO2 and Zr-oxide, evident from the observed round shapes of cubic zirconia and silica-rich glass filling triple junctions of zircon granules. Despite the highly variable effect on textures and Zr phases, shock-related features show no correlation with relatively homogeneous U–Pb or 207Pb/206Pb ages of zircons. Either the shock events occurred very soon after the solidification or recrystallization of the different Zr phases, or the shock events were too brief to result in noticeable Pb loss during shock metamorphism.
DOI: 10.6073/pasta/1f8b7e6739e7d3c353e5e4f5819dbd4e
title: Data from Pliant pathogens: Estimating viral spread when confronted with new vector, host, and environmental conditions

description: To determine the effects of new conditions (host, vector, and nutrient) on pathogen spread rate, we introduced a vector-borne viral plant pathogen, Barley Yellow Dwarf Virus PAV (BYDV-PAV) into hosts, vectors, and host nutrient supplies that it had not encountered for thousands of viral generations. We quantified pathogen prevalence over the course of two serial inoculations under the new conditions.
DOI: 10.5281/zenodo.7941351
title: Chemical reaction networks of glycolonitrile and glycolonitrile-H

description: Reaction networks of glycolonitrile (HOCH<sub>2</sub>CN) and HOCH<sub>2</sub>CHN radical obtained with the automated reaction discovery program AutoMeKin
DOI: 10.5281/zenodo.7941350
title: Chemical reaction networks of glycolonitrile and glycolonitrile-H

description: Reaction networks of glycolonitrile (HOCH<sub>2</sub>CN) and HOCH<sub>2</sub>CHN radical obtained with the automated reaction discovery program AutoMeKin
DOI: 10.35003/r8vftp/iddaxa
title: maps13821-sup-0001-supinfo.docx

description: :unav
DOI: 10.35003/r8vftp/rhnxeh
title: 10.1111-maps.13821Figure138210016.pptx

description: :unav
DOI: 10.35003/r8vftp/zm63vl
title: 10.1111-maps.13821Figure138210012.pptx

description: :unav
DOI: 10.35003/r8vftp/uc1ism
title: 10.1111-maps.13821Figure138210004.pptx

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DOI: 10.35003/r8vftp/cqo9rl
title: 10.1111-maps.13821Figure138210002.pptx

description: :unav
DOI: 10.35003/r8vftp/vw6g05
title: 10.1111-maps.13821Figure138210010.pptx

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DOI: 10.35003/r8vftp/f0zog3
title: 10.1111-maps.13821Figure138210003.pptx

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DOI: 10.35003/r8vftp/kusp7w
title: 10.1111-maps.13821Figure138210018.pptx

description: :unav
DOI: 10.35003/r8vftp/zr91sx
title: 10.1111-maps.13821Figure138210006.pptx

description: :unav
DOI: 10.35003/r8vftp/iigb9x
title: 10.1111-maps.13821Figure138210008.pptx

description: :unav
DOI: 10.35003/r8vftp/igastx
title: 10.1111-maps.13821Figure138210013.pptx

description: :unav
DOI: 10.35003/r8vftp/cswzzs
title: 10.1111-maps.13821Figure138210001.pptx

description: :unav
DOI: 10.35003/r8vftp/vxqmfl
title: README.txt

description: :unav
DOI: 10.35003/r8vftp/gfnxy7
title: 10.1111-maps.13821Figure138210005.pptx

description: :unav
DOI: 10.35003/r8vftp/vutsp5
title: 10.1111-maps.13821Figure138210014.pptx

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DOI: 10.35003/r8vftp/obpqmn
title: 10.1111-maps.13821Figure138210009.pptx

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DOI: 10.35003/r8vftp/mgiae6
title: 10.1111-maps.13821Figure138210007.pptx

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DOI: 10.35003/r8vftp/hpwwa9
title: 10.1111-maps.13821Figure138210011.pptx

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DOI: 10.35003/r8vftp/db6lov
title: 10.1111-maps.13821Figure138210019.pptx

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DOI: 10.35003/r8vftp/ohy0pg
title: 10.1111-maps.13821Figure138210017.pptx

description: :unav
DOI: 10.35003/r8vftp/vgmagv
title: 10.1111-maps.13821Figure138210015.pptx

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DOI: 10.35003/r8vftp
title: Replication Data for: Asteroid 2008 TC3, not a polymict ureilitic but a polymict C1 chondrite parent body? Survey of 249 Almahata Sitta fragments

description: On October 7, 2008, the asteroid 2008 TC3 exploded as it entered the Earth’s atmosphere, producing significant dust (in the atmosphere) and delivering thousands of stones in a strewn field in Sudan, collectively known as the Almahata Sitta (AhS) stones. About 600 fragments were officially recovered in 2008 and 2009. Further rocks were collected since the fall event by local people. From these stones, 249 were classified at the Institut für Planetologie in Münster (MS) known as MS-xxx or MS-MU-xxx AhS subsamples. Most of these rocks are ureilitic in origin (168; 67%): 87 coarse-grained ureilites, 60 fine-grained ureilites, 15 ureilites with variable texture/mineralogy, four trachyandesites, and two polymict breccias. We identified 81 non-ureilitic fragments, corresponding to 33% of the recovered samples studied in Münster. These included chondrites, namely 65 enstatite chondrites (43 EL; 22 EH), 11 ordinary chondrites (OC), one carbonaceous chondrite, and one unique R-like chondrite. Furthermore, three samples represent a unique type of enstatite achondrite. Since all AhS stones must be regarded as individual specimens independent from each other, the number of fresh ureilite and enstatite chondrite falls in our meteorite collections has been increased by several hundred percent. Overall, the samples weigh between &lt;1 and 250 g and have a mean mass of ~15 g. If we consider—almost 15 years after the fall—the mass calculations, observations during and after the asteroid entered the atmosphere, the mineralogy of the C1 stones AhS 91A and AhS 671, and the experimental work on fitting the asteroid spectrum (e.g., Goodrich et al., 2019; Jenniskens et al., 2010; Shaddad et al., 2010), the main portion of the meteoroid was likely made of the fine-grained (carbonaceous) dust and was mostly lost in the atmosphere. In particular, the fact that C1 materials were found has important implications for interpreting asteroid 2008 TC3's early spectroscopic results. Goodrich et al. (2019) correctly suggested that if scientists had not recovered the “water-free” samples (e.g., ureilites, enstatites, and OC) from the AhS strewn field, 2008 TC3 would have been assumed to be a carbonaceous chondrite meteoroid. Considering that the dominating mass of the exploding meteoroid consisted of carbonaceous materials, asteroid 2008 TC3 cannot be classified as a polymict ureilite; consequently, we state that the asteroid was a polymict carbonaceous chondrite breccia, specifically a polymict C1 object that may have formed by late accretion at least 50–100 Ma after calcium–aluminum-rich inclusions.
DOI: 10.34740/kaggle/dsv/5744428
title: Mahanagar Yatayat Dataset
DOI: 10.5281/zenodo.7957852
title: Geospatial, biophysical and socioeconomic data for the Athens municipality on a zipcode resolution

description: A collated dataset from various remote sensing, local and national sources.
DOI: 10.5281/zenodo.7957853
title: Geospatial, biophysical and socioeconomic data for the Athens municipality on a zipcode resolution

description: A collated dataset from various remote sensing, local and national sources.
DOI: 10.25411/aru.22816265
title: Ratings of auditory shape for pitch, loudness, and tempo gestures: Raw data across all triplet contexts

description: This dataset contains all raw gesture-shape ratings acquired during the experiment, notably, across so-called triplet contexts. <br> Data for pitch, loudness, and tempo gestures are in separate CSV files. <br> Each CSV file is formatted in "long format", that is, each row corresponds to one observation (dependent variable) for a specific stimulus condition (combination of independent variables) and one participant. The table columns contain the following information, from left to right: <strong>DV</strong>, dependent variable: Gesture-shape rating for either pitch, loudness or tempo <strong>acousFct</strong>: Acoustical/physical function or scale underlying the pitch, loudness or tempo variation, also denoted as letters A to D <strong>context</strong>: Triplet context of acoustical functions that was evaluated in the experimental trial, that is, ABC, ABD, ACD, BCD <strong>orient</strong>: Orientation of gesture, either increasing or decreasing over time <strong>durat</strong>: Duration, either short or long, not applicable for tempo <strong>level</strong>: Investigated level range, lower vs. higher for pitch, softer vs. louder for loudness, slower vs. faster for tempo <strong>pa</strong>: Participant identification number (arbitrary assignment)
DOI: 10.25411/aru.22816265.v1
title: Ratings of auditory shape for pitch, loudness, and tempo gestures: Raw data across all triplet contexts

description: This dataset contains all raw gesture-shape ratings acquired during the experiment, notably, across so-called triplet contexts. <br> Data for pitch, loudness, and tempo gestures are in separate CSV files. <br> Each CSV file is formatted in "long format", that is, each row corresponds to one observation (dependent variable) for a specific stimulus condition (combination of independent variables) and one participant. The table columns contain the following information, from left to right: <strong>DV</strong>, dependent variable: Gesture-shape rating for either pitch, loudness or tempo <strong>acousFct</strong>: Acoustical/physical function or scale underlying the pitch, loudness or tempo variation, also denoted as letters A to D <strong>context</strong>: Triplet context of acoustical functions that was evaluated in the experimental trial, that is, ABC, ABD, ACD, BCD <strong>orient</strong>: Orientation of gesture, either increasing or decreasing over time <strong>durat</strong>: Duration, either short or long, not applicable for tempo <strong>level</strong>: Investigated level range, lower vs. higher for pitch, softer vs. louder for loudness, slower vs. faster for tempo <strong>pa</strong>: Participant identification number (arbitrary assignment)
DOI: 10.25411/aru.22816247
title: Ratings of auditory shape for pitch and loudess gestures: Averaged data across triplet contexts

description: This dataset contains gesture-shape ratings that were averaged across the so-called triplet contexts. These ratings were used in the analyses of variance (ANOVA) reported in the article. <br> Data for pitch and loudness gestures are in separate CSV files. <br> Each CSV file is formatted in "long format", that is, each row corresponds to one observation (dependent variable) for a specific stimulus condition (combination of independent variables) and one participant. The table columns contain the following information, from left to right: <strong>DV</strong>, dependent variable: Gesture-shape rating for either pitch or loudness <strong>acousFct</strong>: Acoustical/physical function or scale underlying the pitch or loudness variation <strong>orient</strong>: Orientation of gesture, either increasing or decreasing over time <strong>durat</strong>: Duration, either short or long <strong>level</strong>: Investigated level range, lower vs. higher for pitch, softer vs. louder for loudness <strong>pa</strong>: Participant identification number (arbitrary assignment)
DOI: 10.25411/aru.22816247.v1
title: Ratings of auditory shape for pitch and loudess gestures: Averaged data across triplet contexts

description: This dataset contains gesture-shape ratings that were averaged across the so-called triplet contexts. These ratings were used in the analyses of variance (ANOVA) reported in the article. <br> Data for pitch and loudness gestures are in separate CSV files. <br> Each CSV file is formatted in "long format", that is, each row corresponds to one observation (dependent variable) for a specific stimulus condition (combination of independent variables) and one participant. The table columns contain the following information, from left to right: <strong>DV</strong>, dependent variable: Gesture-shape rating for either pitch or loudness <strong>acousFct</strong>: Acoustical/physical function or scale underlying the pitch or loudness variation <strong>orient</strong>: Orientation of gesture, either increasing or decreasing over time <strong>durat</strong>: Duration, either short or long <strong>level</strong>: Investigated level range, lower vs. higher for pitch, softer vs. louder for loudness <strong>pa</strong>: Participant identification number (arbitrary assignment)
DOI: 10.5281/zenodo.7502140
title: IODP Expedition 350 ICP-AES elemental analysis (solids)

description: Elemental contents in hard rock and sediment samples was measured by inductively coupled plasma - atomic emission spectrocopy (ICP-AES). Data are presented by element-wavelength pair (e.g., more than one calcium line may be reported). Elemental lines for which data do not exist for a particular expedition will not appear.