Find research datasets worth reusing
Search datasets from major research repositories and use ShareScore to quickly assess how well each record supports discovery, access, and reuse.
95
datasets available to search
ShareScore release 0.9.0
Dataset results
95 results for “Wind energy”
Resource and Load Compatibility Assessment of Wind Energy Offshore of Humboldt County, California: Data and Software
<p>These files contain the raw data and code used to analyzed wind resource and local load compatibility of offshore wind in Humboldt, California.</p>
JRC - The Role of Rare Earth Elements in Wind Energy and Electric Mobility - Database
<p>This dataset contains supply, demand and recycling scenarios for the rare-earth elements used in wind energy and electric mobility. Information on resources and reserves of all rare-earth elements is also provided.</p> <p>The dataset refers to the following report by the European Commission's Joint Research Centre (JRC):</p> <p>Alves Dias P., Bobba S., Carrara S. and Plazzotta B., The role of rare earth elements in wind energy and electric mobility, EUR 30488 EN, Publication Office of the European Union, Luxembourg, 2020, ISBN 978-92-76-27016-4, doi:10.2760/ 303258, JRC122671</p> <p>The report can be found at the following link:</p> <p><a href="https://ec.europa.eu/jrc/en/publication/eur-scientific-and-technical-research-reports/role-rare-earth-elements-wind-energy-and-electric-mobility">https://ec.europa.eu/jrc/en/publication/eur-scientific-and-technical-research-reports/role-rare-earth-elements-wind-energy-and-electric-mobility</a></p>
High-Frequency Winds Amplify Forward Kinetic Energy Cascades at the Air-Sea Interface
<p>This dataset contains animations of the <span>partitioned currents into balanced motions (BMs) and internal gravity waves (IGWs) expressed in physical domain for COAS (upper row) and LLC (lower row). The si<span>mulations represent KE and gradients of velocity normalized by Coriolis frequency</span></span></p>
Area Potential for Onshore Wind Energy in Germany
<p>Area potential for deployment of onshore wind energy in Germany compiled as a shape file. Calculated polygons consider various social, environmental and economic constraints. Polygon attributes consider statistics on wind quality, form of land-use, among others. A detailed description is provided in: <a href="https://nbn-resolving.org/urn:nbn:de:bsz:14-qucosa2-902715" target="_blank" rel="noopener">https://nbn-resolving.org/urn:nbn:de:bsz:14-qucosa2-902715</a>.</p>
X-Shooting ULLYSES: Massive Stars at low metallicity VII. Stellar and Wind Properties of B supergiants in the SMC - Appendix F: Spectral energy distributions and spectral fits
Open the record for dataset details and reuse information.
Virtual Energy Storage - Wind power
<p>Wind power data of 20,020 wind farms and generalization to Thiessen polygons</p>
STEREO-A PLasma and Supra-Thermal Ion Composition (PLASTIC) He⁺ Counts and Relative Energy Flux in four Velocity Ranges normalized by the Solar Wind Speed, Level 3 (L3), Daily Data
STEREO-A Plasma and Suprathermal Ion Composition, Singly-charged Helium, He⁺, counts and relative differential energy fluxes binned by the ion speed relative to the solar wind bulk speed, four speed ratio bins. STEREO PLASTIC daily suprathermal He⁺ pickup ion signatures include He⁺ energy spectra, directional information, and contenxt information, such as the H⁺ plasma velocity. The four speed ratio, V/Vsw, bin ranges of are: 1.44 to 1.85, 1.85 to 2.50, 2.50 to 3.50, and 3.50 to 8.00. The identification of He⁺ is based on the measurement of energy per charge, E/q, time-of-flight, TOF, and total energy deposited in the solid state detector, SSD. These data include double coincidence measurements by using E/Qi and TOF and triple coincidence measurements by using E/Q, TOF, and SSD, see for example Galvin et al., Space Sci. Rev. 136, p 437-468, 2008. The proton bulk parameters including speed, Vsw, thermal velocity, Vth, and Density, Np, in this file are derived from a one-deminsional, 1-D, Maxwellian fit to a single detector rate with no coincidence required. These proton bulk parameters are corrected for background and dead time. The software version number used to derive the proton bulk parameters is shown in the file header and is described in the section on file formats. The most recent update of the proton bulk parameters can be found on the following STEREO website: http://stereo-ssc.nascom.nasa.gov/data/ins_data/plastic/level2/Protons/ For a full explanation, see the description at: https://stereo-ssc.nascom.nasa.gov/data/ins_data/plastic/level3/HePlus/HePlus_flux/READ_ME_PLASTIC_HePlus_Fluxes.pdf The singly-charged Helium, He⁺, flux data are also available from the STEREO Science Center in ASCII format via: https://stereo-ssc.nascom.nasa.gov/data/ins_data/plastic/level3/HePlus/ Note that this SPASE Numerical Description only describes the MESSENGER Magnetometer data stored in Common Data Files.
PSP Solar Wind Electrons Alphas and Protons (SWEAP) SPAN-A Proton Differential Energy Flux for each Deflector Step, Energy, and Anode, Level 2 (L2), 7 s Data
SPI Level 2 Data----------------File Naming Format: psp_swp_spi_sf00_l2_8dx32ex8a_YYYYMMDD_v01.cdfThis data product contains measurements of differential proton energy flux at each measured deflector step, energy, and anode for the SPAN Ion instrument.Parker Solar Probe SWEAP Rules of the Road------------------------------------------As part of the development of collaboration with the broader Heliophysics community, the mission has drafted a "Rules of the Road" to govern how PSP instrument data are to be used.* 1) Users should consult with the PI to discuss the appropriate use of instrument data or model results and to ensure that the users are accessing the most recently available versions of the data and of the analysis routines. Instrument team Science Operations Centers, SOCs, and/or Virtual Observatories, VOs, should facilitate this process serving as the contact point between PI and users in most cases.* 2) Users should heed the caveats of investigators to the interpretations and limitations of data or model results. Investigators supplying data or models may insist that such caveats be published. Data and model version numbers should also be specified.* 3) Browse products, Quicklook, and Planning data are not intended for science analysis or publication and should not be used for those purposes without consent of the PI.* 4) Users should acknowledge the sources of data used in all publications, presentations, and reports: "We acknowledge the NASA Parker Solar Probe Mission and the SWEAP team led by J. Kasper for use of data.".* 5) Users are encouraged to provide the PI a copy of each manuscript that uses the PI data prior to submission of that manuscript for consideration of publication. On publication, the citation should be transmitted to the PI and any other providers of data.
Wind 3DP SST Open Proton Energy-Angle Distributions
Proton energy-angle distributions 70 keV - 6.8 MeV, often at 24 sec, SST Open, Wind 3DP - R. Lin (UC Berkeley)
Wind 3DP SST Foil Electron Energy-Angle Distributions
Electron energy-angle distributions 27-520 keV, often at 24 sec, SST Foil, Wind 3DP - R. Lin (UC Berkeley)
PSP Solar Wind Electrons Alphas and Protons (SWEAP) SPC Ion Charge Flux Distributions, Electrical Current versus Time and Energy-per-Charge, Level 2 (L2), 0.2185 s Data
SPC Level 2 Ion Data--------------------File Naming Format: psp_swp_spc_l2i_yyyymmdd_v01.cdfSolar Probe Cup, SPC, charge flux distributions comprise electrical current as a function of time and energy-per-charge, with appropriate instrument response elements considered and calibrations applied. This data product contains measurements of ion flux as a function of energy organized into spectra. The SPC instrument measures one-dimensional distributions with a wide field of view. Please refer to the instrument paper for details.This data set covers all periods for which the instrument was turned on and taking data in the solar wind in ion mode. This includes maneuvers affecting the spacecraft attitude and orientation.The MODE_FLAG variable contains information about the type of spectrum being measured. "Ion Full Scan" spectra are marked with MODE_FLAG.DAT = 1. These spectra comprise a broad energy range typically with lower signal-to-noise than the more frequent "Ion Peak Tracking" spectra, which are marked with MODE_FLAG.DAT equal to zero. In the most frequent operating mode, ion full scans are executed about once every 30 s or whenever the peak signal from the solar wind is poorly defined.SPC Encounter 1 Remarks-----------------------Data quality is very good for the duration of the encounter. The solar wind flow was within the optimal field of view for the SPC instrument for nearly the entire encounter. See the data flags for specific exceptions. As with all encounters, signal-to-noise is higher during ingress than egress, which is reflected in the typically smaller uncertainties and less frequent "primary peak low signal" flag events.SPC Cruise Phase Remarks------------------------Measurements recorded during cruise phase are not all transmitted to Earth. The typical return is one spectrum out of every 32.SPC Encounter 2 Remarks-----------------------Due to an erroneous setting in the operating mode for this encounter, ion full scan spectra and certain spectra immediately following ion full scans are of reduced quality. In the affected full scan spectra, the energy steps over an initial portion of the measurement spectra have zero width, i.e. the Level 2 ion variables MV_LO.DAT = MV_HI.DAT, and the corresponding measurements are purely noise. In some cases, this results in a poor determination of the proton "primary peak" energy, which renders additional subsequent full scans that follow subject to the same incompleteness. In other cases, the energy range for the subsequent "ion peak tracking mode" scan is not ideal. The affected Level 3 ion measurements have been flagged with DQF.DAT[22]=1, which stands for "energy ranging/peak tracking error" and/or set to fill. The operating mode has been revised such that future encounters will not be so affected.Parker Solar Probe SWEAP Rules of the Road------------------------------------------As part of the development of collaboration with the broader Heliophysics community, the mission has drafted a "Rules of the Road" to govern how PSP instrument data are to be used.* 1) Users should consult with the PI to discuss the appropriate use of instrument data or model results and to ensure that the users are accessing the most recently available versions of the data and of the analysis routines. Instrument team Science Operations Centers, SOCs, and/or Virtual Observatories, VOs, should facilitate this process serving as the contact point between PI and users in most cases.* 2) Users should heed the caveats of investigators to the interpretations and limitations of data or model results. Investigators supplying data or models may insist that such caveats be published. Data and model version numbers should also be specified.* 3) Browse products, Quicklook, and Planning data are not intended for science analysis or publication and should not be used for those purposes without consent of the PI.* 4) Users should acknowledge the sources of data used in all publications, presentations, and reports: "We acknowledge the NASA Parker Solar Probe Mission and the SWEAP team led by J. Kasper for use of data.".* 5) Users are encouraged to provide the PI a copy of each manuscript that uses the PI data prior to submission of that manuscript for consideration of publication. On publication, the citation should be transmitted to the PI and any other providers of data.
Wind SMS Suite SupraThermal Ion Composition Spectrometer (SMS/STICS) Energy-Resolved Pitch-Angle Distributions (ERPAs), Level 2 (L2), 30-minute Data in Solar Wind
The data include Wind STICS 30-minute Energy-Resolved Pitch-Angle Distributions (ERPAs) for selected ion species using triple coincidence (H+, He+, He2+, C5+, O+, O6+, and Fe10+) and double coincidence (H+, He+, He2+, O+, O6+) measurements in the solar wind. ERPAs organize the data by the angle relative to the magnetic field vector direction, in 7.5 degree bins. The energy separation is preserved at the native resolution of the E/q bins. For details, see https://spdf.gsfc.nasa.gov/pub/data/wind/documents/wind_stics_lv2_release_notes_revD.pdf .The Suprathermal Ion Composition Spectrometer (STICS) is a time of flight (TOF) plasma mass spectrometer, capable of identifying mass and mass per charge for incident ions up to 200 keV/e. It uses an electrostatic analyzer to admit ions of a particular energy per charge (E/Q) into the TOF chamber. The E/Q voltage is stepped through 32 values, sitting at each value for approximately 24 sec., to measure ions over the full E/Q range of 6 - 200 keV/e. Ions then pass through a carbon foil and TOF chamber, before finally impacting on a solid-state detector (SSD) for energy measurement. STICS combines these three measurements of E/Q, TOF and residual energy, producing PHA words. This triple-coincidence technique greatly improves the signal to noise ratio in the data. Measurements of E/Q and TOF without residual energy also produce PHA words. These double-coincidence measurements are characterized by better statistics since ions whose energy does not allow them to be registered by the SSD can still be counted in double-coincidence measurements. However, ion identification in double-coincidence measurements are limited to a select number of ions that are well separated in E/Q - TOF space. The STICS instrument provides full 3D velocity distribution functions, through a combination of multiple telescopes and spacecraft spin. The instrument includes 3 separate TOF telescopes that view 3 separate latitude sectors, as shown in Figure 1 (https://spdf.gsfc.nasa.gov/pub/data/wind/documents/wind_stics_lv2_release_notes_revD.pdf). In addition, the WIND spacecraft spins, allowing the 3 telescopes to trace out a nearly 4π steradian viewing area. The longitudinal sectors are shown in Figure 2. The solar direction is in sectors 8-10 while the earthward direction is in sectors 0-2.
PSP Solar Wind Electrons Alphas and Protons (SWEAP) SPAN-A Electron Energy Spectra, Level 2 (L2), 1.74 s Data
SPAN-E Level 2 ELectron Energy Spectra Data-------------------------------------------File Naming Format: psp_swp_spa_sf1_L2_32E_YYYYMMDD_v01.cdfThe SF1 product is an energy spectrum produced on the spacecraft by summing over the Theta and Phi directions. The units are differential energy flux and eV. The sample filename above includes 32 Energies.The larger Theta angles (deflection angles) are artificially enhanced in the "sf1" energy spectra data products due to the method of spectra production on the SPAN-E instrument (straight summing). Thus, SF1 energy spectra are not recommended for rigid statistical analysis.Parker Solar Probe SWEAP Solar Probe Analyzer, SPAN, Electron Data Release Notes--------------------------------------------------------------------------------November 19, 2019 Initial Data Release--------------------------------------Overview of Measurements------------------------The SWEAP team is pleased to release the data from Encounter 1 and Encounter 2. The files contain data from the time range October 31, 2018 - June 18, 2019.The prime mission of Parker Solar Probe is to take data when within 0.25 AU of the Sun during its orbit. However, there has been some extended campaign measurements outside of this distance. The data are available for those days that are within 0.25 AU as well as those days when the instruments were operational outside of 0.25 AU.Each SWEAP data file includes a set of a particular type of measurements over a single observing day. Measurements are provided in Common Data Format (CDF), a self-documenting data framework for which convenient open source tools exist across most scientific computing platforms. Users are strongly encouraged to consult the global metadata in each file, and the metadata that are linked to each variable. The metadata includes comprehensive listings of relevant information, including units, coordinate systems, qualitative descriptions, measurement uncertainties, methodologies, links to further documentation, and so forth.SPAN-E Level 2 Version 01 Release Notes---------------------------------------The SPAN-Ae and SPAN-B instruments together have fields of view covering >90% of the sky; major obstructions to the FOV include the spacecraft heat shield and other intrusions by spacecraft components. Each individual SPAN-E has FOV of ±60° in Theta and 240° in Phi. The rotation matrices to convert into the spacecraft frame can be found in the individual CDF files, or in the instrument paper.This data set covers all periods for which the instrument was turned on and taking data in the solar wind in ion mode. This includes maneuvers affecting the spacecraft attitude and orientation. Measurements taken by SPAN-B when the spacecraft is pointed away from the sun are taken in sunlight.The data quality flags for the SPAN data can be found in the CDF files as: QUALITY_FLAG (0=good, 1=bad)General Remarks for Version 01 Data-----------------------------------Users interested in field-aligned electrons should take care regarding potential blockages from the heat shield when B is near radial, especially in SPAN-Ae. Artificial reductions in strahl width can result.Due to the relatively high electron temperature in the inner heliosphere, many secondary electrons are generated from spacecraft and instrument surfaces. As a result, electron measurements in this release below 30 eV are not advised for scientific analysis.The fields of view in SPAN-Ae and SPAN-B have many intrusions by the spacecraft, and erroneous pixels discovered in analysis, in particular near the edges of the FOV, should be viewed with skepticism. Details on FOV intrusion are found in the instrument paper, forthcoming, or by contacting the SPAN-E instrument scientist.The instrument mechanical attentuators are engaged during the eight days around perihelia 1 and perihelia 2, which results in a factor of about 10 reduction of the total electron flux into the instrument. During these eight days, halo electron measurements are artificially enhanced in the L2 products as a result of the reduced instrument geometric factor and subsequent ground corrections.A general note for Encounter 1 and Encounter 2 data: a miscalculation in the deflection tables loaded to both SPAN-Ae and SPAN-B resulted in over-deflection of the outermost Theta angles during these encounters. As such, pixels at large Thetas should be ignored. This error was corrected by a table upload prior to Encounter 3.Lastly, when viewing time gaps in the SPAN-E measurements, be advised that the first data point produced by the instrument after a power-on is the maximum value permitted by internal instrument counters. Therefore, the first data point after powerup is erroneous and should be discarded, as indicated by quality flags.SPAN-E Encounter 1 Remarks--------------------------SPAN-E operated nominally for the majority of the first encounter. Exceptions to this include: a few instances of corrupted, higher-energy sweep tables, and an inst
Wind SMS Suite SupraThermal Ion Composition Spectrometer (SMS/STICS) Energy-Resolved Pitch-Angle Distributions (ERPAs), Level 2 (L2), 30-minute Data in Magnetosphere
The data include Wind STICS 30-minute Energy-Resolved Pitch-Angle Distributions (ERPAs) for selected ion species using triple coincidence (H+, He+, He2+, C5+, O+, O6+, and Fe10+) and double coincidence (H+, He+, He2+, O+, O6+) measurements in the magnetosphere. ERPAs organize the data by the angle relative to the magnetic field vector direction, in 7.5 degree bins. The energy separation is preserved at the native resolution of the E/q bins. For details, see https://spdf.gsfc.nasa.gov/pub/data/wind/documents/wind_stics_lv2_release_notes_revD.pdf.The Suprathermal Ion Composition Spectrometer (STICS) is a time of flight (TOF) plasma mass spectrometer, capable of identifying mass and mass per charge for incident ions up to 200 keV/e. It uses an electrostatic analyzer to admit ions of a particular energy per charge (E/Q) into the TOF chamber. The E/Q voltage is stepped through 32 values, sitting at each value for approximately 24 sec., to measure ions over the full E/Q range of 6 - 200 keV/e. Ions then pass through a carbon foil and TOF chamber, before finally impacting on a solid-state detector (SSD) for energy measurement. STICS combines these three measurements of E/Q, TOF and residual energy, producing PHA words. This triple-coincidence technique greatly improves the signal to noise ratio in the data. Measurements of E/Q and TOF without residual energy also produce PHA words. These double-coincidence measurements are characterized by better statistics since ions whose energy does not allow them to be registered by the SSD can still be counted in double-coincidence measurements. However, ion identification in double-coincidence measurements are limited to a select number of ions that are well separated in E/Q - TOF space. The STICS instrument provides full 3D velocity distribution functions, through a combination of multiple telescopes and spacecraft spin. The instrument includes 3 separate TOF telescopes that view 3 separate latitude sectors, as shown in Figure 1 (https://spdf.gsfc.nasa.gov/pub/data/wind/documents/wind_stics_lv2_release_notes_revD.pdf). In addition, the WIND spacecraft spins, allowing the 3 telescopes to trace out a nearly 4π steradian viewing area. The longitudinal sectors are shown in Figure 2. The solar direction is in sectors 8-10 while the earthward direction is in sectors 0-2.
PSP Solar Wind Electrons Alphas and Protons (SWEAP) SPAN-B Electron Energy Spectra, Level 2 (L2), 1.74 s Data
SPAN-E Level 2 ELectron Energy Spectra Data-------------------------------------------File Naming Format: psp_swp_spb_sf1_L2_32E_YYYYMMDD_v01.cdfThe SF1 product is an energy spectrum produced on the spacecraft by summing over the Theta and Phi directions. The units are differential energy flux and eV. The sample filename above includes 32 Energies.The larger Theta angles (deflection angles) are artificially enhanced in the "sf1" energy spectra data products due to the method of spectra production on the SPAN-E instrument (straight summing). Thus, SF1 energy spectra are not recommended for rigid statistical analysis.Parker Solar Probe SWEAP Solar Probe Analyzer, SPAN, Electron Data Release Notes--------------------------------------------------------------------------------November 19, 2019 Initial Data Release--------------------------------------Overview of Measurements------------------------The SWEAP team is pleased to release the data from Encounter 1 and Encounter 2. The files contain data from the time range October 31, 2018 - June 18, 2019.The prime mission of Parker Solar Probe is to take data when within 0.25 AU of the Sun during its orbit. However, there has been some extended campaign measurements outside of this distance. The data are available for those days that are within 0.25 AU as well as those days when the instruments were operational outside of 0.25 AU.Each SWEAP data file includes a set of a particular type of measurements over a single observing day. Measurements are provided in Common Data Format (CDF), a self-documenting data framework for which convenient open source tools exist across most scientific computing platforms. Users are strongly encouraged to consult the global metadata in each file, and the metadata that are linked to each variable. The metadata includes comprehensive listings of relevant information, including units, coordinate systems, qualitative descriptions, measurement uncertainties, methodologies, links to further documentation, and so forth.SPAN-E Level 2 Version 01 Release Notes---------------------------------------The SPAN-Ae and SPAN-B instruments together have fields of view covering >90% of the sky; major obstructions to the FOV include the spacecraft heat shield and other intrusions by spacecraft components. Each individual SPAN-E has FOV of ±60° in Theta and 240° in Phi. The rotation matrices to convert into the spacecraft frame can be found in the individual CDF files, or in the instrument paper.This data set covers all periods for which the instrument was turned on and taking data in the solar wind in ion mode. This includes maneuvers affecting the spacecraft attitude and orientation. Measurements taken by SPAN-B when the spacecraft is pointed away from the sun are taken in sunlight.The data quality flags for the SPAN data can be found in the CDF files as: QUALITY_FLAG (0=good, 1=bad)General Remarks for Version 01 Data-----------------------------------Users interested in field-aligned electrons should take care regarding potential blockages from the heat shield when B is near radial, especially in SPAN-Ae. Artificial reductions in strahl width can result.Due to the relatively high electron temperature in the inner heliosphere, many secondary electrons are generated from spacecraft and instrument surfaces. As a result, electron measurements in this release below 30 eV are not advised for scientific analysis.The fields of view in SPAN-Ae and SPAN-B have many intrusions by the spacecraft, and erroneous pixels discovered in analysis, in particular near the edges of the FOV, should be viewed with skepticism. Details on FOV intrusion are found in the instrument paper, forthcoming, or by contacting the SPAN-E instrument scientist.The instrument mechanical attentuators are engaged during the eight days around perihelia 1 and perihelia 2, which results in a factor of about 10 reduction of the total electron flux into the instrument. During these eight days, halo electron measurements are artificially enhanced in the L2 products as a result of the reduced instrument geometric factor and subsequent ground corrections.A general note for Encounter 1 and Encounter 2 data: a miscalculation in the deflection tables loaded to both SPAN-Ae and SPAN-B resulted in over-deflection of the outermost Theta angles during these encounters. As such, pixels at large Thetas should be ignored. This error was corrected by a table upload prior to Encounter 3.Lastly, when viewing time gaps in the SPAN-E measurements, be advised that the first data point produced by the instrument after a power-on is the maximum value permitted by internal instrument counters. Therefore, the first data point after powerup is erroneous and should be discarded, as indicated by quality flags.SPAN-E Encounter 1 Remarks--------------------------SPAN-E operated nominally for the majority of the first encounter. Exceptions to this include: a few instances of corrupted, higher-energy sweep tables, and an inst
ScienceDex guides
Understand access before you commit
These curated guides explain access requirements, typical timelines, costs, and reuse considerations for widely used research datasets.
Allen Brain Atlas
Allen Brain Atlas is an Allen Institute collection of brain map atlases, datasets, APIs, and analysis tools covering mouse, human, and non-human primate brain resources.
Annotated Behaviour and Observability Dataset (ABODe)
ABODe is a University of Edinburgh DataShare dataset for behavior classification in group-housed mice using home-cage video, identities, bounding boxes, ground-plate positions, and annotator labels.
DANDI Archive for NWB datasets
DANDI is a BRAIN Initiative archive for publishing and sharing neurophysiology data, including electrophysiology, optophysiology, and behavioral data packaged as NWB and related standards.
International Brain Laboratory public data
The International Brain Laboratory public data releases expose standardized mouse decision-making experiments, including Neuropixels recordings, widefield calcium imaging, behavior, and session metadata accessed through the ONE API.
OpenNeuro
OpenNeuro is a free, open platform for sharing neuroimaging datasets, with public search, dataset pages, and download paths for web, S3, DataLad, and the OpenNeuro CLI.