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Data set for journal paper 'Mode I fracture of thick adhesively bonded GFRP composite joints for wind turbine rotor blades' volume2

The description in the read me file is updated here. This data set includes all the related raw data about the journal paper 'Mode I fracture of thick adhesively bonded GFRP composite joints for wind turbine rotor blades' 1.The raw data of thick adhesive double cantilever beam tests under quasi-static loading, such as the DIC pictures and the load-displacement curve. The strain energy release curve and load-displacement prediction curve are also included. All the data excepts the DIC pictures is within one Excel file for each sample. 2.Data for tensile testing (composite and epoxy adhesive). Volume 1 includes the data of UN1,UN2,GN2 and GL2-L. Volume 2 includes the data of 5-GL2-M SAMPLE1. Volume 3 includes the data of 5-GL2-M SAMPLE2 AND 3. Volume 4 includes the data of 5-GL2-M SAMPLE4 and 6-GL2-H SAMPLE 1 and 2. Volume 5 includes the data of 6-GL2-H SAMPLE3 and 4. Volume 6 includes the tensile testing data.

Data set for journal paper 'Mode I fracture of thick adhesively bonded GFRP composite joints for wind turbine rotor blades' volume1

Data set for journal paper 'Mode I fracture of thick adhesively bonded GFRP composite joints for wind turbine rotor blades' volume6

Data set for journal paper 'Mode I fracture of thick adhesively bonded GFRP composite joints for wind turbine rotor blades' volume4

Data set for journal paper 'Mode I fracture of thick adhesively bonded GFRP composite joints for wind turbine rotor blades' volume5

Data set for journal paper 'Mode I fracture of thick adhesively bonded GFRP composite joints for wind turbine rotor blades' volume3

ACE Solar Wind Ion Composition Spectrometer (SWICS) Solar Wind Plasma Elemental and Isotopic Density, Speed, Thermal Speed, Charge State, and Ratio Parameters, Level 2 (L2), Daily Data

This ACE SWICS/SWIMS Data Set contains the He/O, C/O, N/O, Ne/O, Mg/O, Si/O, S/O, Fe/O Abundance Ratios, C, O, Mg, Si, Fe Average Charge States, C+6/C+4, C+6/C+5, O+7/O+6 Charge State Ratios, He+2, C+5, O+6, Fe+10 Speeds and Thermal Speeds, and a Solar Wind Type Parameter that characterizes the Solar Wind as either Streamer, Coronal Hole, Coronal Mass Ejection (CME), or Unidentified. The Solar Wind Ion Composition Spectrometer (SWICS), prior to August 23, 2011 and denoted as SWICS Version 1.1, determines uniquely the Chemical and Ionic Charge State Composition of the Solar Wind, the Temperatures and Mean Speeds of major Solar Wind Ions at all Speeds above 300 km/s for Protons and 170 km/s for Fe+16, and resolves Protons and Helium Isotopes of Solar and Interstellar Sources. SWICS 1.1 measures the Distribution Functions of Interstellar Cloud Pick-Up Ions and Interplanetary Dust Cloud Pick-Up Ions up to Energies of 100 keV/e. The ACE SWICS 1.1 Data Products represent a new Release of the Data with significantly improved Time Series Measurements for the Elemental Abundance, Charge State Composition, and Kinetic Properties of Heavy Ions in the Solar Wind. It is a major new Update produced with completely redesigned Analysis Methods to account more rigorously for Instrumental and Statistical Effects (Shearer et al., 2014). Rare Elements are now identified more reliably and Estimates of Statistical Error are provided. Release Notes are available that describe the Data, the Methods used to determine the Data Values, and Issues concerning Data Quality and Measurement Uncertainty. The Quality of ACE Level 2 Data is such that it is suitable for serious Scientific Study. However, to avoid Confusion and Misunderstanding, it is recommended that Users consult with the appropriate ACE Team Members before publishing Work derived from the Data. The ACE Team has worked hard to ensure that the Level 2 Data are free from Errors, but the Team cannot accept Responsibility for Erroneous Data, or for Misunderstandings about how the Data may be used. This is especially true if the appropriate ACE Team Members are not consulted before Publication. At the very least, Preprints should be forwarded to the ACE Team before Publication. For more Information about the SWICS Instrument, visit the SWICS Home Page at http://solar-heliospheric.engin.umich.edu/ace.

ACE Solar Wind Electron Proton Alpha Monitor (SWEPAM) 64-Second Level 2 Data

Solar Wind Ion parameters from ACE/SWEPAM. Level 2 data, 64-second averages. Parameters include proton density, temperature (radial component) and flow speed, flow velocity vector in GSE, GSM and RTN coordinates, and alpha to proton density ratio. ACE position vectors in GSE and GSM are included. The data are accessible via ftp in HDF and CDF from the ACE Science Center and CDAWeb, respectively, and in ASCII format from the value-added interfaces at those sites. Hourly averaged L2 plasma parameters are also available from these access paths. The "parameter keys" given below are as used by CDAWeb.

Wind Plasma and Radio Waves (WAVES) Electron Plasma Densities, Level H0 (H0), 17.664 s Data

Wind Waves high time resolution plasma densities estimated by using the electron density inferred from the thermal noise peak as recognized by a neural network.

ACE Solar Wind Ion Composition Spectrometer (SWICS) Solar Wind Plasma Elemental and Isotopic Density, Speed, Thermal Speed, Charge State, and Ratio Parameters, Level 2 (L2), 1 h Data

This ACE SWICS/SWIMS Data Set contains the Alpha Particle Number Density, Fe/O Abundance Ratio, C, O, Mg, Si, Fe Average Charge States, C+6/C+4, C+6/C+5, O+7/O+6 Charge State Ratios, He+2, C+5, O+6, Fe+10 Speeds and Thermal Speeds, and a Solar Wind Type Parameter that characterizes the Solar Wind as either Streamer, Coronal Hole, Coronal Mass Ejection (CME), or Unidentified. The Solar Wind Ion Composition Spectrometer (SWICS), prior to August 23, 2011 and denoted as SWICS Version 1.1, determines uniquely the Chemical and Ionic Charge State Composition of the Solar Wind, the Temperatures and Mean Speeds of major Solar Wind Ions at all Speeds above 300 km/s for Protons and 170 km/s for Fe+16, and resolves Protons and Helium Isotopes of Solar and Interstellar Sources. SWICS 1.1 measures the Distribution Functions of Interstellar Cloud Pick-Up Ions and Interplanetary Dust Cloud Pick-Up Ions up to Energies of 100 keV/e. The ACE SWICS 1.1 Data Products represent a new Release of the Data with significantly improved Time Series Measurements for the Elemental Abundance, Charge State Composition, and Kinetic Properties of Heavy Ions in the Solar Wind. It is a major new Update produced with completely redesigned Analysis Methods to account more rigorously for Instrumental and Statistical Effects (Shearer et al., 2014). Rare Elements are now identified more reliably and Estimates of Statistical Error are provided. Release Notes are available that describe the Data, the Methods used to determine the Data Values, and Issues concerning Data Quality and Measurement Uncertainty. The Quality of ACE Level 2 Data is such that it is suitable for serious Scientific Study. However, to avoid Confusion and Misunderstanding, it is recommended that Users consult with the appropriate ACE Team Members before publishing Work derived from the Data. The ACE Team has worked hard to ensure that the Level 2 Data are free from Errors, but the Team cannot accept Responsibility for Erroneous Data, or for Misunderstandings about how the Data may be used. This is especially true if the appropriate ACE Team Members are not consulted before Publication. At the very least, Preprints should be forwarded to the ACE Team before Publication. For more Information about the SWICS Instrument, visit the SWICS Home Page at http://solar-heliospheric.engin.umich.edu/ace.

Wind SMS Suite SupraThermal Ion Composition Spectrometer (SMS/STICS) Ion Velocity Distribution Functions (VDFs), Level 2 (L2), 3-minute Data in Solar Wind

The data include Wind STICS 3-minute 3D velocity distribution functions (VDFs) in three units (phase space density, differential number flux and counts), together with their statistical errors, 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. 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.

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SAKIGAKE SOLAR WIND EXPERIMENT DATA V1.0

The original dataset was called MST5SOW. It was personally delivered by Dr. Oyama. The sample hardcopy listed the column headings with units for the solar wind parameters bulk ion velocity, ion density, and ion temperature. The data format of the tape was included. The recorded jumps in the measured parameters indicate a disturbance at encounter. .

Wind SMS Suite SupraThermal Ion Composition Spectrometer (SMS/STICS) Ion Velocity Distribution Functions (VDFs), Level 2 (L2), 3-minute Data in Magnetosphere

The data include Wind STICS 3-minute 3D velocity distribution functions (VDFs) in three units (phase space density, differential number flux and counts), together with their statistical errors, 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. 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 Pitch Angle Distributions, Level 3 (L3), 13.981 s Data

* SPAN-Electron, SPAN-E, Instrument SPE Level 3 Data* --------------------------------------------------File Naming Format: psp_swp_spb_sf0_l3_pad_YYYYMMDD_v01.cdfThis data product contains measurements of the Electron Pitch Angle Distribution from the SPAN-B 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.

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.

Wind SMS Suite SupraThermal Ion Composition Spectrometer (SMS/STICS) Ion Moments, Level 2 (L2), 3-minute Data in Solar Wind

The data include Wind STICS 3-minute density (0th moment) and mean value of the energy distribution (1st moment), together with their statistical errors, 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. 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.

ACE SWEPAM Solar Wind Weimer Propagated 60 s Resolution Data in GSM Coordinates

ACE Weimer propagated solar wind data and linearly interpolated to have the measurements on the minute at 60 s resolution SWEPAM data in GSM coordinates. This data set consists of propagated solar wind data that has first been propagated to a position just outside of the nominal bow shock (about 17, 0, 0 Re) and then linearly interpolated to 1 min resolution using the interp1.m function in MATLAB. The input data for this data set is a 1 min resolution processed solar wind data constructed by Dr. J.M. Weygand. The method of propagation is similar to the minimum variance technique and is outlined in Dan Weimer et al. [2003; 2004]. The basic method is to find the minimum variance direction of the magnetic field in the plane orthogonal to the mean magnetic field direction. This minimum variance direction is then dotted with the difference between final position vector minus the original position vector and the quantity is divided by the minimum variance dotted with the solar wind velocity vector, which gives the propagation time. This method does not work well for shocks and minimum variance directions with tilts greater than 70 degrees of the sun-earth line. This data set was originally constructed by Dr. J.M. Weygand for Prof. R.L. McPherron, who was the principle investigator of two National Science Foundation studies: GEM Grant ATM 02-1798 and a Space Weather Grant ATM 02-08501. These data were primarily used in superposed epoch studies References: Weimer, D. R. (2004), Correction to Predicting interplanetary magnetic field (IMF) propagation delay times using the minimum variance technique, J. Geophys. Res., 109, A12104, doi:10.1029/2004JA010691. Weimer, D.R., D.M. Ober, N.C. Maynard, M.R. Collier, D.J. McComas, N.F. Ness, C. W. Smith, and J. Watermann (2003), Predicting interplanetary magnetic field (IMF) propagation delay times using the minimum variance technique, J. Geophys. Res., 108, 1026, doi:10.1029/2002JA009405.

ISEE-3 Linearly Interpolated 60 s Resolution Solar Wind Plasma data in GSM Coordinates

ISEE-3 linearly interpolated to have the measurements on the minute at 60 s resolution solar wind plasma data in GSM coordinates. This data set consists of processed solar wind data that has been linearly interpolated to 1 min resolution at the position of the spacecraft using the interp1.m function in MATLAB. This data set was originally constructed by Dr. J.M. Weygand for Prof. R.L. McPherron, who was the principle investigator of two National Science Foundation studies: GEM Grant ATM 02-1798 and a Space Weather Grant ATM 02-08501. These data were primarily used in superposed epoch studies and cross correlation studies on solar wind.

Pioneer Venus Orbiter (PVO) Magnetometer, OMAG, Plasma Analyzer, OPA, Merged Solar Wind Data, 10 min Data

Pioneer Venus Orbiter, PVO, was the first orbiter mission designed to conduct a comprehensive and long term investigation of the planet Venus. PVO measured the detailed structure of the upper atmosphere and ionosphere of Venus and investigated the interaction of the solar wind with the Venusian ionosphere. Over the years from 1978 to 1992, PVO provided nearly continuous measurements of the solar wind from its highly eccentric orbit around Venus. * PI, magnetic field instrument: C.T. Russell, University of California, Los Angeles * PI, plasma instrument: A. Barnes, Ames Research Center, NASA This merged data includes 10-minute averages for selected parameters of the interplanetary magnetic field, solar wind plasma, and spacecraft trajectory. The data were taken when the spacecraft was outside the bow shock of the Venusian ionosphere and was in the solar wind. Venus Solar Orbital (VSO) coordinates are defined with respect to the orbital plane of Venus which is tilted about two degrees from the Ecliptic. The VSO system is Venus-centered with the X axis towards the Sun, the Z axis northward and perpendicular to the orbital plane, and the Y axis completing the right hand system. Time coverage of merged data: 1978-12-06 to 1988-08-07. PVO data were converted to CDF based on the flatfiles from UCLA.

ISEE-3 Linearly Interpolated 60 s Resolution Solar Wind Plasma data in GSE Coordinates

ISEE-3 linearly interpolated to have the measurements on the minute at 60 s resolution solar wind plasma data in GSE coordinates. This data set consists of processed solar wind data that has been linearly interpolated to 1 min resolution at the position of the spacecraft using the interp1.m function in MATLAB. This data set was originally constructed by Dr. J.M. Weygand for Prof. R.L. McPherron, who was the principle investigator of two National Science Foundation studies: GEM Grant ATM 02-1798 and a Space Weather Grant ATM 02-08501. These data were primarily used in superposed epoch studies and cross correlation studies on solar wind.