Find research datasets worth reusing

opencc-by-4.0May 2020View details →

Laboratory measurements of wind, waves, and turbulence in hurricane conditions in the ASIST wind-wave facility

Laboratory measurements of wind, waves, and turbulence in hurricane conditions, collected in September and October of 2018 and January of 2019 in the ASIST wind-wave facility, in the SUSTAIN laboratory at the University of Miami. This dataset includes two experiments, one with fresh water ("fresh") and another with seawater ("salt"), each in 10-m winds from 0 to approximately 42 m/s. Data include: <ul> <li>3-dimensional wind velocity at 20 Hz sampling frequency from Campbell Scientific IRGASON sonic anemometer (collected in 2018)</li> <li>2-dimensional (along-tank and vertical) wind velocity at 1000 Hz sampling frequency from TSI IFA-300 hot film anemometer (collected in 2018)</li> <li>1-dimensional (along-tank) wind velocity at 10 Hz sampling frequency from a pitot anemometer (collected in 2018 and 2019)</li> <li>3-dimensional water velocity in the bottom 5 cm of the tank at 100 Hz sampling velocity from Nortek Vectrino velocimeter. (collected in 2018)</li> <li>Water elevation at 20 Hz sampling frequency at 6 locations in the tank from Senix Toughsonic 30 ultrasonic distance meters (collected in 2019)</li> <li>Along-tank static air pressure difference at 10 Hz sampling frequency from Baratron MKS 226 differential pressure transducer (collected in 2019)</li> </ul> All data is in NetCDF4 format. Experiment set up and positions of instruments are documented in more detail in Curcic and Haus (2020), Revised estimates of ocean surface drag in strong winds, Geophysical Research Letters, <a href="https://agupubs.onlinelibrary.wiley.com/doi/10.1029/2020GL087647">https://agupubs.onlinelibrary.wiley.com/doi/10.1029/2020GL087647</a>. Produced as part of the National Science Foundation Award #1745384, titled "Air-Sea Momentum Transfer in Extreme Wind Conditions". Contact: Milan Curcic <mcurcic@miami.edu>

opencc-by-4.0May 2020View details →

P-S waves 3D velocity model of Los Humeros area from earthquake based travel-time tomography using CAT3D software (OGS)

The dataset contains the 3D velocity model (VP (m/s), VS (m/s) and VP/VS) obtained from the tomographic inversion of seismological data in the area of Los Humeros (Mexico). The model was performed in the frame of the GEMex project (Mexico‐Europe Cooperation for research of enhanced geothermal systems and super-hot geothermal systems, WP5 ‘Detection of deep structures’, Jousset et al., D5.3, 2019). The inversion used 2661 P arrivals and 2272 S arrivals associated to 395 earthquakes recorded by 37 stations. The picking data was provided by Toledo et al., 2019. The inversion was performed by CAT3D software, a tomographic tool developed by OGS, which uses the SIRT method (Simultaneous Iterative Reconstruction Technique, Stewart, 1993) as inversion algorithm and the ray tracing procedure based on minimum time principle (Böhm et al., 1999). The velocities used as initial model for tomography were provided by the interpolated values obtained from the velocity analysis of four 2D seismic lines acquired inside the same investigated area by the tomographic inversion (See GEMex deliverable D5.3). The 3D velocity model is defined by a 3D grid of 61 nodes in X, 69 nodes in Y and 29 nodes in Z, equally spaced by 250 m in all directions. The total dimensions of the model is 15x17x7 km and the borders positions are (m) (WGS 84/UTM ZONE 14N): Xmin = 655000, Xmax = 670000 Ymin = 2168000, Ymax = 2185000 Zmin = -3000, Zmax = 4000

MPU9250 MEMS IMU Sine wave acceleration excitation along the Z axis

MPU9250 MEMS IMU Sine wave acceleration excitation along the Z axis The file Met4FOF_mpu9250_Z_Acc_10_hz_250_hz_6rep_ADC.dump contains a dump of the ADC protbuff messages recorded by the Met4FoF dataaqusition unit during the calibration measurement. The ADC is sampled synchronously to the data ready signals of the MPU9250. The file Met4FOF_mpu9250_Z_Acc_10_hz_250_hz_6rep_Sensor.dump contains a dump of the MPU9250 protbuff messages recorded by the Met4FoF dataaqusition unit during the calibration measurement. Met4FOF_mpu9250_Z_Acc_10_hz_250_hz_6rep.xlsx contains the accelerations recorded by the PTB refferenzsystem for each measurement run. The phase is referred to the analog reference values in the channel Data_11  Met4FOF_mpu9250_Z_Acc_10_hz_250_hz_6rep.csv contains the values from the excel table in panda readable form. 1FE4_AC_CAL.zip contains various measurements of the ADC transfer function as JSON files.

opencc-by-4.0Nov 2023View details →

Van Allen Probes Occurrence Rates of Electromagnetic Ion Cyclotron (EMIC) Waves with Rising Tones

CSV files with the values for the occurrence rates of electromagnetic ion cyclotron (EMIC) waves with rising tones observed by the Van Allen Probes from 2012-09-07 to 2016-07-01 from the paperSigsbee, K., Kletzing, C. A., Faden, J., & Smith, C. W. (2023). Occurrence rates of electromagnetic ion cyclotron (EMIC) waves with rising tones in the Van Allen Probes data set. Journal of Geophysical Research: Space Physics, 128, e2022JA030548. https://doi.org/10.1029/2022JA030548 The below files contain the values from Figures 5 and 6. The first row of each file gives the lower value of each L shell bin (0.0, 0.5, 1.0, 1.5, 2.0, 2.5, 3.0, 3.5, 4.0, 4.5, 5.5, 6.0, 7.0, 7.5).  The first column of each file gives the magnetic local time (MLT) values (0-23) for each bin. rbspab_lshellmlt_minutes_20120907_to_20160701.csv gives the number of minutes spent by the Van Allen Probes in each bin of L shell and MLT.rbspab_emic_lshellmlt_pcnt_20120907_to_20160701.csv gives the percentage of minutes all EMIC waves were observed in each bin of L shell and MLT.rbspab_h_lshellmlt_pcnt_20120907_to_20160701.csv gives the percentage of minutes H+ band EMIC waves were observed in each bin of L shell and MLT.rbspab_hr_lshellmlt_pcnt_20120907_to_20160701.csv gives the percentage of minutes H+ band EMIC waves with rising tones were observed in each bin of L shell and MLT.rbspab_he_lshellmlt_pcnt_20120907_to_20160701.csv gives the percentage of minutes He+ band EMIC waves were observed in each bin of L shell and MLT.rbspab_her_lshellmlt_pcnt_20120907_to_20160701.csv gives the percentage of minutes He+ band EMIC waves with rising tones were observed in each bin of L shell and MLT.rbspab_o_lshellmlt_pcnt_20120907_to_20160701.csv gives the percentage of minutes O+ band EMIC waves with rising tones were observed in each bin of L shell and MLT.The below files contain the values from Figures 7-13.  The first row of each file gives the lower value of each bin of the radial distance RXY in the XY SM plane  (0.0, 0.5, 1.0, 1.5, 2.0, 2.5, 3.0, 3.5, 4.0, 4.5, 5.5, 6.0, 7.0, 7.5) in Earth radii (RE).  The first column of each file gives the lower value of each bin of Z SM in RE (-2.0, -1.75, -1.5, -1.25, -1.0, 0.0, 1.0, 1.25, 1.50, 1.75).  Separate files are provided for four MLT sectors: midnight (21 MLT to 3 MLT), dawn (3 MLT to 9 MLT), noon (9 MLT to 15 MLT), and dusk (15 MLT to 21 MLT).Number of minutes spent by the Van Allen Probes in bins of RXY and Z SM (Figure 7):rbspab_rxyzsm_minutes_midnight_20120907_to_20160701.csv,         rbspab_rxyzsm_minutes_dawn_20120907_to_20160701.csv,             rbspab_rxyzsm_minutes_noon_20120907_to_20160701.csv,         rbspab_rxyzsm_minutes_dusk_20120907_to_20160701.csv             Percentage of minutes all EMIC waves were observed in bins of RXY and Z SM (Figure 8):rbspab_emic_rxyzsm_pcnt_midnight_20120907_to_20160701.csv, rbspab_emic_rxyzsm_pcnt_dawn_20120907_to_20160701.csv, rbspab_emic_rxyzsm_pcnt_noon_20120907_to_20160701.csv, rbspab_emic_rxyzsm_pcnt_dusk_20120907_to_20160701.csv     Percentage of minutes H+ band EMIC waves were observed in bins of RXY and Z SM (Figure 9):rbspab_h_rxyzsm_pcnt_midnight_20120907_to_20160701.csv, rbspab_h_rxyzsm_pcnt_dawn_20120907_to_20160701.csv, rbspab_h_rxyzsm_pcnt_noon_20120907_to_20160701.csv, rbspab_h_rxyzsm_pcnt_dusk_20120907_to_20160701.csv  Percentage of minutes He+ band EMIC waves were observed in bins of RXY and Z SM (Figure 10):rbspab_he_rxyzsm_pcnt_midnight_20120907_to_20160701.csv, rbspab_he_rxyzsm_pcnt_dawn_20120907_to_20160701.csv, rbspab_he_rxyzsm_pcnt_noon_20120907_to_20160701.csv, rbspab_he_rxyzsm_pcnt_dusk_20120907_to_20160701.csv  Percentage of minutes O+ band EMIC waves were observed in bins of RXY and Z SM (Figure 11):rbspab_o_rxyzsm_pcnt_midnight_20120907_to_20160701.csv, rbspab_o_rxyzsm_pcnt_dawn_20120907_to_20160701.csv, rbspab_o_rxyzsm_pcnt_noon_20120907_to_20160701.csv, rbspab_o_rxyzsm_pcnt_dusk_20120907_to_20160701.csv  Percentage of minutes H+ band EMIC waves with rising tones were observed in bins of RXY and Z SM (Figure 12):rbspab_hr_rxyzsm_pcnt_midnight_20120907_to_20160701.csv, rbspab_hr_rxyzsm_pcnt_dawn_20120907_to_20160701.csv, rbspab_hr_rxyzsm_pcnt_noon_20120907_to_20160701.csv, rbspab_hr_rxyzsm_pcnt_dusk_20120907_to_20160701.csv  Percentage of minutes He+ band EMIC waves with rising tones were observed in bins of RXY and Z SM (Figure 13):rbspab_her_rxyzsm_pcnt_midnight_20120907_to_20160701.csv, rbspab_her_rxyzsm_pcnt_dawn_20120907_to_20160701.csv, rbspab_her_rxyzsm_pcnt_noon_20120907_to_20160701.csv, rbspab_her_rxyzsm_pcnt_dusk_20120907_to_20160701.csv

openCC (other)Feb 2023View details →

MCR LTER: Coral Reef: Farmerfish gardens help buffer stony corals against marine heat waves, data for Honeycutt et al., PLOS One 2023

These data were generated in support of the manuscript: Honeycutt RC, Holbrook SJ, Brooks, AJ, and RJ Schmitt, PLOS One In Moorea, French Polynesia, we evaluated the response and fate of stony coral following a major thermal stress event in 2019 that caused a substantial amount of branching coral (dominantly Pocillopora) to bleach and die. We investigated whether Pocillopora colonies that occurred within territorial gardens protected by the farmerfish Stegastes nigricans were less susceptible to or survived bleaching better than Pocillopora on adjacent, undefended substrate. Bleaching prevalence and severity, which were quantified for >1,100 colonies shortly after they bleached, did not differ between colonies within or outside of defended gardens. By contrast, 399 focal colonies followed for one year revealed that a bleached coral within a garden was a third less likely to suffer complete colony death and, for survivors, about twice as likely to recover to its pre-bleaching cover of living tissue compared to Pocillopora outside of a farmerfish garden. Our findings indicate that while residing in a farmerfish garden may not reduce the bleaching susceptibility of a coral during thermal stress, it does help buffer a bleached coral against severe outcomes. This oasis effect of farmerfish gardens, where survival and recovery of thermally-damaged corals are enhanced, is another mechanism that helps explain why large Pocillopora colonies are far more abundant in farmerfish territories than elsewhere in the lagoons of Moorea, despite gardens being much less common. As such, farmerfish may have a growing role in maintaining the resilience of branching corals as the frequency and intensity of marine heat waves continue to increase. This material is based upon work supported by the U.S. National Science Foundation under Grant No. OCE 16-37396 (and earlier awards) as well as a generous gift from the Gordon and Betty Moore Foundation. Research was completed under permits issued

openCC (other)Jun 2025View details →

SBC LTER: Daily averages of modeled significant wave height (Hs) and peak wave period (Tp) in the Santa Barbara Coastal area from the Coastal Data Information Program - Monitoring and Prediction System (CDIP MOP)

From http://cdip.ucsb.edu: The Coastal Data Information Program (CDIP) is a research group at Scripps Institution of Oceanography that monitors coastal waves and nearshore sand levels on regional scales. CDIP maintains a network of optimally-placed, directional wave buoys from San Diego to Eureka. The buoy measurements are used to initialize a high spatial resolution (100m x 100m) linear spectral wave propagation model. The resulting hourly hindcasts and nowcasts of CA coastal wave conditions have a level of accuracy that is not possible with more traditional wind-wave generation models that are initialized with modeled wind fields.

openCustomMay 2022View details →

Wave data for Hog Island Bay, Fowling Point and Upsur Neck, Virginia, 2009

An RBR wave gauge was deployed at 3 locations on the coast of Virginia during 2009.

openCustomMay 2022View details →

ADCP wave and current data at Hog Island and Chimney Pole Marsh, VA 2009

Two acoustic doppler profilers were deployed in on Hog Island and Chimney Pole Marsh in 2009. all quantites (velocity, waves, water elevation, attenuation) are described in the file *.hdr (header file)

North Sea Wave Database (NSWD) 2005-2011

North Sea Wave Database (NSWD) The dataset contains each year of spectral metocean condition for Significant Wave Height (HSIGN) and wave energy period (TMM10), in meters and seconds. Each variable has a year timestap which the data corresponds too i.e 1980. The latitudes and longitudes of the dataset have resolution of 0.025 degrees at each direction. Latitude starting coordinate is 50 degrees and Longitude 0. For more information on the process that developed the dataset, the methodogies followed, calibration, valdiation and sensitivity analysis,  see:  Lavidas, G., & Polinder, H. (2019). North Sea Wave Database (NSWD) and the Need for Reliable Resource Data: A 38 Year Database for Metocean and Wave Energy Assessments. Atmosphere, 10(9), <a href="https://doi.org/10.3390/atmos10090551">https://doi.org/10.3390/atmos10090551 </a> Lavidas, G., & Polinder, H. (2019). Wind effects in the parametrisation of physical characteristics for a nearshore wave model. Proceedings of the 13th European Wave and Tidal Energy Conference 1-6 September 2019, Naples, Italy. The dataset was produced by Dr George Lavidas during the WAVe Resource for Electrical Production (WAVREP, which received funding from the European Union's Horizon 2020 research & innovation programme under the Marie Sklodowska-Curie grant agreement No 787344. The dataset is accompanied by two publication that (i) present the calibration-validation and production (ii) analysis of the dataset. The official CORDIS website is https://cordis.europa.eu/project/id/787344 A list of outcomes for the NSWD and the WAVREP project is found at the researcher's page: <a href="https://www.researchgate.net/project/WAVe-Resource-for-Electrical-Production-WAVREP ">https://www.researchgate.net/project/WAVe-Resource-for-Electrical-Production-WAVREP </a> It can also be found at the official CORDIS website <a href="https://cordis.europa.eu/project/id/787344">https://cordis.europa.eu/project/id/787344</a> Sharing and Access information Creative Commons Attribution (CC BY-SA).  The Creative Commons Attribution license allows others remix, tweak, and build upon your work, as long as they credit you and license their new creations under the identical terms.

North Sea Wave Database (NSWD) 1989-1997

North Sea Wave Database (NSWD) 2012-2017

opencc-by-4.0Oct 2020View details →

Data release for paper "Towards the routine use of subdominant harmonics in gravitational-wave inference: re-analysis of GW190412 with generation X waveform models"

This data release for the paper "Towards the routine use of subdominant harmonics in gravitational-wave inference: re-analysis of GW190412 with generation X waveform models" [<a href="https://arxiv.org/abs/2010.05830">arXiv:2010.2010.05830</a>] contains posterior samples for the GW190412 binary black hole merger event obtained from public GWOSC data with the parallel bilby Bayesian inference package, dynesty nested sampler and a set of waveforms from the "generation X" of phenomenological waveform models: IMRPhenomXAS, IMRPhenomXHM, IMRPhenomXP, IMRPhenomXPHM, IMRPhenomT and IMRPhenomTHM. The provided file is a "meta file" that can be read with the <a href="https://lscsoft.docs.ligo.org/pesummary/">PESummary</a> python package. The posterior samples included correspond to runs [2,6,10,12,14,26] in Table III of the paper (standard settings for each waveform, standar priors and sampler settings of Nlive=2048 and Nact=10 or 50). If you make use of these samples, please cite both this data release and the paper.

opencc-by-4.0Jan 2021View details →

Datasets for "Gravitational waves from the chiral magnetic effect"

<pre>This directory contains an index.html file with links to the run directories and idl plotting routines with secondary data for the other figures for the paper "Gravitational waves from the chiral magnetic effect" by A. Brandenburg, Y. He, T. Kahniashvili, M. Rheinhardt, and J. Schober. If anything turns out to be incomplete, please email brandenb@nordita.org.</pre>

opencc-by-4.0Jan 2021View details →

Code, data and scripts to study wave dynamics in asymmetric material

Supplementary data for [1] Vladislav A. Yastrebov. "Wave propagation through an elastically-asymmetric architected material", 2021, https://arxiv.org/abs/1712.06294v2 See "Readme.md" and indivual "Readme.md" files in folders: "data", "src", "fig"

opencc-by-sa-4.0Oct 2023View details →

Datasets for "Pulsational pair-instability supernovae in gravitational-wave and electromagnetic transients" from Hendriks et al 2023.

Data related to the paper "Pulsational pair-instability supernovae in gravitational-wave and electromagnetic transients" by Hendriks et al 2023 <a href="https://doi.org/10.1093/mnras/stad2857">https://doi.org/10.1093/mnras/stad2857</a>.<ul><li>`EVENTS_V2.2.2_SEMI_HIGH_RES*.tar.gz: main PPISN prescription variation simulation results for the GW mergers. These contain configurations for the populations and the convolved merger results which in turn contain merger rates, merger properties and events that preceded the mergers (RLOF episodes, SNe). These results are used in figures 2, 3, 6, and 7.  Figure 8 uses the SFR used in one of these simulations.</li><li>`EVENTS_V2.2.2_MID_RES*.tar.gz`: PPISNe prescription variation results for the transient rate evolution. These contain configurations for the populations and the convolved merger results which in turn contain merger rates, merger properties and events that preceded the mergers (RLOF episodes, SNe). These results are used in figure 4.</li><li>`grid_single_mass_metallicity_data.tar.gz`: data containing single-star remnant-mass data as a function of initial mass vs. final mass for our fiducial model and three variations: Farmer 2019 PPISN prescription, M_extra_ppisn_ML=10 Msun (i.e. where 10 solarmass of additional mass loss occur for each PPISN), M_co_shift_ppisn=-5 Msun (i.e. the CO core mass range that undergoes PPISN is shifted to lower masses by 5 solarmass). This data is used in figure 5.</li><li>`schematic_overview_data.tar.gz`: data containing single-star remnant-mass data as a function of pre-SN core mass for our fiducial models and several variations: Farmer 2019 PPISN prescription, M_extra_ppisn_ML = 5 Msun, M_co_shift_ppisn=-5 Msun, M_co_shift_ppisn=+5 Msun. This data is used in figure 1.</li><li>`paper_ppisne_scripts-main.tar.gz`: git-repository that contains the routines to generate the figures. The readme in this script should contain enough information, but  relevant to the data here: the user needs to store the files contained in this zenodo repository in a directory that they point to at with an environment variable called `paper_PPISNe_Hendriks2023_data_dir`. These scripts are also hosted on <a href="https://gitlab.com/dhendriks/paper_ppisne_scripts">https://gitlab.com/dhendriks/paper_ppisne_scripts</a></li></ul>

opencc-by-4.0Jun 2020View details →

Wind WAVES TDSF Dataset

Wind Spacecraft: The Wind spacecraft (<a href="https://wind.nasa.gov">https://wind.nasa.gov</a>) was launched on November 1, 1994 and currently orbits the first Lagrange point between the Earth and sun.  A comprehensive review can be found in <a href="https://ui.adsabs.harvard.edu/abs/2021RvGeo..5900714W/abstract">Wilson et al. [2021]</a>.  It holds a suite of instruments from gamma ray detectors to quasi-static magnetic field instruments, Bo.  The instruments used for this data product are the fluxgate magnetometer (MFI) [<a href="https://ui.adsabs.harvard.edu/abs/1995SSRv...71..207L/abstract">Lepping et al., 1995</a>] and the radio receivers (WAVES) [<a href="https://ui.adsabs.harvard.edu/abs/1995SSRv...71..231B/abstract">Bougeret et al., 1995</a>].  The MFI measures 3-vector Bo at ~11 samples per second (sps); WAVES observes electromagnetic radiation from ~4 kHz to >12 MHz which provides an observation of the upper hybrid line (also called the plasma line) used to define the total electron density and also takes time series snapshot/waveform captures of electric and magnetic field fluctuations, called TDS bursts herein. WAVES Instrument: The WAVES experiment [<a href="https://ui.adsabs.harvard.edu/abs/1995SSRv...71..231B/abstract">Bougeret et al., 1995</a>] on the Wind spacecraft is composed of three orthogonal electric field antenna and three orthogonal search coil magnetometers.  The electric fields are measured through five different receivers: Low Frequency FFT receiver called FFT (0.3 Hz to 11 kHz), Thermal Noise Receiver called TNR (4-256 kHz), Radio receiver band 1 called RAD1 (20-1040 kHz), Radio receiver band 2 called RAD2 (1.075-13.825 MHz), and the Time Domain Sampler (TDS).  The electric field antenna are dipole antennas with two orthogonal antennas in the spin plane and one spin axis stacer antenna. The TDS receiver allows one to examine the electromagnetic waves observed by Wind as time series waveform captures. There are two modes of operation, TDS Fast (TDSF) and TDS Slow (TDSS). TDSF returns 2048 data points for two channels of the electric field, typically Ex and Ey (i.e. spin plane components), with little to no gain below ~120 Hz (the data herein has been high pass filtered above ~150 Hz for this reason). TDSS returns four channels with three electric(magnetic) field components and one magnetic(electric) component.  The search coils show a gain roll off ~3.3 Hz [e.g., see <a href="https://ui.adsabs.harvard.edu/abs/2010JGRA..11512104W/abstract">Wilson et al., 2010</a>; <a href="https://ui.adsabs.harvard.edu/abs/2012GeoRL..39.8109W/abstract">Wilson et al., 2012</a>; <a href="https://ui.adsabs.harvard.edu/abs/2013JGRA..118....5W/abstract">Wilson et al., 2013</a> and references therein for more details]. The original calibration of the electric field antenna found that the effective antenna lengths are roughly 41.1 m, 3.79 m, and 2.17 m for the X, Y, and Z antenna, respectively.  The +Ex antenna was broken twice during the mission as of June 26, 2020.  The first break occurred on August 3, 2000 around ~21:00 UTC and the second on September 24, 2002 around ~23:00 UTC.  These breaks reduced the effective antenna length of Ex from ~41 m to 27 m after the first break and ~25 m after the second break [e.g., see <a href="https://ui.adsabs.harvard.edu/abs/2014GeoRL..41..266M/abstract">Malaspina et al., 2014</a>; <a href="https://ui.adsabs.harvard.edu/abs/2016JGRA..121.9369M/abstract">Malaspina & Wilson, 2016</a>]. TDS Bursts: TDS bursts are waveform captures/snapshots of electric and magnetic field data.  The data is triggered by the largest amplitude waves which exceed a specific threshold and are then stored in a memory buffer.  The bursts are ranked according to a quality filter which mostly depends upon amplitude.  Due to the age of the spacecraft and ubiquity of large amplitude electromagnetic and electrostatic waves, the memory buffer often fills up before dumping onto the magnetic tape drive.  If the memory buffer is full, then the bottom ranked TDS burst is erased every time a new TDS burst is sampled.  That is, the newest TDS burst sampled by the instrument is always stored and if it ranks higher than any other in the list, it will be kept.  This results in the bottom ranked burst always being erased.  Earlier in the mission, there were also so called honesty bursts, which were taken periodically to test whether the triggers were working properly.  It was found that the TDSF triggered properly, but not the TDSS.  So the TDSS was set to trigger off of the Ex signals. A TDS burst from the Wind/WAVES instrument is always 2048 time steps for each channel.  The sample rate for TDSF bursts ranges from 1875 samples/second (sps) to 120,000 sps.  Every TDS burst is marked a unique set of numbers (unique on any given date) to help distinguish it from others and to ensure any set of channels are appropriately connected to each other.  For instance, during one spacecraft downlink interval there may be 95% of the TDS bursts with a complete set of channels (i.e., TDSF has two channels, TDSS has four) while the remaining 5% can be missing channels (just example numbers, not quantitatively accurate).  During another downlink interval, those missing channels may be returned if they are not overwritten.  During every downlink, the flight operations team at NASA Goddard Space Fligth Center (GSFC) generate level zero binary files from the raw telemetry data.  Those files are filled with data received on that date and the file name is labeled with that date.  There is no attempt to sort chronologically the data within so any given level zero file can have data from multiple dates within.  Thus, it is often necessary to load upwards of five days of level zero files to find as many full channel sets as possible.  The remaining unmatched channel sets comprise a much smaller fraction of the total. All data provided here are from TDSF, so only two channels.  Most of the time channel 1 will be associated with the Ex antenna and channel 2 with the Ey antenna.  The data are provided in the spinning instrument coordinate basis with associated angles necessary to rotate into a physically meaningful basis (e.g., GSE). TDS Time Stamps: Each TDS burst is tagged with a time stamp called a spacecraft event time or SCET.  The TDS datation time is sampled after the burst is acquired which requires a delay buffer.  The datation time requires two corrections.  The first correction arises from tagging the TDS datation with an associated spacecraft major frame in house keeping (HK) data.  The second correction removes the delay buffer duration.  Both inaccuracies are essentially artifacts of on ground derived values in the archives created by the WINDlib software (K. Goetz, Personal Communication, 2008) found at <a href="https://github.com/lynnbwilsoniii/Wind_Decom_Code">https://github.com/lynnbwilsoniii/Wind_Decom_Code</a>. The WAVES instrument's HK mode sends relevant low rate science back to ground once every spacecraft major frame.  If multiple TDS bursts occur in the same major frame, it is possible for the WINDlib software to assign them the same SCETs.  The reason being that this top-level SCET is only accurate to within +300 ms (in 120,000 sps mode) due to the issues described above (at lower sample rates, the error can be slightly larger).  The time stamp uncertainty is a positive definite value because it results from digitization rounding errors.  One can correct these issues to within +10 ms if using the proper HK data. *** The data stored here have not corrected the SCETs! *** The 300 ms uncertainty, due to the HK corrections mentioned above, results from WINDlib trying to recreate the time stamp after it has been telemetered back to ground.  If a burst stays in the TDS buffer for extended periods of time (i.e., >2 days), the interpolation done by WINDlib can make mistakes in the 11th significant digit.  The positive definite nature of this uncertainty is due to rounding errors associated with the onboard DPU (digital processing unit) clock rollover.  The DPU clock is a 24 bit integer clock sampling at &sim;50,018.8 Hz.  The clock rolls over at &sim;5366.691244092221 seconds, i.e., (16*224)/50,018.8. The sample rate is a temperature sensitive issue and thus subject to change over time.  From a sample of 384 different points on 14 different days, a statistical estimate of the rollover time is 5366.691124061162 ± 0.000478370049 seconds (calculated by Lynn B. Wilson III, 2008).  Note that the WAVES instrument team used UR8 times, which are the number of 86,400 second days from 1982-01-01/00:00:00.000 UTC. The method to correct the SCETs to within +10 ms, were one to do so, is given as follows: <ol> <li>Retrieve the DPU clock times, SCETs, UR8 times, and DPU Major Frame Numbers from the WINDlib libraries on the VAX/ALPHA systems for the TDSS(F) data of interest.</li> <li>Retrieve the same quantities from the HK data.</li> <li>Match the HK event number with the same DPU Major Frame Number as the TDSS(F) burst of interest.</li> <li>Find the difference in DPU clock times between the TDSS(F) burst of interest and the HK event with matching major frame number (Note: The TDSS(F) DPU clock time will always be greater than the HK DPU clock if they are the same DPU Major Frame Number and the DPU clock has not rolled over).</li> <li>Convert the difference to a UR8 time and add this to the HK UR8 time.  The new UR8 time is the corrected UR8 time to within +10 ms.</li> <li>Find the difference between the new UR8 time and the UR8 time WINDlib associates with the TDSS(F) burst. Add the difference to the DPU clock time assigned by WINDlib to get the corrected DPU clock time (Note: watch for the DPU clock rollover).</li> <li>Convert the new UR8 time to a SCET using either the IDL WINDlib libraries or TMLib (STEREO S/WAVES software) libraries of available functions.  This new SCET is accurate to within +10 ms.</li> </ol> One can find a UR8 to UTC conversion routine at <a href="https://github.com/lynnbwilsoniii/wind_3dp_pros">https://github.com/lynnbwilsoniii/wind_3dp_pros</a> in the ~/LYNN_PRO/Wind_WAVES_routines/ folder. Examples of good waveforms can be found in the notes PDF at <a href="https://wind.nasa.gov/docs/wind_waves.pdf">https://wind.nasa.gov/docs/wind_waves.pdf</a>. Data Set Description Each Zip file contains 300+ IDL save files; one for each day of the year with available data.  This data set is not complete as the software used to retrieve and calibrate these TDS bursts did not have sufficient error handling to handle some of the more nuanced bit errors or major frame errors in some of the level zero files.  There is currently (as of June 27, 2020) an effort (by Keith Goetz et al.) to generate the entire TDSF and TDSS data set in one repository to be put on SPDF/CDAWeb as CDF files.  Once that data set is available, it will supercede and replace this one as it will be more complete and all SCETs will be corrected. When one restores any given IDL save file, they will find an IDL structure named struc.  Inside are several tags and for each date there are T number of TDSF bursts, each of which has K (= 2048) time stamps.  The structure contains the following tags: <ul> <li>SCETS:  [T]-Element [string] array of SCETs at start of TDS burst with format 'YYYY-MM-DD/hh:mm:ss.xxx'</li> <li>UNIX:  [T,K]-Element [double] array of quasi-Unix times (i.e., converted from UTC times without removing leap seconds)</li> <li>CH1EXDA_CH2EXYZAC_WAVES:  [T,K,5]-Element [float] array of electric fields [mV/m] in spinning WAVES coordinates, where the components are: <ul> <li>[*,*,0] = Ex in DC-coupled mode from channel 1</li> <li>[*,*,1] = Ex in AC-coupled mode from channel 1</li> <li>[*,*,2] = Ex in AC-coupled mode from channel 2</li> <li>[*,*,3] = Ey in AC-coupled mode from channel 2</li> <li>[*,*,4] = Ez in AC-coupled mode from channel 2</li> </ul> </li> <li>SRATE:  [T]-Element [float] array of sample rates for each TDSF burst [Hz]</li> <li>FILTER_FREQ:  [T]-Element [float] array of soft low pass filter frequencies [Hz]</li> <li>EVENT_NUM:  [T]-Element [long] array of TDS event numbers [N/A]</li> <li>UR8_START:  [T]-Element [double] array of UR8 times at start of TDS burst [# of 86,400 second days from 1982-01-01/00:00:00.000 UTC]</li> <li>EX_START_ANG:  [T]-Element [float] array of counter-clockwise angles between the +Ex antenna and the spacecraft-to-sun line at the start of each TDS burst [e.g., see <a href="https://ui.adsabs.harvard.edu/abs/2016JGRA..121.9369M/abstract">Malaspina & Wilson, 2016</a> for definitions]</li> <li>EX___END_ANG:  [T]-Element [float] array of counter-clockwise angles between the +Ex antenna and the spacecraft-to-sun line at the end of each TDS burst [e.g., see <a href="https://ui.adsabs.harvard.edu/abs/2016JGRA..121.9369M/abstract">Malaspina & Wilson, 2016</a> for definitions]</li> <li>THETA_AX:  [T]-Element [float] array of average counter-clockwise angles between the +Ex antenna and the Earth-to-sun line [e.g., see <a href="https://ui.adsabs.harvard.edu/abs/2016JGRA..121.9369M/abstract">Malaspina & Wilson, 2016</a> for definitions]</li> <li>BO_GSE:  [T,3]-Element [float] array of Bo 3-vectors [nT] in GSE coordinate basis at start of TDS bursts</li> <li>SC_GSE_POS:  [T,3]-Element [float] array of spacecraft position 3-vectors [RE] in GSE coordinate basis at start of TDS bursts</li> <li>SC_SPIN_RATE:  [T]-Element [float] array of spacecraft spin rates [deg/s] at start of TDS bursts</li> <li>JULIAN:  [T]-Element [double] array of Julian day numbers [N/A]</li> <li>EARTH_WAKE:  [T]-Element [byte] array of logical values defining whether spacecraft is in Earth's optical wake [1 = TRUE, 0 = FALSE]</li> <li>LUNAR_WAKE:  [T]-Element [byte] array of logical values defining whether spacecraft is in the lunar optical wake [1 = TRUE, 0 = FALSE]</li> <li>CHANNEL_1_LABS:  [T]-Element [string] array of channel 1 labels defining the source type shown in the CH1EXDA_CH2EXYZAC_WAVES tag</li> <li>CHANNEL_2_LABS:  [T]-Element [string] array of channel 2 labels defining the source type shown in the CH1EXDA_CH2EXYZAC_WAVES tag</li> <li>CHANNEL_1_INT:  [T]-Element [integer] array of channel 1 labels [obsolete]</li> <li>CHANNEL_2_INT:  [T]-Element [integer] array of channel 2 labels [obsolete]</li> <li>UNITS:  [19]-Element [string] array defining the units of each structure tag</li> <li>NOTES:  [11]-Element [string] array defining some useful things about the data set</li> </ul> Note that the angles have all been shifted by +360 degrees to avoid rollover issues.  The reason being that the spacecraft rotates such that EX_START_ANG is always larger than EX___END_ANG.  All angles herein are counter-clockwise angles in the GSE basis. Rotating Bo from GSE to WAVES coordinates Since the quasi-static magnetic field is given in GSE coordinates, one may want to examine the wave fields relative to the Bo direction.  If you examine the attached figure labeled GSE-Basis_to_WAVES_rotation_2.jpg, you will see how to rotated from GSE into WAVES coordinates.  The angle \(\phi\) in the image corresponds to the THETA_AX structure tag values.  The angle \(\pi\) in the image is the actual value of pi in radians.  This is is necessary to flip the GSE vectors to match the WAVES +z-axis, which is pointed toward the south ecliptic pole, not the north like Z-GSE. It is important to rotate Bo into WAVES rather than the electric fields into magnetic field-aligned coordinates since each antenna has different noise and response functions.

opencc-by-4.0Feb 2022View details →

Hydroelastic response of the scaled model of a floating offshore wind turbine platform in waves: HELOFOW Project Database

This dataset contains the data measured during the HELOFOW model test campaign, performed at the Ocean and Hydrodynamic Engineering wave tank of Ecole Centrale Nantes (ECN): decay tests, regular wave tests and irregular waves tests. The preprocessed measured data is contained in MAT files. The model, the measurements and the tests are described in the appended Excel files. A Matlab(R) function is given as a short example to show how the MAT files are structured and how data may be handled for a plot.  As stated in the reference paper (Leroy et al., Ocean Engineering, 2022): "As the size of floating wind turbines continues to increase, floating platforms reach dimensions that make their elastic and hydro-elastic behaviour significant. Several works in connection with the numerical modelling of the elastic behaviour of these wind turbines have been carried out but few validation data are available. This study focuses on the hydro-elastic response of a large floating wind turbine, in regular waves and severe sea-states. A new experimental wind turbine model has been designed to represent a 1:40 Froude-scaled spar platform carrying the DTU 10 MW turbine. The main challenge is here to reproduce a 1st bending mode frequency and hydrodynamic loads representative of a realistic large floating wind turbine. The platform model is made of a flexible backbone, reproducing the correct flexibility, and light floaters fixed on it provide the correctly scaled geometry. This experimental model is tested in various conditions including regular waves of several periods and steepness, and irregular waves of various intensity, including extreme 50-year return period conditions."   This work was carried out within the framework of the WEAMEC, West Atlantic Marine Energy Community, and with funding from the Pays de la Loire Region and Europe (European Regional Development Fund).  HELOFOW project on <a href="https://www.weamec.fr/en/projects/helofow/">the WEAMEC website</a>.