dataesr/scientific-paragraphs-categorization huggingface dataset:
7% enriched uranium data The Sandia Pulsed Reactor Facility at Sandia National Laboratories in New Mexico is the home of the Seven Percent Critical Experiment (7uPCX). This facility was designed and constructed to investigate critical systems containing light water reactor (LWR) fuel with enrichments above 5% 235 U. The 7uPCX assembly is water moderated and contains adjustable arrays of aluminum-clad, square-pitched UO 2 fuel rods enriched to 6. 90%. Two benchmark evaluations [LEU-COMP-THERM-078 and LEU-COMP-THERM-096] have been contributed to the ICSBEP Handbook with a total of 34 critical configurations with lattice arrangements of varying number of fuel rods, water holes, and water-filled gaps. These high-precision experiments are evaluated to have very low benchmark k eff uncertainties of ± 0.
Graphite data Of the numerous graphite-and polyethylene-reflected HEU metal experiments reported for the Oak Ridge Critical Experiments Facility (ORCEF), three configurations for bare annuli with internal graphite cores were evaluated [HEU-MET-FAST-077] following prior evaluation of HEU annuli and cylinders reflected by thin graphite reflectors [HEU-MET-FAST-071] from the same experimental series. These experiments are reported with high accuracy and precision for dimensions and mass of the assembly components, resulting in a 1σ uncertainty in k eff of ±0. 0006 k. An evaluation of the Japan Atomic Energy Agency (JAEA) Very High Temperature Reactor Critical Assembly (VHTRC) [VHTRC-GCR-EXP-001] was prepared for inclusion in the IRPhEP Handbook. The VHTRC was constructed to verify the calculation accuracy related to the neutronic design of the High Temperature Engineering Test Reactor (HTTR).
A comprehensive amount of data was measured during the course of the fouryear program. The remaining seven critical configurations (Cores 4, 5 through 8, and 9 & 10) were evaluated in three additional benchmark reports [PROTEUS-GCR-EXP-002, -003, and -004], complementing previous benchmark evaluation work on Cores 1 through 3 [PROTEUS-GCR-EXP-001]. PROTEUS is a zero-power research reactor based on a cylindrical graphite annulus with a central cylindrical cavity. Cores 1, 1A, 2, and 3 have hexagonal close packing with a 1:2 moderator-to-fuel pebble ratio; Core 4 has random packing with a 1:1 moderator-to-fuel pebble ratio; Cores 5, 6, 7, and 8 have columnar hexagonal point-on point packing with a 1:2 moderator-to-fuel pebble ratio; and Cores 9 and 10 also have columnar hexagonal point-on point packing with a 1:1 moderator-to-fuel pebble ratio.
Heavy water data The RB (Reactor B) reactor (critical facility) at the Vinča Institute of Nuclear Sciences in Belgrade, Serbia, operates using natural or LEU metal fuel in a heavy water tank. Three critical configuration were evaluated for testing neutron accident dosimeters for the IAEA (International Atom Energy Agency) in 1973, for testing an External Neutron Converter (ENC) in 1978, and for investigation of an Experimental Fuel Channel (EFC) in 1982 for creation of an epithermal and fast neutron spectrum in the center of the core [RB-FUND-EXP-001, -002, and -007, respectively]. The 1σ benchmark uncertainty is ±0. 0010 k, ±0. 0015 k, and ±0. 0018 k, respectively, for the three configurations. Neutron spectral and spatial  distributions, as well as gamma ray dose rate benchmark measurements are provided for the ENC configuration.
Potassium data A pair of critical configurations were evaluated from ORCEF that were performed to test the fast neutron cross sections of potassium [HEU-MET-FAST-099, ORCEF-SPACE-EXP-001] as it was a candidate for coolant in some early space power reactor designs, such as the MPRE program. Oralloy annuli were stacked around two empty stainless steel cans for the first configuration. The second configuration (as shown in Fig. 6 ) used an identical loading except that the stainless steel cans were filled with approximately 2. 4 kg of potassium. The benchmark worth of the potassium is 11. 4 ± 1. 2 ¢ (4. 8 ± 0. 5 ¢/kg); however Monte Carlo calculations of the addition of potassium are approximately 70% to 80% lower than the benchmark value. Currently this evaluation represents the only benchmark available for integral testing of potassium cross section data until the aforementioned SCCA potassium measurement is completed.
Neutron streaming through sodium data The ANL ZPPR-12 assembly represented a clean, cylindrical, single-zone core mock-up used to study fuel properties of the Clinch River Breeder Reactor (CRBR) [ZPPR-LMFR-EXP-010]. Measurements included sodium void worth, cell heterogeneity, neutron streaming, and a discrepancy between calculated and measured control rod worths. A critical configuration and the sodium void worth measurements, including neutron streaming, are currently evaluated. One purpose of the ZPPR-12 was to compare sodium void worth measurements in a plate-loaded core versus a pin-loaded core. Sufficient information was unavailable to evaluate the pin-loaded core as a benchmark. Part of the plate-loaded core analysis included rearrangement of the plates to maximize and reduce neutron streaming through the sodium region of the core.
Conclusions The ICSBEP and IRPhEP continue to provide high-quality integral benchmark data from around the world that are of great value for nuclear data testing, uncertainty reduction, criticality safety, reactor physics, and advanced modelling and simulation. Data contributed from 25 countries to these projects will be of value for future decades, enabling current and future activities as long as experimental validation remains relevant. The ICSBEP and IRPhEP are collaborative efforts that involve numerous scientists, engineers, administrative support personnel, and program sponsors from 25 different countries. The authors would like to acknowledge the efforts of all of these dedicated individuals without whom the ICSBEP and IRPhEP would not be possible.
Data Energetic particle, magnetic field, and wave data from five different missions were used for this study. MMS  (Burch, Moore, et al. , 2016)  was launched in March 2015 with the primary science objective to study magnetic reconnection at Earth's magnetopause and in the magnetotail. The mission consists of four identically instrumented spacecraft that are held in tight formation to ensure high-quality, high-resolution multipoint data and the ability to disambiguate spatial from temporal features and calculate currents through a portion of each orbit. In this study, we employ data from the MMS Energetic Particle Detectors (EPD) instrument suite  (Mauk et al. , 2016)  and FIELDS instrument suite  (Torbert et al. , 2016). MMS/EPD consists of two different types of instruments: the Energetic Ion Spectrometers (EIS)  (Mauk et al.
Both burst and fast survey data from FEEPS electron telescopes were used in this study as well as fast survey data from EIS and FEEPS ions. The MMS/FIELDS instrument suite consists of six different instruments: analog and digital fluxgate magnetometers  (Russell et al. , 2016) , a search-coil magnetometer  (LeContel et al. , 2016) , spin-plane and axial electric field double probes  (Ergun et al. , 2016; Lindqvist et al. , 2016) , and an electron drift instrument  (Torbert et al. , 2016). FIELDS provides observations of the magnetic field vector and waveforms up to 16,384 samples/s in burst mode and the electric field vector and waveforms at up to 65,536 samples per second in burst mode. Electric field and magnetic field power spectra are also captured between 1 Hz and 100 kHz and 2 Hz and 6 kHz, respectively.
Fast survey DC magnetic field and E and B field power spectra from level 2 data products were used for this study. Unfortunately, the MMS Fast Plasma Instruments  (Pollock et al. , 2016)  were not turned on for this event. NASA's Van Allen Probes (e. g. ,  Mauk et al. , 2013)  were launched in August 2012 to study the sources, losses, and transport of particles in Earth's radiation belts and ring current. The mission consists of two identically instrumented spacecraft (RBSP-A and RBSP-B) in eccentric, nearequatorial GEO-transfer-like orbits. For this study, we employed data from the Radiation Belt Storm Probes (RBSP; the name of the mission prior to launch, after which it was designated in honor of James Van Allen) Energetic particle, Composition, and Thermal plasma instrument suite  (Spence et al.
, 2013) , the RBSP Ion Composition Experiment (RBSPICE)  (Mitchell et al. , 2013) , and the Electric and Magnetic Fields Instrument Suite for Integrated Science (EMFISIS) instrument suite  (Kletzing et al. , 2013). Level 3 electron and proton flux data products from the Magnetic Electron and Ion Spectrometers (MagEIS) instruments  (Blake et al. , 2013) , proton flux data from RBSPICE level 3 products, and level 3 magnetic field data and level 2 E and B field power spectra from EMFISIS were used for this study. As previously mentioned, NASA's THEMIS mission  (Angelopoulos, 2008)  was launched in 2007. In 2010, the two outermost spacecraft became the ARTEMIS mission at Earth's moon; data from the remaining three THEMIS spacecraft (TH-A, TH-D, and TH-E) were examined for this study. Here we used fast survey data from the THEMIS fluxgate magnetometers  (Auster et al.
, 2008)  and solid-state telescopes (e. g. ,  Angelopoulos, 2008; Turner et al. , 2012). For this event, the THEMIS all-sky imager array in North America was in the afternoon local time sector during our period of interest and thus was unavailable for this study. Electron and proton count rate data from the SOPA instruments, covering the energy range 50 keV to >1 MeV, were also used from six of the Los Alamos National Laboratory spacecraft in GEO (LANL-GEO). The LANL-GEO spacecraft do not carry magnetometers. The Geotail mission (e. g. ,  Mukai et al. , 1994) , a joint endeavor from Institute of Space and Astronautical Science, JAXA, and NASA, was launched in July 1992 and is still successfully operating on orbit around Earth. For this study, we used data from Geotail's Energetic Particles and Ion Composition  (Williams et al.
Each of the 16 spacecraft examined here carries energetic particle instruments for both electrons and ions, the observations from which are summarized in Figures  2  and 3. Figure  2  shows electron observations from 12 spacecraft revealing a complex series of electron injections. The approximate initial observation time of each electron injection at each spacecraft is marked with colored triangles along the plots' x axes, and the (a-l) Energetic electron data from MMS, Van Allen Probes, THEMIS, Geotail, and LANL-GEO spacecraft during the period of interest from 00:00 to 02:30 UT on 7 April 2016. For each plot, the spacecraft responsible for the observations is labeled and the instrument used to make the measurement is labeled on the y axis. The energy bin centers for each of the different energy channels shown on each spacecraft are labeled along the right side of each plot.
RBSP-B observed at least one dispersed injection starting around 01:18 UT, first at the 242 keV energy channel, and it might have also caught the lower energy edge of another, previous injection in the first of two enhancements in the 32 keV channel seen at the same time. MMS observed a combination of at least four dispersed and dispersionless injections. Like LANL-97A, the last injection observed by MMS, starting around 01:13 UT, also displayed clear substructure. Note that while only data from MMS-2 are shown here, they are consistent with the three other MMS spacecraft. With the interspacecraft separation of < 70 km here, the four MMS spacecraft were essentially a single-point observation as far as this study is concerned. RBSP-A observed a series of three dispersed injections, while nearby, LANL-02A observed only one clear dispersed injection signature starting just before 01:30 UT.
Interestingly, no ion injections were observed by any of the spacecraft at L < 6. 9 (i. e. , RBSP-A, RBSP-B, LANL-01A, and LANL97A). Note that we confirmed that RBSPICE (shown in Figure  3 ) and MagEIS ion data (not shown) were consistent on both Van Allen Probes; none of the instruments showed any signature of ion injections. Also, the EIS proton data from MMS (not shown) revealed observations consistent with those from MMS/FEEPS ions (shown in Figure  3 ). To compare the particle observations with any signatures of dipolarization around the system, magnetometer data from Geotail, THEMIS, MMS, and Van Allen Probes are shown in Figure  4. Evidence of dipolarization fronts were not clear at any of the spacecraft, and only at Geotail was a distinct dipolarization signature clear after ~01:10 UT.
Analysis and Results First, we examined the substructure of the electron injections observed around 01:17 UT (blue arrows in Figure  2 ). Fortunately, burst data were captured from MMS between ~01:13 and 01:28 UT. Burst data from the FEEPS electron instruments on MMS-2 are shown in Figure  6 , including omni-directional average flux energy spectrograms (Figure  6a ) and pitch angle distributions for eight different energy channels ranging from 101 to 323 keV (Figures  6b-6i ). From these data, it is clear that MMS observed at least four subinjections at energies >100 keV, all with similar levels of dispersion but an upper energy threshold that increased with each new injection. Note also from Figure  2d  that at energies <100 keV, this looked like a single large injection. For comparison, the electron injections observed by LANL-97A around this same time (~01:17 UT) displayed at least three distinct peaks in multiple energy channels, revealing again that the electron injection was really made up of a series of subinjections.
Geotail, THEMIS, MMS, and RBSP B-GSE Related to the evolution of the electron pitch angle distributions, we next examined the MMS/FIELDS and RBSP/EMFISIS data to report on chorus wave activity observed during this series of injections. Figure  7  shows a combination of electron and wave data from MMS and Van Allen Probes. Electron fluxes summed over the FEEPS channels from ~30 keV up to 60 keV are plotted on a linear y axis in the topmost plot, and wave B field power spectra are plotted in the second plot. Lower band chorus wave activity is clear at frequencies below one half of the equatorial electron cyclotron frequency (0. 5*f ce_eq ), which is plotted with the dash-dotted magenta line (alongside 1* and 0. 1*f ce_eq ). The plots in Figures  7c-7f  show data in the same format from RBSP-B and RBSP-A using <60 keV electrons from MagEIS and wave B field power spectra from EMFISIS.
Finally, the results showing that injection 6 occurred over a broad range of MLT is further supported by ground magnetometer data (not shown here), which indicate that the substorm current wedge started to form around 01:10 UT and extended over at least 8 h in MLT from eastern North America (station FRD in Virginia) to Estonia (station TAR). TAR observed a negative bay in the D (east/west) component, while FRD showed a positive bay in the D component, which is consistent with the perturbations along the eastern and western sides of a substorm current wedge (e. g. ,  Kepko et al. , 2015). Based on these observations, we present the following scenario as explanation for the series of injections from this case study: injections 1-5 resulted from localized DFBs surging earthward from localized and bursty reconnection events in Earth's magnetotail.
Summary and Conclusions On 7 April 2016, a constellation of spacecraft was well positioned throughout the inner magnetosphere and near-Earth plasma sheet inside of L = 13 to observe a series of energetic particle injections building up to a weak substorm (maximum AE ~260 nT) that occurred after ~01:10 UT. Data from 16 spacecraft from the MMS, Van Allen Probes, THEMIS, Geotail, and LANL-GEO missions were examined for this case study. All combined, the spacecraft observed a series of at least six distinct electron injections but only one distinct ion injection. All of the injections were observed in the energy range 30 keV < E < 600 keV for both ions and electrons. The injections occurred under nonstorm magnetospheric conditions (SYM-H > À30 nT) during a period of relatively steady, below-average solar wind and radial though continuously southward IMF.
Acknowledgments The authors are thankful to all of the  MMS, Van Allen Probes, THEMIS, LANL-GEO, Geotail, ACE, Wind, OMNI , and  Kyoto World Data Center for Geomagnetism teams  for making their data available to the public. In addition to coauthors' contributions, we thank, from  Geotail ,  D. Williams  at  JHU/APL  and  CDAWeb for Geotail Energetic Particles and Ion Composition data ; from  ACE, Wind , and OMNI,  J. H. King ,  N. Papatashvilli , and team for the OMNI solar wind data; and  NASA CDAWeb  and mission specific online databases. MMS data are available at <https:// lasp. colorado. edu/mms/sdc/public/>. Van Allen Probes data are available at <http://rbspgway. jhuapl. edu/data_instrumentationSOC>. THEMIS data are available at <http://themis. ssl. berkeley. edu/index. shtml>. LANL-GEO data are available by request to G.
Acknowledgements We thank  Marco Capello , for his assistance during the field operations. This research has been partly conducted with the financial support of  Science Foundation Ireland & the Marie-Curie Action COFUND  under Grant Number  11/SIRG/E2174. N. P. A. research is funded by  Austrian Science Fund (FWF) :  M2218-N29. Seismic data used for this work have been collected in the frame of an internal  INGV  project (GAPSS).
Data availability. Continuous seismic recordings from permanent seismic stations are available on EIDA (http://www. orfeus-eu. org/data/eida/index. html). The seismic data recorded in the framework of RETREAT project (NSF grant EAR-0208652) can be freely download from IRIS data archive: http://ds. iris. edu/ds/nodes/dmc/ data/. Part of the seismic data used for this work have been collected in the frame of an internal INGV project. and are embargoed till 31. 12. 2017. Afterward, continuous seismic data will be made available upon request to D. P. (davide. piccinini@ingv. it).
Acknowledgments This work has been carried out within the framework of the  EUROfusion Consortium  and has received funding from the  Euratom  research and training programme  2014-2018  under grant agreement No  633053. The views and opinions expressed herein do not necessarily reflect those of the  European Commission. P. Vavpetič https://orcid. org/ 0000-0001-6204-7435I. L. Velicu https://orcid. org/ 0000-0002-7236-2495  A. Weckmann https://orcid. org/ 0000-0003-1062-8101M. Wirtz https://orcid. org/ 0000-0002-1857-688XR. Zaplotnik https://orcid. org/ 0000-0002-1366-9147.
I am thankful to the Rare Books and Manuscripts collection of Columbia University for giving me access to the university's yearbooks and other relevant documents. 8. See Notes 6 and 10. 9. Data extracted from the collections of the Ferreira-Mendes Portuguese Archives at the University of Massachusetts Dartmouth; New Bedford Public Library; New Bedford Whaling Museum Library. 10. For this point I am thankful to the discussion on a talk at Casa dos Açores da Nova Inglaterra (New England House of Azores) in 2013, hosted by its president Nélia Alves. 11. That ideology would be developed by  Freyre (1953)  after touring the Portuguese colonies in Africa and was later adopted by the Portuguese government as a way to embellish the colonial governance; the core idea was that the Portuguese were more prone to inhabit the tropics, less racist than other Europeans and more suited to having friendly and amenable relationship with peoples around the world.
Acknowledgements Research for this article influenced the final format of the proposal The Colour of Labourthe Racialized Lives of Migrants, awarded with an  ERC Advanced Grant  ( ERC-2015-AdG 695573 ) in 2016. The analysis was finalized in the context of that project. Preliminary research was conducted during the author's appointment as Hélio and Amélia Pedroso Endowed Chair of Portuguese Studies at the  University of Massachusetts at Dartmouth, MA, USA , Spring 2013. I thank  Frank de Sousa  for the invitation, and challenge, to explore, as an anthropologist, Taft's accounts of the early century Portuguese communities in Fall River and Portsmouth. I thank my colleagues at the  Center for Portuguese Studies and Culture at UMass Dartmouth  for their warm support and for the chance to present a preliminary analysis of the data.
, 2017; Meyer et al. , 2017; Provost et al. , 2017; Olsen et al. , 2017]. The research work was based around the Norwegian Polar Institute research vessel Lance that was assisted to around 838N by the Norwegian coastguard ice-breaker KV Svalbard on four occasions and left to drift passively southward toward the ice edge. The current study concentrates on buoy data from two of such southward drifts. A total of 42 buoys (Tables  1  and 2 ) were deployed in nested arrays at spacings of 5-100 km, separated into a winter deployment in January/ February and a spring deployment in April/May. Instruments were placed on a mixture of first-year and secondyear ice that was characteristic for the region. The sea ice in the array was relatively thin with modal thicknesses between 0. 9 and 1. 7 m and covered by snow with mean depth between 0.
3 and 0. 5 m  [R€ osel et al. , 2016a,2016b]. Sea ice deformation on a smaller scale was simultaneously studied by analyzing ship radar images  [Oikkonen et al. , 2017]. We compare our results to several previous studies which deployed buoy arrays (Figure  1      N-ICE2015 winter array starts considerably earlier in the season than these previous efforts, which allows new insights. In this paper, we present the sea ice buoy data collected during N-ICE2015, study the sea ice dynamics based on these data explore the temporal development of the sea ice deformation processes, connect the information to the previous studies and propose links between the differences observed and changes in the Arctic sea ice cover and climate.
Sea Ice Conditions and Origin To understand the age and origin of ice in the study region and compare ice conditions with previous years, we tracked the ice back in time with a coarse resolution ice drift from satellite observations. We used daily ice motion vectors based on ASCAT scatterometer and SSM/I radiometer data  [Girard-Ardhuin and Ezraty, 2012]  for the winter months and bridged the gap in ice drift data during the summer months by using an unpublished version of summer ASCAT/SSMIS ice drift data by the same provider. Ice was tracked back to its origin for the 5 years between 2011 and 2015 always starting on 15 March of each year at 82:5 N and 20 E (Figure  1 ). The ice drift at a given position is obtained from the 62. 5 km large grid cell of the ASCAT/ SSMI drift data set covering that position.
The previous day's position is estimated from that drift vector and the procedure is repeated going back in time until either land or ice concentrations below 15% for more than 1 day are encountered. Due to the low resolution of the ice drift data and some gaps in the ice drift fields, especially during summer, the ice back-trajectory will diverge from the real trajectory and have some uncertainty. This approach is suitable to determine the sea-ice source region within an approximately Journal of Geophysical Research: Oceans Journal of Geophysical Research: Oceans 10. 1002/2016JC012403 100 km radius. The back-tracking algorithm does not consider new ice growth, i. e. the presented trajectories represent the oldest ice for that region. It does not contain any information of the ice age composition and younger ice can also be present.