dataesr/scientific-paragraphs-categorization huggingface dataset:
The quality of ocean models has increased in the past years especially because of the growing computing capabilities. Hydrological models of water cycle at continental to global scales have also emerged over the last ten years, and assimilation of altimetry in synergy with other mission products into land surface and global climate models, is a current big challenge. Even more, model outputs must be more and more used to simulate observing approaches and scenarios and then provide rationale to justify missions and also to optimize the data acquisition for current missions (see Section 6. 6). Another important point is the fact that space ocean observations relate to only the surface. Modeling can help provide a consistent vertical perspective: a 4D reconstruction. Regarding SWOT again and the need to help with interpreting higher resolution altimetry data, it is expected that models will help further disentangle the questions of the internal wave motions and the balanced dynamics.
For example, by accessing the Copernicus Research and User Support Service (RUS, https://rus-training. eu/) readers can find information on face-to-face lessons, online webinars and e-learning courses on both oceanography and radar altimetry. ESA annually offers training sessions during the Coastal Altimetry Workshop (http://www. coastalt. eu/, training material available for download) and has also funded many toolboxes and tutorials such as the Broadview Radar Altimetry Toolbox (BRAT, http://www. altimetry. info/), designed to facilitate the visualisation and processing of radar altimetry data and the Delay-Doppler Altimetry Studio (DeDop, https://dedop. org/), which is an open-source customizable and modifiable toolbox to process Sentinel-3 SRAL data. However, several regions of the world are under-represented in the international oceanographic, hydrologic, and cryospheric communities.
Programmatic issues After the first technology concept demonstrations mostly conducted in the USA  (Wilson et al. , 2006) , the development of modern altimetry has been based on multifold cooperation and partnership (e. g. Escudier et al. , 2018) : -Partnership between space agencies developing and operating the missions (NASA, CNES, ESA, ISRO, CNSA,. ), extended to operational organizations (NOAA, EUMETSAT, EU/Copernicus Services); -Partnership between space agencies and oceanographic institutions to develop the synergies between the space component, the in situ component and the analysis and forecast capacities; -Partnership between agencies and oceanographic community (science, applications) to optimize the definition of the system, develop the data processing tools, conduct the calibration and validation activities.
On the European side, the Copernicus programme is a key element for the future of altimetry and operational oceanography. The Copernicus programme is in routine mode with 7 satellites launched up to now, combined with services in charge of processing and delivering world-class data products used extensively by a large community of users from science, public bodies, private corporations, start-ups, to citizens. This is a success to be shared with space agencies and also with the community of scientists and operators that are building information products on top of remote sensing data, and users. The future of the programme is on the table. The Arctic, coastal zones and marine biology are the next big priorities for the Copernicus marine service. The European Commission, ESA and EUMETSAT are working together on a long-term scenario.
Acknowledgements This collective synthesis of the worldwide interdisciplinary altimetry community would not have been possible without the support that has been given to each of the contributors by numerous institutions at local, national and intergovernmental levels. At the forefront of this support, we must obviously mention the space agencies CNES, ESA and NASA which have played and still play a decisive role in the development and launch of several prominent altimetry missions from the outset. Other agencies such as DLR, EUMETSAT, ISRO, NOAA, NSOAS and organizations such as CMEMS, also contribute significantly to developments in all forms of altimetry. We are very grateful to all the players in the previous organizations and many others that we cannot list extensively here, and that were all behind this remarkable success of radar altimetric technology and made the many scientific, technical and application developments possible.
Sincere thanks should be specifically addressed to all contributors either individually or as responsible in various capacities (thematic leaders, session chairmen, contributors to round tables, actors from different space agencies or national organizations or international, etc. ), who provided their inputs in different forms to this document. We also warmly thank the reviewers for their helpful comments to improve the article. The views, opinions, and findings contained in this article are those of the authors and should not be construed as an official National Oceanic and Atmospheric Administration (NOAA) or U. S. Government position, policy, or decision. This also applied to other Organizations or Institutes. ). Abileah, R. , Scozzari, A. , Vignudelli, S. , 2017. Envisat RA-2 individual echoes: A unique dataset for a better understanding of inland water altimetry potentialities.
Armitage, T. W. , Kwok, R. , 2019. SWOT and the ice-covered polar oceans: An exploratory analysis. Adv. Space Res. https://doi. org/ 10. 1016/j. asr. 2019. 07. 006 (in this issue). Armitage, T. W. K. , Bacon, S. , Kwok, R. , 2018. Arctic sea level and surface circulation response to the Arctic oscillation. Geophys. Res. Lett. 45, 6576-6584. https://doi. org/10. 1029/2018GL078386. -NSOAS: National Satellite Ocean Application Service -NRT: Near Real Time -OSSE: Observing System Simulation Experiment -OSTST: Ocean Surface Topography Science Team -RADS: Radar Altimetry Database System -SAR: Synthetic Aperature Radar (SARM for SAR mode) -SARIn: SAR Interferometry -SARAL/AltiKa: Satellite with Argos and AltiKa, ISRO/CNES ka-band altimetry satellite (Feb. 2013 -) -SCO: Space Climate Observatory (https://www.
ACKNOWLEDGMENTS The authors are grateful for funding provided by  LABEX WIFI (Laboratory of Excellence  within the  French Program Investments for the Future ,  ANR-10-LABX-24  and  ANR-10-IDEX-0001-02  and by TOTAL R&D. We acknowledge the support from the  European Research Council (ERC)  under the  European Union   Horizon 2020 research and innovation program  (grant agreement No  742335 ,  F-IMAGE  and grant agreement No. 819261 ,  REMINISCENCE ).
DATA AVAILABILITY The seismic data used in this study can be obtained from the Data Management Center of the Incorporated Research Institutions for Seismology (IRIS). The facilities of IRISData Services, and specifically the IRIS Data Management Center, were used for access to waveforms, related metadata, and/or derived products used in this study. IRIS Data Services are funded through the Seismological Facilities for the Advancement of Geoscience (SAGE) Award of the National Science Foundation under Cooperative Support Agreement EAR-1851048.
The comparison of NaCoF 3 to (Mg,Fe)SiO 3 in deformation experiments is essential in order to determine if NaCoF 3 is a relevant experimental analogue. Additionally, understanding how transformation mechanisms vary between analogues and natural compositions, including their effects on deformation and transformation textures, can inform us on the validity of analogues and their ability to predict the behavior of natural samples when direct studies of (Mg,Fe)SiO 3 cannot be performed. Here we use a resistive-heated radial DAC combined with synchrotron radiation at pressures and temperatures between 1. 1 and 29. 6 GPa and 300 and 1013 K, respectively, to observe in situ texture development and phase change from a perovskite to a post-perovskite structure in NaCoF 3. We use these data to model plastic deformation and deformation mechanisms in perovskite.
35 mm. Wavelength was fixed at 0. 4908 Å. Powdered NaCoF 3 perovskite from the study of  Dobson et al. (2011)  was loaded into an X-ray transparent boron epoxy gasket with an 80 µm diameter hole. A platinum flake was also loaded to be used as a pressure marker, using the thermal equation of state parameters of  Zha et al. (2008)  and the EosFit program  (Gonzalez-Platas et al. , 2016). Details on the synchrotron beamline setup and DAC can be found in  Liermann et al. (2015)  and  Immoor et al. (2020). The diamonds we used had a 300 µm culet size. Two thin graphite layers in contact with the anvils and surrounding the diamond tips were used for a restive heater, while two type-R thermocouples were used to monitor temperature. One of the thermocouples is located between both graphite heaters and the second on the diamond anvil next to the culet.
Data analysis Diffraction images were integrated over 5 • azimuthal arcs into 72 spectra and analyzed using the program MAUD (material analysis using diffraction)  (Lutterotti et al. , 1997)  following the general refinement procedure outlined in  Wenk et al. (2014). An example of MAUD refinement is shown in Fig. 2. Graphite peaks become more visible as pressure increases (e. g. , Fig. 2b  at 2θ values 6. 0, 8. 2, 13. 4, and 14. 6 • ). This is due to the closure of the window carved into the heater as the experiment proceeds. We exclude these regions in addition to the 2θ ranges where platinum is overlapping during the refinement process. Diffraction background was fit using polynomial functions. Structural parameters of NaCoF 3 were obtained from  Shirako et al. (2012) , and cell parameters and B factors were further refined using the data.
, 2018). The t/G values are then recalculated from the fitted t and the fixed G values. Do note, however, the G value used when refining t in MAUD has no impact on the final t/G ratio. Also note that MAUD allows for extraction of individual Q(hkl) for each diffraction peak, but the quality of our data and the number of overlapping peaks for perovskite and post-perovskite structures do not allow us to do so. https://doi. org/10. 5194/ejm-33-591-2021 Eur. J. Mineral. , 33, 591-603, 2021 Table  1. Image number, pressure (P ), temperature (T ), lattice parameters, normalized stress, and crystallite size (CS) measured in the experiment. Numbers in parenthesis for temperatures are uncertainties on the last digits, determined from the difference in readings of both thermocouples. Errors are estimated to be 0.
We observe a smooth decrease in unit cell volume with pressure. We used the program EosFit  (Gonzalez-Platas et al. , 2016)  to fit a second-order Birch-Murnaghan equation of state trend for perovskite between 1. 1 GPa and 868 K and 20. 1 GPa and 997 K and for all post-perovskite data. Considering the small ranges in temperature for the measurements, temperature effects were ignored. The resulting bulk modulus for perovskite and post-perovskite in the 868-1013 K range are 74. 9 and 85. 9 GPa, respectively. Based on Fig. 3 , the drop of volume at the perovskite to post-perovskite transition is estimated to be 6. 6 Å 3 Since the pressure and temperature effect on shear modulus is unknown for NaCoF 3 , we report stresses in terms of normalized stress t/G. This quantity is a more appropriate representation of stress, does not require the extrapolation of G, and has been used in past studies to compare materials to each other  (Duffy, 2007; Miyagi et al.
Further studies on analogues might also include the investigation of post-perovskite deformation textures in NaCoF 3 and other analogues, as well as potential post-post-perovskite phases  (Crichton et al. , 2016; Umemoto and Wentzcovitch, 2019). A general understanding of plasticity in perovskite and post-perovskite will help with improving the interpretation of seismic models in terms of mantle dynamics such as heat transfer through convection. Financial support. This research has been supported by the Association Nationale de la Recherche et de la Technologie (TIMEleSS, grant no. ANR-17-CE31-0025) and the Deutsche Forschungsgemeinschaft (grant nos. TH 1530/18-1, SA 2585/3-1, and SP1216/8-1). It was also supported by the bilateral PROCOPE-PPP program (grant nos. PHC 40555PC and DAAD 57390184).
Acknowledgements. The  Chevreul Institute  is thanked for its help in the development of this work through the  ARCHI-CM  project supported by the  "Ministère de l'Enseignement Supérieur de la Recherche et de l'Innovation", the region "Hauts-de-France" , the  ERDF program  of the  European Union , and the  "Métropole Européenne de Lille". This research was carried out at the P02. 2 beamline of the  PETRA III synchrotron at DESY , a member of the  Helmholtz Association (HGF). The authors would also like to thank  Feng Lin  for assistance with VPSC modeling.
Code and data availability. The data were processed using MAUD (http://maud. radiographema. eu, Lutterotti et al. , 1997)  and MTEX (https://mtex-toolbox. github. io, Bachmann et al. , 2010)  which are open source and freely available. VPSC modeling was performed using the Los Alamos visco-plastic self-consistent code available from Ricardo A. Lebensohn and Carlos N. Tomé. Maud and VPSC input files are available on Zenodo using the following link: https: //doi. org/10. 5281/zenodo. 5513910 (Gay et al. , 2021).
X-ray computed tomography (X-CT) X-CT characterization was performed at the synchrotron X-ray beamline PSICHE at SOLEIL synchrotron (France). The measurement was performed with a parallel monochromatic beam of 25 keV and with an exposure time of 500 ms per each projection. A matrix sub volume with a volume of 830 * 1500 * 700 µm was studied in detail. We measured 5900 2D projections of the linear attenuation coefficient (LAC) to reconstruct the LAC variations in 3D, with a final voxel size of ~0. 87 μm. Postprocessing 3D reconstruction was achieved using the Python library Tomopy  (Gursoy et al. 2014). The reconstruction was performed using PyHST2  (Mirone et al. , 2014). Detection of pores and iron-rich phases was then performed thanks to a threshold segmentation  (Dionnet et al. 2020) , and the study of the structures' shape was conducted with Quant3D  (Ketcham et al.
Petrography This chondrite with 14% chondrules supported by 86% fine grained matrix and accretionary chondrule rims is seen in Fig. 1a. The abundances were determined by using the image analysis program Qgis© and the term chondrule here includes complete chondrules, large chondrule fragments, and clusters or aggregates of phenocrysts (Fig. 1b ). About 84% of the chondrules are Type I and about 16% Type II, while a large Al-rich chondrule is included with CAI and AOA in Fig. 1b  as refractory material. Fig. 1b  shows that only 46% of the chondrules have complete or partial fine-grained compact accretionary rims. The chondrule abundance is at the low end of the normal range for CM chondrites but the matrix includes isolated grains (tens of microns in size) likely derived from chondrules. Chondrule size ranges from 15 µm to 2 mm, with many smaller ones being fragments or disrupted loose crystals.
, 2018)  and therefore are not indicative of a higher temperature that could demonstrate that the stability limits for cronstedtite and tochilinite were exceeded in NWA 12563. However, temperatures based on Raman data for the organics in these meteorites are in any case poorly constrained below 220°C  (Busemann et al. , 2007; Quirico et al. , 2018). In a similar fashion, the organic XANES data are also comparable with Paris and Murchison, which reinforces the conclusion that temperature was not significantly higher in NWA 12563. Lacking strong evidence for higher temperature, it would appear that higher fO 2 , low pressure and water/rock ratio, and lower a SiO2 were key factors in producing abundant magnetite  (Brearley, 2004; Yu, 2012; Vacher et al. , 2018)  in NWA 12563, as in WIS 91600, but not in CM2 chondrites.
, 2012). However, peak temperature estimates for some meteorites are far above those which could be achieved by solar heating  (Nakato et al. , 2013). WIS 91600 contains dehydrated saponite in the matrix  (Brearley, 2004; Tonui et al. , 2014). This is interpreted to be due to a milder reheating than that which produced the CY or Belgica chondrites  (Tomeoka et al. , 1989; Tonui et al. , 2014). The bulk H values of NWA 12563 suggest affinities with heated CM chondrites  (Alexander et al. (2013)  though the matrix shows no evidence for desiccation of phyllosilicates (Table  3 ). Olivine Cr composition data show that NWA 12563 has not been reheated above stage 3. 0  (Grossman and Brearley, 2005)  though this method is not sensitive to heating of short duration. It is possible that NWA 12563 represents the precursor material that was slightly heated to become WIS 91600.
INTRODUCTION On September 12, 2019 at 12:49:48 UT a daylight fireball was seen by hundreds of eye-witnesses from the Netherlands and Belgium and a few observers in Northern Germany, Denmark, and the UK. Soon after the event some incidental video recordings (dash, action and security cams) from the Netherlands and Germany appeared in the social media (e. g. , Fig. 1a ). More than 580 reports by witnesses were collected by the International Meteor Organization (IMO) via their fireball reporting website operated by Mike Hankey of the American Meteor Society. The bolide at 14:49:48 CEST local time was also observed by one of the authors (A. P. ) and was registered by one German AllSky6 meteor camera from Herford (AMS21), which can operate even during daylight hours (Fig. 1b ; Fig. S1 ). NASA-JPL's Center for Near Earth Object Studies (CNEOS) has released some basic data of the bolide event: The peak brightness of the fireball was reached over 54.
g. ,  Fuchs et al. , 1973; McSween, 1979a; Mackinnon and Zolensky, 1984; Rubin and Wasson, 1986; Tomeoka and Buseck, 1988; Zolensky and McSween, 1988; Fredriksson and Kerridge, 1988; Grimm and McSween, 1989; Zolensky et al. , 1989a Zolensky et al. , ,b, 1997 Zolensky et al. , , 2002;; Endress and Bischoff, 1993; Johnson and Prinz, 1993; Browning et al. , 1996; Bischoff, 1998; Brearley, 2006; Morlok et al. , 2006; Rubin et al. , 2007; Howard et al. , 2009; Alexander et al. , 2012 Alexander et al. , , 2013;; Tonui et al. , 2014; Garenne et al. , 2014; Visser et al. , 2018). However, as already stated in the Meteoritical Bulletin Database (https://www. lpi. usra. edu/meteor/metbull. php?-code=71098), differences exist between Flensburg and CI, CM, and CR chondrites, which will be discussed in detail in this study in order to achieve an appropriate classification.
The relevance of these observations will be discussed in Section 7. 11. The modal mineral abundances obtained by optical means given in Table  1  are the averages of four independent analyses determined by means of point counting (in all cases more than 1500 points were registered on areas of different sizes ranging from 8 mm 2 to 20 mm 2 covering a total area of about 56 mm 2 ). The data are slightly different to the results obtained by X-ray techniques. A total abundance of $3. 8 vol. % sulfides and $1. 9 vol. % magnetite was obtained from point counting. All these phases are heterogeneously distributed throughout the Flensburg meteorite. Minor amounts of chromite, ilmenite, Ca-phosphate (Fig. S3 ;  Holm, 2020) , and traces of a Fe,Ni,As(Te,S)-rich phase (see below) were also detected.
7 dpm kg À1 could be given, providing evidence for a short or complex exposure history of the meteoroid. The relevant AMS data for Flensburg and corresponding processing blanks, and specific activities for 10 Be, 26 Al, and 41 Ca for Flensburg have been calculated from AMS ratios, ICP-MS results of the liquid aliquot ( 27 Al and nat Ca) or carrier addition ( 9 Be), sample weight and half-lives. The concentrations of the three lighter radionuclides are extremely low ( 10 Be: 0. 0539 ± 0. 0016 dpm kg À1 , 26 Al: 0. 209 ± 0. 030 dpm kg À1 , 41 Ca: 0. 37 +0. 32  -0. 26 dpm kg À1 ). These values are one to more than two orders of magnitude lower than saturation activities under typical irradiation geometries. The 26 Al specific activity, determined from the AMS data, is about a factor of ten lower than the detection limit of gamma-spectrometry.
Clayton and Mayeda (1984)  presented an evolution model to understand the composition of components in the CM2 chondrite Murchison. They suggested that the primordial dust fell on the CCAM line and that interaction with liquid water in the CM chondrite parent body shifted the isotope compositions towards higher d 18 O values. Depending on the water/rock ratio (W/R), either the rocks shift in d 18 O towards higher values (high W/R) or the water shifts towards higher d 18 O (low W/R). The O isotope composition of Flensburg falls on the CCAM  (Clayton, 2008)  in the field of CM chondrites (Fig. 18 ), and only marginally overlaps with CR and CV chondrites (Figs. S13a  and b ). The isotope composition of Flensburg does not overlap with published data on CO chondrites (Fig. S13c ). Recently a CM1 clast in Mukundpura was found that also has a light O isotope composition  (Findlay et al.
This peak position is a result of the presence of phyllosilicates occurring in the samples  (Beck et al. , 2010). The CM, CV, and CH samples show other distinct RBs, which demonstrates the difference between these meteorites and Flensburg. The shoulder in the spectrum of Flensburg at about 11. 29 mm is probably due to the presence of calcite or ankerite  (Green and Schodlok, 2016). Olivine has also a strong feature at this wavelength (e. g. ,  Morlok et al. , 2020)  and, therefore, the feature may indicate the presence of minor amounts of olivine; however, olivine was not positively detected by optical microscopy, SEM, and TEM, but maybe by X-ray techniques (see SM). It is also possible that all observed shoulders are an effect of pentlandite. In this wavelength region, pentlandite also has some weak features (seen in a pentlandite spectrum laag02 taken from RELAB spectral database).
Flensburg and the meteorite fall statistics in Central Europe Considering the meteorite falls of Braunschweig (L6;  Bartoschewitz et al. , 2017) , Z ˇd'ar nad Sazavou (L3;  Spurny ´, 2016; Spurny ´et al. , 2016) , Ejby (H5/6;  Spurny ét al. , 2017; Haack et al. , 2019), Stubenberg (LL6; Ebert and Bischoff, 2016; Spurny ´et al. , 2016; Bischoff et al. , 2017a) , Hradec Kralove(LL5; 2016; The Meteoritical Bulletin), Broek in Waterland (L6, 2017; The Meteoritical Bulletin), and Renchen (L5-6;  Bischoff et al. , 2019b) , Flensburg is the eighth recovered meteorite fall since 2013 impacting on Earth in an area less than 500 km in radius. As estimated from meteorite entries within the Database (The Meteoritical Bulletin), on average, less than ten meteorite falls are recovered globally per year.
ACKNOWLEDGEMENTS We thank  U. Heitmann  ( Mu ¨nster ) for sample preparation, and  Jasper Berndt  (Mu ¨nster),  Beate Schmitte  (Mu ¨nster),  Sabrina Beutner  ( Dresden) , and  Sarah Lentfort  ( Mu ¨nster ) for their analytical assistance and support. We greatly acknowledge the constructive suggestions of  Jemma Davidson  and two further reviewers as well as the help and support of the Associate Editor  Pierre Beck. The help of  Martin Whitehouse  and  Robbin Visser  with providing standards for the analyses and data of carbonates is greatly acknowledged. We also thank  Gerd Baumgarten  and  Felix Bettonvil  for calibrations of video records of the daylight fireball with night time images. The mindfulness of  Erik Due-Hansen  and his kind cooperation with the scientists is highly appreciated.