dataesr/scientific-paragraphs-categorization huggingface dataset:
[111]  made a new method to quantify the efficiency of the magnetic refrigeration. They proposed to achieve the magnetic refrigeration with good performances without the using of thermally switchable components. The studied system consists of a MCM (pure Gd) positioned between two PMs that have a linear alternative movement. To explore a maximum of configurations, they developed a software called HEAt TRAnsfer in PYthon (HEATRAPY). This mathematical model has been developed by  Silva et al. (2018)   [112]. The working cycles are simulated in order to find the best configuration and to determine the temperature range reached by the studied system. They considered the model as validated by comparing the results with COMSOL Multiphysics ® results. With this 1-D model, they have tested 66 combinations of operating modes and found a maximum temperature range of 0.
Silva et al. (2019) The same year, but in another paper, Silva et al. [91]  developed two simple models of the magnetic refrigeration device again with the software HEATRAPY, in order to estimate the temperature range in a system. They also made two 1-D models for: (i) a solid-state magnetocaloric system, and (ii) a hydraulic AMRR system operating with a heat transfer fluid. They applied their model on both studied system and obtained the results shown in (Figure  27 ). Result was better for the magnetocaloric system using heat transfer fluids. They validated the results of the model using thermodynamic verification steps/criteria and results found in the literature. As already seen, they have developed an interesting Python software that allowed to perform multiple modeling runs per year and to study the heat transfers in a multitude of 1.
5-D model by considering the heat conduction and the thermo-physical parameters. Silva et al. (2014)   [113]  worked on a 1-D model with a FDM to optimize the temperature range of a solid-state AMRR applications by using Python language. The same year, but in another paper, Silva et al. [91]  developed two simple models of the magnetic refrigeration device again with the software HEATRAPY, in order to estimate the temperature range in a system. They also made two 1-D models for: (i) a solidstate magnetocaloric system, and (ii) a hydraulic AMRR system operating with a heat transfer fluid. They applied their model on both studied system and obtained the results shown in (Figure  27 ). Result was better for the magnetocaloric system using heat transfer fluids. They validated the results of the model using thermodynamic verification steps/criteria and results found in the literature.
As already seen, they have developed an interesting Python software that allowed to perform multiple modeling runs per year and to study the heat transfers in a multitude of 1. 5-D model by considering the heat conduction and the thermo-physical parameters. Silva et al. (2014)   [113]  worked on a 1-D model with a FDM to optimize the temperature range of a solid-state AMRR applications by using Python language. The same year, but in another paper, Silva et al. [91]  developed two simple models of the magnetic refrigeration device again with the software HEATRAPY, in order to estimate the temperature range in a system. They also made two 1-D models for: (i) a solidstate magnetocaloric system, and (ii) a hydraulic AMRR system operating with a heat transfer fluid. They applied their model on both studied system and obtained the results shown in (Figure  27 ).
Result was better for the magnetocaloric system using heat transfer fluids. They validated the results of the model using thermodynamic verification steps/criteria and results found in the literature. As already seen, they have developed an interesting Python software that allowed to perform multiple modeling runs per year and to study the heat transfers in a multitude of 1. [92]  developed a 1-D model to predict the performances of the AMRR. It consisted of studying the magnetocaloric properties and the thermal performances of the MCM alloys. The MCM of the studied regenerator is composed of threelayered La(Fe,Mn,Si) 13 H y spheroidal particles. The particles are bounded with an epoxy resin, which leads to the formation of epoxy bridges between the particles. These bridges can lead to some potential blockage for fluid flow passages.
The semi-analytical model was optimized with a hybrid method using firstly SciPY and then the sequential least squares quadratic programming method. The studied device is composed of two cylindrical multi-layer regenerators. The magnetic field of the device is generated by two nested concentric Halbach arrays which produce 1. 45 T. They divided the MCM in two parts. The first one-called 'hot layer'-is composed of Gd; and the second one-called 'cold layer'-is an alloy of Gd and GdY. To validate their model, they used two-layer performance data measured by an AMRR test device (Figure25). They finally found that the semi-analytical AMRR model gave good predictive capabilities. A temperature range of 40 K was experimentally measured. One year later, Teyber et al. (2019) [90]  performed another semi-analytical model validated by experimental measurements.
Methods. Models of solar-type stars are computed including atomic diffusion and rotation-induced mixing with the code STAREVOL. We explore different additional transport processes for chemicals and for angular momentum such as penetrative convection, tachocline mixing, and additional turbulence. We constrain the resulting models by simultaneously using the evolution of the surface rotation rate and 7 Li abundance in the solar-type stars of open clusters with different ages, and the solar surface and internal rotation profile as inverted from helioseismology when our models reach the age of the Sun. Results. We show the relevance of penetrative convection for the depletion of 7 Li in pre-main sequence and early main sequence stars. The rotational dependence of the depth of penetrative convection yields an anti-correlation between the initial rotation rate and 7 Li depletion in our models of solar-type stars that is in agreement with the observed trend.
g. Charbonnel & Talon 2005; Talon & Charbonnel 2005). In this work we explore the possibilities to reproduce simultaneously the chemical and rotational constraints for solar-type stars along their evolution up to the end of the MS. In § 2 we present the observational data that we aim to account for with our stellar evolution models. In § 3 we describe the input physics of the models and recall the state-of-the-art expressions from the literature for the different transport processes implemented in the stellar evolution code STAREVOL, and tested in this work. In § 4 we compare the predictions of the so-called Type I models for rotating stars (which only include meridional circulation, shear induced turbulence, and atomic diffusion) to the observational constraints for solar-type stars over a broad age range.
Stellar evolution models We use an updated version of the stellar evolution code STAREVOL (for general information and previous versions, see  Siess et al. 2000; Palacios et al. 2006; Decressin et al. 2009; Lagarde et al. 2012; Amard et al. 2019). All our models are evolved without accretion starting prior to the deuterium birthline on the PMS from initial structures corresponding to homogeneous polytropes. This sets the time zero of our computations.
Input physics We adopt the solar reference abundances from  Asplund et al. (2009)  including the enhancement of neon recommended by  Young (2018)  as reported in Table  1. The opacities are interpolated within the OPAL opacity tables  (Iglesias & Rogers 1996)  when T > 8000 K and the low-temperature opacity tables from the Wichita opacity database when T < 8000 K (Ferguson, J. W. , private communication) that are fully consistent with the adopted solar reference abundances. The equation of state is analytical and follows  Eggleton et al. (1973)  and  Pols et al. (1995) , as described in  Siess et al. (2000). We use the nuclear reactions rates from the NACRE2 database generated using the NetGen web interface  (Xu et al. 2013a,b). In the current version of STAREVOL the full set of stellar structure equations is solved for the whole star; there is no decoupling between the interior and the envelope (where the diffusion approximation becomes valid).
Acknowledgements. We thank  J. W. Ferguson  for providing us with lowtemperature opacity tables adapted to the solar mixture we adopt in this work,  P. Eggenberger  for fruitful discussions, and the anonymous referee for constructive comments on the manuscript. This work was supported by the  Swiss National Science Foundation  (Projects  200021-169125  and  200020-192039 PI C. C. ). We thank the  Programme National de Physique Stellaire (PNPS)  of  CNRS/INSU  cofunded by  CEA  and  CNES. This research has made use of NASA?s Astrophysics Data System Bibliographic Services. LA acknowledges funding from the  European Research Council (ERC)  under the European Union's  Horizon 2020 research and innovation program  (grant agreement No. 682393 AWESoMe-Stars). KCA and SM acknowledge support from the  ERC SPIRE 647383  grant and PLATO & GOLF CNES grants at  CEA/DAp-AIM.
Comparative Test For the primary analysis, we will follow patients who remain alive for 60 calendar days from randomization with primary outcome variable Y * being the follow up day of death. Thus, Y * has discrete support {1, • • • , 60, > 60} days during the follow up period, with Y * > 60 if the patient is alive at the end of 60 day follow up. The discrete support arises from the fact that time of randomization and death each are recorded as a calendar date. If a patient dies during the calendar day on which they are randomized, then Y * = 1; whereas, if a patient dies during the calendar day after they are randomized, then Y * = 2; and so on. While Y * is unknown for any patient who is alive at the end of 60-day follow-up, it is partially observed with Y * > 60. We use an asterisk to distinguish this from the observed time Y , which is subject to additional left-censoring mechanisms arising from loss to follow up and interim data analyses being carried out while some participants are in the midst of follow up.
This factorization illuminates two things: (i) multiple historical data sources could augment the prospective likelihood function each with their own contribution and historical bias parameters, (ii) individual-level historical data are not required for inference, rather sufficient statistics are all that is needed, which in this case are the number at risk and the number who died on each day during the 60-day follow up period. Recognizing that L(β | D n ) has the structure of a logistic regression model and following a similar strategy to  (Polson et al. , 2013) , we developed an efficient and conditionally conjugate Pólya-Gamma Gibbs sampler. We provide additional details in the Supplement  (Murray et al. , 2020) , and freely-available, user-friendly R software for implementation of all models under consideration (see Supplementary Materials).
For the Bayesian methods, after 200 warm-up iterations, we ran our Gibbs sampler for 2,000 iterations and used the resulting samples for posterior calculations. Each Gibbs sampler run for the Comm NPO model took about six minutes. The samplers for other models required fewer steps and were slightly faster, requiring one to five minutes per run. To speed up computations, we simulated trials in parallel on a HP Linux distributed cluster. We simulated 2,000 trials each under a null scenario and a target alternative scenario. For aim (i), prospective control data were generated from a survival distribution with π C,t = π C0,t , for t = 1,. , 60, i. e. ζ = 0 and z = 0, so that C was exactly congruous with the observed historical control data C 0. For the null scenario, the prospective external cooling data were generated from this same survival distribution.
Political context China is a one-party system: the Chinese Communist Party (CCP), headed by Xi Jinping since 2012, has been the only legitimate ruling party since 1949. After assuming office, Xi Jinping started touting his vision and interpretation of the 'China Dream,' which was officially defined as the grand rejuvenation of the Chinese nation  (Mingfu, 2009). According to Xi Jinping, this means bringing greater prosperity to the Chinese people while elevating China's role in the international community  (Kallio, 2015). The 'China Dream' is believed to have stimulated a new wave of nationalism throughout China. In addition, public support for the central government has been steadily increasing in recent years. The China Survey 2008, conducted by Texas A&M University, generated one of the latest datasets regarding Chinese citizens' public support for authority at different levels.
The death of Dr Li pulled the trigger: the hashtag #wewantfreedomofspeech was created on Weibo, the Chinese version of Twitter, after Dr Li's death was announced at 2 am on Friday, and it had over two million views and more than 5,500 posts in five hours  (Li, 2020). Amid fear and calls for justice, based on a variety of current Chinese laws, CAIXIN ran an article to analyse whether the local police department held any authority to admonish Dr Li. Apart from the conclusion that the Wuhan police department's admonishment was not supported by law, they alleged the local authority abused their power and was potentially guilty of serious professional misconduct. Another topic that generated a lot of public discussion was whether the local government should or was obliged to disclose information and data regarding the virus.
Throughout the pandemic, science and academic actors (scholars and academies) have been in the public limelight like never before. Science communication was very prominent, explaining statistics, exponential growths, reproduction rates, aerosols and other medical and statistical data. While only 0. 5% of URLs are expert sources, the single most shared URL in our dataset is a YouTube video by the famous German scientist and science blogger Mai Thi Nguyen-Kim titled 'Corona is just getting started' from April 1. 10 On the other hand, the political conf lict over the question of when to reopen and exit from anti-corona measures led to an instrumentalisation of science and the widespread impression that scientists frequently changed their opinion and could not agree on anything. Surveys show that trust in and reputation of science increased, but only a minority of Germans understand what science is about and how it works  (Petersen, 2020).
During the COVID-19 crisis, many such press conferences were held in European countries. Politicians used press conferences to share general information about the current COVID-19 situation (number of new cases/hospitalisations/deaths etc. ), to communicate concrete rules and measure, and to frame the national and international situation for their citizens. In this chapter, we analyse the Austrian government's televised press conferences as the main channel of communication during the COVID-19 crisis. Our dataset includes all televised national press conferences, taking place almost daily, including weekends, from their start on March 10 until the last press conference on May 27 (n = 64). Within these 64 press conferences, 187 statements were made by 47 different actors. The content of each statement was coded, focusing on the proximity level of the threat(s) communicated (from a threat to the self to a threat to the world) and the main issues discussed.
The VVV has proven to be extremely successful, so much so that a 3 year extension, dubbed the VVV eXtended survey, or VVVX for short, is now underway  (Minniti 2018). The VVVX extends the spatial coverage of near-IR imaging of the bulge out to 10 • in both Galactic latitude and longitude -the entire area of Fig. 1. The VVV team has taken full advantage of this unique database to study BGCs. They have discovered many new GC candidates (e. g. , Moni  Bidin et al. 2011; Minniti et al. 2011 Minniti et al. , 2017a,b;,b; Palma et al. 2019) , found dual horizontal branches in two metal-rich GCs  (Mauro et al. 2012) , investigated structural parameters  (Cohen et al. 2014) , studied variable stars (e. g. ,  Alonso-García et al. 2015) , and provided the deepest VVV-based color-magnitude diagrams (CMDs) to date  (Cohen et al.
5 Gyr precision from purely near-IR ground-based imaging, even in the cluster center. Similar deep GeMS and HST optical-near-IR images for a number of BGCs are now in hand, providing an unprecedented photometric database for a large number of BGCs. However, to measure the best age, and hence pin down the earliest formation epoch of the Galaxy with the smallest error, requires both deep high spatial resolution photometry and high spectral resolution spectroscopy to derive the detailed abundances required for isochrone fitting. The main factors that are still sorely lacking are good [Fe/H], [α/Fe], and [CNO/Fe] values for BGCs, all of which are very scarce. All CMD-based age diagnostics are very sensitive to these key elements. Given our exquisite near-IR photometry exemplified by NGC 6624 (also see, e.
We aim to help gather the first definitive database on the BGC system, search for the oldest object in the Galaxy with an accurate age, study the very complex nature of the GB and uncover any underlying correlations, determine BGC velocities and orbits and investigate multiple populations in the BGC system, and compare them to their halo (and disk) counterparts. As noted above, this demands as complete a sample as possible. The power of this approach is to establish the population of BGCs as an ensemble, finally placing them on a level with and in the context of their hither-to much better-studied halo counterparts, and thus fill in our picture of all Milky Way GC systems, especially the in situ BGCs. CAPOS originally targetted 20 cataloged BGCs, with the goal of bringing the number of bona fide BGCs observed by APOGEE to 28, over half of the total, with CAPOS supplying almost three-fourths of the observed sample.
CAPOS will, together with the SDSS-IV data, provide a legacy database of the BGC system. This will provide much better and completely self-consistent spectroscopic metallicities than currently available for all the observed BGCs, as well as derive detailed abundances for some 20 elements with a wide variety of nucleosynthetic origins, precise to ∼ 0. 05 dex. Current knowledge of their abundances is limited to only a few, if any, spectra of individual stars, and/or crude photometric metallicity estimates, or even integrated light measurements in many cases. We will also obtain excellent radial velocities. Many of the BGCs have only limited or even nonexistent velocity information. CAPOS also targets any recently discovered BGC candidates that can be observed serendipitously with cataloged BGCs, given the large field of view of APOGEE.
ASPCAP results Results presented here are based on the DR16 ASPCAP analysis. Future papers will explore different analysis techniques such as deriving our own atmospheric parameters and using BACCHUS (Brussels Automatic Code for Characterizing High accUracy Spectra -  Masseron et al. 2016 ), which will allow us to compare CAPOS results in closer detail with those derived for BGCs observed by the SDSS APOGEE survey and analyzed using this code and independent atmospheric parameters  (Masseron et al. 2019; Mészáros et al. 2020).
3  (Bica et al. 1998)  to -1. 11  (Ortolani et al. 2019 ), a range of 0. 8 dex. No other high-resolution abundance study has been carried out. However, we note that  Kunder & Butler (2020)  have studied this cluster using the same DR16 ASPCAP database. They identify the same members as we do but derive a slightly higher mean metallicity of -1. 05 since they do not correct the 2G stars. Among the most reliable studies are those of  Dias et al. (2016) , who found -0. 79±0. 09 from low-resolution optical spectra, and several studies using the CaT technique, including  Vásquez et al. (2018) , who yield values ranging from -0. 97 to -1. 09 depending on their calibration, and  Geisler et al. (2021) , who give -0. 75±0. 05. Our value is in poor agreement with H10, but in good to fair agreement with the recent low-resolution spectroscopic studies, although generally more metal-poor.
Given that Si is also affected to some extent by MPs, and that 2G stars generally have smaller [Si/Fe] than 1G stars (see below), we expect the Horta mean [Si/Fe] values, using all stars irrespective of their 1G or 2G nature, to be somewhat lower than our means, using only 1G stars, and their errors to be larger. For the three GCs in common, Horta gives [Si/Fe] = 0. 26±0. 02 for Terzan 2, while we derive 0. 25±0. 01; 0. 22±0. 06 for HP 1 versus our 0. 27±0. 01, and 0. 21±0. 04 for NGC 6540 versus our 0. 27 (only one 1G star). This generally agrees with our expectations. In addition, from the same DR16 ASPCAP database and for the same sample of stars as ours,  Kunder & Butler (2020)   2020 ). All of our BGCs are relatively metal-poor and all fall along the high-α (low-SNeIa) sequence. They also generally follow closely the field star trend at comparable metallicity.
5 Gyr isochrones calculated in the metallicity range from [Fe/H]=-1. 4 to [Fe/H]=-0. 8, appropriate for our sample. Isochrones were obtained from the Padova database  (Bressan et al. 2012). The bump values we find are between 4800 K and 4914 K, depending on the metallicity. We find that all our stars are cooler than the bump, and therefore post-bump stars, with the exception of a couple of targets that lie in this range. We conclude that our sample is not significantly affected by evolutionary effects in its C and N abundances, at least differentially, as virtually all stars lie in the same evolutionary phase. We also find that the N abundance range is very large amongst our targets and that N is very effective in separating 1G and 2G stars. Our study of MP is unfortunately limited by several factors.
Conclusions We present an overview and initial ASPCAP results of CAPOS, the bulge Cluster APOgee Survey. This survey is designed to obtain detailed abundances and kinematics for as complete a sample of bona fide BGCs as possible using the unique advantages of APOGEE in order to exploit their extraordinary Galactic archaeology attributes. We aim to help gather the first definitive database on the BGC system, provide accurate chemical characterizations of some of the oldest objects, and perhaps the oldest, in the Milky Way, study the very complex nature of the GB and uncover any underlying correlations, determine their orbits, and search for MPs in the BGC system and compare them to their halo (and disk) counterparts. CAPOS observed 16 cataloged BGCs, and also several BGC candidates recently uncovered in the same fields, as well as a large number of field stars selected from the general field, the K2 Galactic Archaeology Program (K2GAP), and the EMBLA and PIGS surveys for metal-poor stars.
Here we present initial CAPOS results for seven cataloged BGCs that were analyzed using the APOGEE pipeline ASPCAP as part of the 16th data release of the SDSS IV survey. ASPCAP provides atmospheric parameters, an accurate RV and detailed abundances for some 20 chemical elements. In future papers, we will derive abundances for this sample from boutique analyses, including stars with S/N below the ASPCAP limit, investigate the non-BGC M22, as well as results for the CAPOS field stars observed in DR16. Subsequent papers will include additional BGCs and field stars obtained after the data included in DR16. We find no clustering in metallicity:RV space for our 9 targets in the BGC candidate Minni 51 and thus no evidence for its reality. The observed GC giant targets were carefully selected based on spatial position, existing photometry, radial velocity, proper motion and any spectroscopic metallicity information available in order to maximize cluster membership.