bluuebunny/crossref_metadata_2025_split huggingface dataset:
MEANS OF VISUAL MODELING AND CODE GENERATION FOR FUZZY RULES
Authors: Дородных Никита Олегович , Юрин Александр Юрьевич , Коршунов Сергей Андреевич , Сопп Дмитрий Юрьевич , Шпаченко Дмитрий Сергеевич 
Published: May 2021

Логические и ассоциативные правила по-прежнему являются наиболее распространенным способом представления экспертных знаний и поддержки принятия решений, несмотря на популярность семантических технологий. Эффективное использование правил при принятии решений в случае неточной или неопределенной информации требует разработки специализированных лингвистических (языковых) и программных средств, как для их наглядного отображения, так и генерации программных кодов. В данной работе рассматривается FuzzyRVML, как расширение одного из языков визуального моделирования правил - Rule Visual Modeling Language, предназначенное для моделирования логических правил, содержащих элементы нечеткости. FuzzyRVML поддерживает нечеткий тип данных, понятия лингвистической переменной, терма и коэффициента уверенности. Представлены описания основных элементов и конструкций FuzzyRVML, а также иллюстративный пример, содержащий генерацию кода на FuzzyCLIPS. Программным средством поддержки предлагаемой нотации является Personal Knowledge Base Designer, на основе которого произведены ее оценка и реализация.
Logical and associative rules are still the most common way to represent expert knowledge and support of decision-making. The use of rules in the case of inaccurate or uncertain information requires the development of specialized linguistic (language) means and software, providing their visualization and generation of source codes. In this paper, we propose a FuzzyRVML - an extension of a Rule Visual Modeling Language, designed for modeling logical rules containing elements of fuzziness. FuzzyRVML supports the fuzzy data type, the concepts of linguistic variable, term, and certainty factor. Descriptions of the main elements and constructs of FuzzyRVML are presented, as well as an illustrative example containing code generation in FuzzyCLIPS. Personal Knowledge Base Designer was used to support the notation proposed, as well for its implementation and evaluation.
Dynamics of Crude Oil Price Change and Global Food Commodity Prices
Authors: Onour Ibrahim 
Published: May 2021

Purpose: This study investigates the effect of crude oil price fluctuations (price change as well as volatility) on wheat, sugar, corn, and fertilizers price changes.
Methods: The study employs Markov switching dynamic regression, Dynamic Conditional Correlation (DCC), and Generalized Autoregressive Conditional Hetrosekadicity (GARCH) on monthly data covering the period from January 1988 to April 2018.
Results: The findings of the research support evidence of two states. State 1, pertains to the low volatility of crude oil price, and state 2 belong to the case of the high volatility of crude oil prices. Our results indicated that at state 1, an increase in crude oil prices leads to a decline in food commodity prices, while in state 2, an increase in crude oil price levels causes an increase in food commodity prices. Results of Dynamic Conditional Correlation (DCC) GARCH estimates indicate the coefficients of oil price levels are significant and positively associated with the conditional volatility of the four commodity prices.
Implications: The findings of the research imply that volatility in global food commodity prices is not due to oil price volatility but due to the oil price levels attained at extreme points.
Originality: The paper investigates the impact of different volatility levels of crude oil prices on global food commodity prices.
Thermodynamical Description of Hot, Rapidly Rotating Neutron Stars, Protoneutron Stars, and Neutron Star Merger Remnants
Authors: Koliogiannis P. S. , Moustakidis Ch. C. 
Published: May 2021

Abstract
The prediction of the equation of state of hot, dense nuclear matter is one of the most complicated and interesting problems in nuclear astrophysics. At the same time, knowledge of it is the basic ingredient for some of the most interesting studies. In the present work, we concentrate our study on the construction of the equation of state of hot, dense nuclear matter, related mainly to the interior of the neutron star. We employ a theoretical nuclear model, which includes momentum-dependent interaction among the nucleons, along with state-of-the-art microscopic calculations. Thermal effects are introduced in a self-consistent way, and a set of isothermal and isentropic equations of state are predicted. The predicted equations of state are used in order to acquire and extend the knowledge of the thermal effect on both nonrotating and rapidly rotating with the Kepler frequency neutron stars. The simultaneous study of thermal and rotation effects provides useful information on some of the most important quantities, including the mass (gravitational and baryon) and radius, the Kepler frequency and Kerr parameter, the moment of inertia, etc. These quantities are directly related to studies of protoneutron stars and mainly the hot and rapidly rotating remnant of a binary neutron star merger. Data from the late observations of binary neutron star mergers and the present study may offer useful tools for investigation and help in providing possible constraints on the equation of state of nuclear matter.
Simultaneous Deep Measurements of CO Isotopologues and Dust Emission in Giant Molecular Clouds in the Andromeda Galaxy
Authors: Viaene Sébastien , Forbrich Jan , Lada Charles J. , Petitpas Glen , Faesi Christopher 
Published: May 2021

Abstract
We present simultaneous measurements of emission from dust continuum at 230 GHz and the J = 2–1 12CO, 13CO, and C18O isotopologues at ∼15 pc resolution from individual giant molecular clouds (GMCs) in the Andromeda galaxy (M31). These observations were obtained in an ongoing survey of this galaxy being conducted with the Submillimeter Array. Initial results describing the continuum and 12CO emission have been published earlier. Here, we primarily analyze the observations of 13CO and C18O emission and compare them to the measurements of dust continuum and 12CO emission. We also report additional dust continuum and CO measurements from newly added GMCs to the M31 sample. We detect spatially resolved 13CO emission with high signal-to-noise ratios in 31 objects. We find the extent of the 13CO emission to be nearly comparable to that of 12CO, typically covering 75% of the area of the 12CO emission. We derive 13CO and C18O abundances of 2.9 × 10−6 and 4.4 × 10−7 relative to H2, respectively, by comparison with hydrogen column densities of the same regions derived from the dust continuum observations assuming a Milky Way gas-to-dust ratio. We find the isotopic abundance ratio [13CO]/[C18O] = 6.7 ± 2.9 to be consistent with the Milky Way value (8.1). Finally, we derive the mass-to-light conversion factors for all three CO species to be α
12 = 8.7 ± 3.9, α
13 = 48.9 ± 20.4, and

M
⊙ (K km s−1 pc2)−1 for the J = 2–1 transitions of 12CO, 13CO, and C18O, respectively.
The ALMA Spectroscopic Survey in the HUDF: A Search for [C ii] Emitters at 6 ≤ z ≤ 8
Authors: Uzgil Bade D. , Oesch Pascal A. , Walter Fabian , Aravena Manuel , Boogaard Leindert , Carilli Chris , Decarli Roberto , Díaz-Santos Tanio , Fudamoto Yoshi , Inami Hanae , Bouwens Rychard , Cortes Paulo C. , Cox Pierre , Daddi Emmanuele , González-López Jorge , Labbe Ivo , Popping Gergö , Riechers Dominik , Stefanon Mauro , Van der Werf Paul , Weiss Axel 
Published: May 2021

Abstract
The Atacama Large Millimeter/submillimeter Array (ALMA) Spectroscopic Survey in the Hubble Ultra Deep Field (ASPECS) Band 6 scan (212–272 GHz) covers potential [C ii] emission in galaxies at 6 ≤ z ≤ 8 throughout a 2.9 arcmin2 area. By selecting on known Lyα emitters (LAEs) and photometric dropout galaxies in the field, we perform targeted searches down to a 5σ [C ii] luminosity depth L
[C II] ∼ 2.0 × 108
L
⊙, corresponding roughly to star formation rates (SFRs) of 10–20 M
⊙ yr−1 when applying a locally calibrated conversion for star-forming galaxies, yielding zero detections. While the majority of galaxies in this sample are characterized by lower SFRs, the resulting upper limits on [C ii] luminosity in these sources are consistent with the current literature sample of targeted ALMA observations of z = 6–7 LAEs and Lyman-break galaxies (LBGs), as well as the locally calibrated relations between L
[C ii] and SFR—with the exception of a single [C ii]-deficient, UV-luminous LBG. We also perform a blind search for [C ii]-bright galaxies that may have been missed by optical selections, resulting in an upper limit on the cumulative number density of [C ii] sources with L
[C II] > 2.0 × 108
L
⊙ (5σ) to be less than 1.8 × 10−4 Mpc−3 (90% confidence level). At this luminosity depth and volume coverage, we present an observed evolution of the [C ii] luminosity function from z = 6–8 to z ∼ 0 by comparing the ASPECS measurement to literature results at lower redshift.
ALMA Observations of Giant Molecular Clouds in M33. III. Spatially Resolved Features of the Star formation Inactive Million-solar-mass Cloud
Authors: Kondo Hiroshi , Tokuda Kazuki , Muraoka Kazuyuki , Nishimura Atsushi , Fujita Shinji , Tosaki Tomoka , Zahorecz Sarolta , Miura Rie E. , Kobayashi Masato I. N. , Onodera Sachiko , Torii Kazufumi , Kuno Nario , Sano Hidetoshi , Onishi Toshikazu , Saigo Kazuya , Fukui Yasuo , Kawamura Akiko , Tsuge Kisetsu , Tachihara Kengo 
Published: May 2021

Abstract
We present 12CO (J = 2–1), 13CO (J = 2–1), and C18O (J = 2–1) observations toward GMC-8, one of the most massive giant molecular clouds (GMCs) in M33 using ALMA with an angular resolution of 0.″44 × 0.″27 (∼2 pc × 1 pc). The earlier studies revealed that its high-mass star formation is inactive in spite of a sufficient molecular reservoir with a total mass of ∼106
M
⊙. The high-angular resolution data enable us to resolve this peculiar source down to a molecular clump scale. One of the GMC’s remarkable features is that a round-shaped gas structure (the “Main cloud”) extends over the ∼50 pc scale, which is quite different from the other two active star-forming GMCs dominated by remarkable filaments/shells obtained by our series of studies in M33. The fraction of the relatively dense gas traced by the 13CO data with respect to the total molecular mass is only ∼2%, suggesting that their spatial structure and the density are not well developed to reach an active star formation. The CO velocity analysis shows that the GMC is composed of a single component as a whole, but we found some local velocity fluctuations in the Main cloud and extra blueshifted components at the outer regions. Comparing the CO with previously published large-scale H i data, we suggest that an external atomic gas flow supplied a sufficient amount of material to grow the GMC up to ∼106
M
⊙.
MESA Models with Magnetic Braking
Authors: Gossage Seth , Dotter Aaron , Garraffo Cecilia , Drake Jeremy J. , Douglas Stephanie , Conroy Charlie 
Published: May 2021

Abstract
Two magnetic braking models are implemented in MESA for use in the MIST stellar model grids. Stars less than about 1.3 solar masses are observed to spin down over time through interaction with their magnetized stellar winds (i.e., magnetic braking). This is the basis for gyrochronology and is fundamental to the evolution of lower-mass stars. The detailed physics behind magnetic braking are uncertain, as are 1D stellar evolution models. Thus, we calibrate our models and compare to data from open clusters. Each braking model tested here is capable of reproducing aspects of the data, with important distinctions; neither fully accounts for the observations. The Matt et al. prescription matches the slowly rotating stars observed in open clusters but tends to overestimate the presence of rapidly rotating stars. The Garraffo et al. prescription often produces too much angular momentum loss to accurately match the observed slow sequence for lower-mass stars but reproduces the bimodal nature of slowly and rapidly rotating stars observed in open clusters fairly well. Our models additionally do not reproduce the observed solar lithium depletion, corroborating previous findings that effects other than rotation may be important. We find additional evidence that some level of mass dependency may be missing in these braking models to match the rotation periods observed in clusters older than 1 Gyr better.
Near-IR Observations of the Young Star [BHB2007]-1: A Substellar Companion Opening the Gap in the Disk
Authors: Zurlo Alice , Garufi Antonio , Pérez Sebastián , Alves Felipe O. , Girart Josep M. , Zhu Zhaohuan , Franco Gabriel A. P. , Cleeves L. Ilsedore 
Published: May 2021

Abstract
The presence of planets or substellar objects still embedded in their native protoplanetary disks is indirectly suggested by disk substructures like gaps, cavities, and spirals. However, these companions are rarely detected. We present Very Large Telescope/NACO high-contrast images in the J, H, K

S
, and

bands of the young star [BHB2007]-1 probing the inclined disk in scattered light and revealing the probable presence of a companion. The point source is detected in the

band in spatial correspondence with complementary Very Large Array observations. This object is constrained to have a mass in the range of 37–47 M
Jup and is located at 50 au from the central star, inside the 70 au-large disk cavity recently imaged by the Atacama Large Millimeter/submillimeter Array (ALMA), that is absent from our NACO data (down to 20 au). This mass range is compatible with the upper end derived from the size of the ALMA cavity. The NIR disk brightness is highly asymmetric around the minor axis, with the southern side 5.5 times brighter than the northern side. The constant amount of asymmetry across all wavelengths suggests that it is due to a shadow cast by a misaligned inner disk. The massive companion that we detect could, in principle, explain the possible disk misalignment, as well as the different cavity sizes inferred by the NACO and ALMA observations. The confirmation and characterization of the companion is entrusted to future observations.
Cosmic Evolution of the H2 Mass Density and the Epoch of Molecular Gas
Authors: Garratt T. K. , Coppin K. E. K. , Geach J. E. , Almaini O. , Hartley W. G. , Maltby D. T. , Simpson C. J. , Wilkinson A. , Conselice C. J. , Franco M. , Ivison R. J. , Koprowski M. P. , Lovell C. C. , Pope A. , Scott D. , van der Werf P. 
Published: May 2021

Abstract
We present new empirical constraints on the evolution of

, the cosmological mass density of molecular hydrogen, back to z ≈ 2.5. We employ a statistical approach measuring the average observed 850 μm flux density of near-infrared selected galaxies as a function of redshift. The redshift range considered corresponds to a span where the 850 μm band probes the Rayleigh–Jeans tail of thermal dust emission in the rest frame, and can therefore be used as an estimate of the mass of the interstellar medium. Our sample comprises of ≈150,000 galaxies in the UK InfraRed Telescope Infrared Deep Sky Survey Ultra-Deep Survey field with near-infrared magnitudes K
AB ≤ 25 mag and photometric redshifts with corresponding probability distribution functions derived from deep 12-band photometry. With a sample approximately 2 orders of magnitude larger than in previous works we significantly reduce statistical uncertainties on

to z ≈ 2.5. Our measurements are in broad agreement with recent direct estimates from blank field molecular gas surveys, finding that the epoch of molecular gas coincides with the peak epoch of star formation with

at z ≈ 2. We demonstrate that

can be broadly modeled by inverting the star formation rate (SFR) density with a fixed or weakly evolving star formation efficiency. This “constant efficiency” model shows a similar evolution to our statistically derived

, indicating that the dominant factor driving the peak star formation history at z ≈ 2 is a larger supply of molecular gas in galaxies rather than a significant evolution of the SFR efficiency within individual galaxies.
Implications of the Environments of Radio-detected Active Galactic Nuclei in a Complex Protostructure at z ∼ 3.3
Authors: Shen Lu , Lemaux Brian C. , Lubin Lori M. , Cucciati Olga , Le Fèvre Olivier , Liu Guilin , Fang Wenjuan , Pelliccia Debora , Tomczak Adam , McKean John , Miller Neal A. , Fassnacht Christopher D. , Gal Roy , Hung Denise , Hathi Nimish , Bardelli Sandro , Vergani Daniela , Zucca Elena 
Published: May 2021

Abstract
Radio active galactic nuclei (RAGNs) are mainly found in dense structures (i.e., clusters/groups) at redshifts of z < 2 and are commonly used to detect protoclusters at higher redshift. Here, we attempt to study the host and environmental properties of two relatively faint (L
1.4 GHz ∼ 1025 W Hz−1) RAGNs in a known protocluster at z = 3.3 in the PCl J0227-0421 field, detected using the latest radio observation obtained as part of the Observations of Redshift Evolution in Large-Scale Environments (ORELSE) survey. Using new spectroscopic observations obtained from the Keck/Multi-Object Spectrometer for Infra-Red Exploration as part of the Charting Cluster Construction with the VIMOS Ultra-Deep Survey (VUDS) and ORELSE (C3VO) survey and previous spectroscopic data obtained as part of the VIMOS-Very Large Telescope Deep Survey and VUDS, we revise the three-dimensional overdensity field around this protocluster. The protocluster is embedded in a large-scale overdensity protostructure. This protostructure has an estimated total mass of ∼2.6 × 1015
M
⊙ and contains several overdensity peaks. Both RAGNs are hosted by very bright and massive galaxies, while their hosts show extreme differences in color, indicating that they are of different ages and are in different evolutionary stages. Furthermore, we find that they are not in the most locally dense parts of the protostructure, but are fairly close to the centers of their parent overdensity peaks. We propose a scenario where merging might have already happened in both cases, which lowered the local density of their surrounding area and boosted their stellar mass. This work is the first time that two RAGNs at low luminosity have been found and studied within a high-redshift protostructure.
New Experimental 23Na(α, p)26Mg Reaction Rate for Massive Star and Type Ia Supernova Models
Authors: Hubbard N. J. , Diget C. Aa. , Fox S. P. , Fynbo H. O. U. , Howard A. M. , Kirsebom O. S. , Laird A. M. , Munch M. , Parikh A. , Pignatari M. , Tomlinson J. R. 
Published: May 2021

Abstract
The 23Na(α, p)26Mg reaction has been identified as having a significant impact on the nucleosynthesis of several nuclei between Ne and Ti in Type Ia supernovae, and of 23Na and 26Al in massive stars. The reaction has been subjected to renewed experimental interest recently, motivated by high uncertainties in early experimental data and in the statistical Hauser-Feshbach models used in reaction rate compilations. Early experiments were affected by target deterioration issues and unquantifiable uncertainties. Three new independent measurements instead are utilizing inverse kinematics and Rutherford scattering monitoring to resolve this. In this work we present directly measured angular distributions of the emitted protons to eliminate a discrepancy in the assumptions made in the recent reaction rate measurements, which results in cross sections differing by a factor of 3. We derive a new combined experimental reaction rate for the 23Na(α, p)26Mg reaction with a total uncertainty of 30% at relevant temperatures. Using our new 23Na(α, p)26Mg rate, the 26Al and 23Na production uncertainty is reduced to within 8%. In comparison, using the factor of 10 uncertainty previously recommended by the rate compilation STARLIB, 26Al and 23Na production was changing by more than a factor of 2. In Type Ia supernova conditions, the impact on production of 23Na is constrained to within 15%.
Le phrygien, une langue balkanique perdue en Anatolie
Authors: Anfosso Milena 
Published: May 2021

À partir d’une réflexion extralinguistique sur le mot phrygien βέκος, « pain », inspirée d’un article de Pietro Vannicelli de 1997, on essaiera de mettre brièvement en évidence l’appartenance du phrygien à la Balkanische Sprachbund , et en particulier le profond lien de parenté génétique avec le grec. Les deux langues sont en effet issues du même milieu linguistique balkanique, mais la migration du peuple phrygien vers l’Anatolie à la fin du ii e millénaire avant J.-C. interrompt leur continuité géographique. Le phrygien, attesté uniquement par des inscriptions étalées du ix e siècle avant J.-C. au iii e siècle après J.-C., devient alors une île linguistique balkanique entourée de plusieurs langues indigènes appartenant au groupe anatolien. Le peuple phrygien s’intègre dans ce milieu, comme les influences culturelles, mais aussi certains traits linguistiques, nous en témoignent. Toutefois les liens avec la langue sœur résistent, devenant même plus forts suite à la progressive hellénisation de la péninsule anatolienne par les Grecs, et nous fournissent à travers les inscriptions le matériel pour étudier à rebours leur parenté génétique.
La guerre d’Eumène II et ses alliés contre Pharnace (182-179 av. J.-C.). Problèmes et lectures géopolitiques des suites du traité d’Apamée
Authors: Payen Germain 
Published: May 2021

Quelques années après le traité d’Apamée (188 av. J.-C.), les puissances anatoliennes profitèrent du retrait séleucide pour établir un nouvel équilibre régional. La guerre menée entre 182 et 179 par deux coalitions, regroupant les rois attalide, cappadocien et bithynien, d’une part, et le roi du Pont et un satrape d’Arménie, de l’autre, en fut un moment déterminant. Le traité de paix conclu par ces dynastes en 179, connu par l’intermédiaire de Polybe, est une source importante pour comprendre l’ordre établi à cette occasion. La victoire d’Eumène consacra la position dominante de la dynastie attalide en Anatolie, notamment en Galatie. Plus globalement, les rois et dynastes profitèrent de la situation pour promouvoir leur légitimité sur la scène locale, tandis que la puissante cité de Rhodes resta très en retrait. La zone concernée par les tractations de paix s’étend loin à l’est, jusqu’en Arménie, et au nord, sur la rive septentrionale de la mer Noire. D’un point de vue plus large, le conflit consacra l’autonomie politique de la région à l’égard des puissances séleucide et, surtout romaine. Enfin, plusieurs zones d’ombre, telles que le statut géopolitique de la Galatie ou l’identité politique de Mithridate, satrape d’Arménie, peuvent être en partie éclaircies par la mise en parallèle de ce traité avec d’autres sources.
Méthodes et réflexions du père Ménestrier et des érudits héraldistes. En quête d’un ethos du blason
Authors: Mayaud Guy 
Published: May 2021

Les publications héraldiques du xviie siècle se présentent essentiellement sous un jour didactique. Mais elles témoignent aussi d’un effort de réflexion et de méthode en vue de formaliser un ethos de la connaissance et de l’usage des armes au sein des sociétés du Grand Siècle. Cette entreprise de documentation et de théorisation se cristallise dans l’œuvre du père Claude-François Ménestrier dans une perspective résolument pragmatique.
Une pierre d’aimant qui attire tout. L’héraldique au Portugal au XVII e siècle, un savoir disputé
Authors: Metelo de Seixas Miguel 
Published: May 2021

Au xvii e siècle, la production d’ouvrages héraldiques au Portugal fut abondante mais agitée de polémiques. Celles-ci reposaient largement sur la question du monopole des hérauts de la Couronne en la matière. Le savoir héraldique formait alors un discours complexe de justification de l’ordre politique et social, rendant compte de l’image idéale de la société et permettant, en même temps, d’en corriger les défauts. La rivalité entre officiers royaux et particuliers rendait visible l’équilibre précaire entre la Couronne et les différentes forces sociales qui cherchaient à s’approprier cette matière, dans le contexte de l’union ibérique puis, après 1640, dans celui de la restauration de l’indépendance portugaise sous la maison de Bragance.