bluuebunny/crossref_metadata_2025_split huggingface dataset:
Efectos de dosis creciente de fertilizante mineral con diferentes distancias de siembra en el cultivo desoja (Glycine max L.)
Authors: Florentin Figueredo Nilsa , Lugo Pereira Wilfrido Daniel , Sánchez Jara Raul , López Ávalos Derlys Fernando , Da Silva Oviedo Modesto Osmar , Mongelos Barrios Carlos Alberto , Morel López Eulalio , Caballero Casuriaga Oscar 
Published: December 2022

El trabajo de investigación tuvo como objetivo general, evaluar el efecto diferentes distancias entre plantas con dosis creciente de fertilizantes minerales en cultivo de soja (Glycine max L.). Se realizó en la localidad de San Marcos km 34 de la Ruta V Gral. Bernardino Caballero, distante a 7 Km de la Facultad de Ciencias Agrarias/Universidad Nacional de Concepción, sede Horqueta. El diseño experimental utilizado fue el de Bloques Completos al Azar (DBCA), con un arreglo factorial de 2x5 (dos distancias entre plantas y cinco dosis de fertilizante mineral). Los tratamientos utilizados fueron: factor A: (0,10 cm/pl y 0,20 cm/pl); factor B: (0, 100, 200, 300 y 400 kg.ha-1 de 00-30-20). Los datos obtenidos, se sometieron a análisis de varianza, comparación de medias por el test de Tukey y análisis de regresión. Los tratamientos aplicados influyeron significativamente para el número de vainas por planta, peso de mil granos y rendimiento del cultivo; pero no se observó diferencias en cuanto al número de granos por vaina. Se concluye que la distancia de siembra de 10 cm entre plantas (Factor A) y 300 kg ha-1 de fertilizante mineral (Factor B), presentó mayor rendimiento en el cultivo de soja.
FAKTOR PENGEMBANGAN POTENSI DIRI: MINAT/KEGEMARAN, LINGKUNGAN DAN SELF DISCLOSURE (SUATU KAJIAN STUDI LITERATUR MANAJEMEN PENDIDIKAN DAN ILMU SOSIAL)
Authors: Alfazani M. Rosyid , Khoirunisa A Dinda 
Published: December 2022

Riset terdahulu atau riset yang relevan sangat penting dalam suatu riset atau artikel ilmiah. Riset terdahulu atau riset yang relevan berfungsi untuk memperkuat teori dan penomena hubungan atau pengaruh antar variable. Artikel ini mereview Faktor-faktor yang mempengaruhi pengembangan potensi diri, yaitu: Minat/Kegemaran, Lingkungan dan Self Disclosure, suatu studi literatur manajemen pendidikan dan ilmu sosial. Hasil artikel literature review ini adalah: 1) Minat/kegemaran berpengaruh terhadap Pengembangan Potensi Diri; 2) Lingkungan berpengaruh terhadap Pengembangan Potensi Diri; dan 3) Self Disclosure berpengaruh terhadap Pengembangan Potensi Diri.
The Sensitivity of Eclipse Mapping to Planetary Rotation
Authors: Adams Arthur D. , Rauscher Emily 
Published: December 2022

Abstract
Mapping exoplanets across phases and during secondary eclipse is a powerful technique for characterizing Hot Jupiters in emission. Since these planets are expected to rotate about axes normal to their orbital planes, with rotation periods synchronized with their orbital periods, mapping provides a direct correspondence between the orbital phase and planetary longitude. We develop a framework to understand the information content of planets where their rotation states are not well constrained, by constructing bases of light curves across different rotation rates and obliquities that are orthogonal in integrated flux across the secondary eclipse. These demonstrate that brightness variation during eclipse may arise from a variety of rotation rates, obliquities, and map structures, requiring priors to properly disentangle each of these components. By modeling eclipse observations of the Warm Jupiter HAT-P-18b we demonstrate that, at a signal-to-noise equivalent to ∼10 orbits with JWST, confusion about map structure is likely a concern only at the upper physical limits of possible rotation rates. Even without priors, one may nevertheless be able to put an order-of-magnitude constraint on rotation rate by determining at what rates the fitted map complexity is minimized, a prescription whose efficacy increases if out-of-eclipse data are available to isolate the effects of rotation. Finally, in the limit of maps with longitudinal symmetry, the projected obliquity in the plane of the sky determines the information available during eclipse, ranging from nondetections of structure to a basic constraint on hemispherical asymmetry and orientation depending on the obliquity angle.
Photometric and Spectroscopic Study of the EXor-like Eruptive Young Star Gaia19fct
Authors: Park Sunkyung , Kóspál Ágnes , Ábrahám Péter , Cruz-Sáenz de Miera Fernando , Fiorellino Eleonora , Siwak Michał , Nagy Zsófia , Giannini Teresa , Carini Roberta , Szabó Zsófia Marianna , Lee Jeong-Eun , Lee Jae-Joon , Vitali Fabrizio , Kun Mária , Cseh Borbála , Krezinger Máté , Kriskovics Levente , Ordasi András , Pál András , Szakáts Róbert , Vida Krisztián , Vinkó József 
Published: December 2022

Abstract
Gaia19fct is one of the Gaia-alerted eruptive young stars that has undergone several brightening events. We conducted monitoring observations using multifilter optical and near-infrared photometry, as well as near-infrared spectroscopy, to understand the physical properties of Gaia19fct and investigate whether it fits into the historically defined two classes. We present the analyses of light curves, color variations, spectral lines, and CO modeling. The light curves show at least five brightening events since 2015, and the multifilter color evolutions are mostly gray. The gray evolution indicates that bursts are triggered by mechanisms other than extinction. Our near-infrared spectra exhibit both absorption and emission lines and show time variability throughout our observations. We found lower rotational velocity and lower temperature from the near-infrared atomic absorption lines than from the optical lines, suggesting that Gaia19fct has a Keplerian rotating disk. The CO overtone features show a superposition of absorption and emission components, which is unlike other young stellar objects. We modeled the CO lines, and the result suggests that the emission and absorption components are formed in different regions. We found that although Gaia19fct exhibits characteristics of both types of eruptive young stars, FU Orionis–type objects and EX Lupi–type objects, it shows more similarity with EXors in general.
Lost in Space: Companions’ Fatal Dance around Massive Dying Stars
Authors: Regály Zsolt , Fröhlich Viktória , Vinkó József 
Published: December 2022

Abstract
Discoveries of planet and stellar remnant hosting pulsars challenge our understanding, as the violent supernova explosion that forms the pulsar presumably destabilizes the system. Type II supernova explosions lead to the formation of eccentric bound systems, free-floating planets, neutron stars, pulsars, and white dwarfs. Analytical and numerical studies of high mass-loss rate systems based on perturbation theory so far have focused mainly on planet-star systems. In this paper, we extend our understanding of the fate of planet-star and binary systems by assuming a homologous envelope expansion model using a plausible ejection velocity (1000–10,000 km s−1), and envelope and neutron star masses. The investigation covers secondary masses of 1–10 M
J for planetary companions and 1–20 M
⊙ for stellar companions. We conduct and analyze over 2.5 million simulations assuming different semimajor axes (2.23–100 au), eccentricities (0–0.8), and true anomalies (0–2π) for the companion. In a homologous expansion scenario, we confirm that the most probable outcome of the explosion is the destabilization of the system, while the retention of a bound system requires a highly eccentric primordial orbit. In general, a higher ejecta velocity results in a lower eccentricity orbit independent of secondary mass. The explanation of close-in pulsar planets requires exotic formation scenarios, rather than survival through the type II supernova explosion model. Postexplosion bound star systems gain a peculiar velocity (<100 km s−1), even though the explosion model is symmetric. The applied numerical model allows us to derive velocity components for dissociating systems. The peculiar velocities of free-floating planets and stellar corpses are in the range of 10−6–275 km s−1.
The Star Formation Rate of the Milky Way as Seen by Herschel
Authors: Elia D. , Molinari S. , Schisano E. , Soler J. D. , Merello M. , Russeil D. , Veneziani M. , Zavagno A. , Noriega-Crespo A. , Olmi L. , Benedettini M. , Hennebelle P. , Klessen R. S. , Leurini S. , Paladini R. , Pezzuto S. , Traficante A. , Eden D. J. , Martin P. G. , Sormani M. , Coletta A. , Colman T. , Plume R. , Maruccia Y. , Mininni C. , Liu S. J. 
Published: December 2022

Abstract
We present a new derivation of the Milky Way’s current star formation rate (SFR) based on the data of the Herschel InfraRed Galactic Plane Survey (Hi-GAL). We estimate the distribution of the SFR across the Galactic plane from the star-forming clumps identified in the Hi-GAL survey and calculate the total SFR from the sum of their contributions. The estimate of the global SFR amounts to 2.0 ± 0.7 M
⊙ yr−1, of which 1.7 ± 0.6 M
⊙ yr−1 coming from clumps with reliable heliocentric distance assignment. This value is in general agreement with estimates found in the literature of last decades. The profile of SFR density averaged in Galactocentric rings is found to be qualitatively similar to others previously computed, with a peak corresponding to the Central Molecular Zone and another one around Galactocentric radius R
gal ∼ 5 kpc, followed by an exponential decrease as

log
(

Σ

SFR

/

[

M

⊙

yr

−
1

kpc

−
2

]
)
=
a

R

gal

/

[
kpc
]
+
b

, with a = −0.28 ± 0.01. In this regard, the fraction of SFR produced within and outside the solar circle is 84% and 16%, respectively; the fraction corresponding to the far outer Galaxy (R
gal > 13.5 kpc) is only 1%. We also find that, for R
gal > 3 kpc, our data follow a power law as a function of density, similarly to the Kennicutt–Schmidt relation. Finally, we compare the distribution of the SFR density across the face-on Galactic plane and those of median parameters, such as temperature, luminosity/mass ratio, and bolometric temperature, describing the evolutionary stage of Hi-GAL clumps. We found no clear correlation between the SFR and the clump evolutionary stage.
Demographics of the M-star Multiple Population in the Orion Nebula Cluster
Authors: De Furio Matthew , Liu Christopher , Meyer Michael R. , Reiter Megan , Kraus Adam , Dupuy Trent , Monnier John 
Published: December 2022

Abstract
We present updated results constraining multiplicity demographics for the stellar population of the Orion Nebula Cluster (ONC, a high-mass, high-density star-forming region), across primary masses 0.08–0.7 M
⊙. Our study utilizes archival Hubble Space Telescope data obtained with the Advanced Camera for Surveys using multiple filters (GO-10246). Previous multiplicity surveys in low-mass, low-density associations like Taurus identify an excess of companions to low-mass stars roughly twice that of the Galactic field and find the mass ratio distribution consistent with the field. Previously, we found the companion frequency to low-mass stars in the ONC is consistent with the Galactic field over mass ratios = 0.6–1.0 and projected separations = 30–160 au, without placing constraints on the mass ratio distribution. In this study, we investigate the companion population of the ONC with a double point-spread function (PSF) fitting algorithm sensitive to separations larger than 10 au (0.″025) using empirical PSF models. We identified 44 companions (14 new), and with a Bayesian analysis we estimate the companion frequency to low-mass stars in the ONC = 0.13

−
0.03

+
0.05

and the index of the power-law fit to the mass ratio distribution = 2.08

−
0.85

+
1.03

over all mass ratios and projected separations of 10–200 au. We find the companion frequency in the ONC is consistent with the Galactic field population, likely from states of high transient stellar density, and a probability of 0.002 that it is consistent with that of Taurus. We also find the ONC mass ratio distribution is consistent with the field and Taurus, potentially indicative of its primordial nature, a direct outcome of the star formation process.
Implications of High-density, High-temperature Ridges Observed in Some Two-ribbon Flares
Authors: Longcope Dana , Qiu Jiong 
Published: December 2022

Abstract
Several two-ribbon solar flares observed on the disk, notably including the Bastille flare of 2000 July 14, show an extended ridge of plasma running along the loop tops of the post-reconnection arcade. In that and two more recent examples, the ridge is visible in emission by Fe xxiv at roughly 17 MK, with a high, steadily increasing emission measure suggesting an expanding column of very dense plasma. We find that ridges are consistent with overhead views of long, vertical plasma sheets, such as seen above certain limb flares. Those vertical features show enhanced temperature and density over their entire lengths, making explanations in terms of termination shocks and evaporation collision seem less plausible. We use observations of several ridge events to argue in favor of compression and heating by slow magnetosonic shocks in the reconnection outflow. In this scenario, the ridge is built up as retracting flux piles hot, compressed plasma atop the post-flare arcade. Thanks to the overhead perspective offered by the ridge observations, we are able to measure the reconnection rate and show it to be consistent with the rate of increase in column emission measure across the ridge. This consistency supports the hypothesis that slow shocks and retraction compress the plasma seen in ridges, vertical plasma sheets, and possibly the high-temperature fans through which post-reconnection downflows are observed. Such a unified picture of these diverse features enhances our understanding of the role played by magnetic reconnection in solar flares.
Hubble Space Telescope Observations of Tadpole Galaxies Kiso3867, SBS0, SBS1, and UM461
Authors: Elmegreen Debra Meloy , Elmegreen Bruce G. , Gallagher John S. , Kotulla Ralf , Almeida Jorge Sánchez , Muñoz-Tuñón Casiana , Caon Nicola , Rafelski Marc , Sunnquist Ben , Revalski Mitchell , Andersen Morten 
Published: December 2022

Abstract
Tadpole galaxies are metal-poor dwarfs with typically one dominant star-forming region, giving them a head–tail structure when inclined. A metallicity drop in the head suggests that gas accretion with even lower metallicity stimulated the star formation. Here we present multiband Hubble Space Telescope WFC3 and Advanced Camera for Surveys images of four nearby (<25 Mpc) tadpoles, SBS0, SBS1, Kiso3867, and UM461, selected for their clear metallicity drops shown in previous spectroscopic studies. The properties of the star complexes and compact clusters are measured. Each galaxy contains from three to 10 young stellar complexes with 103–105
M
⊙ of stars ∼3–10 Myr old. Between the complexes, the disk has a typical age of ∼3 Gyr. Numerous star clusters cover the galaxies, both inside and outside the complexes. The combined cluster mass function, made by normalizing the masses and counts before stacking, is a power law with a slope of −1.12 ± 0.14 on a log–log plot and the combined distribution function of cluster lifetime decays with age as t
−0.65±0.24. A comparison between the summed theoretical Lyman continuum (LyC) emission from all the clusters, given their masses and ages, is comparable to or exceeds the LyC needed to excite the observed Hα in some galaxies, suggesting LyC absorption by dust or undetected gas in the halo, or perhaps galaxy escape.
Tidal Distortions as a Bottleneck on Constraining Exoplanet Compositions
Authors: Berardo David , de Wit Julien 
Published: December 2022

Abstract
Improvements in the number of confirmed planets and the precision of observations imply a need to better understand subtle effects that may bias interpretations of exoplanet observations. One such effect is the distortion of a short period planet by its host star, affecting its derived density. We extend the work of Burton et al., Correia, and others, using a gravitational potential formulation to a sample of nearly 200 planets with periods less than 3 days. We find five planets exhibiting density variations of >10% and as many as 20 planets with deviations >5%. We derive an analytic approximation for this deviation as a function of the orbital period, transit depth, and mass ratio between the planet and host star, allowing for rapid determination of such tidal effects. We find that current density error bars are typically larger than tidal deviations but that reducing the uncertainty on transit depth and radial velocity (RV) amplitude by a factor of 3 causes tidal effects to dominate density errors (>50%) in >40% of planets in our sample, implying that in the near future upgraded observational precision will cause shape deviations to become a bottleneck with regards to analysis of exoplanet compositions. These two parameters are found to dominate uncertainties compared to errors on stellar mass and radius. We identify a group of eight planets (including WASP-19 b, HAT-P-7 b, and WASP-12 b) for which current density uncertainties are as much as 4× smaller than the potential shift due to tides, implying a possible 4σ bias on their density estimates.
High-precision Nuclear Chronometer for the Cosmos
Authors: Wu 吴 X. H. 鑫辉 , Zhao 赵 P. W. 鹏巍 , Zhang 张 S. Q. 双全 , Meng 孟 J. 杰 
Published: December 2022

Abstract
Nuclear chronometers, which predict the ages of the oldest stars by comparing the present and initial abundances of long-lived radioactive nuclides, provide an independent dating technique for the cosmos. The idea of synchronizing Th/X, U/X, and Th/U chronometers can impose stringent constraints on the astrophysical conditions in the r-process simulations, giving rise to the Th-U-X chronometer. It is found that the astrophysical uncertainties of nuclear cosmochronology are significantly reduced from more than ±2 billion years to about 0.3 billion years. The Th-U-X chronometer is then applied to estimate the ages of the six metal-poor stars with observed uranium abundances, and the predicted ages are compatible with the cosmic age of 13.8 billion years predicted from the cosmic microwave background radiation but contradict the cosmic age of 11.4 billion years from the gravitational lens measurement.
L’envers de la guerre contre la drogue
Authors: Iglesias Nieto Raúl , Gaussens Pierre 
Published: December 2022

FR – Cet article présente les résultats d’un travail de recherche exploratoire sur le déplacement forcé au Mexique, à partir du cas de sa région nord-est, frontalière avec les États-Unis, dans laquelle plusieurs municipalités ont été touchées par des dynamiques de violence et de dépeuplement ces vingt dernières années (2000-2020), en pleine « guerre de la drogue ». Basée sur une méthodologie quantitative, l’étude développe une analyse spatiale et statistique qui met en relation le déplacement forcé, produit de la violence criminelle, et la présence d’importants gisements d’hydrocarbures dans cette région. Le principal résultat est que les municipalités qui apparaissent comme étant les plus affectées par la violence se trouveraient dans l’aire du Bassin de Burgos, qui contient la plus grande réserve de gaz de schiste du pays.
Aux origines nietzschéennes des ambiguïtés du concept d’entrepreneur : Schumpeter lecteur de Nietzsche
Authors: Colin-Jaeger Nathanaël , Wiedemann Étienne 
Published: December 2022

La figure de l’entrepreneur est aujourd’hui utilisée dans une grande variété de discours publics. Ce travail cherche à remonter à l’une des sources théoriques de la constitution de cette figure : la théorie de l’entrepreneur de Schumpeter (1911a et 1911b). Ce retour montre que Schumpeter, dans son contexte intellectuel et théorique, est amené à importer une anthropologie philosophique en économie, celle de Nietzsche, auteur largement lu dans l’Autriche du début du xx e siècle. En transposant, à l’intérieur de sa théorie économique, certaines caractéristiques majeures du grand homme créatif nietzschéen dans la figure de l’entrepreneur, Schumpeter développe une explication originale de la nature dynamique du marché et de l’évolution économique. Néanmoins il importe aussi de Nietzsche une série d’ambiguïtés, notamment en ce qui concerne l’origine de l’exceptionnalité individuelle de l’entrepreneur, et plus particulièrement de sa puissance créatrice. Une seconde ambiguïté est très largement héritée, qui concerne l’extension du modèle de l’individu entrepreneur : constitue-t-il une théorie de l’action valable pour tous les individus ou uniquement pour un type d’individus particuliers ? Comment concilier exceptionnalité de l’entrepreneur et norme d’un entreprenariat pour tous ? La dernière partie de ce travail s’attache ainsi à explorer ces ambiguïtés, qui apparaissent chez Schumpeter et ses successeurs, notamment Israël Kirzner. Codes JEL : B13, B25, B31, B40.
PREDICTING LOCATION AND EVALUATING PROGRESSION OF CLOGGING IN A PERMEABLE PAVEMENT PARKING LOT
Authors: O’Connor Thomas P. , Borst Michael 
Published: December 2022

ABSTRACT
In 2009, a permeable pavement research and demonstration site was constructed at the Edison Environmental Center, Edison, NJ. Infiltration testing of three original permeable parking rows through August 2012 indicated that clogging occurred along the upgradient edge of these pavements from runoff that drained from adjacent impermeable driving lanes.
A subsequent infiltration testing data collection effort from April 2017 through March 2020 focused on permeable interlocking concrete pavers (PICP) that replaced one of the original permeable surfaces. While the original infiltration study through 2012 used random locations throughout the permeable parking rows, the newer study targeted upgradient edge to identify where clogging would occur. Testing locations along the upgradient edge were selected based on a high-resolution survey (HRS) of the parking lot performed in December 2014. The HRS identified three low spots along the upgradient edge that eventually clogged in the new PICP infiltration study.
The HRS may assist with maintenance routines. The newer study also supports the conclusion of the earlier study with regards to truncating the infiltration testing method, particularly for maintenance assessments.
WHAT HINDERS THE TRANSITION TOWARDS SUSTAINABLE CONSTRUCTION IN CHINA? CRITICAL CHALLENGES AND FUTURE DIRECTIONS
Authors: Chang Ruidong , Song Xiangnan , Omrany Hossein 
Published: December 2022

ABSTRACT
As the largest construction industry in the world, the Chinese construction industry not only has huge sustainability implications for China, but also significantly influences the world’s resource consumption due to its tremendous scale. However, there is a lack of studies identifying the fundamental challenges hindering the transformation towards sustainable construction in China from a holistic triple bottom line perspective of sustainability. This study aims to identify the challenges, thereby revealing the future research directions accelerating the transition towards sustainable construction in China. Through content analysis of both existing literature and government plans, this study identifies the key sustainability challenges, governmental measures, and critical future research opportunities to help tackle the challenges hindering the sustainability transition of the Chinese construction industry. Even though this study focuses on China, it provides a holistic reference for researchers, industry practitioners and policymakers worldwide to understand the sustainability challenges of the construction industry, as the construction industries in many countries face sustainability challenges similar to those in China.