bluuebunny/crossref_metadata_2025_split huggingface dataset:
Trascendencia de la lúdica como dimensión psicoespiritual en el proyecto de vida de los actantes educativos
Authors: Ramírez Almanza Nerio J. 
Published: November 2020

La educación es uno de los elementos esenciales del ser humano y de la sociedad, por tal motivo, los centros de formación deben dar respuestas constantes y oportunas a todo el conglomerado de actantes educativos; de allí que la investigación titulada: Trascendencia de la lúdica como dimensión psicoespiritual en el proyecto de vida de los actantes educativos; y la cual está fundamentada en Newson (1986), Cabrera (2009), Flaceiére (1993), Universidad del Norte (2010),Cordero (2010), Jiménez (2007), Beltrán (2002), Medina (2014), Echeverry y Gómez (2009), Paredes (2003),García (2004). La indagación tiene la finalidad de analizar la trascendencia de la lúdica como dimensión psicoespiritual en el proyecto de vida de los actantes educativos; cuyo abordaje epistemológico se enmarcó en un enfoque cualitativo, bajo la metodología centrada en una revisión bibliográfica. Llegando a la conclusión de que la lúdica como dimensión psicoespiritual, va a transformar el proceso de enseñanza-aprendizaje, puesto que, son los actantes educativos los protagonistas de dicho proceso; y a su vez como dimensión; ya que encamina al hombre al desarrollo emocional y a los talentos personales, ayudando con ello a alcanzar su felicidad; se sugiere a los docentes a nivel andragógico que, diseñen actividades, encuentros, convivencias, ejercicios, que persigan no solo el disfrute de esos actos, sino del crecimiento psicológico y espiritual de los actantes educativos.
Determination of the molecular structure and (m,n) index assignment to the constituent walls of MWCNTs with undetermined diameters and chirality
Authors: Andonovic Viktor , Dimitrov Aleksandar T , Paunovic Perica , Andonovic Beti 
Published: November 2020

Each carbon nanotube (CNT) has its own mathematical representation due to its hexagonal lattice structure. The subjects of research are multi-wall carbon nanotubes (MWCNTs) and determining their structural parameters: innermost and outermost diameters, chiral indices m and n, number of walls and their unit cell parameters. Within this paper low frequency region and corresponding high frequency parts of Raman spectra of three experimentally produced CNTs are considered, as well as use of Python programming for the most accurate (m,n) assignment. Determining the chirality of these samples enables calculation of other structural properties which are performed hereby. Furthermore, this author’s work enables future studies on the samples, as are calculation of different topological indices using the graph representation and the chirality of the studied CNT samples.
Hard X-Ray Excess from the Magnificent Seven Neutron Stars
Authors: Dessert Christopher , Foster Joshua W. , Safdi Benjamin R. 
Published: November 2020

Abstract
We report significant hard X-ray excesses in the energy range 2–8 keV for two nearby isolated neutron stars: RX J1856.6−3754 and RX J0420.0−5022. These neutron stars have previously been observed in soft X-rays to have nearly thermal spectra at temperatures ∼100 eV, which are thought to arise from the warm neutron star surfaces. We find nontrivial hard X-ray spectra well above the thermal surface predictions with archival data from the XMM-Newton and Chandra X-ray telescopes. We analyze possible systematic effects that could generate such spurious signals, such as nearby X-ray point sources and pileup of soft X-rays, but we find that the hard X-ray excesses are robust to these systematics to the extent that is possible to test. We also investigate possible sources of hard X-ray emission from the neutron stars and find no satisfactory explanation with known mechanisms, suggesting that a novel source of X-ray emission is at play. We do not find high-significance hard X-ray excesses from the other five Magnificent Seven isolated neutron stars.
The Nonstandard Properties of a “Standard” PWN: Unveiling the Mysteries of PWN G21.5–0.9 Using Its IR and X-Ray Emission
Authors: Hattori Soichiro , Straal Samayra M. , Zhang Emily , Temim Tea , Gelfand Joseph D. , Slane Patrick O. 
Published: November 2020

Abstract
The evolution of a pulsar wind nebula (PWN) depends on properties of the progenitor star, supernova, and surrounding environment. As some of these quantities are difficult to measure, reproducing the observed dynamical properties and spectral energy distribution (SED) with an evolutionary model is often the best approach to estimating their values. G21.5−0.9, powered by the pulsar J1833−1034, is a well observed PWN for which previous modeling efforts have struggled to reproduce the observed SED. In this study, we reanalyze archival infrared (IR; Herschel, Spitzer) and X-ray (Chandra, NuSTAR, Hitomi) observations. The similar morphology observed between IR line and continuum images of this source indicates that a significant portion of this emission is generated by surrounding dust and gas, and not synchrotron radiation from the PWN. Furthermore, we find that the broadband X-ray spectrum of this source is best described by a series of power laws fit over distinct energy bands. For all X-ray detectors, we find significant softening and decreasing unabsorbed flux in higher energy bands. Our model for the evolution of a PWN is able to reproduce the properties of this source when the supernova ejecta has a low initial kinetic energy E
sn ≈ 1.2 × 1050 erg and the spectrum of particles injected into the PWN at the termination shock is softer at low energies. Lastly, our hydrodynamical modeling of the supernova remnant can reproduce its morphology if there is a significant increase in the density of the ambient medium ∼1.8 pc north of the explosion center.
A Measurement of the CMB E-mode Angular Power Spectrum at Subdegree Scales from 670 Square Degrees of POLARBEAR Data
Authors: Adachi S. , Aguilar Faúndez M. A. O. , Arnold K. , Baccigalupi C. , Barron D. , Beck D. , Bianchini F. , Chapman S. , Cheung K. , Chinone Y. , Crowley K. , Dobbs M. , Bouhargani H. El , Elleflot T. , Errard J. , Fabbian G. , Feng C. , Fujino T. , Galitzki N. , Goeckner-Wald N. , Groh J. , Hall G. , Hasegawa M. , Hazumi M. , Hirose H. , Jaffe A. H. , Jeong O. , Kaneko D. , Katayama N. , Keating B. , Kikuchi S. , Kisner T. , Kusaka A. , Lee A. T. , Leon D. , Linder E. , Lowry L. N. , Matsuda F. , Matsumura T. , Minami Y. , Navaroli M. , Nishino H. , Pham A. T. P. , Poletti D. , Reichardt C. L. , Segawa Y. , Siritanasak P. , Tajima O. , Takakura S. , Takatori S. , Tanabe D. , Teply G. P. , Tsai C. , Vergès C. , Westbrook B. , Zhou Y. ,   (The Polarbear Collaboration)
Published: November 2020

Abstract
We report a measurement of the E-mode polarization power spectrum of the cosmic microwave background (CMB) using 150 GHz data taken from 2014 July to 2016 December with the Polarbear experiment. We reach an effective polarization map noise level of

-

across an observation area of 670 square degrees. We measure the EE power spectrum over the angular multipole range

, tracing the third to seventh acoustic peaks with high sensitivity. The statistical uncertainty on E-mode bandpowers is ∼2.3

at

, with a systematic uncertainty of 0.5

. The data are consistent with the standard ΛCDM cosmological model with a probability-to-exceed of 0.38. We combine recent CMB E-mode measurements and make inferences about cosmological parameters in ΛCDM as well as in extensions to ΛCDM. Adding the ground-based CMB polarization measurements to the Planck data set reduces the uncertainty on the Hubble constant by a factor of 1.2 to

. When allowing the number of relativistic species (

) to vary, we find

, which is in good agreement with the standard value of 3.046. Instead allowing the primordial helium abundance (

) to vary, the data favor

. This is very close to the expectation of 0.2467 from big bang nucleosynthesis. When varying both

and

, we find

and

.
A New Candidate Transitional Millisecond Pulsar in the Subluminous Disk State: 4FGL J0407.7–5702
Authors: Miller Jessie M. , Swihart Samuel J. , Strader Jay , Urquhart Ryan , Aydi Elias , Chomiuk Laura , Dage Kristen C. , Kawash Adam , Shishkovsky Laura , Sokolovsky Kirill V. 
Published: November 2020

Abstract
We report the discovery of a variable optical and X-ray source within the error ellipse of the previously unassociated Fermi Large Area Telescope γ-ray source 4FGL J0407.7–5702. A 22 ks observation from XMM-Newton/European Photon Imaging Camera (EPIC) shows an X-ray light curve with rapid variability and flaring. The X-ray spectrum is well fit by a hard power law with Γ = 1.7. Optical photometry taken over several epochs is dominated by aperiodic variations of moderate amplitude. Optical spectroscopy with Southern Astrophysical Research (SOAR) and Gemini reveals a blue continuum with broad and double-peaked H and He emission, as expected for an accretion disk around a compact binary. Overall, the optical, X-ray, and γ-ray properties of 4FGL J0407.7–5702 are consistent with a classification as a transitional millisecond pulsar in the subluminous disk state. We also present evidence that this source is more distant than other confirmed or candidate transitional millisecond pulsar binaries, and that the ratio of X-ray to γ-ray flux is a promising tool to help identify such binaries, indicating that a more complete census for these rare systems is becoming possible.
An Obscured, Seyfert 2–like State of the Stellar-mass Black Hole GRS 1915+105 Caused by Failed Disk Winds
Authors: Miller J. M. , Zoghbi A. , Raymond J. , Balakrishnan M. , Brenneman L. , Cackett E. , Draghis P. , Fabian A. C. , Gallo E. , Kaastra J. , Kallman T. , Kammoun E. , Motta S. E. , Proga D. , Reynolds M. T. , Trueba N. 
Published: November 2020

Abstract
We report on Chandra grating spectra of the stellar-mass black hole GRS 1915+105 obtained during a novel, highly obscured state. As the source entered this state, a dense, massive accretion disk wind was detected through strong absorption lines. Photoionization modeling indicates that it must originate close to the central engine, orders of magnitude from the outer accretion disk. Strong, nearly sinusoidal flux variability in this phase yielded a key insight: the wind is blueshifted when its column density is relatively low, but redshifted as it approaches the Compton-thick threshold. At no point does the wind appear to achieve the local escape velocity; in this sense, it is a “failed wind.” Later observations suggest that the disk ultimately fails to keep even the central engine clear of gas, leading to heavily obscured and Compton-thick states characterized by very strong Fe K emission lines. Indeed, these later spectra are successfully described using models developed for obscured active galactic nuclei (AGNs). We discuss our results in terms of the remarkable similarity of GRS 1915+105 deep in its “obscured state” to Seyfert 2 and Compton-thick AGNs, and we explore how our understanding of accretion and obscuration in massive black holes is impacted by our observations.
Mg ii Absorbers in High-resolution Quasar Spectra. I. Voigt Profile Models
Authors: Churchill Christopher W. , Evans Jessica L. , Stemock Bryson , Nielsen Nikole M. , Kacprzak Glenn G. , Murphy Michael T. 
Published: November 2020

Abstract
We present the Voigt profile (VP) models, column densities, Doppler b parameters, kinematics, and distribution of components for 422 Mg ii absorbers found in a survey of 249 HIRES and UVES quasar spectra. The equivalent width range of the sample is 0.006 ≤ W

r
(2796) ≤ 6.23 Å and the redshift range is 0.19 ≤ z ≤ 2.55, with a mean of

. Based on historical precedent, we classified 180 absorbers as weak systems (W

r
(2796) < 0.3 Å) and 242 as strong systems (W

r
(2796) ≥ 0.3 Å). Assuming a minimum number of significant components per system, the VP fitting, yielded a total of 2989 components, with an average of 2.7 and 10.3 components found for the weak and strong Mg ii subsamples, respectively. The VP component line density for the full sample is 8.62 ± 0.23 clouds Å−1. The distribution of VP component column density over the range 12.4 ≤ log N(Mg ii) ≤ 17.0 cm−2 is well modeled with a power-law slope of −1.45 ± 0.01. The median Doppler b parameters are 4.5 ± 3.5 km s−1, 6.0 ± 4.5 km s−1, and 5.7 ± 4.4 km s−1 for the weak, strong, and full samples. We modeled the probability of component velocity splitting (the two-point velocity correlation function) of our full sample using a three-component composite Gaussian function. Our resulting velocity dispersions are σ
1 = 25.4 km s−1, σ
2 = 68.7 km s−1, and σ
3 = 207.1 km s−1. These data provide an excellent database for studying the cosmic evolution of Mg ii absorber kinematic evolution.
On the Use of Naked-eye Sunspot Observations during the Maunder Minimum
Authors: Carrasco V. M. S. , Gallego M. C. , Arlt R. , Vaquero J. M. 
Published: November 2020

Abstract
Naked-eye sunspot observations (NESOs) have been recorded for the past two millennia, approximately. These kinds of records were made around the world, mainly in Asian civilizations, and they are compiled in several catalogs. In this work, we analyze solar activity on days of the 19th century when NESOs were recorded. We found that only more than five sunspot groups were recorded in 39% of days corresponding to these NESO events. Furthermore, regarding the largest groups observed on days when NESOs were reported, we show that the uncorrected areas of these groups were below 200 millionths of solar disk (msd) in 3.2% of total cases, while it is 12.9% for areas between 200 and 499 msd. Thus, NESO records do not necessarily imply high solar activity and big sunspot groups. Therefore, these results contradict the interpretations of recent works that, using the same NESO set, suggest the solar activity level during the Maunder Minimum is still an open question. NESO records support the Maunder Minimum as a very low solar activity period.
An Analysis of the North Polar Spur Using HaloSat
Authors: LaRocca Daniel M. , Kaaret Philip , Kuntz K. D. , Hodges-Kluck Edmund , Zajczyk Anna , Bluem Jesse , Ringuette Rebecca , Jahoda Keith M. 
Published: November 2020

Abstract
We present HaloSat X-ray observations of the entirety of the bright X-ray emitting feature known as the North Polar Spur (NPS). The large field of view of HaloSat enabled coverage of the entire bright NPS in only 14 fields, which were each observed for ≈30,000 s. We find that the NPS fields are distinct in both brightness and spectral shape from the surrounding halo fields. We fit the NPS as two thermal components in ionization equilibrium with temperatures

and

. We note a temperature gradient in the NPS hot component with an inner arc temperature warmer than the outer arc. The emission measures we find for the cool component of the NPS is a factor of 3–5 greater than that of the hot component, which suggests that the bulk of the NPS material is in the ≈0.1 keV component. We evaluate distance estimates of 0.4 and 8.0 kpc for the NPS. Our findings suggest a preference for a distant NPS with an energy of ≈ 6 × 1054 erg, an age of ≈ 10 Myr, and pressures consistent with a 10μG magnetic field associated with the Fermi bubbles. The electron density ≈10 × 10−3 cm−3 is consistent with estimates for the shock region surrounding a Galactic-scale event.
Revealing the Spectroscopic Variations of FU Orionis Object V960 Mon with High-resolution Spectroscopy
Authors: Takagi Yuhei , Honda Satoshi , Arai Akira , Takahashi Jun , Oasa Yumiko , Itoh Yoichi 
Published: November 2020

Abstract
We present the results of the high-resolution spectroscopy of the FU Orionis-type star V960 Mon. The brightness of V960 Mon decreased continuously after the outburst was detected in 2014 November. During this dimming event, we carried out medium-resolution spectroscopic monitoring observations and found that the equivalent width of the absorption features showed variations. To further investigate the spectroscopic variations, we conducted a high-resolution spectroscopic observation of V960 Mon with the Subaru Telescope and the High Dispersion Spectrograph on 2018 January 8 and 2020 February 1. By comparing this spectrum with the archival data of the Keck Observatory and the High Resolution Echelle Spectrometer taken between 2014 and 2017, we found that the absorption profiles changed as V960 Mon faded. The line profile of absorption lines such as Fe i and Ca i can be explained by a sum of the spectra of the disk atmosphere and the central star. The model spectrum created to explain the variations of the line profiles suggests that the effective temperature of the central star is ∼5500 K, which is comparable to that of the pre-outburst phase with a distance of 1.6 kpc with Gaia. The spectrum also shows that the effective temperature of the disk atmosphere decreased as V960 Mon faded. The variations of the Hα and Ca ii lines (8498.0, 8542.1 Å) also show that the V960 Mon spectrum became central-star dominant.
Machine Learning as a Flaring Storm Warning Machine: Was a Warning Machine for the 2017 September Solar Flaring Storm Possible?
Authors: Benvenuto F. , Campi C. , Massone A. M. , Piana M. 
Published: November 2020

Abstract
Machine learning is now one of the methodologies of choice for flare forecasting, and supervised techniques, in both their traditional and deep versions, are becoming more frequently used for prediction in this area of space weather. Most studies assess the prediction effectiveness of machine-learning methods by computing confusion matrices, which are typically highly non-diagonal, particularly in applications concerning the forecasting of X-class flares. The present study suggests that the reliability of the outcomes of a supervised machine-learning method could be better assessed by using it as a warning machine, sounding binary alerts unrolled over time, and by comparing the number of alerts sounded by the machine in specific time windows with the number of events actually observed in those time windows. Indeed, when applied to the prediction of the events associated with the 2017 September solar storm, a hybrid LASSO algorithm was able to sound alerts every day a flare actually occurred; it also identified the corresponding flare class. In addition, the machine was able to predict with some accuracy a reliable proxy of the energy budget daily released by magnetic reconnection during the entire course of the storm. Finally, the analysis shows that the combination of sparsity-enhancing machine learning and feature ranking could allow the identification of the prominent role that the Ising energy played as an active region property in the forecasting process.
Prevalence of Amblyopia After Photoscreening
Authors: Laiginhas Rita , Ferreira Cláudia Costa , Leitão Raquel , Geraldes Rafael , Chibante-Pedro João , Monteiro Madalena , de Matos Coimbra 
Published: November 2020

Purpose:
To assess the prevalence of amblyopia in a population of adolescents screened for amblyogenic risk factors at preschool age.

Methods:
Data were retrospectively collected from the preschool screening for amblyogenic risk factors routinely performed in the authors' hospital. A stratified random sampling was used. A school from the region was randomly selected and then two grades were randomly selected. All classes from these grades were evaluated and only children who were previously screened for amblyogenic risk factors were included. Ophthalmological examination included best visual acuity (distance and near, Early Treatment of Diabetic Retinopathy Study scale and Jaeger eye chart) and stereopsis (Randot Stereo Test; Stereo Optical Company, Inc). Sample size was estimated as more than 283 participants. Pertinent data were extracted for analysis.

Results:
A total of 520 children were recruited, and 299 met the inclusion criteria. Fifteen percent of children (n = 46) had results at the screening that prompted a further ophthalmological evaluation and 9% of children (n = 26) had meaningful refractive errors or strabismus. Overall amblyopia prevalence was 1.00%. One of the 3 children who developed amblyopia had microstrabismus, and the remaining 2 children had a previous positive screening result but missed the follow-up evaluations. At the follow-up evaluation, 79.3% (n = 237) of children were not wearing glasses.

Conclusions:
A structured screening may allow the early detection of amblyogenic factors and prevent further vision deterioration in children, thus improving their long-term quality of life. The prevalence of amblyopia in this study was lower than that recently stated for Europe.

[
J Pediatr Ophthalmol Strabismus
. 2020;57(6):372–377.]
Perlindungan Hukum Terhadap Peniruan Merek Mawar + Logo
Authors: David David , Simamora Esther Lita , Sitompul Petrus George Victory , Steven Steven 
Published: November 2020

Abstrak
Hak kekayaan intelektual merupakan kekuatan kreaktifitas dan inovasi yang diterapkan melalui ekspresi artistik. dalam hal ini sumber daya pontesial intelektual seseorang yang tidak terbatas dan dapat diperoleh oleh semua orang. hak kekayaan intelektual merupakan sebuah kekuatan yang dapat digunakan untuk meningkatkan martabat seseorang dan masa depan suatu bangsa, secara material, budaya dan sosial.
Merek digunakan sebagai tanda untuk membedakan produk yang dihasilkan oleh seseorang atau suatu badan hukum denganproduk yang dihasilkan pihak lain. fungsi utama dari sebuah merek adalah agar konsumen dapat mencirikan suatu produk baik barang maupun jasa yang dimiliki oleh perusahaan sehingga dapat dibedakan dari produk perusahaan lain yang serupa atau mirip yang dimiliki oleh pesaingnya.Konsumen yang merasa puas dengan suatu produk dengan merek tersebut di masa yang akan datan,
Pengusaha yang sukses pasti punya kiat dan setiap pelaku usaha kiat suksesnya punpasti berbeda. umumnya pola pemasaran dan keandalan SDM (Sumber Daya Manusia) punya peranan penting dalam membangun suatu usaha namun tidak kalah pentingnya adalah perlunya " Merek Dagang".MAju mundurnya sebuah usaha sangat dipengaruhi oleh merek yang sekaligus sebagai pembawa ciri atau kepribadian suatu usaha oleh karenannya tidak heran sebuah entitas usaha selalu membangun dan menjaga citra merek dagangnya agar tidak dirusak oleh pihak tertentu.
Berdasarkan pasal 1 angka 1 UU no. 20 tahun 2016 definisi merek adalah tanda yang dapat ditampilkan secara grafis berupa gambar, logo, nama, kata, huruf, angka, susunan warna dan bentuk 2 dimensi atau 3 dimensi, suara, hologram atau kombinasi dari 2 atau lebih unsur tersebut untuk membedakan barang atau jasa diproduksi oleh orang atau badan hukum dalam kegiatan perdagangan baeang atau jasa.
PERLINDUNGAN POTRET UNTUK PROMOSI TANPA IZIN PIHAK TERKAIT BERDASARKAN UNDANG-UNDANG NOMOR 28 TAHUN 2014
Authors: Dwika Nurtati , Siregar Emmi , Pratiwi Irda 
Published: November 2020

portrait are photography work with humans objects. And the portrait it self is regulated by copyright law. If a portrait is taken without the consent of the photographed, the photografer will be subject to law number 28 of 2014. if the portrait is used for promotion or published without the must permission of the photographer or the heir, the photografer must first ask permission of the photografer. If the photographer does not have permission to the photographed or the heirs to carry out commercial uses, procurement, distribution, etc., will be subject to article 115 of law number 28 of 2014 concerning copyright. The photographer will be charged with a maximum fine of Rp 500.000.000,00 (five hundred million rupiah). It would be better if a photographer who would take someone’s portrait for promotion would be better to ask permission of the portrait or ask permission from the heirs first