bluuebunny/crossref_metadata_2025_split huggingface dataset:
Transparency of Composite Materials
Authors: Новак Н.В. 
Published: March 2022

На формирование оптических свойств зуба существенное влияние оказывает светопроницаемость его твердых тканей. Эмаль и дентин способны частично пропускать световые лучи, при этом светопроводимость эмали выше, чем дентина.Цель исследования: изучение степени прозрачности светопроницаемых композиционных материалов, используемых при изготовлении эстетических реставраций для имитации прозрачности режущего края зуба.Материалы и методы. Для изучения степени прозрачности светопроницаемых композиционных материалов разных фирм-производителей из этих материалов были изготовлены диски толщиной 0,5 мм и 1,0 мм и изучена светопроницаемость.Результаты. Представлены результаты изучения степени прозрачности светопроницаемых композиционных материалов, используемых для имитации прозрачности режущего края при изготовлении эстетических реставраций зубов. Исследован коэффициент светопроницаемости композитов, проведена визуальная оценка светопроводимости пломбировочных материалов разных фирм, выполнена сравнительная визуальная оценка светопроницаемости прозрачных образцов фотополимеров разной толщины.Заключение. Показано, что чем толще слой светопроницаемого материала, тем больше его вклад в формирование оттенков цвета, слои разной толщины могут существенно преобразовывать оптические свойства, оказывая влияние на цвет и светопроницаемость изготовленной эстетической конструкции.
The transparency of its solid fabrics has significant effect on formation of optical properties of tooth. Enamel and dentine are capable to pass partially light beams, at the same time the transparency of enamel is higher, than dentine.Purpose of the study: studying of degree of transparency of the transparent composite materials used at production of esthetic restorations for imitation of transparency of a cutting edge of tooth. Materials and methods. For studying of degree of transparency of transparent composite materials of different manufacturing firms disks 0.5 mm and 1.0 mm thick were made of these materials and the transparency is studied.Results of studying of degree of transparency of the transparent composite materials used for imitation of transparency of a cutting edge at production of esthetic restorations of teeth are presented. The coefficient of transparency of composites is investigated, the visual assessment of atransparency of sealing materials of different firms is carried out, comparative visual assessment of a transparency of transparent samples of photopolymers of different thickness is executed.Conclusion. It is shown that the layer of transparent material is thicker, the more its contribution to formation of shades of color, layers of different thickness can significantly transform optical properties, having an impact on color and transparency of the made esthetic design.
IMPLEMENTASI KEAMANAN DATA ARSITEKTUR MENGGUNAKAN ALGORITMA KRIPTOGRAFI DENGAN METODE RIVEST CODE (4 RC4)PADA PT.NAVIRI INDAH CEMERLANG
Authors: Rivaldi Ricky , Subandi Subandi 
Published: March 2022

Keamanan dan kerahasiaan data merupakan aspek yang sangat penting dalam dunia informasi saat ini. Terlebih jika data yang disimpan berisi informasi penting dan rahasia, dimana pihak luar tidak diperbolehkan untuk mengetahuinya. Namun di era teknologi informasi dan komunikasi yang semakin maju, semakin marak pula terjadinya pencurian data. Di PT.NAVIRI INDAH CEMERLANG tentu saja terdapat berbagai macam data berupa file yang berisi informasi penting dan rahasia, untuk itu perlu adanya pengamanan agar tidak terjadi pencurian data oleh pihak yang tidak bertanggung jawab . Dengan adanya pencurian data maka aspek keamanan dalam penyimpanan data menjadi sangat penting, karena data yang disimpan dalam keadaan asli (plain) sangat rentan terhadap pencurian data sehingga informasi yang ada didalamnya dapat bocor. Untuk mengatasi masalah diatas maka diperlukan suatu cara untuk mengamankan data. Dengan cara mengimplementasikan suatu metode yang dapat menjaga kerahasiaan informasi, menggunakan Metode kriptografi dengan algoritma Rivest Code 4 (RC4). Algoritma RC4 merupakan bagian dari algoritma simetris yaitu algoritma kriptografi yang mempunyai kunci (key). Disamping dari masalah keamanan file, masalah kecepatan dalam memproses enkripsi dan dekripsi juga harus diperhatikan, dalam membangun aplikasi kriptografi ini, penulis menggunakan Bahasa pemrograman Java. Aplikasi yang dibuat dapat memberikan keamanan terhadap file Di PT.NAVIRI INDAH CEMERLANG sehingga tetap terjaga kerahasiaannya.
Kata kunci : Kriptografi, RC4, Enkrip, Dekrip
Formation conditions and theoretical and methodological aspects of assessment of the economy digital transformation level
Authors: Mickiewicz Bartosz , Volkova Yekaterina 
Published: March 2022

The development of digital technologies in the economy requires the transformation of business processes at the level of organizations focused on a strategic perspective. In the digital economy, obtaining strategic competitive advantages is associated with the formation and development of the potential of organizations. The use of digital technologies leads to the introduction of new methods, tools and services that require infrastructural changes in organizations and contribute to the creation of new products (works, services) that increase the competitiveness and financial stability of organizations. The process of digital transformation of the economy is multi-stage, and each stage has goals, objectives and evaluation criteria. The first step towards the economy digital transformation is to assess the digital potential, digital maturity and readiness of organizations.
The originality lies in the development of theoretical and methodological foundations for assessing the level of the economy digital transformation and in the development of promising areas.
The author's definition of the digital potential of an organization is given as the ability to perform activities to create, introduce, develop and implement information and communication technologies in the context of the transformation of business processes, business models in order to ensure strategic competitive advantages in the markets, financial stability and performance.
The assessment methodology is proposed and the following groups of estimated private indicators have been identified: digital transformation of the organization, intellectual capital, customer interaction: service quality and customer satisfaction, online sales, business environment.
Determined that digital transformation, as the technical and technological core of the digital economy, through the introduction of digital technologies,
transforms the structure of the added value of the product by including the digital and intellectual component in the chain of its creation.
Economic analysis based on indicators in the company
Authors: Ślusarczyk Maciej 
Published: March 2022

The aim of the article is to show suitable and universal methods of economic analysis using the analysis of economic indicators in a combination of research methodology, which focuses on the micro and macro environment of an enterprise embedded in a vibrating, uncertain and constantly changing environment.
The article shows the validity of the centrifugal and centripetal environment analysis method, which results in analytical data in the context of primary measurement and analytical data on the basis of which the analysis of financial ratios can begin.
The author presented the validity of the financial result based on the economic analysis formulas for which specific values were adopted. As a result of combining the research methodology and economic analysis, a measurement and analytical tool was obtained, which forms the basis for strategic action and can be used in in-depth analysis, in which the research and analysis can be subjected to a more detailed examination and the results narrowed down or expanded to include the aspects most relevant to the company.
The result of this analysis is an article that proposes a duality of both methods in terms of analysis and research. Due to the uncertain and oscillating environment, these methods can be assumed to be effective. The validity of the combination of these methods and economic indicators is extremely important and should be analysed in depth, and working with their results will provide a clear analytical picture available at every stage of the company's development.
Potential benefits and risks from Poland’s accession to the euro area
Authors: Dudzik Iwona , Brukwicka Irena 
Published: March 2022

This paper reviews the selected issues related to the potential benefits and risks of Poland’s accession to the euro area. Poland has joined the European Union in 2004. Being a member of the Economic and Monetary Union, Poland was obliged to adopt the euro as its currency, but the date of the above currency introduction was not specified. Poland’s joining the euro area is often discussed in political and economic debates. Such debates benefit primarily from politics and ideology, and the economic issues, associating possible benefits and risks resulting from Poland’s accession to the euro area. The opponents of the common currency deal with issues related to the financial crisis in the territory of the euro zone counties. According to the study conducted in 2010 by the Public Opinion Research Center, it was observed that the number of Poles supporting Poland’s accession to the euro area was decreasing. The survey conducted by CBOS in 2017 showed that the number of respondents who were against Poland’s accession to the euro area was 72%. The purpose of this paper is to analyze the basic benefits and costs that result from the adoption of the common currency by Poland.
The Accretion Process in the DQ Tau Binary System
Authors: Fiorellino E. , Park S. , Kóspál Á. , Ábrahám P. 
Published: March 2022

Abstract
Mass accretion from the circumstellar disk onto the protostar is a fundamental process during star formation. Measuring the mass accretion rate is particularly challenging for stars belonging to binary systems, because it is often difficult to discriminate which component is accreting. DQ Tau is an almost equal-mass spectroscopic binary system where the components orbit each other every 15.8 days. The system is known to display pulsed accretion, i.e., the periodic modulation of the accretion by the components on eccentric orbit. We present multi-epoch ESO/Very Large Telescope X-Shooter observations of DQ Tau, with the aim of determining which component of this system is the main accreting source. We use the absorption lines in the spectra to determine the radial velocity of the two components, and measure the continuum veiling as a function of wavelength and time. We fit the observed spectra with nonaccreting templates to correct for the photospheric and chromospheric contribution. In the corrected spectra, we study in detail the profiles of the emission lines and calculate mass accretion rates for the system as a function of orbital phase. In accordance with previous findings, we detect elevated accretion close to periastron. We measure the accretion rate as varying between 10−8.5 and 10−7.3
M
⊙ yr−1. The emission line profiles suggest that both stars are actively accreting, and the dominant accretor is not always the same component, varying in a few orbits.
Cluster Formation in GGD 12-15: Infall Motion with Rotation of the Natal Clump
Authors: Shimoikura Tomomi , Dobashi Kazuhito , Hirano Naomi , Nakamura Fumitaka , Hirota Tomoya , Matsumoto Tomoaki , Taniguchi Kotomi , Shimajiri Yoshito 
Published: March 2022

Abstract
We report results of observations of the GGD 12-15 region, where cluster formation is actively taking place, using various molecular emission lines. The C18O (J = 1−0) emission line reveals a massive clump in the region with a mass of ∼2800 M
⊙ distributed over ∼2 pc. The distribution of the C18O (J = 3−2) emission is similar to that of a star cluster forming therein, with an elliptical shape of ∼1 pc in size. A bipolar molecular outflow driven by IRS 9Mc, a constituent star of the cluster, is blowing in the direction perpendicular to the elongated C18O (J = 3−2) distribution, covering the entire clump. There is a massive core with a radius of 0.3 pc and a mass of 530 M
⊙ in the center of the clump. There are two velocity components around the core, which are prominent in a position–velocity (PV) diagram along the major axis of the clump. In addition, a PV diagram along the minor axis of the clump, which is parallel to the outflow, shows a velocity gradient opposite to that of the outflow. The velocity structure strongly indicates the infalling motion of the clump. Comparison of the observational data with a simple model of infalling oblate clumps indicates that the clump is undergoing gravitational contraction with rotation.
Dust Dynamics in Transitional Disks: Clumping and Disk Recession
Authors: Bi 毕 Jiaqing 嘉擎 , Fung 馮 Jeffrey 澤之 
Published: March 2022

Abstract
The role of radiation pressure in dust migration and the opening of inner cavities in transitional disks is revisited in this paper. Dust dynamics including radiation pressure is often studied in axisymmetric models, but in this work, we show that highly non-axisymmetric features can arise from an instability at the inner disk edge. Dust grains clump into high density features there, allowing radiation to leak around them and penetrate deeper into the disk, changing the course of dust migration. Our proof-of-concept, two-dimensional, vertically averaged simulations show that the combination of radiation pressure, shadowing, and gas drag can produce a net outward migration, or recession, of the dust component of the disk. The recession speed of the inner disk edge is on the order of 10−5 times Keplerian speed in our parameter space, which is faster than the background viscous flow, assuming a Shakura–Sunyaev viscosity α ≲ 10−3. This speed, if sustained over the lifetime of the disk, can result in a dust cavity as large as tens of astronomical units.
Pearls on a String: Numerous Stellar Clusters Strung Along the Same Orbit
Authors: Coronado Johanna , Fürnkranz Verena , Rix Hans-Walter 
Published: March 2022

Abstract
Stars originate from the dense interstellar medium, which exhibits filamentary structure to scales of ∼1 kpc in galaxies like our Milky Way. We explore quantitatively how much resulting large-scale correlation there is among different stellar clusters and associations in orbit-phase space, characterized here by actions and angles. As a starting point, we identified 55 prominent stellar overdensities in the 6D space of orbit (actions) and orbit-phase (angles) among the ∼2.8 million stars with radial velocities from Gaia EDR3 and with d ≤ 800 pc. We then explored the orbit-phase distribution of all sample stars in the same orbit patch as any one of these 55 overdensities. We find that very commonly numerous other distinct orbit-phase overdensities exist along these same orbits, like pearls on a string. These “pearls” range from known stellar clusters to loose, unrecognized associations. Among orbit patches defined by one initial orbit-phase overdensity, 50% contain at least 8 additional orbit-phase pearls of 10 cataloged members; 20% of them contain 20 additional pearls. This is in contrast to matching orbit patches sampled from a smooth mock catalog, or offset nearby orbit patches, where there are only 2 (or 5, respectively) comparable pearls. Our findings quantify for the first time how common it is for star clusters and associations to form at distinct orbit-phases of nearly the same orbit. This may eventually offer a new way to probe the 6D orbit structure of the filamentary interstellar medium.
Infrared Spectral Energy Distributions and Dust Masses of Sub-solar Metallicity Galaxies at z ∼ 2.3
Authors: Shivaei Irene , Popping Gergö , Rieke George , Reddy Naveen , Pope Alexandra , Kennicutt Robert , Mobasher Bahram , Coil Alison , Fudamoto Yoshinobu , Kriek Mariska , Lyu Jianwei , Oesch Pascal , Sanders Ryan , Shapley Alice , Siana Brian 
Published: March 2022

Abstract
We present results from Atacama Large Millimeter/submillimeter Array (ALMA) 1.2 mm continuum observations of a sample of 27 star-forming galaxies at z = 2.1–2.5 from the MOSFIRE Deep Evolution Field survey with metallicity and star formation rate measurements from optical emission lines. Using stacks of Spitzer, Herschel, and ALMA photometry (rest frame ∼8–400 μm), we examine the infrared (IR) spectral energy distributions (SED) of z ∼ 2.3 subsolar-metallicity (∼0.5 Z
⊙) luminous infrared galaxies (LIRGs). We find that the data agree well with an average template of higher-luminosity local low-metallicity dwarf galaxies (reduced χ
2 = 1.8). When compared with the commonly used templates for solar-metallicity local galaxies or high-redshift LIRGs and ultraluminous IR galaxies, even in the most favorable case (with reduced χ
2 = 2.8), the templates are rejected at >98% confidence. The broader and hotter IR SED of both the local dwarfs and high-redshift subsolar-metallicity galaxies may result from different grain properties or a harder/more intense ionizing radiation field that increases the dust temperature. The obscured star formation rate (SFR) indicated by the far-IR emission of the subsolar-metallicity galaxies is only ∼60% of the total SFR, considerably lower than that of the local LIRGs with ∼96%–97% obscured fractions. Due to the evolving IR SED shape, the local LIRG templates fit to mid-IR data overestimate the Rayleigh–Jeans tail measurements by a factor of 2–20. These templates underestimate IR luminosities if fit to the observed ALMA fluxes by >0.4 dex. At a given stellar mass or metallicity, dust masses at z ∼ 2.3 are an order of magnitude higher than z ∼ 0. Given the predicted molecular gas fractions, the observed z ∼ 2.3 dust-to-stellar mass ratios suggest lower dust-to-molecular gas masses than in local galaxies with similar metallicities.
Stellar Abundance Maps of the Milky Way Disk
Authors: Eilers Anna-Christina , Hogg David W. , Rix Hans-Walter , Ness Melissa K. , Price-Whelan Adrian M. , Mészáros Szabolcs , Nitschelm Christian 
Published: March 2022

Abstract
To understand the formation of the Milky Way’s prominent bar it is important to know whether stars in the bar differ in the chemical element composition of their birth material as compared to disk stars. This requires stellar abundance measurements for large samples across the Milky Way’s body. Such samples, e.g., luminous red giant stars observed by the Sloan Digital Sky Survey’s APOGEE survey, will inevitably span a range of stellar parameters; as a consequence, both modeling imperfections and stellar evolution may preclude consistent and precise estimates of their chemical composition at a level of purported bar signatures, which has left current analyses of a chemically distinct bar inconclusive. Here, we develop a new self-calibration approach to eliminate both modeling and astrophysical abundance systematics among red giant branch (RGB) stars of different luminosities (and hence surface gravity

log
g

). We apply our method to 48,853 luminous APOGEE Data Release 16 RGB stars to construct spatial abundance maps of 20 chemical elements near the Milky Way’s mid-plane, covering galactocentric radii of 0 kpc < R
GC < 20 kpc. Our results indicate that there are no abundance variations whose geometry matches that of the bar, and that the mean abundance gradients vary smoothly and monotonically with galactocentric radius. We confirm that the high-α disk is chemically homogeneous, without spatial gradients. Furthermore, we present the most precise [Fe/H] versus R
GC gradient to date with a slope of − 0.057 ±0.001 dex kpc−1 out to approximately 15 kpc.
In Situ Measurement of the Energy Fraction in Suprathermal and Energetic Particles at ACE, Wind, and PSP Interplanetary Shocks
Authors: David Liam , Fraschetti Federico , Giacalone Joe , Wimmer-Schweingruber Robert F. , Berger Lars , Lario David 
Published: March 2022

Abstract
The acceleration of charged particles by interplanetary shocks (IPs) can drain a nonnegligible fraction of the plasma pressure. In this study, we have selected 17 IPs observed in situ at 1 au by the Advanced Composition Explorer and the Wind spacecraft, and 1 shock at 0.8 au observed by Parker Solar Probe. We have calculated the time-dependent partial pressure of suprathermal and energetic particles (smaller and greater than 50 keV for protons and 30 keV for electrons, respectively) in both the upstream and downstream regions. The particle fluxes were averaged for 1 hr before and 1 hr after the shock time to remove short timescale effects. Using the MHD Rankine–Hugoniot jump conditions, we find that the fraction of the total upstream energy flux transferred to suprathermal and energetic downstream particles is typically ≲16%, in agreement with previous observations and simulations. Notably, by accounting for errors on all measured shock parameters, we have found that for any given fast magnetosonic Mach number, M

f
< 7, the angle between the shock normal and average upstream magnetic field, θ
Bn, is not correlated with the energetic particle pressure; in particular, the partial pressure of energized particles does not decrease for θ
Bn ≳ 45°. The downstream electron-to-proton energy ratio in the range ≳ 140 eV for electrons and ≳ 70 keV for protons exceeds the expected ∼1% and nears equipartition (>0.1) for the Wind events.
Full-sky, Arcminute-scale, 3D Models of Galactic Microwave Foreground Dust Emission Based on Filaments
Authors: Hervías-Caimapo Carlos , Huffenberger Kevin M. 
Published: March 2022

Abstract
We present the DustFilaments code, a full-sky model for the millimeter Galactic emission of thermal dust. Our model, composed of millions of filaments that are imperfectly aligned with the magnetic field, is able to reproduce the main features of the dust angular power spectra at 353 GHz as measured by the Planck mission. Our model is made up of a population of filaments with sizes following a Pareto distribution

∝

L

a

−
2.445

, with an axis ratio between short and long semiaxes ϵ ∼ 0.16 and an angle of magnetic field misalignment with a dispersion rms(θ
LH) = 10°. On large scales, our model follows a Planck-based template. On small scales, our model produces spectra that behave like power laws up to ℓ ∼ 4000 or smaller scales by considering even smaller filaments, limited only by computing power. We can produce any number of Monte Carlo realizations of small-scale Galactic dust. Our model will allow tests of how the small-scale non-Gaussianity affects CMB weak lensing and the consequences for the measurement of primordial gravitational waves or relativistic light relic species. Our model also can generate frequency decorrelation on the modified blackbody spectrum of dust and is freely adjustable to different levels of decorrelation. This can be used to test the performance of component separation methods and the impact of frequency spectrum residuals on primordial B-mode surveys. The filament density we paint in the sky is also able to reproduce the general level of non-Gaussianities measured by Minkowski functionals in the Planck 353 GHz channel map.