bluuebunny/crossref_metadata_2025_split huggingface dataset:
Development and Evolution of Aluminum Industry in China Based on Aluminum Flow Analysis
Authors: Yue Qiang , Fan Zaidong , Zhang Chao , Liu Fen , Wang Heming , Jia Fengrui 
Published: November 2016

AbstractThe whole process of aluminum cycle consists of four stages: Production of alumina and primary aluminum, fabrication and manufacture of aluminum products, use of aluminum final products, and recycling of obsolete aluminum products. Aluminum cycle in China in 2011 was analyzed using alumium flow diagram, and the following indices were obtained: The resource self-support ratio of alumina, aluminum and the whole aluminum industry were 53.18%, 95.58% and 54.85%, respectively; self-produced and net imported aluminum scrap use ratios of the aluminum industry were 4.68% and 7.98%, respectively. Aluminum cycles and aluminum flow indices in China of the year 1990, 1995, 2000, 2005 and 2008–2010 were also analyzed. It was found that from 1990 to 2011, imported Al-containing resources increased and imported bauxite has increased significantly since 2005. Resources self-support ratio of aluminum industry changed gradually from fully self-support to depencdent on the imports of raw materials. Self-produced auminum scrap use ratio presented downtrend basically and the imported aluminum scrap use ratio was greater than self-produced aluminum scrap use ratio after 1995.
The Coordination and Optimization of Closed-Loop Supply Chain with Lots of Factors
Authors: Shi Chengdong , Zhou Guanglu , Bian Dunxin , Wu Meixiang 
Published: November 2016

AbstractConsider a closed-loop supply chain including a manufacturer, a retailer and two third party recyclers as the background. A coordination and optimization model is built by using the downside-risk function, Cournot model and government subsidy excitation function. The effect of risk characteristics, government subsidy and Cournot competition on supply chain is analyzed, and the impact of revenue-and-expense sharing contract is studied in the channel, which shows that the contract cannot coordinate and optimize the closed-loop supply chain. Also, risk sharing contract and expense sharing contract are designed, which can offer the desired downside protection to the retailer, provide more profits to the agents, and accomplish channel coordination and optimization. Moreover, an application example is given for testing the effectiveness and feasibility of the contract, and the bound and rule of the contract parameters are given. Finally, by the analysis of numerical simulation and sensitivity of the model based on the contract, the validity and practicability of the model are verified, and the relationship between government subsidy, risk characteristics, competitive characteristics with the supply chain is obtained. This study provides decision support and decision-making reference for the development of remanufacturing industry.
Multi-Period Mean-Absolute Deviation Fuzzy Portfolio Selection Model with Entropy Constraints
Authors: Zhang Peng , Gong Heshan , Lan Weiting 
Published: November 2016

AbstractThis paper considers a multi-period fuzzy portfolio selection problem maximizing the terminal wealth imposed by risk control, in which the returns of assets are characterized by fuzzy numbers. A fuzzy absolute deviation is originally defined as the risk control of portfolio. Entropy constraints and borrowing constraints are added in the portfolio selection model. Based on the theories of possibility measures, a new multi-period portfolio optimization model with transaction costs is proposed. And then, the proposed model is transformed into a crisp nonlinear programming problem by using fuzzy programming approach. Because of the transaction costs, the multi-period portfolio selection is the dynamic optimization problem with path dependence. Through changing the cost function into a variable, the multi-period portfolio selection is approximately turned into the dynamic programming. Furthermore, the discrete approximate iteration method is designed to obtain the optimal portfolio strategy. Finally, an example is given to illustrate the behavior of the proposed model and the designed algorithm using real data from the Shanghai Stock Exchange.
AEWMA t Control Chart for Short Production Runs
Authors: Chang Zhiyuan , Sun Jinsheng 
Published: November 2016

AbstractOwing to the limited number of inspections during a short run process, it is impossible to get the correct estimate of the population mean and standard deviation during Phase I implementation of control chart. Thetcontrol chart proposed recently can overcome this problem. The EWMAtcontrol chart has been proposed to monitor the process mean, but a single EWMAtcontrol chart cannot perform well for small and large shifts simultaneously, which is known as the “inertia problem”. The adaptive varying smoothing parameter EWMA (AEWMA) control chart can overcome the inertia problem. In this paper, the AEWMAtcontrol chart for short run process is proposed. The truncated average run length and the probability of trigger a signal are adopted to test the performance of short run AEWMAtchart. Based on the investigation of the joint effect of control chart parameters on the performance of AEWMAtchart, a new optimization algorithm is proposed for statistical design of the AEWMA control chart. Simulations are performed for perfect and imperfect setup conditions, the results show that the AEWMAtcontrol chart performs better than the EWMAtcontrol chart.
Use of the Cook Staged Extubation Set via tracheostomy stoma in ICU
Authors: Gibson Alistair , Dunn Mark 
Published: November 2016

SummaryWe present a case demonstrating a previously undescribed use for the Cook Staged Extubation Set (Cook SESTM) via a tracheostomy stoma following decannulation of tracheostomy in a 64‐year‐old male 'at risk' patient. Our experience demonstrates that the Cook SES may be used via a tracheostomy stoma in addition to its described use via the oral route.
El exemplum como estrategia persuasiva en la Rhetorica christiana (1579) de fray Diego Valadés
Authors: Carrasco M. Rolando 
Published: November 2016

En este ensayo, el autor plantea la necesidad de profundizar en la complejidad discursiva de la Rhetorica christiana desde una relectura de sus estrategias argumentativas. Estrategias que se encuentran lo mismo en los planteamientos que en los ejemplos ofrecidos por el fraile franciscano, tanto en la preceptiva oratoria puesta de relieve como en los grabados realizados expresamente para la obra. Rolando Carrasco analiza la importancia que tienen los exempla en su función retórica, puesto que su carácter vivencial les otorga un valor argumentativo de carácter probatorio, como en la mejor tradición jurídica heredada del mundo clásico grecolatino.Por tanto, el lector podrá corroborar que la obra de fray Diego Valadés no sólo tiene una enorme significación literaria, sino también un enorme valor como alegato de orden teológico y jurídico que fue necesario esgrimir en un momento preciso de la historia, cuando se estaba gestando la incorporación de los nativos americanos al mundo occidental.
Enhancement of cognitive performance in mice and in vitro acetyl-cholinesterase inhibitory activity of 3,3’,4’,5,7-pentahydroxyflavone isolated from <i>Cadaba indica</i>
Authors: Dhivya Sundaram , Latha Subbiah , Selvamani Palanisamy 
Published: November 2016

<p class="Abstract"><em>Cadaba indica</em>, a component of traditional siddha medicine, is used for the therapy of gonorrhea, inflammation, eczema etc. The present study shows that it exhibited acetylcholinesterase inhibitory activity (up to 81.5 ± 1.5%) at the concentration of 3 mg/mL, with the IC<sub>50 </sub>value of 1.8 mg/mL. Furthermore, the ethanol extract of<em> C. indica</em> therapy at a dose of 100 mg/kg p.o significantly ameliorated the cognitive impaired mice in Y-maze task. The active ingredient was identified as 3,3’,4’,5,7-pentahydroxyflavone. The above results suggest that <em>C. indica</em> would be a potential natural therapeutic remedy for cognitive disorders mediated by cholinergic dysfunction.</p><p class="Abstract"><strong>Video Clip:</strong></p><p class="Abstract"><a href="https://youtube.com/v/QIEuwPT-lmw">Memory impairment test in mice</a>: 1 min</p><p> </p>
A 1.9 EARTH RADIUS ROCKY PLANET AND THE DISCOVERY OF A NON-TRANSITING PLANET IN THE KEPLER-20 SYSTEM*
Authors: Buchhave Lars A. , Dressing Courtney D. , Dumusque Xavier , Rice Ken , Vanderburg Andrew , Mortier Annelies , Lopez-Morales Mercedes , Lopez Eric , Lundkvist Mia S. , Kjeldsen Hans , Affer Laura , Bonomo Aldo S. , Charbonneau David , Cameron Andrew Collier , Cosentino Rosario , Figueira Pedro , Fiorenzano Aldo F. M. , Harutyunyan Avet , Haywood Raphaëlle D. , Johnson John Asher , Latham David W. , Lovis Christophe , Malavolta Luca , Mayor Michel , Micela Giusi , Molinari Emilio , Motalebi Fatemeh , Nascimbeni Valerio , Pepe Francesco , Phillips David F. , Piotto Giampaolo , Pollacco Don , Queloz Didier , Sasselov Dimitar , Ségransan Damien , Sozzetti Alessandro , Udry Stéphane , Watson Chris 
Published: November 2016

ABSTRACT
Kepler-20 is a solar-type star (V = 12.5) hosting a compact system of five transiting planets, all packed within the orbital distance of Mercury in our own solar system. A transition from rocky to gaseous planets with a planetary transition radius of ∼1.6

has recently been proposed by several articles in the literature. Kepler-20b (

∼ 1.9

) has a size beyond this transition radius; however, previous mass measurements were not sufficiently precise to allow definite conclusions to be drawn regarding its composition. We present new mass measurements of three of the planets in the Kepler-20 system that are facilitated by 104 radial velocity measurements from the HARPS-N spectrograph and 30 archival Keck/HIRES observations, as well as an updated photometric analysis of the Kepler data and an asteroseismic analysis of the host star (

=

and

=

). Kepler-20b is a

planet in a 3.7 day period with a mass of

, resulting in a mean density of

, indicating a rocky composition with an iron-to-silicate ratio consistent with that of the Earth. This makes Kepler-20b the most massive planet with a rocky composition found to date. Furthermore, we report the discovery of an additional non-transiting planet with a minimum mass of

and an orbital period of ∼34 days in the gap between Kepler-20f (P ∼ 11 days) and Kepler-20d (P ∼ 78 days).
A NEW MILKY WAY SATELLITE DISCOVERED IN THE SUBARU/HYPER SUPRIME-CAM SURVEY
Authors: Homma Daisuke , Chiba Masashi , Okamoto Sakurako , Komiyama Yutaka , Tanaka Masayuki , Tanaka Mikito , Ishigaki Miho N. , Akiyama Masayuki , Arimoto Nobuo , Garmilla José A. , Lupton Robert H. , Strauss Michael A. , Furusawa Hisanori , Miyazaki Satoshi , Murayama Hitoshi , Nishizawa Atsushi J. , Takada Masahiro , Usuda Tomonori , Wang Shiang-Yu 
Published: November 2016

ABSTRACT
We report the discovery of a new ultra-faint dwarf satellite companion of the Milky Way (MW) based on the early survey data from the Hyper Suprime-Cam Subaru Strategic Program. This new satellite, Virgo I, which is located in the constellation of Virgo, has been identified as a statistically significant (5.5σ) spatial overdensity of star-like objects with a well-defined main sequence and red giant branch in the color–magnitude diagram. The significance of this overdensity increases to 10.8σ when the relevant isochrone filter is adopted for the search. Based on the distribution of the stars around the likely main-sequence turnoff at r ∼ 24 mag, the distance to Virgo I is estimated as 87 kpc, and its most likely absolute magnitude calculated from a Monte Carlo analysis is M

V
= −0.8 ± 0.9 mag. This stellar system has an extended spatial distribution with a half-light radius of

pc, which clearly distinguishes it from a globular cluster with comparable luminosity. Thus, Virgo I is one of the faintest dwarf satellites known and is located beyond the reach of the Sloan Digital Sky Survey. This demonstrates the power of this survey program to identify very faint dwarf satellites. This discovery of Virgo I is based only on about 100 square degrees of data, thus a large number of faint dwarf satellites are likely to exist in the outer halo of the MW.
THE FORMATION OF AN INVERSE S-SHAPED ACTIVE-REGION FILAMENT DRIVEN BY SUNSPOT MOTION AND MAGNETIC RECONNECTION
Authors: Yan X. L. , Priest E. R. , Guo Q. L. , Xue Z. K. , Wang J. C. , Yang L. H. 
Published: November 2016

ABSTRACT
We present a detailed study of the formation of an inverse S-shaped filament prior to its eruption in active region NOAA 11884 from 2013 October 31 to November 2. In the initial stage, clockwise rotation of a small positive sunspot around the main negative trailing sunspot formed a curved filament. Then the small sunspot cancelled with the negative magnetic flux to create a longer active-region filament with an inverse S-shape. At the cancellation site a brightening was observed in UV and EUV images and bright material was transferred to the filament. Later the filament erupted after cancellation of two opposite polarities below the upper part of the filament. Nonlinear force-free field extrapolation of vector photospheric fields suggests that the filament may have a twisted structure, but this cannot be confirmed from the current observations.
PHOTO-STABILITY OF SUPER-HYDROGENATED PAHs DETERMINED BY ACTION SPECTROSCOPY EXPERIMENTS
Authors: Wolf M. , Kiefer H. V. , Langeland J. , Andersen L. H. , Zettergren H. , Schmidt H. T. , Cederquist H. , Stockett M. H. 
Published: November 2016

ABSTRACT
We have investigated the photo-stability of pristine and super-hydrogenated pyrene cations (

) by means of gas-phase action spectroscopy. Optical absorption spectra and photo-induced dissociation mass spectra are presented. By measuring the yield of mass-selected photo-fragment ions as a function of laser pulse intensity, the number of photons (and hence the energy) needed for fragmentation of the carbon backbone was determined. Backbone fragmentation of pristine pyrene ions (

) requires absorption of three photons of energy just below 3 eV, whereas super-hydrogenated hexahydropyrene (C16H

) must absorb two such photons and fully hydrogenated hexadecahydropyrene (C16H

) only a single photon. These results are consistent with previously reported dissociation energies for these ions. Our experiments clearly demonstrate that the increased heat capacity from the additional hydrogen atoms does not compensate for the weakening of the carbon backbone when pyrene is hydrogenated. In photodissociation regions, super-hydrogenated Polycyclic Aromatic Hydrocarbons (PAHs) have been proposed to serve as catalysts for H2 formation. Our results indicate that carbon backbone fragmentation may be a serious competitor to H2 formation at least for small hydrogenated PAHs like pyrene.
THE QUENCHING TIMESCALE AND QUENCHING RATE OF GALAXIES
Authors: Lian Jianhui , Yan Renbin , Zhang Kai , Kong Xu 
Published: November 2016

ABSTRACT
The average star formation rate (SFR) in galaxies has been declining since the redshift of 2. A fraction of galaxies quench and become quiescent. We constrain two key properties of the quenching process: the quenching timescale and the quenching rate among galaxies. We achieve this by analyzing the galaxy number density profile in NUV−u color space and the distribution in NUV−u versus u − i color–color diagram with a simple toy-model framework. We focus on galaxies in three mass bins between 1010 and 1010.6
M
⊙. In the NUV−u versus u − i color–color diagram, the red u − i galaxies exhibit a different slope from the slope traced by the star-forming galaxies. This angled distribution and the number density profile of galaxies in NUV−u space strongly suggest that the decline of the SFR in galaxies has to accelerate before they turn quiescent. We model this color–color distribution with a two-phase exponential decline star formation history. The models with an e-folding time in the second phase (the quenching phase) of 0.5 Gyr best fit the data. We further use the NUV−u number density profile to constrain the quenching rate among star-forming galaxies as a function of mass. Adopting an e-folding time of 0.5 Gyr in the second phase (or the quenching phase), we found the quenching rate to be 19%/Gyr, 25%/Gyr and 33%/Gyr for the three mass bins. These are upper limits of the quenching rate as the transition zone could also be populated by rejuvenated red-sequence galaxies.
RAMAN SCATTERING BY MOLECULAR HYDROGEN AND NITROGEN IN EXOPLANETARY ATMOSPHERES
Authors: Oklopčić Antonija , Hirata Christopher M. , Heng Kevin 
Published: November 2016

ABSTRACT
An important source of opacity in exoplanet atmospheres at short visible and near-UV wavelengths is Rayleigh scattering of light on molecules. It is accompanied by a related, albeit weaker process—Raman scattering. We analyze the signatures of Raman scattering imprinted in the reflected light and the geometric albedo of exoplanets, which could provide information about atmospheric properties. Raman scattering affects the geometric albedo spectra of planets in the following ways. First, it causes filling-in of strong absorption lines in the incident radiation, thus producing sharp peaks in the albedo. Second, it shifts the wavelengths of spectral features in the reflected light causing the so-called Raman ghost lines. Raman scattering can also cause a broadband reduction of the albedo due to wavelength shifting of a stellar spectrum with red spectral index. Observing the Raman peaks in the albedo could be used to measure the column density of gas, thus providing constraints on the presence of clouds in the atmosphere. Observing the Raman ghost lines could be used to spectroscopically identify the main scatterer in the atmosphere, even molecules like H2 or N2, which do not have prominent spectral signatures in the optical wavelength range. If detected, ghost lines could also provide information about the temperature of the atmosphere. In this paper, we investigate the effects of Raman scattering in hydrogen- and nitrogen-dominated atmospheres. We analyze the feasibility of detecting the signatures of Raman scattering with the existing and future observational facilities, and of using these signatures as probes of exoplanetary atmospheres.
RECOMMENDED THERMAL RATE COEFFICIENTS FOR THE C + H3
+ REACTION AND SOME ASTROCHEMICAL IMPLICATIONS
Authors: Vissapragada S. , Buzard C. F. , Miller K. A. , O’Connor A. P. , Ruette N. de , Urbain X. , Savin D. W. 
Published: November 2016

ABSTRACT
We incorporate our experimentally derived thermal rate coefficients for C +

forming CH+ and CH2
+ into a commonly used astrochemical model. We find that the Arrhenius–Kooij equation typically used in chemical models does not accurately fit our data and instead we use a more versatile fitting formula. At a temperature of 10 K and a density of 104 cm−3, we find no significant differences in the predicted chemical abundances, but at higher temperatures of 50, 100, and 300 K we find up to factor of 2 changes. In addition, we find that the relatively small error on our thermal rate coefficients, ∼15%, significantly reduces the uncertainties on the predicted abundances compared to those obtained using the currently implemented Langevin rate coefficient with its estimated factor of 2 uncertainty.
THE KEPLER DICHOTOMY IN PLANETARY DISKS: LINKING KEPLER OBSERVABLES TO SIMULATIONS OF LATE-STAGE PLANET FORMATION
Authors: Moriarty John , Ballard Sarah 
Published: November 2016

ABSTRACT
NASA’s Kepler Mission uncovered a wealth of planetary systems, many with planets on short-period orbits. These short-period systems reside around 50% of Sun-like stars and are similarly prevalent around M dwarfs. Their formation and subsequent evolution is the subject of active debate. In this paper, we simulate late-stage, in situ planet formation across a grid of planetesimal disks with varying surface density profiles and total mass. We compare simulation results with observable characteristics of the Kepler sample. We identify mixture models with different primordial planetesimal disk properties that self-consistently recover the multiplicity, radius, period and period ratio, and duration ratio distributions of the Kepler planets. We draw three main conclusions. (1) We favor a “frozen-in” narrative for systems of short-period planets, in which they are stable over long timescales, as opposed to metastable. (2) The “Kepler dichotomy,” an observed phenomenon of the Kepler sample wherein the architectures of planetary systems appear to either vary significantly or have multiple modes, can naturally be explained by formation within planetesimal disks with varying surface density profiles. Finally, (3) we quantify the nature of the “Kepler dichotomy” for both GK stars and M dwarfs, and find that it varies with stellar type. While the mode of planet formation that accounts for high multiplicity systems occurs in 24% ± 7% of planetary systems orbiting GK stars, it occurs in 63% ± 16% of planetary systems orbiting M dwarfs.
INTERFEROMETRIC MONITORING OF GAMMA-RAY BRIGHT AGNs. I. THE RESULTS OF SINGLE-EPOCH MULTIFREQUENCY OBSERVATIONS
Authors: Lee Sang-Sung , Wajima Kiyoaki , Algaba Juan-Carlos , Zhao Guang-Yao , Hodgson Jeffrey A. , Kim Dae-Won , Park Jongho , Kim Jae-Young , Miyazaki Atsushi , Byun Do-Young , Kang Sincheol , Kim Jeong-Sook , Kim Soon-Wook , Kino Motoki , Trippe Sascha 
Published: November 2016

ABSTRACT
We present results of single-epoch very long baseline interferometry (VLBI) observations of gamma-ray bright active galactic nuclei (AGNs) using the Korean VLBI Network (KVN) at the 22, 43, 86, and 129 GHz bands, which are part of a KVN key science program, Interferometric Monitoring of Gamma-Ray Bright AGNs. We selected a total of 34 radio-loud AGNs of which 30 sources are gamma-ray bright AGNs with flux densities of >6 × 10−10 ph cm−2 s−1. Single-epoch multifrequency VLBI observations of the target sources were conducted during a 24 hr session on 2013 November 19 and 20. All observed sources were detected and imaged at all frequency bands, with or without a frequency phase transfer technique, which enabled the imaging of 12 faint sources at 129 GHz, except for one source. Many of the target sources are resolved on milliarcsecond scales, yielding a core-jet structure, with the VLBI core dominating the synchrotron emission on a milliarcsecond scale. CLEAN flux densities of the target sources are 0.43–28 Jy, 0.32–21 Jy, 0.18–11 Jy, and 0.35–8.0 Jy in the 22, 43, 86, and 129 GHz bands, respectively. Spectra of the target sources become steeper at higher frequency, with spectral index means of −0.40, −0.62, and −1.00 in the 22–43 GHz, 43–86 GHz and 86–129 GHz bands, respectively, implying that the target sources become optically thin at higher frequencies (e.g., 86–129 GHz).