bluuebunny/crossref_metadata_2025_split huggingface dataset:
Effect of withdrawal rate and zinc content on pore structure and morphology of lotus-type porous Cu–Zn alloys fabricated using continuous casting
Authors: Li Zaijiu , Tian Juanjuan , Zhu Shaowu , Chen Jialin , Xie Ming 
Published: June 2016

AbstractA continuous casting technique was developed to fabricate lotus-type porous alloys. This type of porous Cu–Zn (2, 6, and 10 wt.%) alloy was successfully fabricated by using the continuous casting technique under a hydrogen gas pressure of 0.6 MPa at various withdrawal rates. The influences of processing parameters on the pore structure and morphology were investigated. For the porous Cu-2Zn alloys, an increased withdrawal rate will result in slightly increased porosity, but a decreased average pore diameter. The pore morphology becomes more and more inhomogeneous with increasing Zn content, and the porosity tends to firstly decrease and subsequently increase. Such tendencies are correlated with the Zn content and corresponding width of the mushy zone.
Expert Knowledge for Modeling Functional Health from Sensor Data
Authors: Pol Margriet , Buurman Bianca , Kröse Ben , Robben Saskia 
Published: June 2016

Summary
Background: ICT based solutions are increasingly introduced for active and healthy ageing. In this context continuous monitoring of older adults with domestic sensor systems has been suggested to provide important information about their functional health. However, there is not yet a solid model for the interpretation of the sensor data.
Objectives: The aim of our study is to define a set of predictors of functional health that can be measured with domestic sensors and to determine thresholds that identify relevant changes in these predictors.
Methods: On the basis of literature we develop a model that relates functional health predictors to features derived from sensor data. The parameters of this model are determined on the basis of a study among health experts (n = 38). The use of the full model is illustrated with three cases.
Results: We identified 25 predictors and their attributes. For 12 of them that can be measured with passive infrared motion sensors we determined their parameters: the attribute thresholds and the urgency thresholds.
Conclusions: With the parametrized predictors in the model, domestic sensors can be deployed to assess functional health in a standardized way. Three case examples showed how the model can be used as a screening instrument for functional decline.
The Importance of Context: Risk-based De-identification of Biomedical Data
Authors: Kuhn Klaus , Prasser Fabian , Kohlmayer Florian 
Published: June 2016

Summary
Background: Data sharing is a central aspect of modern biomedical research. It is accompanied by significant privacy concerns and often data needs to be protected from re-identification. With methods of de-identification datasets can be transformed in such a way that it becomes extremely difficult to link their records to identified individuals. The most important challenge in this process is to find an adequate balance between an increase in privacy and a decrease in data quality.
Objectives: Accurately measuring the risk of re-identification in a specific data sharing scenario is an important aspect of data de-identification. Overestimation of risks will significantly deteriorate data quality, while underestimation will leave data prone to attacks on privacy. Several models have been proposed for measuring risks, but there is a lack of generic methods for risk-based data de-identification. The aim of the work described in this article was to bridge this gap and to show how the quality of de-identified datasets can be improved by using risk models to tailor the process of de-identification to a concrete context.
Methods: We implemented a generic de-identification process and several models for measuring re-identification risks into the ARX de-identification tool for biomedical data. By integrating the methods into an existing framework, we were able to automatically transform datasets in such a way that information loss is minimized while it is ensured that re-identification risks meet a user-defined threshold. We performed an extensive experimental evaluation to analyze the impact of using different risk models and assumptions about the goals and the background knowledge of an attacker on the quality of de-identified data.
Results: The results of our experiments show that data quality can be improved significantly by using risk models for data de-identification. On a scale where 100 % represents the original input dataset and 0 % represents a dataset from which all information has been removed, the loss of information content could be reduced by up to 10 % when protecting datasets against strong adversaries and by up to 24 % when protecting datasets against weaker adversaries.
Conclusions: The methods studied in this article are well suited for protecting sensitive biomedical data and our implementation is available as open-source software. Our results can be used by data custodians to increase the information content of de-identified data by tailoring the process to a specific data sharing scenario. Improving data quality is important for fostering the adoption of de-identification methods in biomedical research.
ORBITS OF SUBSYSTEMS IN FOUR HIERARCHICAL MULTIPLE STARS
Authors: Tokovinin Andrei 
Published: June 2016

ABSTRACT
Seven spectroscopic orbits in nearby solar-type multiple stars are presented. The primary of the chromospherically active star HIP 9642 is a 4.8 day double-lined pair; the outer 420 year visual orbit is updated, but remains poorly constrained. HIP 12780 is a quadruple system consisting of the resolved 6.7 year pair FIN 379 Aa,Ab, for which the combined orbit, masses, and orbital parallax are determined here, and the single-lined binary Ba,Bb with a period of 27.8 days. HIP 28790 is a young quintuple system composed of two close binaries, Aa,Ab and Ba,Bb, with periods of 221 and 13 days, respectively, and a single distant component C. Its subsystem Ba,Bb is peculiar, having a spectroscopic mass ratio of 0.89 but a magnitude difference of ∼2.2 mag. HIP 64478 also contains five stars: the A-component is a 29 year visual pair with a previously known 4 day twin subsystem, while the B-component is a contact binary with a period of 5.8 hr, seen nearly pole-on.
ORBITS OF FOUR YOUNG TRIPLE-LINED MULTIPLE SYSTEMS
Authors: Tokovinin Andrei 
Published: June 2016

ABSTRACT
Each of the nearby triple systems HIP 7601, 13498, 23824, and 113597 (HD 10800, 18198, 35877, 217379) consist of solar-type dwarfs with comparable masses, where all three components are resolved spectrally, while the outer pairs are resolved both visually and spectrally. These stars are relatively young (between 100 and 600 Myr) and chromospherically active (X-ray sources), although they rotate slowly. I determine the spectroscopic orbits of the inner subsystems (periods 19.4, 14.1, 5.6, 20.3 days) and the orbits of the outer systems (periods 1.75, 51, 27, 500 years, respectively). For HIP 7601 and 13498, the combined spectro-interferometric outer orbits produce direct measurement of the masses of all of the components, allowing for a comparison with stellar models. The 6708 Å lithium line is present and its strength is measured in each component individually by subtracting the contributions of the other components. The inner and outer orbits of HIP 7601 are nearly circular, likely co-planar, and have a modest period ratio of 1:33. This study contributes to the characterization of hierarchical multiplicity in the solar neighborhood and provides data for testing stellar evolutionary models and chronology.
THE IMPACT OF STELLAR MULTIPLICITY ON PLANETARY SYSTEMS. I. THE RUINOUS INFLUENCE OF CLOSE BINARY COMPANIONS
Authors: Kraus Adam L. , Ireland Michael J. , Huber Daniel , Mann Andrew W. , Dupuy Trent J. 
Published: June 2016

ABSTRACT
The dynamical influence of binary companions is expected to profoundly influence planetary systems. However, the difficulty of identifying planets in binary systems has left the magnitude of this effect uncertain; despite numerous theoretical hurdles to their formation and survival, at least some binary systems clearly host planets. We present high-resolution imaging of 382 Kepler Objects of Interest (KOIs) obtained using adaptive-optics imaging and nonredundant aperture-mask interferometry on the Keck II telescope. Among the full sample of 506 candidate binary companions to KOIs, we super-resolve some binary systems to projected separations of <5 au, showing that planets might form in these dynamically active environments. However, the full distribution of projected separations for our planet-host sample more broadly reveals a deep paucity of binary companions at solar-system scales. For a field binary population, we should have found 58 binary companions with projected separation ρ < 50 au and mass ratio q > 0.4; we instead only found 23 companions (a 4.6σ deficit), many of which must be wider pairs that are only close in projection. When the binary population is parametrized with a semimajor axis cutoff a
cut and a suppression factor inside that cutoff S
bin, we find with correlated uncertainties that inside

au, the planet occurrence rate in binary systems is only

times that of wider binaries or single stars. Our results demonstrate that a fifth of all solar-type stars in the Milky Way are disallowed from hosting planetary systems due to the influence of a binary companion.
MULTIPLEXING PRECISION RVs: SEARCHING FOR CLOSE-IN GAS GIANTS IN OPEN CLUSTERS
Authors: Bailey III John I. , Mateo Mario , White Russel J. , Shectman Stephen A. , Crane Jeffrey D. , Olszewski Edward W. 
Published: June 2016

ABSTRACT
We present a multiplexed high-resolution (R ∼ 50,000 median) spectroscopic survey designed to detect exoplanet candidates in two southern star clusters (NGC 2516 and NGC 2422) using the Michigan/Magellan Fiber System (M2FS) on the Magellan/Clay telescope at Las Campanas Observatory. With 128 available fibers in our observing mode, we are able to target every star in the core half-degree of each cluster that could plausibly be a solar-analog member. Our template-based spectral fits provide precise measurements of fundamental stellar properties—T
eff (±30 K), [Fe/H] and [α/Fe] (±0.02 dex), and

(±0.3 km s−1)—and radial velocities (RVs) by using telluric absorption features from 7160 to 7290 Å as a wavelength reference for 251 mid-F to mid-K stars (126 in NGC 2516 and 125 in NGC 2422) that comprise our survey. In each cluster, we have obtained ∼10–12 epochs of our targets. Using repeat observations of an RV standard star, we show our approach can attain a single-epoch velocity precision of 25–60 m s−1 over a broad range of signal-to-noise ratios throughout our observational baseline of 1.1 years. Our technique is suitable for nonrapidly rotating stars cooler than mid-F. In this paper, we describe our observational sample and analysis methodology and present a detailed study of the attainable precision and measurement capabilities of our approach. Subsequent papers will provide results for stars observed in the target clusters, analyze our data set of RV time series for stellar jitter and stellar and substellar companions, and consider the implications of our findings on the clusters themselves.
THE MUSCLES TREASURY SURVEY. III. X-RAY TO INFRARED SPECTRA OF 11 M AND K STARS HOSTING PLANETS
Authors: P. Loyd R. O. , France Kevin , Youngblood Allison , Schneider Christian , Brown Alexander , Hu Renyu , Linsky Jeffrey , Froning Cynthia S. , Redfield Seth , Rugheimer Sarah , Tian Feng 
Published: June 2016

ABSTRACT
We present a catalog of panchromatic spectral energy distributions (SEDs) for 7 M and 4 K dwarf stars that span X-ray to infrared wavelengths (5 Å –5.5 μm). These SEDs are composites of Chandra or XMM-Newton data from 5–∼50 Å, a plasma emission model from ∼50–100 Å, broadband empirical estimates from 100–1170 Å, Hubble Space Telescope data from 1170–5700 Å, including a reconstruction of stellar Lyα emission at 1215.67 Å, and a PHOENIX model spectrum from 5700–55000 Å. Using these SEDs, we computed the photodissociation rates of several molecules prevalent in planetary atmospheres when exposed to each star’s unattenuated flux (“unshielded” photodissociation rates) and found that rates differ among stars by over an order of magnitude for most molecules. In general, the same spectral regions drive unshielded photodissociations both for the minimally and maximally FUV active stars. However, for O3 visible flux drives dissociation for the M stars whereas near-UV flux drives dissociation for the K stars. We also searched for an far-UV continuum in the assembled SEDs and detected it in 5/11 stars, where it contributes around 10% of the flux in the range spanned by the continuum bands. An ultraviolet continuum shape is resolved for the star

ϵ

Eri that shows an edge likely attributable to Si ii recombination. The 11 SEDs presented in this paper, available online through the Mikulski Archive for Space Telescopes, will be valuable for vetting stellar upper-atmosphere emission models and simulating photochemistry in exoplanet atmospheres.
SOLUBILITY OF ROCK IN STEAM ATMOSPHERES OF PLANETS
Authors: Fegley Bruce , Jacobson Nathan S. , Williams K. B. , Plane J. M. C. , Schaefer L. , Lodders Katharina 
Published: June 2016

ABSTRACT
Extensive experimental studies show that all major rock-forming elements (e.g., Si, Mg, Fe, Ca, Al, Na, K) dissolve in steam to a greater or lesser extent. We use these results to compute chemical equilibrium abundances of rocky-element-bearing gases in steam atmospheres equilibrated with silicate magma oceans. Rocky elements partition into steam atmospheres as volatile hydroxide gases (e.g., Si(OH)4, Mg(OH)2, Fe(OH)2, Ni(OH)2, Al(OH)3, Ca(OH)2, NaOH, KOH) and via reaction with HF and HCl as volatile halide gases (e.g., NaCl, KCl, CaFOH, CaClOH, FAl(OH)2) in much larger amounts than expected from their vapor pressures over volatile-free solid or molten rock at high temperatures expected for steam atmospheres on the early Earth and hot rocky exoplanets. We quantitatively compute the extent of fractional vaporization by defining gas/magma distribution coefficients and show that Earth's subsolar Si/Mg ratio may be due to loss of a primordial steam atmosphere. We conclude that hot rocky exoplanets that are undergoing or have undergone escape of steam-bearing atmospheres may experience fractional vaporization and loss of Si, Mg, Fe, Ni, Al, Ca, Na, and K. This loss can modify their bulk composition, density, heat balance, and interior structure.
SPENDING TOO MUCH TIME AT THE GALACTIC BAR: CHAOTIC FANNING OF THE OPHIUCHUS STREAM
Authors: Price-Whelan Adrian M. , Sesar Branimir , Johnston Kathryn V. , Rix Hans-Walter 
Published: June 2016

ABSTRACT
The Ophiuchus stellar stream is peculiar: (1) its length is short given the age of its constituent stars, and (2) several probable member stars have dispersions in sky position and velocity that far exceed those seen within the stream. The stream’s proximity to the Galactic center suggests that its dynamical history is significantly influenced by the Galactic bar. We explore this hypothesis with models of stream formation along orbits consistent with Ophiuchus’ properties in a Milky Way potential model that includes a rotating bar. In all choices for the rotation parameters of the bar, orbits fit to the stream are strongly chaotic. Mock streams generated along these orbits qualitatively match the observed properties of the stream: because of chaos, stars stripped early generally form low-density, high-dispersion “fans” leaving only the most recently disrupted material detectable as a strong over-density. Our models predict that there should be a significant amount of low-surface-brightness tidal debris around the stream with a complex phase-space morphology. The existence of or lack of these features could provide interesting constraints on the Milky Way bar and would rule out formation scenarios for the stream. This is the first time that chaos has been used to explain the properties of a stellar stream and is the first demonstration of the dynamical importance of chaos in the Galactic halo. The existence of long, thin streams around the Milky Way, presumably formed along non- or weakly chaotic orbits, may represent only a subset of the total population of disrupted satellites.
A HARD X-RAY STUDY OF THE NORMAL STAR-FORMING GALAXY M83 WITH NuSTAR
Authors: Yukita M. , Hornschemeier A. E. , Lehmer B. D. , Ptak A. , Wik D. R. , Zezas A. , Antoniou V. , Maccarone T. J. , Replicon V. , Tyler J. B. , Venters T. , Argo M. K. , Bechtol K. , Boggs S. , Christensen F. E. , Craig W. W. , Hailey C. , Harrison F. , Krivonos R. , Kuntz K. , Stern D. , Zhang W. W. 
Published: June 2016

ABSTRACT
We present the results from sensitive, multi-epoch NuSTAR observations of the late-type star-forming galaxy M83 (d = 4.6 Mpc). This is the first investigation to spatially resolve the hard (

E
>
10

keV) X-ray emission of this galaxy. The nuclear region and ∼20 off-nuclear point sources, including a previously discovered ultraluminous X-ray source, are detected in our NuSTAR observations. The X-ray hardnesses and luminosities of the majority of the point sources are consistent with hard X-ray sources resolved in the starburst galaxy NGC 253. We infer that the hard X-ray emission is most likely dominated by intermediate accretion state black hole binaries and neutron star low-mass X-ray binaries (Z-sources). We construct the X-ray binary luminosity function (XLF) in the NuSTAR band for an extragalactic environment for the first time. The M83 XLF has a steeper XLF than the X-ray binary XLF in NGC 253, which is consistent with previous measurements by Chandra at softer X-ray energies. The NuSTAR integrated galaxy spectrum of M83 drops quickly above 10 keV, which is also seen in the starburst galaxies NGC 253, NGC 3310, and NGC 3256. The NuSTAR observations constrain any active galactic nucleus (AGN) to be either highly obscured or to have an extremely low luminosity of ≲1038 erg s−1 (10–30 keV), implying that it is emitting at a very low Eddington ratio. An X-ray point source that is consistent with the location of the nuclear star cluster with an X-ray luminosity of a few times 1038 erg s−1 may be a low-luminosity AGN but is more consistent with being an X-ray binary.
IMAGING THE ELUSIVE H-POOR GAS IN THE HIGH adf PLANETARY NEBULA NGC 6778
Authors: García-Rojas Jorge , Corradi Romano L. M. , Monteiro Hektor , Jones David , Rodríguez-Gil Pablo , Cabrera-Lavers Antonio 
Published: June 2016

ABSTRACT
We present the first direct image of the high-metallicity gas component in a planetary nebula (NGC 6778), taken with the OSIRIS Blue Tunable Filter centered on the O ii
λ4649+50 Å optical recombination lines (ORLs) at the 10.4 m Gran Telescopio Canarias. We show that the emission of these faint O ii ORLs is concentrated in the central parts of the planetary nebula and is not spatially coincident either with emission coming from the bright [O iii] λ5007 Å collisionally excited line (CEL) or the bright Hα recombination line. From monochromatic emission line maps taken with VIMOS at the 8.2 m Very Large Telescope, we find that the spatial distribution of the emission from the auroral [O iii] λ4363 line resembles that of the O ii ORLs but differs from nebular [O iii] λ5007 CEL distribution, implying a temperature gradient inside the planetary nebula. The centrally peaked distribution of the O ii emission and the differences with the [O iii] and H i emission profiles are consistent with the presence of an H-poor gas whose origin may be linked to the binarity of the central star. However, determination of the spatial distribution of the ORLs and CELs in other PNe and a comparison of their dynamics are needed to further constrain the geometry and ejection mechanism of the metal-rich (H-poor) component and hence, understand the origin of the abundance discrepancy problem in PNe.
Impacto económico del Campeonato del Mundo de Escalada. Gijón 8-14 de Septiembre del 2014
Authors: Baños José , Rodríguez Plácido 
Published: June 2016

Purpose: This study aims to assess the economic impact for the economy of the Principality of Asturias, of the World Climbing Championship held in Gijon in 2014.Design/methodology/approach: Various instruments are available to assess the economic impact of a sporting event in a city or region. Among them is the Input-Output (I-O) analysis, which is used in this study.Findings: We analyse the economic impacts of the expenditure by non-residents in the Principality of Asturias in a comprehensive study that categorises the individuals attending the Championship according to their accommodation choice and to different visitor categories (i.e. athletes, technicians, managers, etc.). The study also takes into account the expenditure on infrastructure and organization incurred by the organizer of the competition: the City Council of Gijon. The economic impact on the economy of Asturias of the 2014 World Climbing Championship held in Gijón is calculated in terms of the Gross Value Added (GVA).Originality/value: When a public institution organizes an activity, an assessment of whether the expenditure has an economic return or leads to an unjustifiable expenditure of public money, is required.
¿La transparencia de las páginas web ayudan en la captación de clientes? Análisis de los campos de golf en Andalucía
Authors: García-Tascón Marta , Pradas-García Marcos 
Published: June 2016

Purpose: The aim of this study is to analyze the degree of transparency of the Web pages of organizations that belong to the world of sports, specifically golf courses in Andalusia.Design/methodology/approach: We performed a descriptive analysis of the conditions of transparency of 92 Web pages of golf clubs registered on the official website of the Royal Golf Federation of Andalusia (RFGA). A questionnaire created/adapted ad hoc is used for this study having as a reference the questionnaire used by Barrio and Martin (2012) that analyze the performance of the 4 conditions of transparency of Web pages.Findings: To reflect a high degree of transparency, they show a higher compliance than 75% in 8 of the 10 variables. The Web page becomes an element to quantify the performance of the field without investing too much in other promotional channels to attract as many customers as possible.Research limitations: In some Web pages, the access to information entailed a significant investment of time because they did not have the characteristic of being intuitive. In some cases was not available all required information.Practical implications: Knowledge of this information allows the director or manager identifies possible areas of improvement to optimize their management, while transparency offered by the golf courses is improved.Social implications: This study highlights the need for teaching the user to evaluate the quality, transparency and being critical with the information found on Web pages.Originality/value: The analysis of transparency allows clubs to be reflective of its golf courses. It becomes the tool that the manager can use to display part of all its virtues and to evaluate the social behavior of their customers, to attract possible clients and perform actions with the stakeholders in the golf industry.