bluuebunny/crossref_metadata_2025_split huggingface dataset:
Hubungan Motivasi dengan Kinerja Kader Posyandu di Kecamatan Bulo Kabupaten Polewali Mandar
Authors: Hariani Hariani , Ramlah Ramlah 
Published: June 2019

Posyandu akan meningkatkan kinerja kader Posyandu. Namun permasalahan yang terjadi adalah masih banyak kader yang kurang termotivasi dalam kegiatan Posyandu. Persentase kader aktif secara nasional adalah 69,2% dan angka drop out kader sekitar 30,8%. Tujuan penelitian ini adalah untuk mengetahui hubungan motivasi dengan kinerja kader Posyandu di Kecamatan Bulo. Jenis penelitian ini adalah penelitian kuantitatif dengan desain observasional (cross sectional). Populasi adalah seluruh kader Posyandu di Kecamatan Bulo sebanyak 53 kader dan sampel adalah total sampling sebanyak 53 kader. Variabel dalam penelitian ini adalah tanggung jawab, insentif, hubungan kerja dan prosedur kerja kader Posyandu. Instrument yang digunakan adalah kuesioner dan wawancara. Data dalam penelitian ini dianalisis dengan analisis univariat dan bivariate dengan menggunakan uji Chi-square dengan dengan α = 0,05. Dari hasil analisis bivariat ada variabel berhubungan dan tidak berhubungan dengan kinerja kader Posyandu. Berdasarkan tanggung jawab diperoleh p value = 1,000 > α = 0,05, insentif diperoleh p value = 0,005 < α = 0,05, hubungan kerja diperoleh p value= 0.005 < α = 0,05 dan prosedur kerja diperoleh p value = 0,031 < α = 0,05. Disimpulkan bahwa tidak terdapat hubungan tanggung jawab dengan kinerja kader Posyandu dan terdapat hubungan insentif, hubungan kerja dan prosedur kerja dengan kinerja kader Posyandu. Posyandu yang ada didaerahnya karena Posyandu merupakan pelayanan dasar yang dapat mendeteksi penyakit balita serta ibu hamil secara cepat.
TCHELLO D’BARROS: “Uma obra de arte não precisa ser outra coisa senão um elo entre duas almas com afinidades estéticas”.
Authors: Barcellos Renata 
Published: June 2019

O olhar crítico sobre a arte contemporânea, o acesso à educação e à leitura, as questões políticas envolvidas nesse processo e as leis de incentivo à cultura ganham relevo na entrevista concedida a Renata Barcellos pelo multiartista Tchello d’Barros. Sua obra transita por várias linguagens das artes visuais (desenho, pintura, gravura, fotografia, vídeo, instalação), constituindo-se ainda de uma produção literária bastante diversificada, que inclui prosa (contos, crônicas, artigos) e poesia (versos livres, sonetos, haicais, poesia visual, cordéis). Não à toa, o entrevistado é visto como um dos maiores nomes da Poesia Visual no Brasil e no mundo.
LEGAL FRAMEWORKS OF TACTIC ACTIONS CONSTABULARY IN THE CONDITIONS OF EMERGENCY SITUATIONS
Authors: Sambor M. , Gudovych O. , Mazurenko V. 
Published: June 2019

The article deals with problems in the sphere of management and action organization of The National Police, being a part of a specialized Civil Protection Service of enforcement of public order in emergency situations – that is realizations and providing of rescue and salvage operations, evacuation and etc.
The need for improvement of the legal and organizational mechanisms for the provision of effective performance of specialized Enforcement of Public Order Services in case of emergencies according to the main tasks of the Service.
Synthesis of Complex Organic Molecules in Soft X-Ray Irradiated Ices
Authors: Ciaravella A. , Jiménez-Escobar A. , Cecchi-Pestellini C. , Huang C. H. , Sie N. E. , Caro G. M. Muñoz , Chen Y. J. 
Published: June 2019

Abstract
We study the chemical evolution of H2O:CO:NH3 ice mixtures irradiated with soft X-rays, in the range of 250–1250 eV. We identify many nitrogen-bearing molecules such as, e.g., OCN−,

, HNCO, CH3CN, HCONH2, and NH2COCONH2. Several infrared features are compatible with glycine or its isomers. During the irradiation, we detected through mass spectroscopy many species desorbing the ice. Such findings support the infrared identifications and reveal less abundant species without clear infrared features. Among them, m/z = 57 has been ascribed to methyl isocyanate (CH3NCO), a molecule of prebiotic relevance, recently detected in protostellar environments. During the warm-up after the irradiation, several infrared features including the 2168 cm−1 band of OCN−, the 1690 cm−1 band of formamide, and the 1590 cm−1 band associated with three different species, HCOO−, CH3NH2, and

survive up to room temperature. Interestingly, many high masses have also been detected. Possible candidates are methylformate, (m/z = 60, HCOOCH3), ethanediamide (m/z = 88, NH2COCONH2), and N-acetyl-L-aspartic acid (m/z = 175). The latter species is compatible with the presence of the m/z = 43, 70, and 80 fragments. Photodesorption of organics is relevant for the detection of such species in the gas phase of cold environments, where organic synthesis in ice mantles should dominate. We estimate the gas-phase enrichment of some selected species in the light of a protoplanetary disk model around young solar-type stars.
The z = 0.54 LoBAL Quasar SDSS J085053.12+445122.5. II. The Nature of Partial Covering in the Broad-absorption-line Outflow
Authors: Leighly Karen M. , Terndrup Donald M. , Lucy Adrian B. , Choi Hyunseop , Gallagher Sarah C. , Richards Gordon T. , Dietrich Matthias , Raney Catie 
Published: July 2019

Abstract
It has been known for 20 years that the absorbing gas in broad-absorption-line quasars does not completely cover the continuum emission region, and that partial covering must be accounted for to accurately measure the column density of the outflowing gas. However, the nature of partial covering itself is not understood. Extrapolation of the SimBAL spectral synthesis model of the Hubble Space Telescope Cosmic Origins Spectrograph UV spectrum from SDSS J0850+4451 reported by Leighly et al. to nonsimultaneous rest-frame optical and near-infrared spectra reveals evidence that the covering fraction has wavelength dependence and is a factor of 2.5 times higher in the UV than in the optical and near-infrared bands. The difference in covering fraction can be explained if the outflow consists of clumps that are small and either structured or clustered relative to the projected size of the UV continuum emission region and have a more diffuse distribution on size scales comparable to the size of the near-infrared continuum emission region. The lower covering fraction over the larger physical area results in a reduction of the measured total column density by a factor of 1.4–1.5 compared with the UV-only solution. This experiment demonstrates that we can compare rest-frame UV and near-infrared absorption lines, specifically He i*λ10830, to place constraints on the uniformity of absorption gas in broad-absorption-line quasars.
Interstellar Neutral Gas Species and Their Pickup Ions inside the Heliospheric Termination Shock: The Large-scale Structures
Authors: Sokół Justyna M. , Kubiak Marzena A. , Bzowski Maciej 
Published: June 2019

Abstract
We study the distribution of the interstellar neutral (ISN) gas density and the pickup ion (PUI) density of hydrogen, helium, neon, and oxygen in the heliosphere for heliocentric distances from inside 1 au up to the solar wind termination shock (TS), both in and out of the ecliptic plane. We discuss similarities and differences in the large-scale structures of the ISN gas and PUIs formed in the heliosphere between various species. We discuss the distribution of ISN gas and PUI densities for two extreme phases of the solar activity cycle, it is the solar minimum and the solar maximum. We identify the location of the ISN gas density cavity of various species. We study the relative abundance ratios of Ne/O, H/He, Ne/He, and O/He for ISN gas and PUIs densities and their variation with location in the heliosphere. We also discuss the modulation of relative abundance ratios of ISN gas and PUIs along the TS. We conclude that the preferable locations for detection of He+ and Ne+ PUIs are in the downwind hemisphere within 1 au, whereas for H+ and O+ PUIs the preferable locations for detection are for distances from Jupiter to Pluto orbits.
A Study of the 20 day Superorbital Modulation in the High-mass X-Ray Binary IGR J16493-4348
Authors: Coley Joel B. , Corbet Robin H. D. , Fürst Felix , Huxtable Gregory , Krimm Hans A. , Pearlman Aaron B. , Pottschmidt Katja 
Published: July 2019

Abstract
We report on Nuclear Spectroscopic Telescope Array (NuSTAR), Neil Gehrels Swift Observatory (Swift) X-ray Telescope (XRT), and Swift Burst Alert Telescope (BAT) observations of IGR J16493-4348, a wind-fed supergiant X-ray binary showing significant superorbital variability. From a discrete Fourier transform of the BAT light curve, we refine its superorbital period to be 20.058 ± 0.007 days. The BAT dynamic power spectrum and a fractional root mean square analysis both show strong variations in the amplitude of the superorbital modulation, but no observed changes in the period are found. The superorbital modulation is significantly weaker between MJD 55,700 and MJD 56,300. The joint NuSTAR and XRT observations, which were performed near the minimum and maximum of one cycle of the 20 day superorbital modulation, show that the flux increases by more than a factor of two between superorbital minimum and maximum. We find no significant changes in the 3–50 keV pulse profiles between superorbital minimum and maximum, which suggests a similar accretion regime. Modeling the pulse-phase-averaged spectra we find a possible Fe Kα emission line at 6.4 keV at superorbital maximum. This feature is not significant at superorbital minimum. While we do not observe any significant differences between the pulse-phase-averaged spectral continua apart from the overall flux change, we find that the hardness ratio near the broad main peak of the pulse profile increases from superorbital minimum to maximum. This suggests the spectral shape hardens with increasing luminosity. We discuss different mechanisms that might drive the observed superorbital modulation.
Extreme CO Isotopologue Line Ratios in ULIRGS: Evidence for a Top-heavy IMF
Authors: Brown Toby , Wilson Christine D. 
Published: June 2019

Abstract
We present high-resolution ALMA observations of the C18O, 13CO, and 12CO J = 1–0 isotopologues in three nearby ultraluminous infrared galaxies (ULIRGS; Arp 220, IRAS 13120-5453, and IRAS 17208-0014) and one nearby post-merger galaxy (NGC 2623). In all four systems, we measure high 12CO/C18O and 12CO/13CO integrated line ratios while the 13CO/C18O ratio is observed to be extremely low in comparison to typical star-forming disks, supporting previous work. We investigate whether these unusual line ratios are due to dynamical effects, astrochemistry within the gas, or nucleosynthesis in stars. Assuming both lines are optically thin, low 13CO/C18O values suggest that C18O is more abundant than 13CO in the interstellar medium of these systems. A plausible explanation is that local ULIRGs and their progeny have an excess in massive star formation; in other words, they are producing a top-heavy stellar initial mass function.
The Impact of Line Misidentification on Cosmological Constraints from Euclid and Other Spectroscopic Galaxy Surveys
Authors: Addison G. E. , Bennett C. L. , Jeong D. , Komatsu E. , Weiland J. L. 
Published: June 2019

Abstract
We perform forecasts for how baryon acoustic oscillation (BAO) scale and redshift-space distortion (RSD) measurements from future spectroscopic emission line galaxy surveys such as Euclid are degraded in the presence of spectral line misidentification. Using analytic calculations verified with mock galaxy catalogs from lognormal simulations, we find that constraints are degraded in two ways, even when the interloper power spectrum is modeled correctly in the likelihood. First, there is a loss of signal-to-noise ratio for the power spectrum of the target galaxies, which propagates to all cosmological constraints and increases with contamination fraction, f

c
. Second, degeneracies can open up between f

c
and cosmological parameters. In our calculations, this typically increases BAO scale uncertainties at the 10%–20% level when marginalizing over parameters determining the broadband power spectrum shape. External constraints on f

c
or parameters determining the shape of the power spectrum, for example, from cosmic microwave background measurements, can remove this effect. There is a near-perfect degeneracy between f

c
and the power spectrum amplitude for low f

c
values, where f

c
is not well determined from the contaminated sample alone. This has the potential to strongly degrade RSD constraints. The degeneracy can be broken with an external constraint on f

c
, for example, from cross-correlation with a separate galaxy sample containing the misidentified line or deeper subsurveys.
Diffusive versus Free-streaming Cosmic-Ray Transport in Molecular Clouds
Authors: Silsbee Kedron , Ivlev Alexei V. 
Published: June 2019

Abstract
Understanding the cosmic-ray (CR) ionization rate is crucial in order to simulate the dynamics of molecular clouds, and interpret the chemical species observed in these objects. Calculating the CR ionization rate requires both accurate knowledge of the spectrum of MeV to GeV protons at the edge of the cloud as well as a model for the propagation of CRs into molecular clouds. Some models for the propagation of CRs in molecular clouds assume them to stream freely along magnetic field lines, while in others they propagate diffusively due to resonant scattering off of magnetic disturbances excited by MHD turbulence present in the medium. We discuss the conditions under which CR diffusion can operate in a molecular cloud, calculate the local CR spectrum and ionization rate in both a free-streaming and diffusive propagation model, and highlight the different results from the two models. We also apply these two models to the propagation through the ISM to obtain the proton spectrum seen by Voyager 1, and show that such a spectrum favors a diffusive propagation model.
Determining the Best Method of Calculating the Large Frequency Separation For Stellar Models
Authors: Viani Lucas S. , Basu Sarbani , Corsaro Enrico , Ball Warrick H. , Chaplin William J. 
Published: July 2019

Abstract
Asteroseismology of solar-like oscillators often relies on the comparisons between stellar models and stellar observations in order to determine the properties of stars. The values of the global seismic parameters, ν
max (the frequency where the smoothed amplitude of the oscillations peak) and Δν (the large frequency separation), are frequently used in grid-based modeling searches. However, the methods by which Δν is calculated from observed data and how Δν is calculated from stellar models are not the same. Typically for observed stars, especially for those with low signal-to-noise data, Δν is calculated by taking the power spectrum of a power spectrum, or with autocorrelation techniques. However, for stellar models, the actual individual mode frequencies are calculated and the average spacing between them directly determined. In this work we try to determine the best way to combine model frequencies in order to obtain Δν that can be compared with observations. For this we use stars with high signal-to-noise observations from Kepler as well as simulated Transiting Exoplanet Survey Satellite data of Ball et al. We find that when determining Δν from individual mode frequencies the best method is to use the ℓ = 0 modes with either no weighting or with a Gaussian weighting around ν
max.
Polarization of Kilonova Emission from a Black Hole–Neutron Star Merger
Authors: Li 李 Yan 彦 , Shen 申 Rong-Feng 荣锋 
Published: July 2019

Abstract
A multi-messenger, black hole (BH)–neutron star (NS) merger event still remains to be detected. The tidal (dynamical) ejecta from such an event, thought to produce a kilonova, is concentrated in the equatorial plane and occupies only part of the whole azimuthal angle. In addition, recent simulations suggest that the outflow or wind from the post-merger remnant disk, presumably anisotropic, can be a major ejecta component responsible for a kilonova. For any ejecta whose photosphere shape deviates from the spherical symmetry, the electron scattering at the photosphere causes a net polarization in the kilonova light. Recent observational and theoretical polarization studies have been focused on the NS–NS merger kilonova AT2017gfo. We extend those works to the case of a BH–NS merger kilonova. We show that the degree of polarization at the first ∼1 hr can be up to ∼3% if a small amount (10−4
M
⊙) of free neutrons have survived in the fastest component of the dynamical ejecta, whose beta-decay causes a precursor in the kilonova light. The polarization degree can be ∼0.6% if free neutrons survived in the fastest component of the disk wind. Future polarization detection of a kilonova will constrain the morphology and composition of the dominant ejecta component, therefore helping to identify the nature of the merger.
Stellar Winds As a Mechanism to Tilt the Spin Axes of Sun-like Stars
Authors: Spalding Christopher 
Published: June 2019

Abstract
The rotation axis of the Sun is misaligned from the mean angular momentum plane of the solar system by about 6°. This obliquity significantly exceeds the ∼1°–2° distribution of inclinations among the planetary orbits and therefore requires a physical explanation. In concert, Sun-like stars are known to spin down by an order of magnitude throughout their lifetimes. This spindown is driven by the stellar wind, which carries angular momentum from the star. If the mean angular momentum axis of the stellar wind deviates from that of the stellar spin axis, it will lead to a component of the spindown torque that acts to tilt the star. Here, we show that solar-like tilts of 6° naturally arise during the first 10–100 Myr after planet formation as a result of stellar winds that deviate by about 10° from the star’s spin axis. These results apply to the idealized case of a dipole field, mildly inclined to the spin axis. Time-variability in the misalignment between the magnetic and spin poles is modeled as stochastic fluctuations, autocorrelated over timescales comparable to the primordial spindown time of several million years. In addition to wind direction, time-variability in mass-loss rate and magnetic topology over the stellar lifetime may alternatively generate obliquity. We hypothesize that the gaseous environments of young, open clusters may provide forcing over sufficient timescales to tilt the astrospheres of young stars, exciting modest obliquities. The more extreme, retrograde stellar obliquities of extrasolar planetary systems likely arise through separate mechanisms.
Toward Defining Primary and Secondary Nonresponse in Rheumatoid Arthritis Patients Treated with Anti-TNF: Results from the BioTRAC and OBRI Registries
Authors: Keystone Edward C. , Rampakakis Emmanouil , Movahedi Mohammad , Cesta Angela , Stutz Melissa , Sampalis John S. , Nantel Francois , Maslova Karina , Bombardier Claire 
Published: July 2019

Objective.Although most patients with rheumatoid arthritis (RA) respond to anti–tumor necrosis factor (anti-TNF) treatment, some present with initial nonresponse (1ry nonresponse) or lose initial responsiveness (2ry nonresponse). We compared the rate of real-world “nonresponse” to first anti-TNF as reported by treating physicians to the nonresponse rate per accepted definitions and recommended treat-to-target strategies.Methods.Patients were included from the Biologic Treatment Registry Across Canada (BioTRAC) and Ontario Best Practices Research Initiative (OBRI) registries who were taking their first anti-TNF, with ≥ 1 followup visit. Posthoc reclassification of physician-reported nonresponse was based on prior achievement of 28-joint count Disease Activity Score based on erythrocyte sedimentation rate (DAS28-ESR) low disease activity (LDA), Clinical Disease Activity Index (CDAI) LDA, or good/moderate European League Against Rheumatism (EULAR) response, and actual time of physician-reported nonresponse.Results.Among 736 BioTRAC and 640 OBRI patients, 13.7% and 18%, respectively, discontinued their anti-TNF because of physician-reported nonresponse. Based on reclassification using disease activity, 65.6% (BioTRAC) and 87.2% (OBRI) of 1ry nonresponders did not achieve DAS28-ESR LDA, 65.6%/90.7% CDAI LDA, and 46.9%/61.5% good/moderate EULAR response. Among 2ry nonresponders, 50.7%/47.8% did not achieve DAS28-ESR LDA, 37.7%/52.9% CDAI LDA, and 15.9%/19.6% good/moderate EULAR response before treatment discontinuation. Regarding actual time of nonresponse, 18.8% of BioTRAC and 60.8% of OBRI 1ry nonresponders discontinued at ≤ 6 months. In both registries, a high proportion of 2ry nonresponders discontinued their anti-TNF after 12 months (87.0% BioTRAC, 60.9% OBRI).Conclusion.Physician-reported 1ry nonresponse was more correlated with non-achievement of DAS28-ESR LDA or CDAI LDA, whereas 2ry nonresponse with actual time of discontinuation. Further work is needed to confirm the importance of response and type of response to the initial anti-TNF in identifying patients most likely to benefit from a second biologic agent treatment.
The Longitudinal Course of Fatigue in Antineutrophil Cytoplasmic Antibody–associated Vasculitis
Authors: O’Malley Lucy , Druce Katie L. , Chanouzas Dimitrios , Morgan Matthew D. , Jones Rachel , Jayne David R.W. , Basu Neil , Harper Lorraine 
Published: July 2019

Objective.Fatigue is common and burdensome in antineutrophil cytoplasmic antibody–associated vasculitis (AAV). This study aimed to understand how fatigue changes over time following treatment initiation and to determine whether individuals with the poorest prognosis can be robustly identified.Methods.One hundred forty-nine patients with AAV and new-onset disease recruited to 2 clinical trials (RITUXVAS and MYCYC) were followed for 18 months. Fatigue was measured at baseline and 6-month intervals using the vitality domain of the Medical Outcomes Study Short Form-36 quality of life questionnaire and compared to a cohort of 470 controls. Group-based trajectory modeling (GBTM) determined trajectories of the symptom to which baseline characteristics and ongoing fatigue scores were compared.Results.Fatigue levels at diagnosis were worse in patients than controls [median (interquartile range; IQR) 30 (10–48) vs 70 (55–80); p < 0.001], with 46% of patients reporting severe fatigue. Fatigue improved after 6 months of treatment but remained worse than in controls (p < 0.001). GBTM revealed varied trajectories of fatigue: low fatigue stable (n = 23), moderate baseline fatigue improvers (n = 29), high baseline fatigue improvers (n = 61), and stable baseline high fatigue (n = 37). Participants who followed stable high fatigue trajectories had lower vasculitis activity compared to improvers, but no other demographic or clinical variables differed.Conclusion.This study longitudinally measured fatigue levels in patients with AAV. Although most patients improved following treatment, an important subgroup of patients reported persistently high levels of fatigue that did not change. Few clinical or laboratory markers distinguished these patients, suggesting alternative interventions specific for fatigue are required. [clinicaltrialsregister.eu, RITUXVAS EudraCT number: 2005-003610-15; MYCYC EudraCT number: 2006-001663-33]