bluuebunny/crossref_metadata_2025_split huggingface dataset:
Analisis Faktor Yang Memengaruhi Kualitas Pelayanan Kesehatan Dengan Metode Servqual Di Puskesmas Wilayah Kerja Dinas Kesehatan Aceh Timur Tahun 2018
Authors: Hermansyah Hermansyah , Darmana Ayi , Nur'aini Nur'aini 
Published: November 2019

ABSTRAK
Pendahuluan, pelayanan kesehatan yang bermutu adalah pelayanan kesehatan yang harus memperhatikan empat unsur pokok. Berdasarkan survei yang dilakukan tentang pelayanan Puskesmas kepada pasien sebanyak 10 orang, 6 pasien diantaranya merasa kualitas pelayanan di Puskesmas belum maksimal, sedangkan 4 orang lainnya menyatakan pelayanan sudah maksimal. Tujuan penelitian ini adalah untuk mengetahui faktor yang memengaruhi kualitas pelayanan kesehatan dengan Metode Servqual. Metode, desain penelitian yang digunakan dalam penelitian ini adalah Cross Sectional. Populasi dalam penelitian ini sebanyak 7.635 orang dan sampel yang diambil dengan cara accidental sampling yaitu sebanyak 99 orang. Metode pengumpulan data yaitu data primer dan data sekunder. Analisa data yang digunakan yaitu uji regresi binary logistic. Hasil, hasil penelitian menunjukkan bahwa keadaan fisik memiliki nilai sig-p 0,007 < 0,05, kehandalan sig-p 0,008 < 0,05, ketanggapan sig-p 0,011 < 0,05 dan jaminan sig-p 0,034 < 0,05 yang artinya keadaan fisik, kehandalan, ketanggapan dan jaminan memiliki pengaruh terhadap kualitas pelayanan kesehatan, sedangkan kepedulian tidak memiliki pengaruh terhadap kualitas pelayanan kesehatan karena memiliki nilai sig-p 0,325 > 0,05. Saran, diharapkan dapat menjadi acuan bagi masyarakat dan bagi kader-kader di Puskesmas agar lebih memahami pentingnya kualitas pelayanan yang sesuai dengan peraturan kementerian kesehatan guna meningkatkan pelayanan kesehatan yang diberikan kepada pasien secara maksimal.
Kata Kunci : Faktor Kualitas Pelayanan Kesehatan, Metode Servqual
Spatially Resolved Stellar Kinematics of the Ultra-diffuse Galaxy Dragonfly 44. II. Constraints on Fuzzy Dark Matter
Authors: Wasserman Asher , van Dokkum Pieter , Romanowsky Aaron J. , Brodie Jean , Danieli Shany , Forbes Duncan A. , Abraham Roberto , Martin Christopher , Matuszewski Matt , Villaume Alexa , Tamanas John , Profumo Stefano 
Published: November 2019

Abstract
Given the absence of directly detected dark matter (DM) as weakly interacting massive particles, there is strong interest in the possibility that DM is an ultralight scalar field, here denoted as “fuzzy” DM. Ultra-diffuse galaxies, with the sizes of giant galaxies and the luminosities of dwarf galaxies, have a wide range of DM halo masses, thus providing new opportunities for exploring the connections between galaxies and their DM halos. Following up on new integral field unit spectroscopic observations and dynamics modeling of the DM-dominated ultra-diffuse galaxy Dragonfly 44 in the outskirts of the Coma Cluster, we present models of fuzzy DM constrained by the stellar dynamics of this galaxy. We infer a scalar field mass of

, consistent with other constraints from galaxy dynamics but in tension with constraints from Lyα forest power spectrum modeling. While we are unable to statistically distinguish between fuzzy DM and “normal” cold DM models, we find that the inferred properties of the fuzzy DM halo satisfy a number of predictions for halos in a fuzzy DM cosmology. In particular, we find good agreement with the predicted core size–halo mass relation and the predicted transition radius between the quantum pressure-dominated inner region and the outer halo region.
The M101 Satellite Luminosity Function and the Halo–Halo Scatter among Local Volume Hosts
Authors: Bennet P. , Sand D. J. , Crnojević D. , Spekkens K. , Karunakaran A. , Zaritsky D. , Mutlu-Pakdil B. 
Published: November 2019

Abstract
We have obtained deep Hubble Space Telescope (HST) imaging of 19 dwarf galaxy candidates in the vicinity of M101. Advanced Camera for Surveys HST photometry for two of these objects showed resolved stellar populations and tip of the red giant branch derived distances (D ∼ 7 Mpc) consistent with M101 group membership. The remaining 17 were found to have no resolved stellar populations, meaning they are either part of the background NGC 5485 group or are distant low surface brightness (LSB) galaxies. It is noteworthy that many LSB objects that had previously been assumed to be M101 group members based on projection have been shown to be background objects, indicating the need for future diffuse dwarf surveys to be very careful in drawing conclusions about group membership without robust distance estimates. In this work we update the satellite luminosity function of M101 based on the presence of these new objects down to M

V
= −8.2. M101 is a sparsely populated system with only nine satellites down to M

V
≈ −8, as compared with 26 for M31 and 24.5 ± 7.7 for the median host in the Local Volume. This makes M101 by far the sparsest group probed to this depth, although M94 is even sparser to the depth at which it has been examined (M

V
= −9.1). M101 and M94 share several properties that mark them as unusual compared with the other Local Volume galaxies examined: they have a very sparse satellite population but also have high star-forming fractions among these satellites; such properties are also found in the galaxies examined as part of the Satellites around Galactic Analogs survey. We suggest that these properties appear to be tied to the wider galactic environment, with more isolated galaxies showing sparse satellite populations that are more likely to have had recent star formation, while those in dense environments have more satellites that tend to have no ongoing star formation. Overall, our results show a level of halo-to-halo scatter between galaxies of similar mass that is larger than is predicted in the lambda cold dark matter model.
Population Synthesis of Black Hole Binaries with Normal-star Companions. I. Detached Systems
Authors: Shao Yong , Li Xiang-Dong 
Published: November 2019

Abstract
Optical observations of normal stars in binary systems with massive unseen objects have been proposed to search for candidate black holes (BHs) and provide a direct measurement of their dynamical masses. In this paper, we have performed binary population synthesis calculations to simulate the potential population of detached binaries containing BHs and normal-star companions in the Galaxy. We focus on the influence of the BH progenitors. In the traditional model, BHs in binaries evolve from stars more massive than ∼25M
⊙. However, it is difficult for this model to produce BH low-mass X-ray binaries. Recent investigations of massive star evolution have suggested that the BH progenitors have masses as low as ∼15M
⊙. Based on this model, we provide the expected distributions of various parameters for detached BH binaries with normal-star companions, including the component masses, the orbital parameters of the binary systems, the radial velocity semi-amplitudes, and the astrometric signatures of the optical companions. Our calculations show that there are thousands of such detached binaries in the Galaxy, and hundreds of them are potentially observable systems with luminous companions brighter than 20 mag. In addition, detached BH binaries are dominated by those with main-sequence companions and only a small percent of them are expected to have giant companions.
Measurement of the Extragalactic Background Light Spectral Energy Distribution with VERITAS
Authors: Abeysekara A. U. , Archer A. , Benbow W. , Bird R. , Brill A. , Brose R. , Buchovecky M. , Calderon-Madera D. , Christiansen J. L. , Cui W. , Daniel M. K. , Falcone A. , Feng Q. , Fernandez-Alonso M. , Finley J. P. , Fortson L. , Furniss A. , Gent A. , Giuri C. , Gueta O. , Hanna D. , Hassan T. , Hervet O. , Holder J. , Hughes G. , Humensky T. B. , Johnson C. A. , Kaaret P. , Kertzman M. , Kieda D. , Krause M. , Krennrich F. , Kumar S. , Lang M. J. , Maier G. , Moriarty P. , Mukherjee R. , Nievas-Rosillo M. , O’Brien S. , Ong R. A. , Pfrang K. , Pohl M. , Prado R. R. , Pueschel E. , Quinn J. , Ragan K. , Reynolds P. T. , Ribeiro D. , Richards G. T. , Roache E. , Rovero A. C. , Sadeh I. , Santander M. , Sembroski G. H. , Shahinyan K. , Sushch I. , Svraka T. , Weinstein A. , Wells R. M. , Wilcox P. , Wilhelm A. , Williams D. A. , Williamson T. J , Zitzer B. 
Published: November 2019

Abstract
The extragalactic background light (EBL), a diffuse photon field in the optical and infrared range, is a record of radiative processes over the universe’s history. Spectral measurements of blazars at very high energies (>100 GeV) enable the reconstruction of the spectral energy distribution (SED) of the EBL, as the blazar spectra are modified by redshift- and energy-dependent interactions of the gamma-ray photons with the EBL. The spectra of 14 VERITAS-detected blazars are included in a new measurement of the EBL SED that is independent of EBL SED models. The resulting SED covers an EBL wavelength range of 0.56–56 μm, and is in good agreement with lower limits obtained by assuming that the EBL is entirely due to radiation from cataloged galaxies.
The Long-standing Closure Crisis in Coronal Plasmas
Authors: Scudder J. D. 
Published: November 2019

Abstract
Coronal and solar wind physics have long used plasma fluid models to motivate physical explanations of observations; the hypothesized model is introduced into a fluid simulation to see if observations are reproduced. This procedure is called Verification of Mechanism (VoM) modeling; it is contingent on the self consistency of the closure that made the simulation possible. Inner corona VoMs typically assume weak gradient Spitzer–Braginskii closures. Four prominent coronal VoMs in place for decades are shown to contradict their closure hypotheses, demonstrably shaping coronal and solar wind research. These findings have been possible since 1953. This unchallenged evolution is worth understanding, so that similarly flawed VoMs do not continue to mislead new research. As a first step in this direction, this paper organizes four a posteriori quantitative tests for the purpose of easily screening the physical integrity of a proposed VoM. A fifth screen involving the thermal force, the tandem of the heat flux, has been shown to be mandatory when VoMs involve species-specific energy equations. VoM modeling will soon be required to advance Parker Solar Probe and Solar Orbiter science. Such modeling cannot advance the physical understanding sought by these missions unless the closures adopted (i) are demonstrated to be self consistent for the VoM plasma Knudsen numbers, (ii) are verified a posteriori as possessing nonnegative VDFs throughout the simulated volume, and (iii) include the physical completeness of thermal force physics when the VoM requires species-specific energy equations.
Prevalence of SED Turndown among Classical Be Stars: Are All Be Stars Close Binaries?
Authors: Klement Robert , Carciofi A. C. , Rivinius T. , Ignace R. , Matthews L. D. , Torstensson K. , Gies D. , Vieira R. G. , Richardson N. D. , de Souza A. Domiciano , Bjorkman J. E. , Hallinan G. , Faes D. M. , Mota B. , Gullingsrud A. D. , de Breuck C. , Kervella P. , Curé M. , Gunawan D. 
Published: November 2019

Abstract
Rapid rotation is a fundamental characteristic of classical Be stars and a crucial property allowing for the formation of their circumstellar disks. Past evolution in a mass and angular momentum transferring binary system offers a plausible solution to how Be stars attained their fast rotation. Although the subdwarf remnants of mass donors in such systems should exist in abundance, only a few have been confirmed due to tight observational constraints. An indirect method of detecting otherwise hidden companions is offered by their effect on the outer parts of Be star disks, which are expected to be disrupted or truncated. In the context of the infrared and radio continuum excess radiation originating in the disk, the disk truncation can be revealed by a turndown in the spectral energy distribution due to reduced radio flux levels. In this work, we search for signs of spectral turndown in a sample of 57 classical Be stars with radio data, which include new data for 23 stars and the longest-wavelength detections so far (λ ≈ 10 cm) for two stars. We confidently detect the turndown for all 26 stars with sufficient data coverage (20 of which are not known to have close binary companions). For the remaining 31 stars, the data are inconclusive as to whether the turndown is present or not. The analysis suggests that many if not all Be stars have close companions influencing their outer disks. If confirmed to be subdwarf companions, the mass transfer spin-up scenario might explain the existence of the vast majority of classical Be stars.
A Three-phase Approach to Grain Surface Chemistry in Protoplanetary Disks: Gas, Ice Surfaces, and Ice Mantles of Dust Grains
Authors: Ruaud Maxime , Gorti Uma 
Published: November 2019

Abstract
We study the effects of grain surface reactions on the chemistry of protoplanetary disks where gas, ice surface layers, and icy mantles of dust grains are considered as three distinct phases. Gas-phase and grain surface chemistry is found to be mainly driven by photoreactions and dust temperature gradients. The icy disk interior has three distinct chemical regions: (i) the inner midplane with low far-UV (FUV) fluxes and warm dust (≳15 K) that lead to the formation of complex organic molecules, (ii) the outer midplane with higher FUV from the interstellar medium and cold dust where hydrogenation reactions dominate, and (iii) a molecular layer above the midplane but below the water condensation front where photodissociation of ices affects gas-phase compositions. Some common radicals, e.g., CN and C2H, exhibit a two-layered vertical structure and are abundant near the CO photodissociation front and near the water condensation front. The three-phase approximation in general leads to lower vertical column densities than two-phase models for many gas-phase molecules owing to reduced desorption, e.g., H2O, CO2, HCN, and HCOOH decrease by roughly two orders of magnitude. Finally, we find that many observed gas-phase species originate near the water condensation front; photoprocesses determine their column densities, which do not vary significantly with key disk properties such as mass and dust/gas ratio.
The Next Generation Virgo Cluster Survey. XVII. A Search for Planetary Nebulae in Virgo Cluster Globular Clusters
Authors: Sun Weijia , Peng Eric W. , Ko Youkyung , Côté Patrick , Ferrarese Laura , Lee Myung Gyoon , Liu Chengze , Longobardi Alessia , Chilingarian Igor V. , Spengler Chelsea , Zabludoff Ann I. , Zhang Hong-Xin , Cuillandre Jean-Charles , Gwyn Stephen D. J. 
Published: November 2019

Abstract
The occurrence of planetary nebulae (PNe) in globular clusters (GCs) provides an excellent chance to study low-mass stellar evolution in a special (low-metallicity, high stellar density) environment. We report a systematic spectroscopic survey for the [O iii] 5007 Å emission line of PNe in 1469 Virgo GCs and 121 Virgo ultra-compact dwarfs (UCDs), mainly hosted in the giant elliptical galaxies M87, M49, M86, and M84. We detected zero PNe in our UCD sample and discovered one PN (

) associated with an M87 GC. We used the [O iii] detection limit for each GC to estimate the luminosity-specific frequency of PNe, α, and measured α in the Virgo cluster GCs to be

. The value of α in the Virgo GCs is among the lowest reported in any environment, due in part to the large sample size, and it is 5–6 times lower than that for the Galactic GCs. We suggest that α decreases toward brighter and more massive clusters, sharing a similar trend as the binary fraction, and the discrepancy between the Virgo and Galactic GCs can be explained by the observational bias in extragalactic surveys toward brighter GCs. This low but nonzero efficiency in forming PNe may highlight the important role played by binary interactions in forming PNe in GCs. We argue that a future survey of less massive Virgo GCs will be able to determine whether PN production in the Virgo GCs is governed by an internal process (mass, density, binary fraction) or if it is largely regulated by the external environment.
Global Radiation Magnetohydrodynamic Simulations of sub-Eddington Accretion Disks around Supermassive Black Holes
Authors: Jiang 燕 Yan-Fei 飞姜 , Blaes Omer , Stone James M. , Davis Shane W. 
Published: November 2019

Abstract
We conduct global three-dimensional radiation magnetohydrodynamic simulations of the inner regions of accretion flows around a 5 × 108
M
⊙ black hole, with mass accretion rates reaching 7% and 20% of the Eddington value. We choose initial field topologies that result in an inner disk supported by magnetic pressure, with surface density significantly smaller than the values predicted by the standard thin-disk model as well as a much larger disk scale height. The disks do not show any sign of thermal instability over many thermal timescales. More than half of the accretion is driven by radiation viscosity in the optically thin coronal region for the case of the lower accretion rate, while accretion in the optically thick part of the disk is driven by the Maxwell and Reynolds stresses from turbulence caused by magnetorotational instability. Optically thin plasma with gas temperatures ≳108 K is generated only in the inner ≈10 gravitational radii in both simulations, and is more compact in the case of the higher accretion rate. Such plasma does not form at larger radii because the surface density increases outward with radius, causing less dissipation outside the photosphere. In contrast to standard thin-disk models, the surface density in our simulations increases with increasing mass accretion rate at each radius. This causes a relatively weaker hot plasma component for the simulation with a higher accretion rate. We suggest that these results may provide a physical mechanism for understanding some of the observed properties of coronae and spectra of active galactic nuclei.
Testing Stellar Evolution with Asteroseismic Inversions of a Main-sequence Star Harboring a Small Convective Core
Authors: Bellinger Earl P. , Basu Sarbani , Hekker Saskia , Christensen-Dalsgaard Jørgen 
Published: November 2019

Abstract
The goal of stellar evolution theory is to predict the structure of stars throughout their lifetimes. Usually, these predictions can be assessed only indirectly, for example by comparing predicted and observed effective temperatures and luminosities. Thanks now to asteroseismology, which can reveal the internal structure of stars, it becomes possible to compare the predictions from stellar evolution theory to actual stellar structures. In this work, we present an inverse analysis of the oscillation data from the solar-type star KIC 6225718, which was observed by the Kepler space observatory during its nominal mission. As its mass is about 20% greater than solar, this star is predicted to transport energy by convection in its nuclear-burning core. We find significant differences between the predicted and actual structure of the star in the radiative interior near to the convective core. In particular, the predicted sound speed is higher than observed in the deep interior of the star, and too low at a fractional radius of 0.25 and beyond. The cause of these discrepancies is unknown, and is not remedied by known physics in the form of convective overshooting or elemental diffusion.
NuSTAR and Chandra Observations of New X-Ray Transients in the Central Parsec of the Galaxy
Authors: Mori Kaya , Hailey Charles J. , Mandel Shifra , Schutt Theo , Bachetti Matteo , Coerver Anna , Baganoff Frederick K. , Dykaar Hannah , Grindlay Jonathan E. , Haggard Daryl , Heuer Keri , Hong Jaesub , Hord Benjamin J. , Jin Chichuan , Nynka Melania , Ponti Gabriele , Tomsick John A. 
Published: November 2019

Abstract
We report NuSTAR and Chandra observations of two X-ray transients, SWIFT J174540.7−290015 (T15) and SWIFT J174540.2−290037 (T37), which were discovered by the Neil Gehrels Swift Observatory in 2016 within r ∼ 1 pc of Sgr A*. NuSTAR detected bright X-ray outbursts from T15 and T37, likely in the soft and hard states, with 3–79 keV luminosities of 8 × 1036 and 3 × 1037 erg s−1, respectively. No X-ray outbursts have previously been detected from the two transients and our Chandra ACIS analysis puts an upper limit of L
X ≲ 2 × 1031 erg s−1 on their quiescent 2–8 keV luminosities. No pulsations, significant quasi-periodic oscillations, or type I X-ray bursts were detected in the NuSTAR data. While T15 exhibited no significant red noise, the T37 power density spectra are well characterized by three Lorentzian components. The declining variability of T37 above ν ∼ 10 Hz is typical of black hole (BH) transients in the hard state. NuSTAR spectra of both transients exhibit a thermal disk blackbody, X-ray reflection with broadened Fe atomic features, and a continuum component well described by Comptonization models. Their X-ray reflection spectra are most consistent with high BH spin (a
* ≳ 0.9) and large disk density (n

e
∼ 1021 cm−3). Based on the best-fit ionization parameters and disk densities, we found that X-ray reflection occurred near the inner-disk radius, which was derived from the relativistic broadening and thermal disk component. These X-ray characteristics suggest the outbursting BH-low-mass X-ray binary scenario for both transients and yield the first BH spin measurements from X-ray transients in the central 100 pc region.
Could HCN Be Responsible for the Formamide Synthesis in Earth’s Primitive Atmosphere?
Authors: Vichietti R. M. , Spada R. F. K. , da Silva A. B. F. , Machado F. B. C. , Haiduke R. L. A. 
Published: November 2019

Abstract
The forward and reverse H2O + HCN ↔ HCONH2 global reactions were studied along temperatures from 200 to 4000 K. Equilibrium geometries and vibrational frequencies were obtained from calculations at the Coupled Cluster theory with single and double excitations (CCSD)/cc-pVDZ level; whereas enthalpies, Gibbs energies, and thermal rate constants were achieved by means of the CCSD(T)/CBS//CCSD/cc-pVDZ combined treatment. The estimates performed considering physical and chemical conditions proposed for the primitive atmosphere of Earth indicate that the formamide concentration might be 3.0–4.4 times larger than the one for HCN at 700 K, suggesting that this forward gas phase reaction could provide an efficient production route for formamide during an age just before the formation of early oceans. This route is also considerably fast once the chemical equilibrium is attained in some decades at this temperature. In short, our research reinforces that more complex organic compounds, such as formamide, could be synthetized in the Earth’s primordial atmosphere, even considering a neutral atmosphere scenario composed mainly by H2O, CO2, and some N2.