bluuebunny/crossref_metadata_2025_split huggingface dataset:
ANALISIS KESENJANGAN ANTARA EKSPEKTASI KONSUMEN TERHADAP PERSEPSI JASA PELAYANAN (Studi Kasus pada Bengkel Cat dan Las Mobil Warna Indah di Kediri)
Authors: Satriyono Gandung , Ruhamak M. Dian 
Published: August 2018

In the early survey, the researcher got the features of Warna Indah Car Workshop in not only claimed to give good service but also be able to compete for its survival by giving the best service quality. The purpose of this research is to prove whether any differentiate between perception and expectation from customers toward the service quality dimension at Warna Indah Car Color and Weld Workshop in Kediri which including tangibles, reliability, responsiveness, assurance, and empathy. This research used cross sectional method and the variable was measured once. The population of the research was customers of Warna Indah Car Color and Weld Workshop in Kediri. The data collected used interview, observation, and questionnaire. Based on the calculation of product moment correlation by using software SPSS V22, it was gotten, there was a a gap for each service quality and the highest gap was service quality dimension of T1 indicator ( the location of Warna Indah Workshop), it was analyze by using Kartesius diagram in quadrant B with the low priority -0.15, the average value of service quality ( perception) 3.8125 and service hope ( expectation) 3.9625. Tujuan dari penelitian ini adalah untuk membuktikan apakah terdapat kesenjangan antara persepsi dan ekspetasi konsumen terhadap dimensi kualitas pelayanan yang ada di Bengkel Las dan Cat Warna Indah yang meliputi Tangibles, Reliability, Responsiveness, Assurance dan Empathy. Target khusus dalam penelitian ini adalah dimensi kualitas pelayanan manakah yang menjadi prioritas utama untuk diperbaiki agar kesenjangan konsumen dapat di atasi. Penelitian ini menggunakan metode cross sectional, dimana variabel penelitian diukur sekali saja. Adapun populasi dalam penelitian ini adalah pelanggan pengguna jasa Bengkel Las Dan Cat Mobil Warna Indah Di Kediri. Teknik pengumpulan data memakai interview, observasi dan kuisioner. Dengan adanya penelitian ini diharapkan mampu mengetahui kesenjangan konsumen pada Bengkel Las Dan Cat Warna Indah agar kesenjangan tersebut dapat diatasi serta ke depannya kualitas layanan pada Bengkel Cat Warna Indah dapat lebih ditingkatkan sehingga konsumen merasa puas dan kesenjangan tidak muncul di kemudian hari.
PENGARUH KECERDASAN EMOSIONAL TERHADAP KINERJA GURU DI SMP NEGERI 4 KEDIRI
Authors: Satriyono Gandung , Vitasmoro Pamadya 
Published: August 2018

The purpose of the study is to find out the emotional intelligence which consists of social awareness, self management, social awareness, and relationship management toward the contextual performance.This research used quantitative method with double regression analyzes. The respondent was 45 teachers. From the research is gotten that the emotional intelligence and teachers contextual performance is good enough and very good and the variable of emotional intelligence influences significantly toward the teacher’s contextual performance. It means, the dependent variable namely emotional intelligence ( social awareness, self management, empathy, and relationship management) can explain the independent variable ( contextual performance) is bigger than another variable out of this research. So, it can be concluded that emotional intelligence influences the teacher’s contextual performance. Tujuan dari penelitian ini adalah untuk mengetahui kecerdasan emosional yang terdiri dari kesadaran sosial, manajemen diri, kesadaran sosial, dan manajemen hubungan terhadap kinerja kontekstual. Penelitian ini menggunakan metode kuantitatif dengan analisis regresi berganda. Respondennya adalah 45 guru. Dari penelitian didapatkan bahwa kecerdasan emosi dan kinerja kontekstual guru cukup baik dan sangat baik serta variabel kecerdasan emosional berpengaruh signifikan terhadap kinerja kontekstual guru. Artinya, variabel dependen yaitu kecerdasan emosional (social awareness, self management, empathy, dan relationship management) dapat menjelaskan variabel independen (kinerja kontekstual) lebih besar dari variabel lain dari penelitian ini. Jadi, dapat disimpulkan bahwa kecerdasan emosi mempengaruhi kinerja kontekstual guru.
A New Hyper-runaway Star Discovered from LAMOST and Gaia: Ejected Almost in the Galactic Rotation Direction
Authors: Li Yin-Bi , Luo A-Li , Zhao Gang , Lu You-Jun , Zhang Xue-Sen , Zhang Fu-Peng , Du Bing , Zuo Fang , Zhang Lan , Huang Yang , Xiang Mao-Sheng , Zhao Jing-Kun , Zhao Yong-Heng , Han Zhan-Wen 
Published: August 2018

Abstract
In this paper, we report the discovery of a new late-B-type unbound hyper-runaway star (LAMOST-HVS4) from the LAMOST spectroscopic surveys. According to its atmospheric parameters, it is either a B-type main-sequence (MS) star or a blue horizontal branch (BHB) star. Its Galactocentric distance and velocity are 30.3 ± 1.6 kpc and 586 ± 7 km s−1 if it is an MS star, and they are 13.2 ± 3.7 kpc and 590 ± 7 km s−1 if a BHB star. We track its trajectories back and find that the trajectories intersect with the Galactic disk, and the Galactic center lies outside of the intersection region at the 3σ confidence level. We investigate a number of mechanisms that could be responsible for the ejection of the star and find that it is probably ejected from the Galactic disk by supernova explosion or multiple-body interactions in dense young stellar clusters.
Zodiacal Light Beyond Earth Orbit Observed with Pioneer 10
Authors: Matsumoto T. , Tsumura K. , Matsuoka Y. , Pyo J. 
Published: August 2018

Abstract
We reanalyze the Imaging Photopolarimeter data from Pioneer 10 to study the zodiacal light in the B and R bands beyond Earth orbit, applying an improved method to subtract integrated star light (ISL) and diffuse Galactic light (DGL). We found that there exists a significant instrumental offset, making it difficult to examine the absolute sky brightness. Instead, we analyzed the differential brightness, i.e., the difference in sky brightness from the average at high ecliptic latitude, and compared with that expected from the model zodiacal light. At a heliocentric distance of r < 2 au, we found a fairly good correlation between the J-band model zodiacal light and the residual sky brightness after subtracting the ISL and DGL. The reflectances of the interplanetary dust derived from the correlation study are marginally consistent with previous works. The zodiacal light is not significantly detectable at r > 3 au, as previously reported. However, a clear discrepancy from the model is found at r = 2.94 au which indicates the existence of a local dust cloud produced by the collision of asteroids or dust trail from active asteroids (or main-belt comets). Our result confirms that the main component of the zodiacal light (smooth cloud) is consistent with the model even beyond the earth orbit, which justifies the detection of the extragalactic background light after subtracting the zodiacal light based on the model.
Visual Orbit and Individual Masses of the Single-lined Spectroscopic Binary 94 AQR A (HD 219834A; MCA 74)
Authors: Docobo José A. , Tamazian Vakhtang S. , Campo Pedro P. , Piccotti Luca 
Published: August 2018

Abstract
By combining our improved visual orbit with the last spectroscopic solution of the single-lined spectroscopic binary, MCA 74 (ADS 16672Aa, Ab; HD 219834A), we derived its orbital solution to have a period of 6.321 years. Using the Gaia parallax, a systemic mass of 1.87 ± 0.09

and a mass ratio of q = 0.725 were obtained, which yielded individual masses of 1.07 ± 0.06

and 0.80 ± 0.04

for the main and the secondary components, respectively. The mass and the absolute magnitude of +3.52 confirm that the primary is a late G5–G8 subgiant, while the same parameters of the secondary (Mv = +6.52) suggest that it is an early K2–K3 dwarf.
The APOGEE-2 Survey of the Orion Star-forming Complex. II. Six-dimensional Structure
Authors: Kounkel Marina , Covey Kevin , Suárez Genaro , Román-Zúñiga Carlos , Hernandez Jesus , Stassun Keivan , Jaehnig Karl O , Feigelson Eric D. , Ramírez Karla Peña , Roman-Lopes Alexandre , Rio Nicola Da , Stringfellow Guy S , Kim J. Serena , Borissova Jura , Fernández-Trincado José G. , Burgasser Adam , García-Hernández D. A. , Zamora Olga , Pan Kaike , Nitschelm Christian 
Published: August 2018

Abstract
We present an analysis of spectroscopic and astrometric data from APOGEE-2 and Gaia DR2 to identify structures toward the Orion Complex. By applying a hierarchical clustering algorithm to the six-dimensional stellar data, we identify spatially and/or kinematically distinct groups of young stellar objects with ages ranging from 1 to 12 Myr. We also investigate the star-forming history within the Orion Complex and identify peculiar subclusters. With this method we reconstruct the older populations in the regions that are currently largely devoid of molecular gas, such as Orion C (which includes the σ Ori cluster) and Orion D (the population that traces Ori OB1a, OB1b, and Orion X). We report on the distances, kinematics, and ages of the groups within the Complex. The Orion D group is in the process of expanding. On the other hand, Orion B is still in the process of contraction. In λ Ori the proper motions are consistent with a radial expansion due to an explosion from a supernova; the traceback age from the expansion exceeds the age of the youngest stars formed near the outer edges of the region, and their formation would have been triggered when they were halfway from the cluster center to their current positions. We also present a comparison between the parallax and proper-motion solutions obtained by Gaia DR2 and those obtained toward star-forming regions by the Very Long Baseline Array.
Cool-core Clusters: The Role of BCG, Star Formation, and AGN-driven Turbulence
Authors: Prasad Deovrat , Sharma Prateek , Babul Arif 
Published: August 2018

Abstract
Recent observations of cool cluster cores that include the BCG gravity claim that the observed threshold in min(t
cool/t
ff) (cooling time to free-fall time ratio) lies at a somewhat higher value, close to 10–30, compared with the threshold seen in numerical simulations. There are only a few clusters in which this ratio falls much below 10. In this paper, we compare 3D hydrodynamic simulations of feedback active galactic nuclei (AGNs) jets interacting with the intracluster medium, with and without a BCG potential. We find that, for a fixed feedback efficiency, the presence of a BCG does not significantly affect the temperature, but increases (decreases) the core density (entropy) on average. Most importantly, min(t
cool/t
ff) is only affected slightly by the inclusion of the BCG gravity. Also notable is that the lowest value of min(t
cool/t
ff) in the NFW+BCG runs is about twice as large as in the NFW runs. We also look at the role of depletion of cold gas due to star formation, and show that it only affects the rotationally dominant component, while the radially dominant component remains largely unaffected. Stellar gas depletion also increases the repetition rate of AGN jets. The distribution of metals due to AGN jets in our simulations is predominantly along the jet direction, and the equatorial spread of metals is less compared with the observations. We also show that the turbulence in cool-core clusters is weak, which is consistent with recent Hitomi results on the Perseus cluster.
An ALMA Survey of Faint Disks in the Chamaeleon I Star-forming Region: Why Are Some Class II Disks so Faint?
Authors: Long 龙 Feng 凤 , Herczeg 沈雷 Gregory J. 歌 , Pascucci Ilaria , Apai Dániel , Henning Thomas , Manara Carlo F. , Mulders Gijs D. , Szűcs László. , Hendler Nathanial P. 
Published: August 2018

Abstract
ALMA surveys of nearby star-forming regions have shown that the dust mass in the disk is correlated with the stellar mass, but with a large scatter. This scatter could indicate either different evolutionary paths of disks or different initial conditions within a single cluster. We present ALMA Cycle 3 follow-up observations for 14 Class II disks that were low signal-to-noise (S/N) detections or non-detections in our Cycle 2 survey of the ∼2 Myr old Chamaeleon I star-forming region. With five times better sensitivity, we detect millimeter dust continuum emission from six more sources and increase the detection rate to 94% (51/54) for Chamaeleon I disks around stars earlier than M3. The stellar-disk mass scaling relation reported in Pascucci et al. is confirmed with these updated measurements. Faint outliers in the F
mm–M
* plane include three non-detections (CHXR71, CHXR30A, and T54) with dust mass upper limits of 0.2 M
⊕ and three very faint disks (CHXR20, ISO91, and T51) with dust masses ∼0.5 M
⊕. By investigating the SED morphology, accretion property and stellar multiplicity, we suggest for the three millimeter non-detections that tidal interaction by a close companion (≲100 au) and internal photoevaporation may play a role in hastening the overall disk evolution. The presence of a disk around only the secondary star in a binary system may explain the observed stellar SEDs and low disk masses for some systems.
Magnetic Suppression of Zonal Flows on a Beta Plane
Authors: Constantinou Navid C. , Parker Jeffrey B. 
Published: August 2018

Abstract
Zonal flows in rotating systems have been previously shown to be suppressed by the imposition of a background magnetic field aligned with the direction of rotation. Understanding the physics behind the suppression may be important in systems found in astrophysical fluid dynamics, such as stellar interiors. However, the mechanism of suppression has not yet been explained. In the idealized setting of a magnetized beta plane, we provide a theoretical explanation that shows how magnetic fluctuations directly counteract the growth of weak zonal flows. Two distinct calculations yield consistent conclusions. The first, which is simpler and more physically transparent, extends the Kelvin–Orr shearing wave to include magnetic fields and shows that a weak, long-wavelength shear flow organizes magnetic fluctuations to absorb energy from the mean flow. The second calculation, based on the quasilinear, statistical CE2 framework, is valid for arbitrary wavelength zonal flow and predicts a self-consistent growth rate of the zonal flow. We find that a background magnetic field suppresses zonal flow if the bare Alfvén frequency is comparable to or larger than the bare Rossby frequency. However, suppression can occur for even smaller magnetic fields if the resistivity is sufficiently small enough to allow sizable magnetic fluctuations. Our calculations reproduce the

scaling that describes the boundary of zonation, as found in previous work, and we explicitly link this scaling to the amplitude of magnetic fluctuations.
ALMA Observations of Supernova Remnant N49 in the LMC. I. Discovery of CO Clumps Associated with X-Ray and Radio Continuum Shells
Authors: Yamane Y. , Sano H. , van Loon J. Th. , Filipović M. D. , Fujii K. , Tokuda K. , Tsuge K. , Nagaya T. , Yoshiike S. , Grieve K. , Voisin F. , Rowell G. , Indebetouw R. , Lakićević M. , Temim T. , Staveley-Smith L. , Rho J. , Long K. S. , Park S. , Seok J. , Mizuno N. , Kawamura A. , Onishi T. , Inoue T. , Inutsuka S. , Tachihara K. , Fukui Y. 
Published: August 2018

Abstract
N49 (LHA 120-N49) is a bright X-ray supernova remnant (SNR) in the Large Magellanic Cloud. We present new 12CO (J = 1–0, 3–2), H i, and 1.4 GHz radio continuum observations of the SNR N49 using Mopra, ASTE, ALMA, and ATCA. We have newly identified three H i clouds using ATCA with an angular resolution of ∼20″: one associated with the SNR and the others located in front of the SNR. Both the CO and H i clouds in the velocity range from 281 to 291 km s−1 are spatially correlated with both the soft X-rays (0.2–1.2 keV) and the hard X-rays (2.0–7.0 keV) of N49 on a ∼10 pc scale. CO 3–2/1–0 intensity ratios indicate higher values of the CO cloud toward the SNR shell with an angular resolution of ∼45″, and thus a strong interaction was suggested. Using the ALMA, we have spatially resolved CO clumps embedded within or along the southeastern rim of N49 with an angular resolution of ∼3″. Three of the CO clumps are rim brightened on a 0.7–2 pc scale in both hard X-rays and the radio continuum: this provides further evidence for dynamical interactions between the CO clumps and the SNR shock wave. The enhancement of the radio synchrotron radiation can be understood in terms of magnetic field amplification around the CO clumps via a shock–cloud interaction. We also present a possible scenario in which the recombining plasma that dominates the hard X-rays from N49 was formed via thermal conduction between the SNR shock waves and the cold/dense molecular clumps.
Super-Eddington Winds from Type I X-Ray Bursts
Authors: Yu Hang , Weinberg Nevin N. 
Published: August 2018

Abstract
We present hydrodynamic simulations of spherically symmetric super-Eddington winds from radius-expansion type I X-ray bursts. Previous studies assumed a steady-state wind and treated the mass-loss rate as a free parameter. Using MESA, we follow the multi-zone time-dependent burning, the convective and radiative heating of the atmosphere during the burst rise, and the launch and evolution of the optically thick radiation-driven wind as the photosphere expands outward to radii r
ph ≳ 100 km. We focus on neutron stars (NSs) accreting pure helium and study bursts over a range of ignition depths. We find that the wind ejects ≈0.2% of the accreted layer, nearly independent of ignition depth. This implies that ≈30% of the nuclear energy release is used to unbind matter from the NS surface. We show that ashes of nuclear burning are ejected in the wind and dominate the wind composition for bursts that ignite at column depths ≳109 g cm−2. The ejecta are composed primarily of elements with mass numbers A > 40, which we find should imprint photoionization edges on the burst spectra. Evidence of heavy-element edges has been reported in the spectra of strong radius-expansion bursts. We find that after ≈1 s, the wind composition transitions from mostly light elements (4He and 12C), which sit at the top of the atmosphere, to mostly heavy elements (A > 40), which sit deeper down. This may explain why the photospheric radii of all superexpansion bursts show a transition after ≈1 s from a superexpansion (

) to a moderate expansion (

).
Offsets of Masers with Respect to the Middle of the Perseus Arm and the Corotation Radius in the Milky Way
Authors: Vallée Jacques P. 
Published: August 2018

Abstract
The radial distance to the corotation radius

R

coro

(where the angular speed of the gas and stars,

Ω

gas

, in orbit around the Galactic center (GC) is equal to the angular speed of the spiral arm pattern,

Ω

sp

) has often been predicted (at various places), but not measured with high precision. Here we test the locations of masers with respect to the Perseus arm (Table 1). Our analysis of the masers and H ii regions near the Perseus arm (mostly located on the inner arm side, by about 0.4 ± 0.1 kpc from the cold CO mid-arm) shows that the corotation

R

coro

must be >10.8 kpc from the GC (Figure 1). This implies that the angular rotation speed of the spiral pattern

Ω

sp

< 21.3 km s−1 kpc−1. Another test in Galactic quadrant II shows that the radial velocity of the masers is generally more negative than that of the CO mid-arm (Figure 2), indicating a deceleration with respect to the CO mid-arm, by about 9 ± 3 km s−1. This implies that

Ω

sp

< 20.7 km s−1 kpc−1, and thus

R

coro

> 11.1 kpc. Finally, comparing our results with other published results (Table 2), we find a statistical mean corotation radius

R

coro

predicted to be near 12 ± 1 kpc from the GC (beyond the Perseus arm; before the Cygnus arm), and a mean angular spiral pattern speed,

Ω

sp

, predicted to be near 19 ± 2 km s−1 kpc−1.
The CHIME Fast Radio Burst Project: System Overview
Authors:   The CHIME/FRB Collaboration, Amiri M. , Bandura K. , Berger P. , Bhardwaj M. , Boyce M. M. , Boyle P. J. , Brar C. , Burhanpurkar M. , Chawla P. , Chowdhury J. , Cliche J.-F. , Cranmer M. D. , Cubranic D. , Deng M. , Denman N. , Dobbs M. , Fandino M. , Fonseca E. , Gaensler B. M. , Giri U. , Gilbert A. J. , Good D. C. , Guliani S. , Halpern M. , Hinshaw G. , Höfer C. , Josephy A. , Kaspi V. M. , Landecker T. L. , Lang D. , Liao H. , Masui K. W. , Mena-Parra J. , Naidu A. , Newburgh L. B. , Ng C. , Patel C. , Pen U.-L. , Pinsonneault-Marotte T. , Pleunis Z. , Ravandi M. Rafiei , Ransom S. M. , Renard A. , Scholz P. , Sigurdson K. , Siegel S. R. , Smith K. M. , Stairs I. H. , Tendulkar S. P. , Vanderlinde K. , Wiebe D. V. 
Published: August 2018

Abstract
The Canadian Hydrogen Intensity Mapping Experiment (CHIME) is a novel transit radio telescope operating across the 400–800 MHz band. CHIME is composed of four 20 m × 100 m semicylindrical paraboloid reflectors, each of which has 256 dual-polarization feeds suspended along its axis, giving it a ≳200 deg2 field of view. This, combined with wide bandwidth, high sensitivity, and a powerful correlator, makes CHIME an excellent instrument for the detection of fast radio bursts (FRBs). The CHIME Fast Radio Burst Project (CHIME/FRB) will search beam-formed, high time and frequency resolution data in real time for FRBs in the CHIME field of view. Here we describe the CHIME/FRB back end, including the real-time FRB search and detection software pipeline, as well as the planned offline analyses. We estimate a CHIME/FRB detection rate of 2–42 FRBs sky–1 day–1 normalizing to the rate estimated at 1.4 GHz by Vander Wiel et al. Likely science outcomes of CHIME/FRB are also discussed. CHIME/FRB is currently operational in a commissioning phase, with science operations expected to commence in the latter half of 2018.
L’opinion publique au fondement du droit de punir : fragments d’une nouvelle théorie de la peine ?
Authors: Dubé Richard , Garcia Margarida 
Published: August 2018

Cet article porte sur les références à la notion d’opinion publique dans les débats parlementaires canadiens visant l’adoption de lois pénales plus sévères. La confiance du public dans l’administration de la justice est alors au cœur des préoccupations législatives et engendre une stratégie de « séduction » qui va jusqu’à loger au second rang l’objectif de la protection de la société. Cette stratégie parait s’appuyer sur des fondements du droit de punir différents de ceux auxquels les théories de la peine de la « rationalité pénale moderne » de Pires (1998, 2001) avaient pu nous habituer depuis le milieu du XVIII e siècle. Nous y voyons, au cœur même de cette rationalité pénale, l’émergence d’une théorie de l’approbation publique et de nouveaux obstacles à l’évolution du droit criminel moderne.
Sociabilité carcérale et réinsertion
Authors: François Axelle , Nolet Anne-Marie , Morselli Carlo 
Published: August 2018

Prenant appui sur les recherches actuelles dans le traitement de la délinquance et mobilisant l’analyse des réseaux sociaux, cet article interroge l’influence de la sociabilité carcérale sur les perceptions individuelles à l’égard de la réinsertion. Les résultats d’une enquête menée auprès de 22 résidents d’une maison de transition située à Montréal suggèrent que plus le niveau de sociabilité carcérale est élevé, plus les résidents ont une vision négative de leur réinsertion, et inversement. En cohérence avec le phénomène général d’institutionnalisation, ce résultat et l’étude dans son ensemble autorisent la réflexion quant aux interventions conduites auprès de personnes contrevenantes.