bluuebunny/crossref_metadata_2025_split huggingface dataset:
PENGARUH ENTREPRENEURSHIP, BUSINESS COACHING, MENTORING DAN KOMUNITAS KREATIF TERHADAP KINERJA INDUSTRI KREATIF
Authors: Anjaningrum Widiya Dewi , Sapoetra Yudistira Arya 
Published: October 2018

This study aims to determine the influence of entrepreneurship, business coaching, mentoring and creative communities both simultaneously and partially to the creative industries performance. Entrepreneurship is reflected by the instrumental, prestigious, sociable, takeover, self-sufficiency, hard work, self-confidence, innovative, leadership, action oriented, simple thinking and focus on effort. While business coaching and mentoring is reflected by the forms of training and coaching activities provided by the government and others, the frequency of training and coaching, the duration of assessment and implementation. While the creative community is measured on four aspects, that are, the nature, membership, way of working and relationships with other communities. Performance is indicated by customer growth rate, customer satisfaction level, customer satisfaction level, number of new products, level of job satisfaction and productivity level. Collecting data is done through direct survey to the research object, the creative industry actors who are members of MCF (Malang Creative Fusion). The results show that entrepreneurship, business coaching, mentoring and creative community have simultaneously influence to the creative industries performance. Also, that four independent variables, partially, has positive significant influence to the creative industries
performance. So, in order to achieve optimal creative industry performance, it is expected that entrepreneurship in each creative industry actors, collaboration and synergy of quadruple helix are improved.
PENGARUH KUALITAS PRODUK, KUALITAS PELAYANAN DAN DIGITAL MARKETING TERHADAP LOYALITAS PELANGGAN
Authors: Sidi Agus Purnomo 
Published: October 2018

This research is a kind of field research, case study on Kedai Hj.S Jl.Kesumba Malang Town customers that aims to know how the influence of product quality, service quality and digital marketing to customer loyalty. The data were taken directly from the respondents through a questionnaire survey with Likert scale by random sampling to as many as 80 respondents. The results of data analysis using SPSS 23 software shows that both product quality, service quality and digital marketing have a significant effect on customer loyalty. Thus, to increase customer loyalty, it is suggested that Hj.S management to improve the product quality, or at least maintain the product quality, speed up the service processing and increase the social media usage.
STRATEGI PENINGKATAN KINERJA PERUSAHAAN MELALUI PENGELOLAAN SUMBER DAYA MANUSIA DAN KEPUASAN KERJA DAN DAMPAKNYA TERHADAP PRODUKTIVITAS KARYAWAN
Authors: Iskandar Dhany 
Published: October 2018

One of the key issues in a company's success in achieving its vision and mission is the quality of Human Resources (HR). The Objektive of this study is to determine the importance of human resource management strategies and job satisfaction that has an impact the productivity of employees. 1. In this research, we observed the appliedship Human Resources on management of PT Swadharma Sarana Informatika (SSI), PT. Sarana Reswara Abadi (SRA) and PT. Reswara Prima Express (Respex), Based on service target and its operation, 2. In this research, we prepare questionaire for our respondents which will be interviewed and the outcome will be used for the analysis on the achievement in company’s performance is probability the corporate productivity. 3. It can be identified what strategy does the company to achieve its vision and mission. 4. It can be concluded that the quality of human resources need to be improved the target on the company's performance from the point of the current performance.
An Optical Study of Two VY Sculptoris-type Cataclysmic Binary Stars: V704 And and RX J2338+431
Authors: Weil Kathryn E. , Thorstensen John R. , Haberl Frank 
Published: October 2018

Abstract
We report observations of the known cataclysmic variable star (CV) V704 And, and also confirm that the optical counterpart of the ROSAT Galactic Plane Survey source RX J2338+431 is a heretofore-neglected CV. Photometric and spectroscopic observations from MDM Observatory show both systems to be nova-like variables that exhibit dips of 4–5 mag from their mean brightnesses, establishing them as members of the VY Scl subclass. From high-state emission-line radial velocities, we determine orbital periods of 0.151424(3) days (3.63 hr) for V704 And and 0.130400 (1) days (3.13 hr) for RX J2338+431. In V704 And, we find that the Hα emission-line measures cluster into distinct regions on a plot of equivalent width versus full width at half-maximum, which evidently correspond to high, intermediate, and low photometric states. This allows us to assign spectra to photometric states when contemporaneous photometry is not available, an apparently novel method that may be useful in studies of other novalikes. Our low-state spectra of RX J2338+431 show features of an M-type secondary star, from which we estimate a distance of 890 ± 200 pc, in good agreement with the Gaia DR2 parallax.
The VLA/ALMA Nascent Disk and Multiplicity (VANDAM) Survey of Perseus Protostars. VI. Characterizing the Formation Mechanism for Close Multiple Systems
Authors: Tobin John J. , Looney Leslie W. , Li Zhi-Yun , Sadavoy Sarah I. , Dunham Michael M. , Segura-Cox Dominique , Kratter Kaitlin , Chandler Claire J. , Melis Carl , Harris Robert J. , Perez Laura 
Published: October 2018

Abstract
We present Atacama Large Millimeter/submillimeter Array observations of multiple protostar systems in the Perseus molecular cloud, previously detected by the Karl G. Jansky Very Large Array. We observe 17 close (<600 au separation) multiple systems at 1.3 mm in continuum and five molecular lines (i.e., 12CO, C18O, 13CO, H2CO, SO) to characterize the circum-multiple environments in which these systems are forming. We detect at least one component in the continuum for the 17 multiple systems. In three systems one companion is not detected, and for two systems the companions are unresolved at our observed resolution. We also detect circum-multiple dust emission toward eight out of nine Class 0 multiples. Circum-multiple dust emission is not detected toward any of the eight Class I multiples. Twelve systems are detected in the dense gas tracers toward their disks/inner envelopes. For these 12 systems, we use the dense gas observations to characterize their formation mechanism. The velocity gradients in the circum-multiple gas are clearly orthogonal to the outflow directions in eight out of the 12 systems, consistent with disk fragmentation. Moreover, only two systems with separations <200 au are inconsistent with disk fragmentation, in addition to the two widest systems (>500 au). Our results suggest that disk fragmentation via gravitational instability is an important formation mechanism for close multiple systems, but further statistics are needed to better determine the relative fraction formed via this method.
Solar Coronal Modeling by Path-conservative HLLEM Riemann Solver
Authors: Li Caixia , Feng Xueshang , Xiang Changqing , Zhang Man , Li Huichao , Wei Fengsi 
Published: October 2018

Abstract
In this paper, we employ a path-conservative HLLEM finite-volume method (FVM) to solve the solar wind magnetohydrodynamics (MHD) systems of extended generalized Lagrange multiplier (EGLM) formulation with Galilean invariance (G-EGLM MHD equations). The governing equations of single-fluid solar wind plasma MHD are advanced by using a one-step MUSCL-type time integration with the logarithmic spacetime reconstruction. The code is programmed in FORTRAN language with Message Passing Interface parallelization in spherical coordinates with a six-component grid system. Then, the large-scale solar coronal structures during Carrington rotations (CRs) 2048, 2069, 2097, and 2121 are simulated by inputting the line-of-sight magnetic field provided by the Global Oscillation Network Group (GONG). These four CRs belong to the declining, minimum, rising, and maximum phases of solar activity. Numerical results basically generate the observed characteristics of structured solar wind and thus show the code’s capability of simulating solar corona with complex magnetic topology.
Evolution of Circumbinary Protoplanetary Disks with Photoevaporative Winds Driven by External Far-ultraviolet Radiation
Authors: Shadmehri M. , Ghoreyshi S. M. , Alipour N. 
Published: October 2018

Abstract
Lifetimes of protoplanetary disks (PPDs) are believed to be severely constrained by material-depleting mechanisms, including photoevaporative winds due to the host star radiation or external radiation sources. Most previous studies focused on exploring the role of the winds in the exposed PPDs with a single star; however, the evolution of the circumbinary disks with the photoevaporative winds driven by the host star radiation and external radiation sources deserves further exploration. In this study, we investigate the evolution of the circumbinary PPDs with the photoevaporative winds induced by the external far-ultraviolet radiation field. We show that this mass-loss process can significantly constrain properties of a circumbinary PPD, including its lifetime, mass, and radius. The lifetime of a circumbinary PPD, for instance, is found to be about a factor of two longer than a similar circumstellar disk, and this enhancement strongly depends on the viscosity parameter. But our model shows that viscosity dependence of the disk lifetime in the circumbinary case is more pronounced compared to the circumstellar case. We also show that dispersal of a circumbinary PPD occurs over a longer time as the disk temperature distribution becomes steeper. Our results also imply that a dead zone in a photoevaporative circumbinary PPD extends over a larger radial range in comparison to a circumstellar disk counterpart. We also show that our calculations are in agreement with the observed circumbinary PPDs orbiting equal-mass binaries.
Direction-finding Analysis of the 2012 July 6 Type II Solar Radio Burst at Low Frequencies
Authors: Mäkelä Pertti , Gopalswamy Nat , Akiyama Sachiko 
Published: October 2018

Abstract
The 2012 July 6 X1.1 flare at S13W59 and a halo coronal mass ejection (CME) with a space speed of ∼1900 km s−1 were associated with type III and type II radio bursts. The metric-to-decametric type II radio burst extended down to ∼5 MHz. Simultaneously, a slowly drifting feature with a harmonic structure was observed by Wind and Solar Terrestrial Relations Observatory radio receivers around and below 1 MHz, above the strong type III radio burst at lower frequencies. The radio direction-finding analysis of this lower-frequency interplanetary (IP) type II radio burst indicates that the radio source was located near the nose and possibly toward the southern flank of the CME-driven shock. These results provide an independent confirmation of the previous suggestions that when the metric and IP type II bursts are overlapping, the lower-frequency IP type II radio burst originates near the shock nose, whereas the source of the higher-frequency metric type II burst is closer to the Sun in the shock flank region. These results further support the idea that the coronal and IP type II bursts are produced by the same CME-driven shock.
Scattered Short Gamma-Ray Bursts as Electromagnetic Counterparts to Gravitational Waves and Implications of GW170817 and GRB 170817A
Authors: Kisaka Shota , Ioka Kunihito , Kashiyama Kazumi , Nakamura Takashi 
Published: October 2018

Abstract
In the faint short gamma-ray burst sGRB 170817A followed by the gravitational waves (GWs) from a merger of two neutron stars (NSs) GW170817, the spectral peak energy is too high to explain only by canonical off-axis emission. We investigate the off-axis appearance of an sGRB prompt emission scattered by a cocoon, which is produced through the jet–merger–ejecta interaction, with either subrelativistic or mildly relativistic velocities. We show that the observed properties of sGRB 170817A, in particular the high peak energy, can be consistently explained by the Thomson-scattered emission with a typical sGRB jet, together with its canonical off-axis emission, supporting that an NS–NS merger is the origin of sGRBs. The scattering occurs at ≲1010–1012 cm not far from the central engine, implying the photospheric or internal shock origin of the sGRB prompt emission. The boundary between the jet and cocoon is sharp, which could be probed by future observations of off-axis afterglows. The scattering model predicts a distribution of the spectral peak energy that is similar to the observed one but with a cutoff around ∼MeV energy and its correlations with the luminosity, duration, and time lag from GWs, providing a way to distinguish it from alternative models.
Stormy Weather in 3C 196.1: Nuclear Outbursts and Merger Events Shape the Environment of the Hybrid Radio Galaxy 3C 196.1
Authors: Ricci F. , Lovisari L. , Kraft R. P. , Massaro F. , Paggi A. , Liuzzo E. , Tremblay G. , Forman W. R. , Baum S. , O’Dea C. , Wilkes B. 
Published: October 2018

Abstract
We present a multiwavelength analysis based on archival radio, optical, and X-ray data of the complex radio source 3C 196.1, whose host is the brightest cluster galaxy of a z = 0.198 cluster. HST data show Hα+[N ii] emission aligned with the jet 8.4 GHz radio emission. An Hα+[N ii] filament coincides with the brightest X-ray emission, the northern hotspot. Analysis of the X-ray and radio images reveals cavities located at galactic and cluster scales. The galactic-scale cavity is almost devoid of 8.4 GHz radio emission and the southwestern Hα+[N ii] emission is bounded (in projection) by this cavity. The outer cavity is cospatial with the peak of 147 MHz radio emission, and hence we interpret this depression in X-ray surface brightness as being caused by a buoyantly rising bubble originating from an active galactic nuclei outburst ∼280 Myr ago. A Chandra snapshot observation allowed us to constrain the physical parameters of the cluster, which has a cool core with a low central temperature ∼2.8 keV, low central entropy index ∼13 keV cm2 and a short cooling time of ∼500 Myr, which is < 0.05 of the age of the universe at this redshift. By fitting jumps in the X-ray density, we found Mach numbers between 1.4 and 1.6, consistent with a shock origin. We also found compelling evidence of a past merger, indicated by a morphology reminiscent of gas sloshing in the X-ray residual image. Finally, we computed the pressures, enthalpies E
cav and jet powers P
jet associated with the cavities: E
cav ∼ 7 × 1058 erg, P
jet ∼ 1.9 × 1044 erg s−1 for the inner cavity and E
cav ∼ 3 × 1060 erg, P
jet ∼ 3.4 × 1044 erg s−1 for the outer cavity.
NGC 6791: A Probable Bulge Cluster without Multiple Populations*
Authors: Villanova Sandro , Carraro Giovanni , Geisler Doug , Monaco Lorenzo , Assmann Paulina 
Published: October 2018

Abstract
NGC 6791 is a unique stellar cluster, key to our understanding of both the multiple stellar population phenomenon and the evolution and assembly of the Galaxy. However, despite many investigations, its nature is still very controversial. Geisler et al. found evidence suggesting that it was the first open cluster to possess multiple populations, but several subsequent studies did not corroborate this. It has also been considered a member of the thin or thick disk or even the bulge, and either as an open or globular cluster or even the remnant of a dwarf galaxy. Here we present and discuss detailed abundances derived from high-resolution spectra obtained with UVES at VLT and HIRES at Keck of 17 evolved stars of this cluster. We obtained a mean [Fe/H] = +0.313 ± 0.005, in good agreement with recent estimates, and with no indication of star-to-star metallicity variation, as expected. We also did not find any variation in Na, in spite of having selected the very same stars as in Geisler et al., where an Na variation was claimed. This points to the presence of probable systematics in the lower-resolution spectra of this very high metallicity cluster analyzed in that work. In fact, we find no evidence for an intrinsic spread in any element, corroborating recent independent APOGEE data. The derived abundances indicate that NGC 6791 very likely formed in the Galactic bulge and that the proposed association with the thick disk is unlikely, despite its present Galactic location. We confirm the most recent hypothesis suggesting that the cluster could have formed in the bulge and radially migrated to its current location, which appears to be the best explanation for this intriguing object.
Early Science with the Large Millimeter Telescope: An Energy-driven Wind Revealed by Massive Molecular and Fast X-Ray Outflows in the Seyfert Galaxy IRAS 17020+4544
Authors: Longinotti A. L. , Vega O. , Krongold Y. , Aretxaga I. , Yun M. , Chavushyan V. , Feruglio C. , Gómez-Ruiz A. , Montaña A. , León-Tavares J. , Olguín-Iglesias A. , Giroletti M. , Guainazzi M. , Kotilainen J. , Panessa F. , Zapata L. A. , Cruz-Gonzalez I. , Patiño-Álvarez V. M. , Rosa-Gonzalez D. , Carramiñana A. , Carrasco L. , Costantini E. , Dultzin D. , Guichard J. , Puerari I. , Santos-Lleo M. 
Published: October 2018

Abstract
We report on the coexistence of powerful gas outflows observed in millimeter and X-ray data of the radio-loud narrow-line Seyfert 1 Galaxy IRAS 17020+4544. Thanks to the large collecting power of the Large Millimeter Telescope (LMT), a prominent line arising from the 12CO(1–0) transition was revealed in recent observations of this source. The complex profile is composed by a narrow double-peak line and a broad wing. While the double-peak structure may be arising in a disk of molecular material, the broad wing is interpreted as the signature of a massive outflow of molecular gas with an approximate bulk velocity of −660 km s−1. This molecular wind is likely associated to a multi-component X-ray ultra-fast outflow with velocities reaching up to ∼ 0.1c and column densities in the range 1021–23.9 cm−2 that was reported in the source prior to the LMT observations. The momentum load estimated in the two gas phases indicates that within the observational uncertainties the outflow is consistent with being propagating through the galaxy and sweeping up the gas while conserving its energy. This scenario, which has been often postulated as a viable mechanism of how active galactic nucleus (AGN) feedback takes place, has so far been observed only in ultraluminous infrared galaxy sources. IRAS 17020+4544 with bolometric and infrared luminosity, respectively, of 5 × 1044 erg s−1 and 1.05 × 1011
L
⊙ appears to be an example of AGN feedback in a NLSy1 Galaxy (a low power AGN). New proprietary multi-wavelength data recently obtained on this source will allow us to corroborate the proposed hypothesis.
ASASSN-18ey: The Rise of a New Black Hole X-Ray Binary
Authors: Tucker M. A. , Shappee B. J. , Holoien T. W.-S. , Auchettl K. , Strader J. , Stanek K. Z. , Kochanek C. S. , Bahramian A. ,   ASAS-SN, Dong Subo , Prieto J. L. , Shields J. , Thompson Todd A. , Beacom John F. , Chomiuk L. ,   ATLAS, Denneau L. , Flewelling H. , Heinze A. N. , Smith K. W. , Stalder B. , Tonry J. L. , Weiland H. , Rest A. , Huber M. E. , Rowan D. M. , Dage K. 
Published: October 2018

Abstract
We present the discovery of ASASSN-18ey (MAXI J1820+070), a new black hole low-mass X-ray binary (LMXB) discovered by the All-Sky Automated Survey for SuperNovae (ASAS-SN). A week after ASAS-SN discovered ASASSN-18ey as an optical transient, it was detected as an X-ray transient by MAXI/GCS. Here, we analyze ASAS-SN and Asteroid Terrestrial-impact Last Alert System pre-outburst optical light curves, finding evidence of intrinsic variability for several years prior to the outburst. While there was no long-term rise leading to the outburst, as has been seen in several other systems, the start of the outburst in the optical preceded that in the X-rays by 7.20 ± 0.97 days. We analyze the spectroscopic evolution of ASASSN-18ey from pre-maximum to >100 days post-maximum. The spectra of ASASSN-18ey exhibit broad, asymmetric, double-peaked Hα emission. The Bowen blend (λ ≈ 4650 Å) in the post-maximum spectra shows highly variable double-peaked profiles, likely arising from irradiation of the companion by the accretion disk, typical of low-mass X-ray binaries. The optical and X-ray luminosities of ASASSN-18ey are consistent with black hole low-mass X-ray binaries, both in outburst and quiescence.
Multiple intelligences and video games: Assessment and intervention with TOI software
Authors: Garmen Pablo , Rodríguez Celestino , García-Redondo Patricia , San-Pedro-Veledo Juan-Carlos 
Published: October 2018

Howard Gardner revolutionized the concept of intelligence with his Multiple Intelligences Theory. His vision was widely supported by the educational community, which considers different forms of learning and accessing knowledge. Despite its impact, there is still a lack of development of tools that can easily, practically and reliably evaluate multiple intelligences. This work describes the design, development, and piloting of TOI (Tree of Intelligences) software, a digital tool to evaluate multiple intelligences and perform interventions through video games. The aim of the study is to present the design of the TOI software and test its operation, analysing the distribution of the results game by game and checking whether there are differences according to gender or school year. A total of 372 primary school students participated, aged 5 to 9 years old (M=7.04, SD=.871), from three schools in Asturias and Madrid. The results show that 9 out of 10 games had a normal distribution and that there were no gender differences in most games, but there were differences in relation to the school year. We concluded that due to its operation and design TOI software has the potential be a suitable instrument for the evaluation and intervention of multiple intelligences.
Howard Gardner revolucionó el concepto de inteligencia con su Teoría de las Inteligencias Múltiples. Su visión fue acogida por la comunidad educativa como la oportunidad para una educación más personalizada y que atienda las diferentes formas de aprender y acceder al conocimiento. A pesar de su impacto, todavía hoy hay una carencia en cuanto al desarrollo de herramientas capaces de evaluar de forma sencilla, práctica y fiable las inteligencias múltiples. Por ello, este trabajo plantea el diseño, desarrollo y pilotaje del software TOI, del inglés ‘Tree of Intelligences’, una herramienta digital para evaluar e intervenir las inteligencias múltiples a través de los videojuegos. El objetivo del estudio es presentar el diseño de TOI y testar su funcionamiento, analizando la distribución de los resultados juego a juego y comprobando si existen diferencias en función del género y el curso. Participaron un total de 372 estudiantes de primero a tercer curso de educación primaria de tres centros de Asturias y Madrid, con edades comprendidas entre 5 y 9 años (M=7.04, DT=.871). Los resultados muestran que 9 de 10 juegos presentan una distribución normal y que no existen diferencias en función del género en la mayoría de los juegos, pero sí en relación al curso. Se concluye que por su funcionamiento y diseño el software TOI puede ser un adecuado instrumento de evaluación e intervención de las inteligencias múltiples.