bluuebunny/crossref_metadata_2025_split huggingface dataset:
KONSEP TANGGUNG JAWAB EMMANUEL LEVINAS DAN IMPLIKASINYA BAGI KEBERAGAMAAN INDONESIA
Authors: Doren Kamilus Pati 
Published: February 2019

ABSTRACT: "Am I my brother's guard?" This question becomes a reflection of individuals as social being who meet with other people every day in their differences. This question inspires the conscience of each person to take the right attitude when dealing with others. And the attitude referred to here is responsibility in the concept of levinas, which is different from everyday understanding. This thought was then tried to collide with diversity in Indonesia, especially the attitude of religious people when dealing with adherents of other religions. so that the moment of meeting with others truly becomes an ethical moment towards meeting, based on this attitude of responsibility. Based on library data, the author tries to describe the concept of levinas responsibility so that ultimately every difference can be seen as a gift and shared wealth. Through reflection on the unique concept of the responsibility of levinas, the authors put it as a foundation for the relations of religious life and Indonesian society, which often experience clashes due to pluralistic reasons. It is very appropriate, if Levinas's responsibilities are implied into the lives of our people because also the essence of Levinas's thinking actually has a strong foundation in our country's philosophy.Â KEYWORDS:Â responsibility, plurality, religion, others, le visage, meetingÂ Â
Pendidikan Karakter pada Anak Usia Dini
Authors: Sinaga Rida 
Published: February 2019

ABSTRACT: This article entitled â€œCharacter Education at Early Childhoodâ€ focuses on character education which is done in Bina Kasih Kindergarten at Rumah Sumbul Village, Sibolangit. This research used qualitative method and the data was gathered by direct observation, interview, and survey. Data analysis used triangular model with various data sources and various data gathering method. The characters which were going to be observed at the children out from this education in Bina Kasih Kindergarten were responsibility, discipline, sociability, autonomy, trustworthy, cooperative, God-loving, sense of respect, sympathy and empathy, confidence, cleanliness and healthiness, as well as competence. This research found that character education at early childhood produces character transformation at children and therefore character education at school needs to be done since early childhood.Â KEYWORDS: education, character transformation, early childhood.Â Â
Rekomendasi Praktis untuk Rekonsiliasi
Authors: Putra Andreas Maurenis 
Published: February 2019

ABSTRACT: Today, humans are always faced with the complexity of the acute world situation. This situation is nothing but an increasingly worsening environmental crisis. This emergency situation is inseparable from the increasingly exalted anthropocentric ego. The assumption that eliminates intrinsic value to other ecosystems and the wrong way of life leads to the separation of relations between humans and the surrounding reality.The interdependent context between all ecosystems is degraded due to the wrong attitude of life from humans. The loss of the relationship brought a variety of environmental damage which caused the destruction of human existence itself. Poverty, hunger, war, global warming, floods and drought are a few of the critical phenomena of nature. For these increasingly emergency natural phenomena, this thesis is written as a critical reflection for humans to re-examine their nature as religious, social and ecological creatures as well as concrete action that must be done to reconstruct relations (reconciliation) with nature, with the surrounding environment and especially reconciliation with his own life through ecological metanoia and a new lifestyle.Â KEYWORDS: relation, antrophosentrism ego, ecological exigent, multidimensional perspective, awareness, reconciliation, repentance and new lifestyle.
Col-OSSOS: Color and Inclination Are Correlated throughout the Kuiper Belt
Authors: Marsset Michaël , Fraser Wesley C. , Pike Rosemary E. , Bannister Michele T. , Schwamb Megan E. , Volk Kathryn , Kavelaars J. J. , Alexandersen Mike , Chen Ying-Tung , Gladman Brett J. , Gwyn Stephen D. J. , Lehner Matthew J. , Peixinho Nuno , Petit Jean-Marc , Wang Shiang-Yu 
Published: February 2019

Abstract
Both physical and dynamical properties must be considered to constrain the origins of the dynamically excited distant solar system populations. We present high-precision (g–r) colors for 25 small (H
r > 5) dynamically excited trans-Neptunian objects (TNOs) and centaurs acquired as part of the Colours of the Outer Solar System Origins Survey. We combine our data set with previously published measurements and consider a set of 229 colors of outer solar system objects on dynamically excited orbits. The overall color distribution is bimodal and can be decomposed into two distinct classes, termed gray and red, that each has a normal color distribution. The two color classes have different inclination distributions: red objects have lower inclinations than the gray ones. This trend holds for all dynamically excited TNO populations. Even in the worst-case scenario, biases in the discovery surveys cannot account for this trend; it is intrinsic to the TNO population. Considering that TNOs are the precursors of centaurs, and that their inclinations are roughly preserved as they become centaurs, our finding solves the conundrum of centaurs being the only outer solar system population identified so far to exhibit this property. The different orbital distributions of the gray and red dynamically excited TNOs provide strong evidence that their colors are due to different formation locations in a disk of planetesimals with a compositional gradient.
Discovery of a Damped Lyα System in a Low-z Galaxy Group: Possible Evidence for Gas Inflow and Nuclear Star Formation
Authors: Borthakur Sanchayeeta , Momjian Emmanuel , Heckman Timothy M. , Catinella Barbara , Vogt Frédéric P. A. , Tumlinson Jason 
Published: February 2019

Abstract
We present a low-redshift (z = 0.029) damped Lyα (DLA) system in the spectrum of a background quasi-stellar object (QSO). The DLA is associated with an interacting galaxy pair within a galaxy group. We detected weak Lyα emission centered at the absorption trough of the DLA. The emission was likely tracing the neutral H i reservoir around the galaxies in the interacting pair, which scattered the Lyα generated by star formation within those galaxies. We also found that the interacting pair is enveloped by a large H i cloud with

M
(
H

I
)
=
2
×

10

10

M

⊙

. We discovered blueshifted 21 cm H i emission, corresponding to M(H i) =

2
×

10

9

M

⊙

, associated with J151225.15+012950.4—one of the galaxies in the interacting pair. The blueshifted H i was tracing gas flowing into the galaxy from behind and toward us. Gas at similar blueshifted velocities was seen in the QSO sight line, thus suggesting the presence of a filamentary structure of the order of 100 kpc feeding the galaxy. We estimated a mass inflow rate of

2

M

⊙

yr

−
1

into the galaxy, which matches the star formation rate estimated from Hα emission. It is likely that the inflow of enormous amounts of gas has triggered star formation in this galaxy. The sudden acquisition of cold gas may lead to a starburst in this galaxy like those commonly seen in simulations.
Optical Flux and Spectral Variability of the TeV Blazar PG 1553+113
Authors: Pandey Ashwani , Gupta Alok C. , Wiita Paul J. , Tiwari S. N. 
Published: January 2019

Abstract
We present the results of our optical (VRI) observations of the TeV blazar PG 1553+113 over eight nights in 2016 April. We monitored the blazar quasi-simultaneously in V and R bands each night and examined the light curves (LCs) for intraday flux and color variations using two of the most powerful tests: the power-enhanced F-test and the nested ANOVA test. The source was found to be significantly (>99%) variable in both V and R bands only on April 13, while clear variations only in R band LCs were seen on April 8 and 12. No temporal variation was seen in the color during the observation period. We did not find any significant correlation between V − R color index and R magnitude on any observing night. We found a mean optical spectral index of ∼0.83 ± 0.02 with a maximum variation of 0.21 by fitting a power law (F

ν
∝ ν
−α
) in the optical (VRI) spectral energy distribution of PG 1553+113. We briefly discuss the possible physical processes responsible for the observed flux and spectral variability.
Quantifying Star Formation Activity in the Inner 1 kpc of Local MIR Bright QSOs
Authors: Martínez-Paredes M. , Aretxaga I. , González-Martín O. , Alonso-Herrero A. , Levenson N. A. , Ramos Almeida C. , López-Rodríguez E. 
Published: January 2019

Abstract
We examine star formation activity in a distant (z < 0.1) and flux-limited sample of quasars (QSOs). Midinfrared (MIR) spectral diagnostics at high spatial resolution (∼0.4 arcsec) yield star formation rates (SFRs) in the inner regions (∼300 pc–1 kpc) for 13 of 20 of the sample members. We group these objects according to the size probed by the high angular resolution spectroscopy, with characteristic scales of <0.7 and ∼0.7–1 kpc. Using the polycyclic aromatic hydrocarbon (PAH) feature at 11.3 μm, we measure SFRs around 0.2 and 1.6 M
⊙ yr−1. We also measure the larger aperture PAH-derived SFRs in the individual IRS/Spitzer spectra of the sample and obtain a clear detection in ∼58% of them. We compare smaller and larger aperture measurements and find that they are similar, suggesting that star formation activity in these QSOs is more centrally concentrated, with the inner region (≲1 kpc) accounting for the majority of star formation measured on these scales, and that PAH molecules can be present in most local MIR-bright QSOs within a few hundred parsecs from the central engine. By comparison with merger simulations, we find that our estimation of the SFR and black hole (BH) accretion rates are consistent with a scenario in which the star formation activity is centrally peaked as predicted by simulations.
What is a Macrospicule?
Authors: Loboda Ivan P. , Bogachev Sergej A. 
Published: February 2019

Abstract
Macrospicules are typically described as solar jets that are larger and more long-lived than spicules, and visible mostly in transition-region spectral lines. They show a broad variation in properties, which pose substantial difficulties for their identification, modeling, and the understanding of their role in the mass and energy balance of the solar atmosphere. In this study, we focused on a subpopulation of these jets that follow parabolic trajectories when observed in the He ii 304 Å line using high-cadence observations of the Atmospheric Imaging Assembly on board the Solar Dynamics Observatory to accumulate a statistically significant sample, which included 330 such events. We found these jets to be typically narrow (3–6 Mm), collimated flows of plasma, which reach heights of about 25 Mm, thus being among the smallest jets observed in the extreme ultraviolet (EUV). Combined with the rise velocities of 70–140 km s−1 and lifetimes of around 15 minutes, this makes them plausible candidates for the EUV counterpart of type II spicules. Moreover, we have found their dynamics to be inconsistent with a purely ballistic motion; instead, there is a strong correlation between the initial velocities and decelerations of the jets, which indicates that they may be driven by magnetoacoustic shocks with a dominant period of 10 ± 2 minutes. This makes these EUV jets similar in their dynamics to conventional, or type I, spicules, thus justifying the name of macro-spicules in this case, while a substantial difference in the shock periods (1–2 minutes for the chromospheric jets) suggests a dissimilarity in the formation conditions.
Untwisting and Disintegration of a Solar Filament Associated with Photospheric Flux Cancellation
Authors: Chen Huadong , Zheng Ruisheng , Li Leping , Ma Suli , Bi Yi , Yang Shuhong 
Published: February 2019

Abstract
Using the high-resolution observations from the New Vacuum Solar Telescope (NVST) jointly with the Solar Dynamics Observatory data, we investigate two successive confined eruptions (Erup1 and Erup2) of a small filament in a decaying active region on 2017 November 10. During the process of Erup1, the overlying magnetic arcade is observed to inflate with the rising filament at the beginning and then stop during the explosion. In the hot EUV channel, a coronal sigmoidal structure appears during the first eruption and fades away after the second one. The untwisting rotation and disintegration of the filament in Erup2 are clearly revealed by the NVST Hα intensity data, hinting at a pre-existing twisted configuration for the filament. By tracking two rotating features in the filament, the average rotational angular velocity of the unwinding filament is found to be ∼10.°5 min−1. A total twist of ∼1.3π is estimated to be stored in the filament before the eruption, which is far below the criteria for kink instability. Several hours prior to the event, some photospheric flux activities, including the flux convergence and cancellation, are detected around the northern end of the filament, where some small-scale EUV brightenings are also captured. Moreover, strongly sheared transverse fields are found in the canceling magnetic features from the vector magnetograms. Our observational results support the flux cancellation model, in which the interaction between the converging and sheared opposite-polarity fluxes destabilizes the filament and triggers the ensuing ejection.
The Temporal Requirements of Directly Observing Self-gravitating Spiral Waves in Protoplanetary Disks with ALMA
Authors: Hall Cassandra , Dong Ruobing , Rice Ken , Harries Tim J. , Najita Joan , Alexander Richard , Brittain Sean 
Published: February 2019

Abstract
We investigate how the detectability of signatures of self-gravity in a protoplanetary disk depends on its temporal evolution. We run a one-dimensional model for secular timescales to follow the disk mass as a function of time. We then combine this with three-dimensional global hydrodynamics simulations that employ a hybrid radiative transfer method to approximate realistic heating and cooling. We simulate ALMA continuum observations of these systems and find that structures induced by the gravitational instability (GI) are readily detectable when q = M
disk/M
* ≳ 0.25 and R
outer ≲ 100 au. The high accretion rate generated by gravito-turbulence in such a massive disk drains its mass to below the detection threshold in ∼104 years, or approximately 1% of the typical disk lifetime. Therefore, disks with spiral arms detected in ALMA dust observations, if generated by self-gravity, must either be still receiving infall to maintain a high q value, or have just emerged from their natal envelope. Detection of substructure in systems with lower q is possible, but would require a specialist integration with the most extended configuration over several days. This disfavors the possibility of GI-caused spiral structure in systems with q < 0.25 being detected in relatively short integration times, such as those found in the DSHARP ALMA survey. We find no temporal dependence of detectability on dynamical timescales.
The Southern H ii Region Discovery Survey. I. The Bright Catalog
Authors: Wenger Trey V. , Dickey John. M. , Jordan C. H. , Balser Dana S. , Armentrout W. P. , Anderson L. D. , Bania T. M. , Dawson J. R. , McClure-Griffiths N. M. , Shea Jeanine 
Published: January 2019

Abstract
The census of Galactic H ii regions is vastly incomplete in the southern sky. We use the Australia Telescope Compact Array to observe 4–10

radio continuum and hydrogen radio recombination line (RRL) emission from candidate H ii regions in the Galactic zone

. In this first data release, we target the brightest H ii region candidates and observe 282 fields in the direction of at least one previously known or candidate H ii region. We detect radio continuum emission and RRL emission in 275 (97.5%) and 258 (91.5%) of these fields, respectively. We catalog the ∼7 GHz radio continuum peak flux densities and positions of 80 previously known and 298 candidate H ii regions. After averaging ∼18 RRL transitions, we detect 77 RRL velocity components toward 76 previously known H ii regions and 267 RRL velocity components toward 256 H ii region candidates. The discovery of RRL emission from these nebulae increases the number of known Galactic H ii regions in the surveyed zone by 82% to 568 nebulae. In the fourth quadrant, we discover 50 RRLs with positive velocities, placing those sources outside the solar circle. Including the pilot survey, the Southern H ɪɪ Region Discovery Survey has now discovered 295 Galactic H ii regions. In the next data release, we expect to add ∼200 fainter and more distant nebulae.
Experimental Radiative Lifetimes, Branching Fractions, and Oscillator Strengths of Some Levels in Er i and Er ii
Authors: Yu Qi , Wang Xinghao , Li Qiu , Li Yongfan , Dai Zhenwen 
Published: January 2019

Abstract
Radiative lifetimes for 104 levels of Erbium (Er) i in the energy range between 31,926.003 and 44,525.705 cm−1 and 51 levels of Er ii from 31,381.779 to 47,840.962 cm−1 were measured by a time-resolved laser-induced fluorescence method. Branching fraction (BF) determinations for 356 lines from 47 out of 104 Er i levels and 122 lines related to 19 out of 51 Er ii levels were completed based on the emission spectra of hollow cathode lamps recorded using the 1.0 m Fourier transform spectrometer and are available from the digital library of National Solar Observatory on Kitt Peak, USA (http://diglib.nso.edu/). By combining these BFs and the lifetime results measured in this work, absolute transition probabilities and oscillator strengths were determined for 352 lines of Er i and 92 lines of Er ii for the first time, increasing the total number of lines with experimental transition probabilities to over 910 for Er i and over 540 for Er ii.
Time Delay between Neutrinos and Gamma-Rays in Short Gamma-Ray Bursts
Authors: Penacchioni A. V. , Civitarese O. 
Published: January 2019

Abstract
In this Letter we make an estimate of the time delay between signals, recorded at detectors on Earth, of neutrinos and photons originated in a short gamma-ray burst. We describe the geometry and dynamics of the system according to the Fireshell model. The delay in the photon’s arrival time is produced because the system is originally opaque to radiation; thus, the photons remain trapped and thermalize until the transparency condition is reached. We calculate the time interval between neutrino emission and photon emission in the black hole frame and transform it to the observer frame using Lorentz transformations. We obtain a difference in the arrival time at Earth of

.
Discrete and Continuous Ejection Models of the Radio Source Associated with GW170817
Authors: Punsly Brian 
Published: February 2019

Abstract
The gravity wave source, GW170817, and associated gamma-ray burst (GRB), GRB 170817A, produced radio emission that was detected in multiple epochs of Very Long Baseline Interferometry (VLBI) and with broadband radio photometry. Three unique pieces of observational evidence were determined: a discrete radio-emitting region that moves with an apparent velocity of ≈4c, a discrete region that includes all of the radio flux, and a likely synchrotron self absorption (SSA) spectral turnover on day ∼110 and day ∼160 after ejection. This unprecedented wealth of data for a GRB provides a unique opportunity to understand the radio-emitting plasma that was ejected by the putative merger event. The velocity can constrain the kinematics, and the SSA turnover has been used to constrain the size to one that is much smaller than can be done with an unresolved VLBI image, allowing one to estimate the associated plasmoid size directly from the data and improve estimates of the energetics. Models of the radio emission for both a turbulent, protonic, discrete ballistic ejection and a high dissipation region within an otherwise invisible Poynting flux dominated positron–electron jet are considered. On days ∼110 and ∼160 post-merger, for the range of models presented, the jet power is 2 × 1039–8 × 1040 erg s−1 and the ballistic plasmoid kinetic energy is 3 × 1045–1.5 × 1047 erg. Even though only valid after day 110, this independent analysis augments traditional GRB light curve studies, providing additional constraints on the merger event.
A new species of Clavicornaltica (Coleoptera: Chrysomelidae), discovered and described on a field course to Kuala Belalong, Brunei
Authors: Schilthuizen Menno , Berenyi Alfie , Limin Army , Brahim Aqilah , Cicuzza Daniele , Eales Anthony , Escoubas Pierre , Grafe Ulmar , de Groot Michiel , Hayden William , Paterno Marta , Jambul Rafi'ah , Slik J. W. , Ting Teck Wah Dennis , Tucker Angela , Njunjić Iva 
Published: January 2019

Clavicornaltica is a genus of very small flea beetles living in the leaf litter layer of Asian forests, easily sampled with Winkler extraction. The genus is presumably very rich in species, but their taxonomy is hampered by their small size and morphological uniformity.
On a ‘taxon expedition’-style field course at Kuala Belalong Field Studies Centre in Brunei Darussalam (Borneo), a new species, Clavicornalticabelalongensis n. sp., was discovered and taxonomically treated by the course participants. We also present the first DNA barcodes for the genus.
Les praticiens en Approche centrée sur la personne travaillent avec des clients et non avec des patients
Authors: Wilkins Paul , Leal Mauricio 
Published: January 2019

Le terme de « client » utilisé par Rogers de préférence à celui de « patient », loin d’être anodin, témoigne d’une conception de la personne prise dans son potentiel d’évolution. Cette perspective a un impact déterminant sur la manière dont la relation thérapeutique va se constituer.
Development of an Auditory Rehabilitation Tool for children with Cochlear Implants through a Mobile-Based VR and AR serious game
Authors: Hatzigiannakoglou Paul D , Okalidou Areti 
Published: January 2019

It is known that the development of auditory skills in children with hearing loss, who use assistive listening devices, requires training and practice. The aims of this research were a) to describe an auditory training software developed in order to help children with cochlear implants and/or hearing aids improve their auditory skills and monitor their performance, and b) to demonstrate the usability of the auditory training tool. The software is mobile-based and uses VR (Virtual Reality) and Immersive technology. In order to use it, the user must wear a VR headset. This technology was adopted because these devices are considered to be innovative, and are especially popular among children. The software was tested on fourteen hearing-impaired children. Eleven of these children use a cochlear implant and three use hearing aids. The results of this research show that the children with hearing loss were able to play the game successfully. This positive outcome supports the use of VR and Immersive technology as Auditory Training Tools.
Vignettes of interdisciplinary technical art history investigation
Authors: Stoner Joyce Hill 
Published: February 2019

The Foundation of the American Institute for Conservation oral history archive, which began in 1975, contains almost 300 interviews with pioneer conservators, conservation scientists, and art historians. Technical examination and technical art history, as exemplified by Roger H. Marijnissen’s publications, has undergone many changes since the 1950s; this article briefly surveys the field, focusing on the examination of easel paintings, with the aid of voices and personal observations from the interviews available in the international oral history archive of the Foundation of the American Institute for Conservation.