bluuebunny/crossref_metadata_2025_split huggingface dataset:
RESTORATIVE JUSTICE DALAM UNDANG-UNDANG SPPA: IMPLIKASINYA BAGI PEKERJAAN SOSIAL
Authors: Suharto Edi 
Published: February 2017

Act No. 11 Year 2012 on the Juvenile Justice Systemthat now come into force, grounded in the concept of restorative justice. Restorative justice is the completion of the criminal case together relevant parties in order to seek a fair settlement with the emphasis on restoring back to its original state. To achieve this restorative justice efforts for settling disputes diversion or transfer of children from the criminal justice process to the outside of the criminal justice process. At this diversion efforts have implications for social work. If previously a social worker who has a small role for children in conflict with the law (ABH), it is now a greater role. So it is necessary to enhance the quality and quantity of social workers. Improved quality and quantity must be followed by efforts such as education and training. Institutional quality of social welfare services should also be strengthened because it is the institution that will hold ABH when diversion efforts agreed by the parties.Keyword: Restorative Justice; Diversion; Social Workers ABSTRAKUU SPPA yang sekarang mulai berlaku, berpijak pada paradigma restorative justice. Restorative justice merupakan penyelesaian perkara tindak pidana bersama-sama pihak terkait dalam rangka mencari penyelesaian yang adil dengan menekankan pemulihan kembali pada keadaan semula. Untuk mencapai keadilan restoratif ini dilakukan upaya diversi atau pengalihan penyelesaian perkara anak dari proses peradilan pidana ke proses di luar peradilan pidana. Pada upaya diversi inilah memiliki dampak bagi pekerjaan sosial. Jika sebelumnya pekerja sosial mempunyai peranan yang kecil kepada anak yang berhadapan dengan hukum (ABH), maka kini peranannya lebih besar. Sehingga dibutuhkan peningkatan kualitas maupun kuantitas. Peningkatan kualitas maupun kuantitas harus diikuti dengan upaya seperti pendidikan dan pelatihan. Kualitas kelembagaan pelayanan kesejahteraan sosial juga harus diperkuat karena lembaga inilah yang akan menampung ABH ketika upaya diversi disepakati para pihak.Kata Kunci: Restoratif Justice; Diversi; Pekerja Sosial
Care With The Potential Organ Donor In The Intensive Care Unit
Authors: Barreto de Carvalho Francisca Patrícia , Morais Oliveira Kênnia Stephanie , Dos Santos Silva Glauber Weder , Nóbrega Melo Geórgia , Enggle de Araújo Alves Thiago , Arrais Ana Cristina , Rocha Leite Ilana Deyse , Lopes Fernandes Amélia Carolina , Clebeson Oliveira Lucidio , Ribeiro Soares Francisco Rafael 
Published: February 2017

Introduction: Organ transplants have expanded throughout the country, being extremely significant for the population.
Objective: To know the reality of organ harvesting and describe the care with the potential organ donor in an Intensive Care Unit (ICU) and compare it with the pertinent literature.
Method: It is a research of exploratory and descriptive nature, with a qualitative approach. The data were analyzed through the content analysis idealized by Bardin.
Results: The findings indicate that the resolution of care and procedures with the potential donor is essential to the success of transplants in our country.
Conclusions: Several difficulties have been encountered, as the lack of human and material resources generating impasses in the specific care of the potential organ donor and the lack of provision of continuing education.
Keywords: Organ donation; Intensive Care Unit; Nursing.
Chewing Duration Time Of Various Food Textures In Young Adults
Authors: Coutinho Vitcel Raísa , Fernandes de Oliveira José Fagny , Santos Ciro , Soares Pontes Emerson , De Holanda Ferreira Danilo Augusto , Jordão do Amaral Ana Karênina De Freitas 
Published: February 2017

OBJECTIVE: To obtain reference values of chewing time of several food textures in young adults.
METHOD: descriptive study with a quantitative approach that was developed in a clinical reference, being the population composed of 40 young adults between 18-30 years of age, of both genres. As exclusion criteria: those with neuromuscular and / or degenerative diseases or consequences thereof, as well as subjects who were making use of any orthodontic / orthopedic resource. We conducted a dental evaluation, followed by a clinical assessment. One at a time, the following foods were offered: French bread, wafer biscuit, roasted cashews, for voluntary chewing. To measure the food chewing time, we used a stopwatch, and this collection procedure was filmed. Data analysis was performed by means of the SPSS statistics 20.0 (IBM®) program.
RESULTS: There was a statistically significant difference (p < 0.05) between the medians of chewing time of French bread, wafer biscuit and cashew nuts, which were 33.0s (interquartile amplitude 29.0 - 40.0), 10.0s (interquartile amplitude 8.25-12.0) and 18.5s (interquartile amplitude 15.0-23.75), respectively.
CONCLUSION: The texture of foods influences the length of mastication. The more rigid is the food, the more cycles and mandibular movements, and therefore the longer the duration of chewing.
Planetary Torque in 3D Isentropic Disks
Authors: Fung Jeffrey , Masset Frédéric , Lega Elena , Velasco David 
Published: February 2017

Abstract
Planetary migration is inherently a three-dimensional (3D) problem, because Earth-size planetary cores are deeply embedded in protoplanetary disks. Simulations of these 3D disks remain challenging due to the steep resolution requirements. Using two different hydrodynamics codes, FARGO3D and PEnGUIn, we simulate disk–planet interaction for a one to five Earth-mass planet embedded in an isentropic disk. We measure the torque on the planet and ensure that the measurements are converged both in resolution and between the two codes. We find that the torque is independent of the smoothing length of the planet’s potential (r
s), and that it has a weak dependence on the adiabatic index of the gaseous disk (γ). The torque values correspond to an inward migration rate qualitatively similar to previous linear calculations. We perform additional simulations with explicit radiative transfer using FARGOCA, and again find agreement between 3D simulations and existing torque formulae. We also present the flow pattern around the planets that show active flow is present within the planet’s Hill sphere, and meridional vortices are shed downstream. The vertical flow speed near the planet is faster for a smaller r
s or γ, up to supersonic speeds for the smallest r
s and γ in our study.
Absence of an X-shaped Structure in the Milky Way Bulge Using Mira Variable Stars
Authors: López-Corredoira Martín 
Published: February 2017

Abstract
The stellar density distribution of the bulge is analyzed through one of its tracers. We use oxygen-rich Mira variables from the Catchpole et al. survey and OGLE-III survey as standard candles. The average age of these stars is around 9 Gyr. The population traced by Mira variables matches a boxy bulge prediction, not an X-shaped one, because only one peak is observed in the density along the analyzed lines of sight, whereas the prediction of an X-shape gives two clear peaks.
The Planetary Accretion Shock. I. Framework for Radiation-hydrodynamical Simulations and First Results
Authors: Marleau Gabriel-Dominique , Klahr Hubert , Kuiper Rolf , Mordasini Christoph 
Published: February 2017

Abstract
The key aspect determining the postformation luminosity of gas giants has long been considered to be the energetics of the accretion shock at the surface of the planet. We use one-dimensional radiation-hydrodynamical simulations to study the radiative loss efficiency and to obtain postshock temperatures and pressures and thus entropies. The efficiency is defined as the fraction of the total incoming energy flux that escapes the system (roughly the Hill sphere), taking into account the energy recycling that occurs ahead of the shock in a radiative precursor. We focus in this paper on a constant equation of state (EOS) to isolate the shock physics but use constant and tabulated opacities. While robust quantitative results will have to await a self-consistent treatment including hydrogen dissociation and ionization, the results presented here show the correct qualitative behavior and can be understood from semianalytical calculations. The shock is found to be isothermal and supercritical for a range of conditions relevant to the core accretion formation scenario (CA), with Mach numbers

. Across the shock, the entropy decreases significantly by a few times

. While nearly 100% of the incoming kinetic energy is converted to radiation locally, the efficiencies are found to be as low as roughly 40%, implying that a significant fraction of the total accretion energy is brought into the planet. However, for realistic parameter combinations in the CA scenario, we find that a nonzero fraction of the luminosity always escapes the Hill sphere. This luminosity could explain, at least in part, recent observations in the young LkCa 15 and HD 100546 systems.
The Candidate Progenitor of the Type IIn SN 2010jl Is Not an Optically Luminous Star
Authors: Fox Ori D. , Dyk Schuyler D. Van , Dwek Eli , Smith Nathan , Filippenko Alexei V. , Andrews Jennifer , Arendt Richard G. , Foley Ryan J. , Kelly Patrick L. , Miller Adam A. , Shivvers Isaac 
Published: February 2017

Abstract
A blue source in pre-explosion Hubble Space Telescope (HST)/Wide-Field Planetary Camera 2 (WFPC2) images falls within the 5σ astrometric error circle (∼0.″24) derived from post-explosion ground-based imaging of SN 2010jl. At the time the ground-based astrometry was published, however, the SN had not faded sufficiently for post-explosion HST follow-up observations to determine a more precise astrometric solution and/or confirm if the pre-explosion source had disappeared, both of which are necessary to ultimately disentangle the possible progenitor scenarios. Here we present HST/WFC3 imaging of the SN 2010jl field obtained in 2014, 2015, and 2016 when the SN had faded sufficiently to allow for new constraints on the progenitor. The SN, which is still detected in the new images, is offset by 0.″061 ± 0.″008 (15 ± 2 pc) from the underlying and extended source of emission that contributes at least partially, if not entirely, to the blue source previously suggested as the candidate progenitor in the WFPC2 data. This point alone rules out the possibility that the blue source in the pre-explosion images is the exploding star, but may instead suggest an association with a young (<5–6 Myr) cluster and still argues for a massive (>30 M
⊙) progenitor. We obtain new upper limits on the flux from a single star at the SN position in the pre-explosion WFPC2 and Spitzer/IRAC images that may ultimately be used to constrain the progenitor properties.
Cold CO Gas in the Envelopes of FU Orionis-type Young Eruptive Stars
Authors: Kóspál Á. , Ábrahám P. , Csengeri T. , Henning Th. , Moór A. , Güsten R. 
Published: February 2017

Abstract
FU Orionis-type objects (FUors) are young stellar objects experiencing large optical outbursts due to highly enhanced accretion from the circumstellar disk onto the star. FUors are often surrounded by massive envelopes, which play a significant role in the outburst mechanism. Conversely, the subsequent eruptions might gradually clear up the obscuring envelope material and drive the protostar on its way to become a disk-only T Tauri star. Here we present an APEX 12CO and 13CO survey of eight southern and equatorial FUors. We measure the mass of the gaseous material surrounding our targets, locate the source of the CO emission, and derive physical parameters for the envelopes and outflows, where detected. Our results support the evolutionary scenario where FUors represent a transition phase from envelope-surrounded protostars to classical T Tauri stars.
Implications for Extraterrestrial Hydrocarbon Chemistry: Analysis of Ethylene (C2H4) and D4-Ethylene (C2D4) Ices Exposed to Ionizing Radiation via Combined Infrared Spectroscopy and Reflectron Time-of-flight Mass Spectrometry
Authors: Abplanalp Matthew J. , Kaiser Ralf I. 
Published: February 2017

Abstract
The processing of the hydrocarbon ice, ethylene (C2H4/C2D4), via energetic electrons, thus simulating the processes in the track of galactic cosmic-ray particles, was carried out in an ultrahigh vacuum apparatus. The chemical evolution of the ices was monitored online and in situ utilizing Fourier transform infrared spectroscopy (FTIR) and during temperature programmed desorption, via a quadrupole mass spectrometer utilizing electron impact ionization (EI-QMS) and a reflectron time-of-flight mass spectrometer utilizing a photoionization source (PI-ReTOF-MS). Several previous in situ studies of ethylene ice irradiation using FTIR were substantiated with the detection of six products: [CH4 (CD4)], acetylene [C2H2 (C2D2)], the ethyl radical [C2H5 (C2D5)], ethane [C2H6 (C2D6)], 1-butene [C4H8 (C4D8)], and n-butane [C4H10 (C4D10)]. Contrary to previous gas phase studies, the PI-ReTOF-MS detected several groups of hydrocarbon with varying degrees of saturation: C
n
H2n+2 (n = 4–10), C
n
H2n
(n = 2–12, 14, 16), C
n
H2n−2 (n = 3–12, 14, 16), C
n
H2n−4 (n = 4–12, 14, 16), C
n
H2n−6 (n = 4–10, 12), C
n
H2n−8 (n = 6–10), and C
n
H2n−10 (n = 6–10). Multiple laboratory studies have shown the facile production of ethylene from methane, which is a known ice constituent in the interstellar medium. Various astrophysically interesting molecules can be associated with the groups detected here, such as allene/methylacetylene (C3H4) or 1, 3-butadiene (C4H6) and its isomers, which have been shown to lead to polycyclic aromatic hydrocarbons. Finally, several hydrocarbon groups detected here are unique to ethylene ice versus ethane ice and may provide understanding of how complex hydrocarbons form in astrophysical environments.
Photoionization Models for the Inner Gaseous Disks of Herbig Be Stars: Evidence against Magnetospheric Accretion?*
Authors: Patel P. , Sigut T. A. A. , Landstreet J. D. 
Published: February 2017

Abstract
We investigate the physical properties of the inner gaseous disks of three hot Herbig B2e stars, HD 76534, HD 114981, and HD 216629, by modeling CFHT-ESPaDOns spectra using non-LTE radiative transfer codes. We assume that the emission lines are produced in a circumstellar disk heated solely by photospheric radiation from the central star in order to test whether the optical and near-infrared emission lines can be reproduced without invoking magnetospheric accretion. The inner gaseous disk density was assumed to follow a simple power-law in the equatorial plane, and we searched for models that could reproduce observed lines of H i (Hα and Hβ), He i, Ca ii, and Fe ii. For the three stars, good matches were found for all emission line profiles individually; however, no density model based on a single power-law was able to reproduce all of the observed emission lines. Among the single power-law models, the one with the gas density varying as ∼10−10(R
*/R)3 g cm−3 in the equatorial plane of a 25 R
* (0.78 au) disk did the best overall job of representing the optical emission lines of the three stars. This model implies a mass for the Hα-emitting portion of the inner gaseous disk of ∼10−9
M
*. We conclude that the optical emission line spectra of these HBe stars can be qualitatively reproduced by a ≈1 au, geometrically thin, circumstellar disk of negligible mass compared to the central star in Keplerian rotation and radiative equilibrium.
Logamediate Inflation in f(T) Teleparallel Gravity
Authors: Rezazadeh Kazem , Abdolmaleki Asrin , Karami Kayoomars 
Published: February 2017

Abstract
We study logamediate inflation in the context of f(T) teleparallel gravity. f(T)-gravity is a generalization of the teleparallel gravity which is formulated on the Weitzenbock spacetime, characterized by the vanishing curvature tensor (absolute parallelism) and the non-vanishing torsion tensor. We consider an f(T)-gravity model which is sourced by a canonical scalar field. Assuming a power-law f(T) function in the action, we investigate an inflationary universe with a logamediate scale factor. Our results show that, although logamediate inflation is completely ruled out by observational data in the standard inflationary scenario based on Einstein gravity, it can be compatible with the 68% confidence limit joint region of Planck 2015 TT,TE,EE+lowP data in the framework of f(T)-gravity.
Magnetohydrodynamic Simulations of the Formation of Molecular Clouds toward the Stellar Cluster Westerlund 2: Interaction of a Jet with a Clumpy Interstellar Medium
Authors: Asahina Yuta , Kawashima Tomohisa , Furukawa Naoko , Enokiya Rei , Yamamoto Hiroaki , Fukui Yasuo , Matsumoto Ryoji 
Published: February 2017

Abstract
The formation mechanism of CO clouds observed with the NANTEN2 and Mopra telescopes toward the stellar cluster Westerlund 2 is studied by 3D magnetohydrodynamic simulations, taking into account the interstellar cooling. These molecular clouds show a peculiar shape composed of an arc-shaped cloud on one side of the TeV γ-ray source HESS J1023-575 and a linear distribution of clouds (jet clouds) on the other side. We propose that these clouds are formed by the interaction of a jet with clumps of interstellar neutral hydrogen (H i). By studying the dependence of the shape of dense cold clouds formed by shock compression and cooling on the filling factor of H i clumps, we found that the density distribution of H i clumps determines the shape of molecular clouds formed by the jet–cloud interaction: arc clouds are formed when the filling factor is large. On the other hand, when the filling factor is small, molecular clouds align with the jet. The jet propagates faster in models with small filling factors.
A Small Fullerene (C24) may be the Carrier of the 11.2 μm Unidentified Infrared Band
Authors: Bernstein L. S. , Shroll R. M. , Lynch D. K. , Clark F. O. 
Published: February 2017

Abstract
We analyze the spectrum of the 11.2 μm unidentified infrared band (UIR) from NGC 7027 and identify a small fullerene (C24) as a plausible carrier. The blurring effects of lifetime and vibrational anharmonicity broadening obscure the narrower, intrinsic spectral profiles of the UIR band carriers. We use a spectral deconvolution algorithm to remove the blurring, in order to retrieve the intrinsic profile of the UIR band. The shape of the intrinsic profile—a sharp blue peak and an extended red tail—suggests that the UIR band originates from a molecular vibration–rotation band with a blue band head. The fractional area of the band-head feature indicates a spheroidal molecule, implying a nonpolar molecule and precluding rotational emission. Its rotational temperature should be well approximated by that measured for nonpolar molecular hydrogen, ∼825 K for NGC 7027. Using this temperature, and the inferred spherical symmetry, we perform a spectral fit to the intrinsic profile, which results in a rotational constant implying C24 as the carrier. We show that the spectroscopic parameters derived for NGC 7027 are consistent with the 11.2 μm UIR bands observed for other objects. We present density functional theory (DFT) calculations for the frequencies and infrared intensities of C24. The DFT results are used to predict a spectral energy distribution (SED) originating from absorption of a 5 eV photon, and characterized by an effective vibrational temperature of 930 K. The C24 SED is consistent with the entire UIR spectrum and is the dominant contributor to the 11.2 and 12.7 μm bands.
Advanced LIGO Constraints on Neutron Star Mergers and r-process Sites
Authors: Côté Benoit , Belczynski Krzysztof , Fryer Chris L. , Ritter Christian , Paul Adam , Wehmeyer Benjamin , O’Shea Brian W. 
Published: February 2017

Abstract
The role of compact binary mergers as the main production site of r-process elements is investigated by combining stellar abundances of Eu observed in the Milky Way, galactic chemical evolution (GCE) simulations, and binary population synthesis models, and gravitational wave measurements from Advanced LIGO. We compiled and reviewed seven recent GCE studies to extract the frequency of neutron star–neutron star (NS–NS) mergers that is needed in order to reproduce the observed [Eu/Fe] versus [Fe/H] relationship. We used our simple chemical evolution code to explore the impact of different analytical delay-time distribution functions for NS–NS mergers. We then combined our metallicity-dependent population synthesis models with our chemical evolution code to bring their predictions, for both NS–NS mergers and black hole–neutron star mergers, into a GCE context. Finally, we convolved our results with the cosmic star formation history to provide a direct comparison with current and upcoming Advanced LIGO measurements. When assuming that NS–NS mergers are the exclusive r-process sites, and that the ejected r-process mass per merger event is 0.01 M

, the number of NS–NS mergers needed in GCE studies is about 10 times larger than what is predicted by standard population synthesis models. These two distinct fields can only be consistent with each other when assuming optimistic rates, massive NS–NS merger ejecta, and low Fe yields for massive stars. For now, population synthesis models and GCE simulations are in agreement with the current upper limit (O1) established by Advanced LIGO during their first run of observations. Upcoming measurements will provide an important constraint on the actual local NS–NS merger rate, will provide valuable insights on the plausibility of the GCE requirement, and will help to define whether or not compact binary mergers can be the dominant source of r-process elements in the universe.
Lensing Constraints on the Mass Profile Shape and the Splashback Radius of Galaxy Clusters∗
Authors: Umetsu Keiichi , Diemer Benedikt 
Published: February 2017

Abstract
The lensing signal around galaxy clusters can, in principle, be used to test detailed predictions for their average mass profile from numerical simulations. However, the intrinsic shape of the profiles can be smeared out when a sample that spans a wide range of cluster masses is averaged in physical length units. This effect especially conceals rapid changes in gradient such as the steep drop associated with the splashback radius, a sharp edge corresponding to the outermost caustic in accreting halos. We optimize the extraction of such local features by scaling individual halo profiles to a number of spherical overdensity radii, and apply this method to 16 X-ray-selected, high-mass clusters targeted in the Cluster Lensing And Supernova survey with Hubble. By forward-modeling the weak- and strong-lensing data presented by Umetsu et al., we show that, regardless of the scaling overdensity, the projected ensemble density profile is remarkably well described by a Navarro–Frenk–White (NFW) or Einasto profile out to

R
∼
2.5

h

−
1

Mpc

, beyond which the profiles flatten. We constrain the NFW concentration to

c

200
c

=
3.66
±
0.11

at

M

200
c

≃
1.0
×

10

15

h

−
1

M

⊙

, consistent with and improved from previous work that used conventionally stacked lensing profiles, and in excellent agreement with theoretical expectations. Assuming the profile form of Diemer & Kravtsov and generic priors calibrated from numerical simulations, we place a lower limit on the splashback radius of the cluster halos, if it exists, of

R

sp

3
D

/

r

200
m

>
0.89

(

R

sp

3
D

>
1.83

h

−
1

Mpc

) at 68% confidence. The corresponding density feature is most pronounced when the cluster profiles are scaled by

r

200
m

, and smeared out when scaled to higher overdensities.