bluuebunny/crossref_metadata_2025_split huggingface dataset:
Pengetahuan Dan Sikap Mahasiswa Keperawatan Tentang Keperawatan Paliatif Di Universitas Advent Indonesia
Authors: Perangin-angin Mori A 
Published: March 2020

Penelitian ini dilatarbelakangi oleh tingginya angka penderita yang membutuhkan keperawatan paliatif, yaitu sebesar 40 milyar, namun hanya 14% yang sudah menerimanya, sedangkan 86% lainnya belum. Salah satu penyebabnya adalah kurangnya pengetahuan, ketrampilan dan kapasitas tenaga kesehatan dalam memberikan perawatan paliatif Tujuan penelitian ini adalah untuk mengetahui tingkat pengetahuan dan sikap serta mengetahui apakah terdapat hubungan antara pengetahuan dan sikap mahasiswa terhadap keperawatan paliatif. Metode yang digunakan dalam penelitian ini adalah deskriptif korelasi cross sectional dengan menggunakan tehnik purposive sampling. Populasi dan sampel dalam penelitian ini adalah seluruh mahasiswa tingkat 3 program studi S1 Fakultas ILmu Keperawatan Universitas Advent Bandung yang belum mengambil mata ajar Keperawatan Paliatif yang berjumlah 48 orang. Pengumpulan data dilakukan pada bulan April 2019. Untuk mengukur tingkat pengetahuan digunakan kuesioner The Palliative Care Quiz for Nursing (PCQN), sedangkan untuk mengukur sikap digunakan kuesioner Frommelt’s Attitude Toward Care of the Dying (FATCOD) scale. Hasil menunjukkan bahwa tingkat pengetahuan mahasiswa tentang keperawatan paliatif adalah 43.9% yaitu dalam kategori kurang, sedangkan sikap mahasiswa dalam kategori positif. Hasil uji korelasi Spearman menunjukkan bahwa tidak terdapat hubungan yang signifikan antara pengetahuan dan sikap dengan nilai p > 0,05. Kesimpulannya adalah mahasiswa keperawatan mempunyai tingkat pengetahuan yang rendah tentang keperawatan paliatif namun mempunyai sikap yang positif, tidak terdapat hubungan yang signifikan antara tingkat pengetahuan dan sikap. Saran agar keperawatan paliatif dapat memperoleh perhatian yang lebih besar untuk meningkatkan pengetahuan, sikap dan pembentukan kemampuan mahasiswa keperawatan dalam perawatan paliatif.
Correlation between Loss of E-cadherin, Matrix-metalloproteinases and c-Jun expression in Oral Carcinogenesis
Authors: Vajaria Bhairavi N. , Patel Kinjal R. , Begum Rasheedunnisa , Shah Franky D. , Patel Jayendra B. , Joshi Geeta M. , Patel Prabhudas S. 
Published: March 2020

Background: Earlier invitro studies have observed that loss of E-cadherin is responsible for progression and metastasis of cancer by upregulation of c-Jun protein. There being lack of simultaneous evaluation of matrix metalloproteinase (MMP) -2 and -9, E-cadherin and c-Jun mRNA and protein.
Objective: This study aimed to correlate the above-mentioned parameters to evaluate the pathway of oral carcinogenesis.
Methods: The study included 100 controls, 50 patients with oral precancerous conditions (OPC) and 100 oral cancer patients. MMPs were evaluated by gelatin zymography, ECAD and CJUN mRNA and protein expression by semi quantitative RT-PCR and western blot respectively.
Results: The levels of active and total MMP-2 and MMP-9 were significantly higher in patients with OPC and oral cancer patients as compared to controls. A significant increase in truncated E-cadherin and c-Jun protein was observed in malignant tissues as compared to adjacent normal tissues while CJUN mRNA levels were comparable. Higher values of c-Jun protein and MMPs, and lower values of ECAD mRNA were associated with reduced overall survival. A positive correlation was observed between truncated E-cadherin, MMPs and c-Jun protein.
Conclusions: MMPs modulate cell-cell adhesion by increasing truncation of E-cadherin resulting in loss of E-cadherin which is responsible for upregulation of c-Jun protein in oral cancer.
Clinical–pathologic Agreement for Oral Lesions in an Oral Medicine Setting
Authors: Villa Alessandro , Nordio Francesco , Strohmenger Laura , Abati Silvio 
Published: March 2020

Background: Histopathological examination remains the gold standard for the diagnosis of oral mucosal lesions. To date little is known on the clinical–pathologic agreement for oral lesions diagnosed by oral medicine experts.
Objective: This retrospective study attempts to quantify the clinical–pathologic agreement for oral lesions diagnosed by oral medicine experts.
Methods: Data were collected retrospectively from the medical records of all new oral medicine consultations. The clinical diagnosis provided by an oral medicine expert was compared to the histopathological diagnosis. Clinical–pathologic agreement was estimated as the percentage agreement and was measured using weighted Kappa.
Results: The most common oral lesions were oral lichen planus (34.7%), traumatic fibroma (23.4%), squamous cell carcinoma (SCC) or severe dysplasia (6.7%), mucous membrane pemphigoid (MMP) (5.7%), leukoplakia (5.6%) and squamous papilloma (4.3%). The overall clinical–pathologic agreement for all lesions had a weighted kappa of 0.81 [95%CI 0.78% to 0.85%]. The concordance for the most common oral lesions in the study population was 90.2%, with a weighted kappa of 0.88 [95%CI 0.85% to 0.92%]. The clinical–pathologic agreement for SCC/severe dysplasia was 78.7%, for traumatic fibroma 91.4%, for leukoplakia 97.4%, for oral lichen planus 93.8%, for squamous papilloma 96.7% and for MMP 65%.
Conclusions: The overall concordance between clinical and histopathological diagnosis for oral lesions was excellent. Dentists have the unique opportunity to refer patients to oral medicine experts for diagnosis and management of oral diseases. Given their expertise patients may require fewer visits for diagnostic purposes.
Equilibrium Tidal Response of Jupiter: Detectability by the Juno Spacecraft
Authors: Wahl Sean M. , Parisi Marzia , Folkner William M. , Hubbard William B. , Militzer Burkhard 
Published: March 2020

Abstract
An observation of Jupiter's tidal response is anticipated for the ongoing Juno spacecraft mission. We combine self-consistent, numerical models of Jupiter's equilibrium tidal response with observed Doppler shifts from the Juno gravity science experiment to test the sensitivity of the spacecraft to tides raised by the Galilean satellites and the Sun. The concentric Maclaurin spheroid (CMS) method finds the equilibrium shape and gravity field of a rotating, liquid planet with the tide raised by a satellite, expanded in Love numbers (k

nm
). We present improvements to the CMS theory that eliminate an unphysical center-of-mass offset and study in detail the convergence behavior of the CMS approach. We demonstrate that the dependence of k

nm
with orbital distance is important when considering the combined tidal response for Jupiter. Conversely, the details of the interior structure have a negligible influence on k

nm
for models that match the zonal harmonics J
2, J
4, and J
6, already measured to high precision by Juno. As the mission continues, improved coverage of Jupiter’s gravity field at different phases of Io’s orbit is expected to yield an observed value for the degree-two Love number (k
22) and potentially select higher-degree k

nm
. We present a test of the sensitivity of the Juno Doppler signal to the calculated k

nm
, which suggests the detectability of k
33, k
42, and k
31, in addition to k
22. A mismatch of a robust Juno observation with the remarkably small range in calculated Io equilibrium, k
22 = 0.58976 ± 0.0001, would indicate a heretofore uncharacterized dynamic contribution to the tides.
Detection of Fluorine in Hot Extreme Helium Stars
Authors: Bhowmick Anirban , Pandey Gajendra , Lambert David L. 
Published: March 2020

Abstract
The main objective of this paper is to explore abundances of fluorine in hot extreme helium stars (EHes). Overabundance of fluorine is a characteristic feature for cool EHes and R Coronae Borealis stars and further enforces their close connection. For hot EHes this relationship with the cooler EHes, based on their fluorine abundance is unexplored. We present in this paper the first abundance estimates of fluorine determined from singly ionized fluorine lines (F ii) for 10 hot EHe stars from optical spectra. Fluorine abundances were determined using the F ii lines in two windows centered at 3505 Å and 3850 Å. Six of the 10 stars show significant enhancement of fluorine similar to the cool EHes. Two carbon-poor hot EHes show no signature of fluorine and have a significant low upper limit for the F abundance. These fluorine abundances are compared with the other elemental abundances observed in these stars, which provide an idea about the formation and evolution of these stars. The trends of fluorine with C, O, and Ne show that significant helium burning after a CO–He white dwarf merger can account for a majority of the observed abundances. Predictions from simulations of white dwarf mergers are discussed in light of the observed abundances.
Dynamical Relics of the Ancient Galactic Halo
Authors: Yuan Zhen , Myeong G. C. , Beers Timothy C. , Evans N. W. , Lee Young Sun , Banerjee Projjwal , Gudin Dmitrii , Hattori Kohei , Li Haining , Matsuno Tadafumi , Placco Vinicius M. , Smith M. C. , Whitten Devin D. , Zhao Gang 
Published: March 2020

Abstract
We search for dynamical substructures in the LAMOST DR3 very metal-poor (VMP) star catalog. After cross-matching with Gaia DR2, there are ∼3300 VMP stars with available high-quality astrometric information that have halo-like kinematics. We apply a method based on the self-organizing map StarGO to find groups clustered in the 4D space of orbital energy and angular momentum. We identify 57 dynamically tagged groups (DTGs), which we label DTG-1 to DTG-57. Most of them belong to existing massive substructures in the nearby halo, such as the Gaia Sausage or Sequoia. The stream identified by Helmi et al. is recovered, but the two disjointed portions of the substructure appear to have distinct dynamical properties. The very retrograde substructure Rg5 found previously by Myeong et al. is also retrieved. We report six new DTGs with highly retrograde orbits, two with very prograde orbits, and 12 with polar orbits. By mapping other data sets (APOGEE halo stars, and catalogs of r-process-enhanced and carbon-enhanced metal-poor [CEMP] stars) onto the trained neuron map, we can associate stars with detailed chemical abundances with the DTGs and look for associations with chemically peculiar stars. The highly eccentric Gaia Sausage groups contain representatives of both debris from the satellite itself (which is α-poor) and the Splashed Disk, sent up into eccentric halo orbits from the encounter (and which is α-rich). The new prograde substructures also appear to be associated with the Splashed Disk. The DTGs belonging to the Gaia Sausage host two relatively metal-rich r-II stars and six CEMP stars in different subclasses, consistent with the idea that the Gaia Sausage progenitor is a massive dwarf galaxy. Rg5 is dynamically associated with two highly r-process-enhanced stars with [Fe/H] ∼ −3. This finding indicates that its progenitor might be an ultrafaint dwarf galaxy that has experienced r-process enrichment from neutron star mergers.
Three-dimensional Projection Effects on Chemistry in a Planck Galactic Cold Clump
Authors: Ge J. X. , Mardones Diego , He J. H. , Rawlings Jonathan M C , Liu Sheng-Yuan , Lee Jeong-Eun , Tatematsu Ken’ichi , Liu Tie , Zhu Lei , Chang Qiang , Inostroza Natalia , Feng S. 
Published: March 2020

Abstract
Offsets of molecular line emission peaks from continuum peaks are very common but frequently difficult to explain with a single spherical cloud chemical model. We propose that the spatial projection effects of an irregular three-dimensional (3D) cloud structure can be a solution. This work shows that the idea can be successfully applied to the Planck cold clump G224.4-0.6 by approximating it with four individual spherically symmetric cloud cores whose chemical patterns overlap with each other to produce observable line maps. With the empirical physical structures inferred from the observation data of this clump and a gas-grain chemical model, the four cores can satisfactorily reproduce its 850 μm continuum map and the diverse peak offsets of CCS, HC3N, and N2H+ simultaneously at chemical ages of about 8 × 105 ∼ 3 × 106 yr. The 3D projection effects on chemistry has the potential to explain such asymmetrical distributions of chemicals in many other molecular clouds.
Dependencies of Kappa Parameter on the Core Energy of Kappa Distributions and Plasma Parameter in the Case of the Magnetosphere of the Earth
Authors: Kirpichev I. P. , Antonova E. E. 
Published: March 2020

Abstract
Formation of kappa distribution functions and their relaxation to Maxwellian distributions are the main feature of astrophysical and space collisionless plasmas. In this work, we use the magnetosphere of the Earth as a giant plasma laboratory to study the properties of ion kappa distribution functions. Four years of measurements, performed by the multi-satellite Time History of Events and Macroscale Interactions during Substorms (THEMIS) mission during quiet geomagnetic conditions, at geocentric distances from three Earth radii (R
E) to the magnetopause at daytime (of the order of 10R
E), and up to 20R
E at night time are used for the analyses. We find a dependence of the k parameter on the core energy E
0 of a single kappa distribution inside the magnetospheric ring current and in the plasma sheet, for different values of the plasma parameter (the ratio between the plasma and magnetic pressures). We show that k increases with E
0 for all values of plasma parameter, which supports earlier results obtained for the magnetospheres of the Earth, Jupiter, and Saturn, but using lower statistics. However, contrary to previous results, our studies show that the relation between k and E
0 is nonlinear, and most probably is a power law with a nearly constant index. The results obtained are relevant to solve the problem of thermalization of kappa distributions.
A Companion Star Launching Jets in the Wind Acceleration Zone of a Giant Star
Authors: Hillel Shlomi , Schreier Ron , Soker Noam 
Published: March 2020

Abstract
By conducting three-dimensional hydrodynamical simulations we find that jets that a main-sequence companion launches as it orbits inside the wind acceleration zone of an asymptotic giant branch star can efficiently remove mass from that zone. We assume that during the intensive wind phase a large fraction of the gas in the acceleration zone does not reach the escape velocity. Therefore, in the numerical simulations we blow the wind with a velocity just below the escape velocity. We assume that a main-sequence companion accretes mass from the slow wind via an accretion disk, and launches two opposite jets perpendicular to the equatorial plane. This novel flow interaction shows that, by launching jets, a companion outside a giant star, but close enough to be in the acceleration zone of a slow intensive wind, can enhance the mass-loss rate from the giant star by ejecting some gas that would otherwise fall back onto the giant star. The jets are bent inside the wind acceleration zone and eject mass in a belt on the two sides of the equatorial plane. The jet–wind interaction contains instabilities that mix the shocked jets’ gas with the wind, leading to energy transfer from the jets to the wind. Our new simulations add to the rich variety of jet-induced outflow morphologies from evolved stars.
Radio/X-Ray Correlation in the Mini-outbursts of Black Hole X-Ray Transient GRS 1739–278
Authors: Xie Fu-Guo , Yan Zhen , Wu Zhongzu 
Published: March 2020

Abstract
We present quasi-simultaneous radio and X-ray observations of the black hole X-ray binary GRS 1739–278 during the 2015–2016 mini-outbursts, i.e., between 2015 June 10 and 2016 October 31, with the X-ray-to-radio time interval being less than one day. The monitor campaign was run by Swift in the X-rays and by VLA in the radio (at both 5 and 8 GHz). We find that the brightest radio emission is actually achieved during the soft sate, and the spectrum is marginally optically thick with the spectral index α ≈ −0.28 ± 0.17 (flux F

ν
∝ ν

α
). For the radio emission in the hard state, we find a large diversity in the spectral index, i.e., a majority of radio spectra are optically thick with −0.5 ≲ α ≲ 0.5, while a few are optically thin, with α being lower than −1 in certain cases. We then investigate the correlation between the luminosities in radio (monochromatic at 5 GHz,

) and 1–10 keV X-rays (

) during the hard state. We find that for more than two orders of magnitude variation in the X-ray luminosity, this source exhibits a flat correlation with p ≈ 0.16 (in the form of

), i.e., it belongs to the “outlier” (to the standard correlation with p ≈ 0.6) category that may follow a hybrid correlation. Both the slope and the corresponding luminosity range agree well with those in H1743–322, the prototype of the hybrid correlation. Theoretical implications of our results are discussed.
On the Chemical and Kinematic Consistency between N-rich Metal-poor Field Stars and Enriched Populations in Globular Clusters
Authors: Tang Baitian , Fernández-Trincado J. G. , Liu Chao , Yu Jincheng , Yan Hongliang , Gao Qi , Shi Jianrong , Geisler Douglas 
Published: March 2020

Abstract
Interesting chemically peculiar field stars may reflect their stellar evolution history and their possible origin in a different environment from where they are found now; this is one of the most important research fields in Galactic archeology. To explore this further, we have used the CN–CH bands around 4000 Å to identify N-rich metal-poor field stars in LAMOST DR3. Here we expand our N-rich, metal-poor field star sample to ∼100 stars in LAMOST DR5, where 53 of them are newly found in this work. We investigate light elements of common stars between our sample and APOGEE DR14. While Mg, Al, and Si abundances generally agree with the hypothesis that N-rich metal-poor field stars come from enriched populations in globular clusters, it is still inconclusive for C, N, and O. After integrating the orbits of our N-rich field stars and a control sample of normal metal-poor field stars, we find that N-rich field stars have different orbital parameter distributions compared to the control sample—specifically, apocentric distances, maximum vertical amplitude (Z
max), orbital energy, and z-direction angular momentum (Lz
). The orbital parameters of N-rich field stars indicate that most of them are inner-halo stars. The kinematics of N-rich field stars support their possible GC origin. The spatial and velocity distributions of our bona fide N-rich field star sample are important observational evidence to constrain simulations of the origin of these interesting objects.
Resolution Study for Three-dimensional Supernova Simulations with the Prometheus-Vertex Code
Authors: Melson Tobias , Kresse Daniel , Janka Hans-Thomas 
Published: March 2020

Abstract
We present a carefully designed, systematic study of the angular resolution dependence of simulations with the Prometheus-Vertex neutrino-hydrodynamics code. Employing a simplified neutrino heating–cooling scheme in the Prometheus hydrodynamics module allows us to sample the angular resolution between 4° and 0.°5. With a newly implemented static mesh refinement (SMR) technique on the Yin-Yang grid, the angular coordinates can be refined in concentric shells, compensating for the diverging structure of the spherical grid. In contrast to previous studies with Prometheus and other codes, we find that higher angular resolution and therefore lower numerical viscosity provides more favorable explosion conditions and faster shock expansion. We discuss the possible reasons for the discrepant results. The overall dynamics seem to converge at a resolution of about 1°. Applying the SMR setup to marginally exploding progenitors is disadvantageous for the shock expansion, however, because the kinetic energy of downflows is dissipated to internal energy at resolution interfaces, leading to a loss of turbulent pressure support and a steeper temperature gradient. We also present a way to estimate the numerical viscosity on grounds of the measured turbulent kinetic energy spectrum, leading to smaller values that are better compatible with the flow behavior witnessed in our simulations than results following calculations in previous literature. Interestingly, the numerical Reynolds numbers in the turbulent, neutrino-heated postshock layer (some 10 to several hundred) are in the ballpark of expected neutrino drag effects on the relevant length scales. We provide a formal derivation and quantitative assessment of the neutrino drag terms in an appendix.
Current State and Influencing Factors of Nurse Resilience and Perceived Job-Related Stressors
Authors: Leng Min , Xiu Hong , Yu Peng , Feng Juan , Wei Yuling , Cui Yanuan , Zhang Mingming , Zhou Yun , Wei Holly 
Published: March 2020

Background:
Resilience is a characteristic and skill that nurses can learn. This study examined the current state and influencing factors of nurse resilience and nurse perceived job-related stressors.

Method:
This cross-sectional survey study was conducted at a university-affiliated hospital in China between May and August 2018. The Connor-Davidson Resilience Scale was used to measure nurse resilience.

Results:

A total of 2,981 nurses participated in the study, with an average resilience score of 61.35 ± 13.12. Nurse resilience was significantly correlated with age, years of employment, clinical rank, and education (
p
< .05). Main job-related stressors included frequent inspections and examinations, heavy workload, mandatory overtime, and low wages.

Conclusion:

The participants had resilience scores that were lower than in the general public in the United States and China, as well as in nurses in developed countries. This study indicated a need for hospital leaders to find ways to reduce nurse work-related stress. Building nurse resilience should be an important focus for leaders.

[
J Contin Educ Nurs
. 2020;51(3):132–137.]
Geophysical measurements for site effects characterisation in the urban area of Girona, Spain
Authors: Macau Albert , Benjumea Beatriz , Gabàs Anna , Bellmunt Fabian , Figueras Sara 
Published: March 2020

ABSTRACTAmplitude level, duration, and spectral content of earthquake ground motions are strongly influenced by local soil conditions. Reliable estimation of site effects is, therefore, crucial in order to avoid damage to infrastructures and mitigate other losses. Traditional geophysical exploration techniques are restricted in urban environments due to the presence of anthropogenic noises causing low seismic signal‐to‐noise ratio and other logistical issues. These problems are even more critical when the maximum investigation depth extends to hundreds of metres.The city of Girona, located in northeastern Spain, has seismic hazard represented by a peak ground acceleration value of 0.08 g for a return period of 500 years. The city was built at the confluence of four rivers, generating a complex surface geology with bedrock outcrops and the presence of stiff soils, soft soils, and also a volcanic basalt layer. This paper presents the results of the geophysical work, which was carried out in order to characterise the soil layers present in the urban area of Girona. All information obtained in this research will be useful in computing the amplification of ground motion and to perform microzonation studies. We have obtained the shear‐wave velocity profile in the study area using a combination of seismic noise array and multichannel analysis of surface waves techniques. Using the horizontal‐to‐vertical spectral ratio method, we have obtained the soil fundamental frequency. The combination of shear‐wave velocity and values of soil fundamental frequency provides a complete map of the bedrock topography. The expected velocity inversion due to the presence of shallow basalt flow has been targeted. Electrical resistivity tomography is found to be suitable to define the volcanic basalt thickness. This thickness value is used to constrain the inversion of surface wave dispersion curves and reduce shear‐wave velocity uncertainty. The new methodology overcomes the limitations that are typical to urban conditions and other geological complexities.