bluuebunny/crossref_metadata_2025_split huggingface dataset:
Estudio de las propiedades estructurales y magnéticas de Gd0.257-XNdXFe0.743 obtenido por aleamiento mecánico
Authors: Martínez Sánchez Hugo , Rojas Martínez Yebrayl , Oyola Lozano Dagoberto , Bustos Rodríguez Humberto 
Published: September 2017

En este trabajo presentamos el estudio de las propiedades estructurales y magnéticas de la composición Gd0,257-xNdxFe0,743 con x=0, 0,1285, 0,257 preparada por Aleamiento mecánico en atmósfera de argón y con tiempo de molienda de 72 horas, usando un molino planetario FRITSCH PULVERISETTE 7 de alta energía. La caracterización magnética y estructural se realizó por Espectroscopia Mössbauer (MS) y Difracción de rayos x (XRD) respectivamente. Los tres difractogramas presentan un pico intenso, correspondientes a la fase α-Fe, su intensidad disminuye a medida que se sustituye el Gd por el Nd, mostrándose la mínima intensidad cuando x=0,257, y a su vez se observa un incremento progresivo en su ancho, estos efectos se atribuyen a la rica presencia de átomos de Nd en los lugares del hierro. Los espectros Mössbauer (EM) se ajustaron con distribuciones de campo hiperfino, sextetos y singletes usando el programa Mosfit. Los espectros muestran que al sustituir los átomos de Gd por los de Nd el orden magnético se afecta de tal manera que aparecen sitios de hierro que muestran desorden magnético.
SỰ THAM GIA CỦA NGƯỜI DÂN TRONG QUẢN LÝ ĐẦU TƯ CÔNG XÂY DỰNG NÔNG THÔN MỚI Ở VÙNG ĐỒI NÚI TỈNH THỪA THIÊN HUẾ
Authors: KN Khoa , Thuyết Cao Thị 
Published: September 2017

Tóm tắt: Sự tham gia của cộng đồng có vai trò rất quan trọng trong các hoạt động quản lý đầu tư công xây dựng nông thôn mới. Tuy nhiên, hiện nay sự tham gia đó của cộng đồng ở các địa phương còn nhiều hạn chế. Nghiên cứu nhằm tìm hiểu và phân tích thực trạng sự tham gia của người dân, cộng đồng trong quản lý đầu tư công xây dựng nông thôn mới và các yếu tố ảnh hưởng đến sự tham gia này. Nghiên cứu đã thực hiện khảo sát tại 2 xã đại diện cho vùng đồi núi của tỉnh Thừa Thiên Huế. Kết quả nghiên cứu cho thấy tỷ lệ hộ tham gia các cuộc họp về lập kế hoạch xây dựng các công trình ở cấp thôn/bản chiếm tỷ lệ khá cao 63,35 % ở hai xã điều tra. Hầu như người dân không được tham gia vào các hoạt động khảo sát thiết kế, lựa chọn đơn vị thi công và đơn vị giám sát với các tỷ lệ số người trả lời tương ứng lần lượt là 95,9 %, 97,3 %, 93,3 %. Trong công việc giám sát, đánh giá đầu tư có tính quyết định đến chất lượng công trình thì hầu như người dân hai xã nghiên cứu cũng không được tham gia, chiếm 80,95 % số người được hỏi. Có 4 yếu tố chính ảnh hưởng đến sự tham gia của người dân trong quản lý đầu tư xây dựng nông thôn mới (NTM), bao gồm: qui định pháp lý chưa rõ ràng; năng lực của người dân còn hạn chế; năng lực, trình độ, nhận thức của cán bộ thôn/xã còn yếu kém; phong tục tập quán, hương ước của cộng đồng dân cư.Từ khóa: xây dựng nông thôn mới, quản lý đầu tư, sự tham gia
ỨNG DỤNG GIS VÀ TIẾN TRÌNH PHÂN TÍCH THỨ BẬC PHÂN VÙNG THÍCH HỢP NUÔI TÔM THẺ CHÂN TRẮNG (Litopenaeus vannamei) TẠI HUYỆN ĐÔNG HÒA, TỈNH PHÚ YÊN
Authors: Thái Lê Văn , Linh Nguyễn Hoàng Khánh , Liêm Nguyễn Duy 
Published: September 2017

Tóm tắt: Mục tiêu của nghiên cứu này nhằm tích hợp GIS và Tiến trình Phân tích Thứ bậc xác định các khu vực thích hợp cho nuôi tôm thẻ chân trắng trên địa bàn huyện Đông Hòa, tỉnh Phú Yên. Tám yếu tố cần thiết cho nuôi tôm được phân thành hai nhóm chính, bao gồm: điều kiện xây dựng ao nuôi, điều kiện cơ sở hạ tầng và kinh tế - xã hội. Dựa trên AHP, tính toán trọng số của các yếu tố, sau đó ứng dụng GIS phân vùng thích hợp nuôi tôm. Kết quả cho thấy có khoảng 24,64% diện tích của huyện Đông Hòa (6.552 ha), phân bố trên địa bàn nhiều xã, hội đủ các điều kiện đất đai rất thích hợp cho tôm thẻ chân trắng phát triển. Với kết quả đạt được, đã chứng minh tính hữu dụng của việc tích hợp GIS và AHP trong phân vùng thích hợp nuôi tôm thẻ chân trắng, cung cấp tài liệu tham khảo hữu ích cho công tác quy hoạch vùng nuôi loài tôm này trên địa bàn nghiên cứu.Từ khóa: GIS, Tiến trình phân tích thứ bậc(AHP), Tôm thẻ chân trắng (Litopenaeus vannamei).
NEW RECORDS AND AN UPDATED CHECKLIST OF AMPHIBIANS (AMPHIBIA) FROM PHU YEN PROVINCE, VIETNAM
Authors: Dang Do Trong 
Published: September 2017

<p><strong>Abstract. </strong>We herein provide an updated checklist of 33 amphibian species from Phu Yen Province, Vietnam. Eight of them are reported for the first time from this province, namely <em>Ophryophryne gerti, O. hansi, Xenophrys major, </em><em>Glyphoglossus molossus, Kaloula indochinensis, Microhyla berdmorei, M. nanapollexa, </em>and <em>Amolops spinapectoralis.</em> Additional data of morphological characters of afore mentioned species were also provided. The number of amphibian species recorded was highest from Tay Hoa district (18 species), followed by Song Hinh district (15 species), Dong Xuan district (10 species), Tuy Hoa city (8 specise), Son Hoa district (8 species), Dong Hoa (4 specise), and Tuy An district (3 species). In terms of conservation concern, three species are listed in the IUCN Red List (2016) and one species is listed in the Vietnam Red Data Book (2007). </p>
A STUDY ON HYDROTHERMAL SYNTHESIS OF METAL–ORGANIC FRAMEWORK MIL-101
Authors: Châu Võ Thị Thanh , Đức Hoàng Văn 
Published: September 2017

<p>In the present paper, a synthesis of MIL-101 by hydrothermal process was demonstrated. The obtained samples were characterized by powder X-ray diffraction (PXRD), transmission electron microscope (TEM), nitrogen adsorption/desorption isotherms at 77K, X-ray photoelectron spectroscopy (XPS). The results showed that MIL-101 synthesized by optimal conditions exhibited high crystallinity and surface area. The obtained MIL-101 possesses high stability in water and several organic solvents.</p><p><strong>Keywords:</strong> MIL-101, hydrothermal synthesis, metal organic framework-101. </p>
DESCRIPTION OF INFLUENCE NEGATIVE STIGMA ON PATIENTS POSITIVE HIV IN NGANJUK
Authors: Cahyono Sony Wahyu Tri 
Published: September 2017

ABSTRACT The negative stigma received by HIV positive people is very influential in life. HIV positive people are considered as people who have violated immoral norms in society. HIV positive patients will usually get social sanctions in the form of exclusion, gossip, ridicule, avoided, and even expelled from the community environment. Negative stigma received by HIV positive people not only from the community environment, but there is also a stigma that comes from the family. The form of stigma in the form of discrimination to HIV positive people from family like do not want to eat together, do not want to handshake, do not want to sleep together even do not want to consider family again.This study used qualitative method with phenomenology approach. This study explored the experiences of HIV positive people who get negative stigma from family and society. Participants in this study as many as 5 people. Technique of taking data from informant by using in-depth interview on each participant.This research produces three themes that have been gained from the in-depth interviews. The theme is getting negative stigma from family and society, hiding health status, withdrawing.Factors of the theme found are a description of the effect of negative stigma on HIV positive patients. It is hoped that further research development will improve in the questionnaire to see howfar the negative stigma in HIV positive people is affected. Keywords: Stigma, and HIV positive
Formation of Double Neutron Star Systems
Authors: Tauris T. M. , Kramer M. , Freire P. C. C. , Wex N. , Janka H.-T. , Langer N. , Podsiadlowski Ph. , Bozzo E. , Chaty S. , Kruckow M. U. , Heuvel E. P. J. van den , Antoniadis J. , Breton R. P. , Champion D. J. 
Published: September 2017

Abstract
Double neutron star (DNS) systems represent extreme physical objects and the endpoint of an exotic journey of stellar evolution and binary interactions. Large numbers of DNS systems and their mergers are anticipated to be discovered using the Square Kilometre Array searching for radio pulsars, and the high-frequency gravitational wave detectors (LIGO/VIRGO), respectively. Here we discuss all key properties of DNS systems, as well as selection effects, and combine the latest observational data with new theoretical progress on various physical processes with the aim of advancing our knowledge on their formation. We examine key interactions of their progenitor systems and evaluate their accretion history during the high-mass X-ray binary stage, the common envelope phase, and the subsequent Case BB mass transfer, and argue that the first-formed NSs have accreted at most

. We investigate DNS masses, spins, and velocities, and in particular correlations between spin period, orbital period, and eccentricity. Numerous Monte Carlo simulations of the second supernova (SN) events are performed to extrapolate pre-SN stellar properties and probe the explosions. All known close-orbit DNS systems are consistent with ultra-stripped exploding stars. Although their resulting NS kicks are often small, we demonstrate a large spread in kick magnitudes that may, in general, depend on the past interaction history of the exploding star and thus correlate with the NS mass. We analyze and discuss NS kick directions based on our SN simulations. Finally, we discuss the terminal evolution of close-orbit DNS systems until they merge and possibly produce a short γ-ray burst.
and the Diffuse Interstellar Bands: An Independent Laboratory Check
Authors: Spieler Steffen , Kuhn Martin , Postler Johannes , Simpson Malcolm , Wester Roland , Scheier Paul , Ubachs Wim , Bacalla Xavier , Bouwman Jordy , Linnartz Harold 
Published: September 2017

Abstract
In 2015, Campbell et al. presented spectroscopic laboratory gas phase data for the fullerene cation,

, that coincide with the reported astronomical spectra of two diffuse interstellar band (DIB) features at 9633 and 9578 Å. In the following year, additional laboratory spectra were linked to three other and weaker DIBs at 9428, 9366, and 9349 Å. The laboratory data were obtained using wavelength-dependent photodissociation spectroscopy of small (up to three) He-tagged

ion complexes, yielding rest wavelengths for the bare

cation by correcting for the He-induced wavelength shifts. Here we present an alternative approach to derive the rest wavelengths of the four most prominent

absorption features, using high-resolution laser dissociation spectroscopy of

embedded in ultracold He droplets. Accurate wavelengths of the bare fullerene cation are derived from linear wavelength shifts recorded for

species with n up to 32. A careful analysis of all of the available data results in precise rest wavelengths (in air) for the four most prominent

bands: 9631.9(1) Å, 9576.7(1) Å, 9427.5(1) Å, and 9364.9(1) Å. The corresponding bandwidths have been derived and the relative band intensity ratios are discussed.
Balmer Filaments in Tycho’s Supernova Remnant: An Interplay between Cosmic-ray and Broad-neutral Precursors
Authors: Knežević Sladjana , Läsker Ronald , van de Ven Glenn , Font Joan , Raymond John C. , Bailer-Jones Coryn A. L. , Beckman John , Morlino Giovanni , Ghavamian Parviz , Hughes John P. , Heng Kevin 
Published: September 2017

Abstract
We present Hα spectroscopic observations and detailed modeling of the Balmer filaments in the supernova remnant (SNR) Tycho (SN 1572). We used GH
α
FaS (Galaxy Hα Fabry–Pérot Spectrometer) on the William Herschel Telescope with a 3.′4 × 3.′4 field of view, 0.″2 pixel scale, and

σ

instr

=
8.1

km s−1 resolution at 1″ seeing for ∼10 hr, resulting in 82 spatial−spectral bins that resolve the narrow Hα line in the entire SN 1572 northeastern rim. For the first time, we can therefore mitigate artificial line broadening from unresolved differential motion and probe Hα emission parameters in varying shock and ambient medium conditions. Broad Hα line remains unresolved within spectral coverage of 392 km s−1. We employed Bayesian inference to obtain reliable parameter confidence intervals and to quantify the evidence for models with multiple line components. The median Hα narrow-line (NL) FWHM of all bins and models is

W

NL

=
(
54.8
±
1.8
)

km s−1 at the 95% confidence level, varying within [35, 72] km s−1 between bins and clearly broadened compared to the intrinsic (thermal) ≈20 km s−1. Possible line splits are accounted for, significant in

≈
18
%

of the filament, and presumably due to remaining projection effects. We also find widespread evidence for intermediate-line emission of a broad-neutral precursor, with a median

W

IL

=
(
180
±
14
)

km s−1 (95% confidence). Finally, we present a measurement of the remnant’s systemic velocity,

V

LSR

=
−
34

km s−1, and map differential line-of-sight motions. Our results confirm the existence and interplay of shock precursors in Tycho’s remnant. In particular, we show that suprathermal NL emission is near-universal in SN 1572, and that, in the absence of an alternative explanation, collisionless SNR shocks constitute a viable acceleration source for Galactic TeV cosmic-ray protons.
Modeling Coronal Response in Decaying Active Regions with Magnetic Flux Transport and Steady Heating
Authors: Ugarte-Urra Ignacio , Warren Harry P. , Upton Lisa A. , Young Peter R. 
Published: September 2017

Abstract
We present new measurements of the dependence of the extreme ultraviolet (EUV) radiance on the total magnetic flux in active regions as obtained from the Atmospheric Imaging Assembly (AIA) and the Helioseismic and Magnetic Imager on board the Solar Dynamics Observatory. Using observations of nine active regions tracked along different stages of evolution, we extend the known radiance—magnetic flux power-law relationship (

I
∝

Φ

α

) to the AIA 335 Å passband, and the Fe xviii 93.93 Å spectral line in the 94 Å passband. We find that the total unsigned magnetic flux divided by the polarity separation (

Φ

/

D

) is a better indicator of radiance for the Fe xviii line with a slope of

α
=
3.22
±
0.03

. We then use these results to test our current understanding of magnetic flux evolution and coronal heating. We use magnetograms from the simulated decay of these active regions produced by the Advective Flux Transport model as boundary conditions for potential extrapolations of the magnetic field in the corona. We then model the hydrodynamics of each individual field line with the Enthalpy-based Thermal Evolution of Loops model with steady heating scaled as the ratio of the average field strength and the length (

B

¯

/

L

) and render the Fe xviii and 335 Å emission. We find that steady heating is able to partially reproduce the magnitudes and slopes of the EUV radiance—magnetic flux relationships and discuss how impulsive heating can help reconcile the discrepancies. This study demonstrates that combined models of magnetic flux transport, magnetic topology, and heating can yield realistic estimates for the decay of active region radiances with time.
Strange Quark Stars in Binaries: Formation Rates, Mergers, and Explosive Phenomena
Authors: Wiktorowicz G. , Drago A. , Pagliara G. , Popov S. B. 
Published: September 2017

Abstract
Recently, the possible coexistence of a first family composed of “normal” neutron stars (NSs) with a second family of strange quark stars (QSs) has been proposed as a solution of problems related to the maximum mass and to the minimal radius of these compact stellar objects. In this paper, we study the mass distribution of compact objects formed in binary systems and the relative fractions of quark and NSs in different subpopulations. We incorporate the strange QS formation model provided by the two-families scenario, and we perform a large-scale population synthesis study in order to obtain the population characteristics. According to our results, the main channel for strange QS formation in binary systems is accretion from a secondary companion on an NS. Therefore, a rather large number of strange QSs form by accretion in low-mass X-ray binaries and this opens the possibility of having explosive GRB-like phenomena not related to supernovae and not due to the merger of two NSs. The number of double strange QS systems is rather small, with only a tiny fraction that merge within a Hubble time. This drastically limits the flux of strangelets produced by the merger, which turns out to be compatible with all limits stemming from Earth and lunar experiments. Moreover, this value of the flux rules out at least one relevant channel for the transformation of all NSs into strange QSs by strangelets’ absorption.
The Direct Effect of Toroidal Magnetic Fields on Stellar Oscillations: An Analytical Expression for the General Matrix Element
Authors: Kiefer René , Schad Ariane , Roth Markus 
Published: September 2017

Abstract
Where is the solar dynamo located and what is its modus operandi? These are still open questions in solar physics. Helio- and asteroseismology can help answer them by enabling us to study solar and stellar internal structures through global oscillations. The properties of solar and stellar acoustic modes are changing with the level of magnetic activity. However, until now, the inference on subsurface magnetic fields with seismic measures has been very limited. The aim of this paper is to develop a formalism to calculate the effect of large-scale toroidal magnetic fields on solar and stellar global oscillation eigenfunctions and eigenfrequencies. If the Lorentz force is added to the equilibrium equation of motion, stellar eigenmodes can couple. In quasi-degenerate perturbation theory, this coupling, also known as the direct effect, can be quantified by the general matrix element. We present the analytical expression of the matrix element for a superposition of subsurface zonal toroidal magnetic field configurations. The matrix element is important for forward calculations of perturbed solar and stellar eigenfunctions and frequency perturbations. The results presented here will help to ascertain solar and stellar large-scale subsurface magnetic fields, and their geometric configuration, strength, and change over the course of activity cycles.
The EDGE-CALIFA Survey: Interferometric Observations of 126 Galaxies with CARMA
Authors: Bolatto Alberto D. , Wong Tony , Utomo Dyas , Blitz Leo , Vogel Stuart N. , Sánchez Sebastián F. , Barrera-Ballesteros Jorge , Cao Yixian , Colombo Dario , Dannerbauer Helmut , García-Benito Rubén , Herrera-Camus Rodrigo , Husemann Bernd , Kalinova Veselina , Leroy Adam K. , Leung Gigi , Levy Rebecca C. , Mast Damián , Ostriker Eve , Rosolowsky Erik , Sandstrom Karin M. , Teuben Peter , van de Ven Glenn , Walter Fabian 
Published: September 2017

Abstract
We present interferometric CO observations, made with the Combined Array for Millimeter-wave Astronomy (CARMA) interferometer, of galaxies from the Extragalactic Database for Galaxy Evolution survey (EDGE). These galaxies are selected from the Calar Alto Legacy Integral Field Area (CALIFA) sample, mapped with optical integral field spectroscopy. EDGE provides good-quality CO data (3σ sensitivity

before inclination correction, resolution ∼1.4 kpc) for 126 galaxies, constituting the largest interferometric CO survey of galaxies in the nearby universe. We describe the survey and data characteristics and products, then present initial science results. We find that the exponential scale lengths of the molecular, stellar, and star-forming disks are approximately equal, and galaxies that are more compact in molecular gas than in stars tend to show signs of interaction. We characterize the molecular-to-stellar ratio as a function of Hubble type and stellar mass and present preliminary results on the resolved relations between the molecular gas, stars, and star-formation rate. We then discuss the dependence of the resolved molecular depletion time on stellar surface density, nebular extinction, and gas metallicity. EDGE provides a key data set to address outstanding topics regarding gas and its role in star formation and galaxy evolution, which will be publicly available on completion of the quality assessment.
Galaxies as High-resolution Telescopes
Authors: Barnacka Anna 
Published: September 2017

Abstract
Recent observations show a population of active galaxies with milliarcsecond offsets between optical and radio emission. Such offsets can be an indication of extreme phenomena associated with supermassive black holes including relativistic jets, binary supermassive black holes, or even recoiling supermassive black holes. However, the multi-wavelength structure of active galaxies at a few milliarcseconds cannot be resolved with direct observations. We propose using strong gravitational lensing to elucidate the multi-wavelength structure of sources. When sources are located close to the caustic of a lensing galaxy, even a small offset in the position of the sources results in a drastic difference in the position and magnification of mirage images. We show that the angular offset in the position of the sources can be amplified more than 50 times in the observed position of mirage images. We find that at least 8% of the observed gravitationally lensed quasars will be in the caustic configuration. The synergy between SKA and Euclid will provide an ideal set of observations for thousands of gravitationally lensed sources in the caustic configuration, which will allow us to resolve the multi-wavelength structure for a large ensemble of sources and to study the physical origin of radio emissions, their connection to supermassive black holes, and their cosmic evolution.
Failed Radiatively Accelerated Dusty Outflow Model of the Broad Line Region in Active Galactic Nuclei. I. Analytical Solution
Authors: Czerny B. , Li Yan-Rong , Hryniewicz K. , Panda S. , Wildy C. , Sniegowska M. , Wang J.-M. , Sredzinska J. , Karas V. 
Published: September 2017

Abstract
The physical origin of the broad line region in active galactic nuclei is still unclear despite many years of observational studies. The reason is that the region is unresolved, and the reverberation mapping results imply a complex velocity field. We adopt a theory-motivated approach to identify the principal mechanism responsible for this complex phenomenon. We consider the possibility that the role of dust is essential. We assume that the local radiation pressure acting on the dust in the accretion disk atmosphere launches the outflow of material, but higher above the disk the irradiation from the central parts causes dust evaporation and a subsequent fallback. This failed radiatively accelerated dusty outflow is expected to represent the material forming low ionization lines. In this paper we formulate simple analytical equations to describe the cloud motion, including the evaporation phase. The model is fully described just by the basic parameters of black hole mass, accretion rate, black hole spin, and viewing angle. We study how the spectral line generic profiles correspond to this dynamic. We show that the virial factor calculated from our model strongly depends on the black hole mass in the case of enhanced dust opacity, and thus it then correlates with the line width. This could explain why the virial factor measured in galaxies with pseudobulges differs from that obtained from objects with classical bulges, although the trend predicted by the current version of the model is opposite to the observed trend.