bluuebunny/crossref_metadata_2025_split huggingface dataset:
Vulnerabilidad, trabajo y salud en mujeres de la tercera edad en Ameca, Jalisco
Authors: Navarro Ochoa Angélica 
Published: January 2017

En esta investigación se analizan las condiciones de vida de los adultos mayores, en especial de las mujeres en Ameca, Jalisco, México. Examinar su situación, desde un enfoque de género, permite mostrar la complejidad de las relaciones que construyen para enfrentar la desigualdad, el empobrecimiento y una mayor vulnerabilidad, en comparación con los hombres. El estudio es cualitativo, aunque no se descartó el análisis cuantitativo. A partir de entrevistas a profundidad, se reconstruyen experiencias de algunas adultas mayores que enfrentan desamparo, incapacidad o maltrato, y que tienen que trabajar para sobrevivir. Este trabajo contribuye a visibilizar la situación riesgosa y vulnerable de esta población, y los resultados muestran que existe una relación entre sus padecimientos y el exceso de trabajo físico que realiza. Por tanto, la condición de vida de los ancianos es vulnerable, debido a circunstancias familiares, culturales y económicas, que se reflejan en pobreza, abandono y marginalidad.
ANALISIS GENDER TERHADAP TINGKAT KEBERHASILAN PELAKSANAAN CSR BIDANG PEMBERDAYAAN EKONOMI LOKAL PT HOLCIM INDONESIA Tbk
Authors: Luciani Prastiwi Debbie , Sumarti Titik 
Published: January 2017

<em><span style="font-size: 11pt;">Baitul Maal wa Tamwil (BMT) Swadaya Pribumi is Corporate Social Responsibility (CSR) of local economic empowerment by PT Holcim Indonesia Tbk. Gender analysis is used as an analysis tools to see the success rate of BMT Swadaya Pribumi from a gender perspective by understanding the roles (division of labour) in the household, access, control to get resources (credit, training, and mentoring efforts), and the benefits for participants. Quantitatively, BMT is successful and it has considerd gender practical and strategic gender needs are different between the participants of women and men</span></em>
Optimization of cutting parameters for surface roughness in turning of studs manufactured from AISI 5140 steel using the Taguchi method
Authors: Kahraman Funda 
Published: January 2017

Abstract
This study focuses on optimizing cutting parameters based on the Taguchi method to minimize surface roughness in turning of studs manufactured from AISI 5140 steel. The Taguchi method, which is a powerful tool for designing optimized quality, is used to find the optimum surface roughness in turning operations. Rotational speed, feed rate and depth of cut were considered as control factors for the surface roughness, and L9 orthogonal array was determined for experiment trials. An orthogonal array, a signal-to-noise ratio, and an analysis of variance were employed to investigate the surface roughness characteristics of AISI 5140 steel. Minimum surface roughness was obtained at 2000 rpm rotational speed, 0.2 mm × rev−1 feed rate and 0.5 mm depth of cut. Optimal surface roughness was calculated as 1.70 μm by using optimal level of design parameters. Confirmation test showed that Taguchi method can be used precisely for optimizing the cutting parameters in turning of AISI 5140 steel. Through this study, it is possible to not only obtained the optimum surface roughness for turning operations, but also the main cutting parameters affecting the performance of turning operations. The developed model can be used in the metal machining industries in order to determine the optimum cutting parameters for minimum surface roughness.
MULTI-EPOCH DETECTIONS OF WATER ICE ABSORPTION IN EDGE-ON DISKS AROUND HERBIG Ae STARS: PDS 144N AND PDS 453
Authors: Terada Hiroshi , Tokunaga Alan T. 
Published: January 2017

ABSTRACT
We report the multi-epoch detections of water ice in 2.8–4.2

spectra of two Herbig Ae stars, PDS 144N (A2 IVe) and PDS 453 (F2 Ve), which have an edge-on circumstellar disk. The detected water ice absorption is found to originate from their protoplanetary disks. The spectra show a relatively shallow absorption of water ice of around 3.1

for both objects. The optical depths of the water ice absorption are ∼0.1 and ∼0.2 for PDS 144N and PDS 453, respectively. Compared to the water ice previously detected in low-mass young stellar objects with an edge-on disk with a similar inclination angle, these optical depths are significantly lower. It suggests that stronger UV radiation from the central stars effectively decreases the water ice abundance around the Herbig Ae stars through photodesorption. The water ice absorption in PDS 453 shows a possible variation of the feature among the six observing epochs. This variation could be due to a change of absorption materials passing through our line of sight to the central star. The overall profile of the water ice absorption in PDS 453 is quite similar to the absorption previously reported in the edge-on disk object d216-0939, and this unique profile may be seen only at a high inclination angle in the range of 76°–80°.
PHYSICAL CONTACT BETWEEN THE +20 km s−1 CLOUD AND THE GALACTIC CIRCUMNUCLEAR DISK
Authors: Takekawa Shunya , Oka Tomoharu , Tanaka Kunihiko 
Published: January 2017

ABSTRACT
This paper reports the discovery of evidence for physical contact between the Galactic circumnuclear disk (CND) and an exterior giant molecular cloud. The central 10 pc of our Galaxy has been imaged in the HCN J = 1–0, HCO+
J = 1–0, CS J = 2–1, H13CN J = 1–0, SiO J = 2–1, SO N

J
= 23–12, and HC3N J = 11–10 lines using the Nobeyama Radio Observatory 45 m radio telescope. Based on our examination of the position–velocity maps of several high-density probe lines, we have found that an emission “bridge” may be connecting the +20 km s−1 cloud (M–0.13–0.08) and the negative-longitude extension of the CND. Analyses of line intensity ratios imply that the chemical property of the bridge is located between the +20 km s−1 cloud and the CND. We introduce a new interpretation that a part of the CND may be colliding with the 20 km s−1 cloud and the collision may be responsible for the formation of the bridge. Such collisional events could promote mass accretion onto the CND or into the inner ionized cavity, which may be further tested by proper motion studies.
CORONAL JETS SIMULATED WITH THE GLOBAL ALFVÉN WAVE SOLAR MODEL
Authors: Szente J. , Toth G. , Manchester IV W. B. , Holst B. van der , Landi E. , Gombosi T. I. , DeVore C. R. , Antiochos S. K. 
Published: January 2017

ABSTRACT
This paper describes a numerical modeling study of coronal jets to understand their effects on the global corona and their contribution to the solar wind. We implement jets into a well-established three-dimensional, two-temperature magnetohydrodynamic (MHD) solar corona model employing Alfvén-wave dissipation to produce a realistic solar-wind background. The jets are produced by positioning a compact magnetic dipole under the solar surface and rotating the boundary plasma around the dipole's magnetic axis. The moving plasma drags the magnetic field lines along with it, ultimately leading to a reconnection-driven jet similar to that described by Pariat et al. We compare line-of-sight synthetic images to multiple jet observations at EUV and X-ray bands, and find very close matches in terms of physical structure, dynamics, and emission. Key contributors to this agreement are the greatly enhanced plasma density and temperature in our jets compared to previous models. These enhancements arise from the comprehensive thermodynamic model that we use and, also, our inclusion of a dense chromosphere at the base of our jet-generating regions. We further find that the large-scale corona is affected significantly by the outwardly propagating torsional Alfvén waves generated by our polar jet, across 40° in latitude and out to 24 R
⊙. We estimate that polar jets contribute only a few percent to the steady-state solar-wind energy outflow.
THE ORIGIN OF THE IRON-RICH KNOT IN TYCHO’S SUPERNOVA REMNANT
Authors: Yamaguchi Hiroya , Hughes John P. , Badenes Carles , Bravo Eduardo , Seitenzahl Ivo R. , Martínez-Rodríguez Héctor , Park Sangwook , Petre Robert 
Published: January 2017

ABSTRACT
X-ray observations of supernova remnants (SNRs) allow us to investigate the chemical inhomogeneity of ejecta, offering unique insight into the nucleosynthesis in supernova explosions. Here we present detailed imaging and spectroscopic studies of the “Fe knot” located along the eastern rim of the Type Ia SNR Tycho (SN 1572) using Suzaku and Chandra long-exposure data. Surprisingly, the Suzaku spectrum of this knot shows no emission from Cr, Mn, or Ni, which is unusual for the Fe-rich regions in this SNR. Within the framework of the canonical delayed-detonation models for SN Ia, the observed mass ratios

,

, and

(at 90% confidence) can only be achieved for a peak temperature of (5.3–5.7)

K and a neutron excess of

. These constraints rule out the deep, dense core of a Chandrasekhar-mass white dwarf as the origin of the Fe knot and favor either incomplete Si burning or an α-rich freeze-out regime, probably close to the boundary. An explosive He burning regime is a possible alternative, although this hypothesis is in conflict with the main properties of this SNR.
PLANETESIMAL COLLISIONS AS A CHONDRULE FORMING EVENT
Authors: Wakita Shigeru , Matsumoto Yuji , Oshino Shoichi , Hasegawa Yasuhiro 
Published: January 2017

ABSTRACT
Chondritic meteorites contain unique spherical materials named chondrules: sub-mm sized silicate grains once melted in a high temperature condition in the solar nebula. We numerically explore one of the chondrule forming processes—planetesimal collisions. Previous studies have found that impact jetting via protoplanet–planetesimal collisions can make chondrules with 1% of the impactors’ mass, when the impact velocity exceeds 2.5 km s−1. Based on the mineralogical data of chondrules, undifferentiated planetesimals would be more suitable for chondrule-forming collisions than potentially differentiated protoplanets. We examine planetesimal–planetesimal collisions using a shock physics code and find two things: one is that planetesimal–planetesimal collisions produce nearly the same amount of chondrules as protoplanet–planetesimal collisions (∼1%). The other is that the amount of produced chondrules becomes larger as the impact velocity increases when two planetesimals collide with each other. We also find that progenitors of chondrules can originate from deeper regions of large targets (planetesimals or protoplanets) than small impactors (planetesimals). The composition of targets is therefore important, to fully account for the mineralogical data of currently sampled chondrules.
ENERGETIC PARTICLE TRANSPORT ACROSS THE MEAN MAGNETIC FIELD: BEFORE DIFFUSION
Authors: Laitinen T. , Dalla S. 
Published: January 2017

ABSTRACT
Current particle transport models describe the propagation of charged particles across the mean field direction in turbulent plasmas as diffusion. However, recent studies suggest that at short timescales, such as soon after solar energetic particle (SEP) injection, particles remain on turbulently meandering field lines, which results in nondiffusive initial propagation across the mean magnetic field. In this work, we use a new technique to investigate how the particles are displaced from their original field lines, and we quantify the parameters of the transition from field-aligned particle propagation along meandering field lines to particle diffusion across the mean magnetic field. We show that the initial decoupling of the particles from the field lines is slow, and particles remain within a Larmor radius from their initial meandering field lines for tens to hundreds of Larmor periods, for 0.1–10 MeV protons in turbulence conditions typical of the solar wind at 1 au. Subsequently, particles decouple from their initial field lines and after hundreds to thousands of Larmor periods reach time-asymptotic diffusive behavior consistent with particle diffusion across the mean field caused by the meandering of the field lines. We show that the typical duration of the prediffusive phase, hours to tens of hours for 10 MeV protons in 1 au solar wind turbulence conditions, is significant for SEP propagation to 1 au and must be taken into account when modeling SEP propagation in the interplanetary space.
SEARCHING FOR BINARY SUPERMASSIVE BLACK HOLES VIA VARIABLE BROAD EMISSION LINE SHIFTS: LOW BINARY FRACTION
Authors: Wang Lile , Greene Jenny E. , Ju Wenhua , Rafikov Roman R. , Ruan John J. , Schneider Donald P. 
Published: January 2017

ABSTRACT
Supermassive black hole binaries (SMBHs) are expected to result from galaxy mergers, and thus are natural byproducts (and probes) of hierarchical structure formation in the universe. They are also the primary expected source of low-frequency gravitational wave emission. We search for binary BHs using time-variable velocity shifts in broad Mg ii emission lines of quasars with multi-epoch observations. First, we inspect velocity shifts of the binary SMBH candidates identified in Ju et al., using Sloan Digital Sky Survey spectra with an additional epoch of data that lengthens the typical baseline to ∼10 yr. We find variations in the line of sight velocity shifts over 10 yr that are comparable to the shifts observed over 1–2 yr, ruling out the binary model for the bulk of our candidates. We then analyze 1438 objects with eight-year median time baselines, from which we would expect to see velocity shifts >1000

from sub-parsec binaries. We find only one object with an outlying velocity of 448

, indicating—based on our modeling—that ≲1% (the value varies with different assumptions) of SMBHs that are active as quasars reside in binaries with ∼0.1 pc separations. Binaries either sweep rapidly through these small separations or stall at larger radii.
NUMERICAL INTEGRAL OF RESISTANCE COEFFICIENTS IN DIFFUSION
Authors: Zhang Q. S. 
Published: January 2017

ABSTRACT
The resistance coefficients in the screened Coulomb potential of stellar plasma are evaluated to high accuracy. I have analyzed the possible singularities in the integral of scattering angle. There are possible singularities in the case of an attractive potential. This may result in a problem for the numerical integral. In order to avoid the problem, I have used a proper scheme, e.g., splitting into many subintervals where the width of each subinterval is determined by the variation of the integrand, to calculate the scattering angle. The collision integrals are calculated by using Romberg’s method, therefore the accuracy is high (i.e., ∼10−12). The results of collision integrals and their derivatives for −7 ≤ ψ ≤ 5 are listed. By using Hermite polynomial interpolation from those data, the collision integrals can be obtained with an accuracy of 10−10. For very weakly coupled plasma (ψ ≥ 4.5), analytical fittings for collision integrals are available with an accuracy of 10−11. I have compared the final results of resistance coefficients with other works and found that, for a repulsive potential, the results are basically the same as others’; for an attractive potential, the results in cases of intermediate and strong coupling show significant differences. The resulting resistance coefficients are tested in the solar model. Comparing with the widely used models of Cox et al. and Thoul et al., the resistance coefficients in the screened Coulomb potential lead to a slightly weaker effect in the solar model, which is contrary to the expectation of attempts to solve the solar abundance problem.
A COUPLED 2 × 2D BABCOCK–LEIGHTON SOLAR DYNAMO MODEL. II. REFERENCE DYNAMO SOLUTIONS
Authors: Lemerle Alexandre , Charbonneau Paul 
Published: January 2017

ABSTRACT
In this paper we complete the presentation of a new hybrid 2 × 2D flux transport dynamo (FTD) model of the solar cycle based on the Babcock–Leighton mechanism of poloidal magnetic field regeneration via the surface decay of bipolar magnetic regions (BMRs). This hybrid model is constructed by allowing the surface flux transport (SFT) simulation described in Lemerle et al. to provide the poloidal source term to an axisymmetric FTD simulation defined in a meridional plane, which in turn generates the BMRs required by the SFT. A key aspect of this coupling is the definition of an emergence function describing the probability of BMR emergence as a function of the spatial distribution of the internal axisymmetric magnetic field. We use a genetic algorithm to calibrate this function, together with other model parameters, against observed cycle 21 emergence data. We present a reference dynamo solution reproducing many solar cycle characteristics, including good hemispheric coupling, phase relationship between the surface dipole and the BMR-generating internal field, and correlation between dipole strength at cycle maximum and peak amplitude of the next cycle. The saturation of the cycle amplitude takes place through the quenching of the BMR tilt as a function of the internal field. The observed statistical scatter about the mean BMR tilt, built into the model, acts as a source of stochasticity which dominates amplitude fluctuations. The model thus can produce Dalton-like epochs of strongly suppressed cycle amplitude lasting a few cycles and can even shut off entirely following an unfavorable sequence of emergence events.
TIMING OF 29 PULSARS DISCOVERED IN THE PALFA SURVEY
Authors: Lyne A. G. , Stappers B. W. , Bogdanov S. , Ferdman R. D. , Freire P. C. C. , Kaspi V. M. , Knispel B. , Lynch R. , Allen B. , Brazier A. , Camilo F. , Cardoso F. , Chatterjee S. , Cordes J. M. , Crawford F. , Deneva J. S. , Hessels J. W. T. , Jenet F. A. , Lazarus P. , Leeuwen J. van , Lorimer D. R. , Madsen E. , McKee J. , McLaughlin M. A. , Parent E. , Patel C. , Ransom S. M. , Scholz P. , Seymour A. , Siemens X. , Spitler L. G. , Stairs I. H. , Stovall K. , Swiggum J. , Wharton R. S. , Zhu W. W. , Aulbert C. , Bock O. , Eggenstein H.-B. , Fehrmann H. , Machenschalk B. 
Published: January 2017

ABSTRACT
We report on the discovery and timing observations of 29 distant long-period pulsars found in the ongoing Arecibo L-band Feed Array pulsar survey. Following discovery with the Arecibo Telescope, confirmation and timing observations of these pulsars over several years at Jodrell Bank Observatory have yielded high-precision positions and measurements of rotation and radiation properties. We have used multi-frequency data to measure the interstellar scattering properties of some of these pulsars. Most of the pulsars have properties that mirror those of the previously known pulsar population, although four show some notable characteristics. PSRs J1907+0631 and J1925+1720 are young and are associated with supernova remnants or plerionic nebulae: J1907+0631 lies close to the center of SNR G40.5−0.5, while J1925+1720 is coincident with a high-energy Fermi γ-ray source. One pulsar, J1932+1500, is in a surprisingly eccentric, 199 day binary orbit with a companion having a minimum mass of 0.33 M
⊙. Several of the sources exhibit timing noise, and two, PSRs J0611+1436 and J1907+0631, have both suffered large glitches, but with very different post-glitch rotation properties. In particular, the rotational period of PSR J0611+1436 will not recover to its pre-glitch value for about 12 years, a far greater recovery timescale than seen following any other large glitches.
SPITZER PHOTOMETRY OF ∼1 MILLION STARS IN M31 AND 15 OTHER GALAXIES*
Authors: Khan Rubab 
Published: January 2017

ABSTRACT
We present Spitzer IRAC 3.6–8 μm and Multiband Imaging Photometer 24 μm point-source catalogs for M31 and 15 other mostly large, star-forming galaxies at distances ∼3.5–14 Mpc, including M51, M83, M101, and NGC 6946. These catalogs contain ∼1 million sources including ∼859,000 in M31 and ∼116,000 in the other galaxies. They were created following the procedures described in Khan et al. through a combination of point-spread function (PSF) fitting and aperture photometry. These data products constitute a resource to improve our understanding of the IR-bright (3.6–24 μm) point-source populations in crowded extragalactic stellar fields and to plan observations with the James Webb Space Telescope.
i-process Nucleosynthesis and Mass Retention Efficiency in He-shell Flash Evolution of Rapidly Accreting White Dwarfs
Authors: Denissenkov Pavel A. , Herwig Falk , Battino Umberto , Ritter Christian , Pignatari Marco , Jones Samuel , Paxton Bill 
Published: January 2017

Abstract
Based on stellar evolution simulations, we demonstrate that rapidly accreting white dwarfs (WDs) in close binary systems are an astrophysical site for the intermediate neutron-capture process. During recurrent and very strong He-shell flashes in the stable H-burning accretion regime H-rich material enters the He-shell flash convection zone.

reactions release enough energy to potentially impact convection, and i process is activated through the

reaction. The H-ingestion flash may not cause a split of the convection zone as it was seen in simulations of He-shell flashes in post-AGB and low-Z asymptotic giant branch (AGB) stars. We estimate that for the production of first-peak heavy elements this site can be of similar importance for galactic chemical evolution as the s-process production by low-mass AGB stars. The He-shell flashes result in the expansion and, ultimately, ejection of the accreted and then i-process enriched material, via super-Eddington-luminosity winds or Roche-lobe overflow. The WD models do not retain any significant amount of the accreted mass, with a He retention efficiency of

depending on mass and convective boundary mixing assumptions. This makes the evolutionary path of such systems to supernova Ia explosion highly unlikely.
Effectiveness of an Eyelid Thermal Pulsation Procedure to Treat Recalcitrant Dry Eye Symptoms After Laser Vision Correction
Authors: Schallhorn Craig S. , Schallhorn Julie M. , Hannan Stephen , Schallhorn Steven C. 
Published: January 2017

PURPOSE:
To provide an initial retrospective evaluation of the effectiveness of a thermal pulsation system to treat intractable patient-reported dye eye symptoms following laser vision correction.

METHODS:
A total of 109 eyes of 57 patients underwent thermal pulsation therapy (LipiFlow; TearScience, Morrisville, NC) for the treatment of dry eye symptoms following laser vision correction. A standardized dry eye questionnaire, the Standard Patient Evaluation of Eye Dryness (SPEED II), was administered to all patients before and after thermal pulsation therapy. The primary outcome was patient-reported dry eye symptoms as measured by this questionnaire.

RESULTS:

The mean patient age was 49 years (interquartile range [IQR]: 38 to 60), 70% were female, and the primary refractive procedure was LASIK (n = 91, 83%) or photorefractive keratectomy (PRK) (n = 18, 17%). Patients underwent thermal pulsation therapy at a mean of 40.5 months (IQR: 27.6 to 55.0) after the primary procedure. The mean pre-therapy SPEED II questionnaire score was 17.5 (IQR: 14 to 21), with a reduced mean post-therapy score of 10.2 (IQR: 6 to 14; 95% confidence interval [CI]: 8.8 to 11.5,
P
< .001). Patients with PRK tended to report more improvement. At the follow-up clinical evaluation, objective improvements were noted in tear break-up time (+1.9 sec; 95% CI: 1.3 to 2.5), reduction in grade of meibomian gland dysfunction (−0.69; 95% CI: −0.54 to −0.84), and corneal staining (−0.74; 95% CI: −0.57 to −0.91).

CONCLUSIONS:
In this initial retrospective evaluation, a significant improvement in patient-reported dry eye symptoms was observed following thermal pulsation therapy. This treatment modality may have utility in the management of dry eye symptoms following laser vision correction, but further study is needed to define its role.

[
J Refract Surg.
2017;33(1):30–36.]