bluuebunny/crossref_metadata_2025_split huggingface dataset:
Conversation Maps and Diabetes Education Groups: An Evaluation at an Australian Rural Health Service
Authors: Kewming Sue , D’Amore Angelo , Mitchell Eleanor K.L. 
Published: February 2016

Objective. The rural Central Gippsland Health Service (CGHS) assists patients with diabetes through the provision of diabetes education. The purpose of this study was to compare and evaluate the CGHS 5-week didactic program and a modified group-participatory Conversation Maps diabetes education program.
Method. A pre- and post-program survey was conducted of clients who attended the two different diabetes education programs. The survey consisted of a self-constructed demographic questionnaire, the Diabetes Knowledge Test, the Diabetes Empowerment Scale, and the Diabetes Self-Care Activities Measure.
Results. For the CGHS program, there were no differences between pre- and post-program surveys in knowledge scores (11.05 ± 3.56 vs. 12.75 ± 4.19, P = 0.0883, n = 20), self-care activities (4.46 ± 1.11 vs. 4.83 ± 0.68, P = 0.0832, n = 12), or empowerment scores (7.16 ± 1.60 vs. 7.92 ± 1.26, P = 0.0540, n = 17).
For the modified Conversation Maps program, there were significant improvements between pre- and post-program surveys in knowledge scores (12.42 ± 4.15 vs. 15.54 ± 3.79, P = 0.0004, n = 26), self-care activities (4.74 ± 1.09 vs. 5.32 ± 0.80, P = 0.0139, n = 24), and empowerment scores (6.56 ± 2.19 vs. 8.11 ± 1.46, P = 0.0016, n = 21).
The greatest difference between the two programs was observed in knowledge gain (P = 0.0178). Overall, participants were satisfied with both programs, with no difference seen in satisfaction levels (P = 0.9763). A1C results improved in both programs to a mean of 6.7% (P = 0.0071 for CGHS and P = 0.0092 for Conversation Maps).
Conclusion. The modified Conversation Maps program resulted in significant improvements for rural participants.
Effects of Self-Efficacy and Locus of Control on Future Preconception Counseling Plans of Adult Women With Type 1 Diabetes
Authors: Grady Caroline M. , Geller Pamela A. 
Published: February 2016

Objective. The American Diabetes Association (ADA) recommends that women with diabetes attend preconception counseling and improve blood glucose levels before pregnancy to decrease risks of adverse outcomes. However, two-thirds of women with diabetes do not plan their pregnancies. Research has examined views regarding preconception counseling of pregnant women with diabetes, but perceptions of women with diabetes who have never been pregnant have not been explored. The purpose of this study was to examine the relationship between women’s locus of control, self-efficacy, and outcome expectations of preconception counseling.
Design and Methods. A sample of 147 nulligravid women with type 1 diabetes (mean age 25.9 years) was recruited online to complete a self-report survey. Measures included a sociodemographics form, a study-specific questionnaire regarding diabetes management and education, the Reproductive Health Attitudes and Behaviors instrument, and the Diabetes-Specific Locus of Control measure.
Results. A standard multiple linear regression analysis indicated that self-efficacy was positively associated with expectations of preconception counseling (P &lt;0.001), whereas self-blame was negatively associated (P = 0.001). Three-fourths of the women reported not receiving preconception counseling from health care providers.
Conclusion. Self-efficacy was positively associated with women’s expectation of preconception counseling usefulness, whereas self-blame for poor disease management was inversely related. The low reported rates of preconception counseling demonstrate that ADA recommendations for starting preconception counseling at puberty have not been followed uniformly. Women with diabetes should be provided education to increase their belief that they have control over their disease, which may lead to positive perceptions of preconception counseling and healthier pregnancies.
Failure Analysis on a Fractured Rim Star of a Formula Student Racing Car
Authors: Daubach K. , Gummel A. , Kohns L. , Kerscher E. 
Published: February 2016

Abstract
As part of the Formula Student, students independently built new racing cars every year which compete in various disciplines. The Kaiserslautern Racing Team, founded in 2007, has developed and constructed a racing car under Formula Student regulations every year since their foundation. At first, vehicles with combustion engines were built, until in season 2011/2012, the change to electric engines was realized. One of the main objectives for the second electric vehicle (season 2012/2013) was a weight reduction by 100 kg, which required adjustments in all components. For the chassis, this meant a change from 13 to 10 inch rims which were to be bought from a commercial vendor.
A three-piece rim from a US vendor was purchased. Since the installed rim stars showed excessive manufacturing tolerances, for the first time, self-constructed stars were produced and used with the purchased rim base.
Although the rims were designed using an FEM program, as well as an high safety factor the component failed at a test run after the season.
As part of the accompanying seminar to the lecture on damage analysis at TU Kaiserslautern, the cause of the rim failure was investigated. Here, the damage analysis was performed under VDI policy 3822.
Microstructure Preparation Using Glow Discharge Plasma Taking the Examples of Ni-Ti, Cu-Zn and a Ni-Based Alloy
Authors: Undisz A. , Freiberg K. E. , Seide A. , Koenen T. , Rettenmayr M. 
Published: February 2016

Abstract
The present work investigates the universal applicability of glow discharge plasmas for the microstructure representation of different materials taking the example of Ni-Ti alloys, Cu-Zn alloys, and the Ni based alloy “Hastelloy C 276”. Results are compared with the results provided by classical etching methods. Microstructures became visible for the previously mechanically polished materials within a few seconds, even without detailed optimization of the excitation conditions of the glow discharge plasma. The results partially significantly outperfomed the results of the classical preparation techniques with respect to the detectability of structural details such as grain and phase boundaries. Due to the demonstrated wide and relatively uncomplicated applicability, the per se established glow discharge technology is expected to have a huge potential for application for a rapid and high-contrast microstructure representation.
EVOLUTION OF THE X-RAY PROPERTIES OF THE TRANSIENT MAGNETAR XTE J1810–197
Authors: Alford J. A. J. , Halpern J. P. 
Published: February 2016

ABSTRACT
We report on X-ray observations of the 5.54 s transient magnetar XTE J1810–197 using the XMM-Newton and Chandra observatories, analyzing new data from 2008 through 2014, and re-analyzing data from 2003 through 2007 with the benefit of these six years of new data. From the discovery of XTE J1810–197 during its 2003 outburst to the most recent 2014 observations, its 0.3–10 keV X-ray flux has declined by a factor of about 50 from 4.1 × 10−11 to 8.1 × 10−13 erg cm−2 s−1. Its X-ray spectrum has now reached a steady state. Pulsations continue to be detected from a 0.3 keV thermal hot spot that remains on the neutron star (NS) surface. The luminosity of this hot spot exceeds XTE J1810–197’s spin-down luminosity, indicating continuing magnetar activity. We find that XTE J1810–197’s X-ray spectrum is best described by a multiple component blackbody model in which the coldest 0.14 keV component likely originates from the entire NS surface, and the thermal hot-spot is, at different epochs, well described by an either one- or two-component blackbody model. A 1.2 keV absorption line, possibly due to resonant proton scattering, is detected at all epochs. The X-ray flux of the hot spot decreased by

between 2008 and 2009 March, the same period during which XTE J1810–197 became radio quiet.
THE DEVELOPMENT OF EXPLOSIONS IN AXISYMMETRIC AB INITIO CORE-COLLAPSE SUPERNOVA SIMULATIONS OF 12–25
STARS
Authors: Bruenn Stephen W. , Lentz Eric J. , Hix W. Raphael , Mezzacappa Anthony , Harris J. Austin , Messer O. E. Bronson , Endeve Eirik , Blondin John M. , Chertkow Merek Austin , Lingerfelt Eric J. , Marronetti Pedro , Yakunin Konstantin N. 
Published: February 2016

ABSTRACT
We present four ab initio axisymmetric core-collapse supernova simulations initiated from 12, 15, 20, and 25

zero-age main sequence progenitors. All of the simulations yield explosions and have been evolved for at least 1.2 s after core bounce and 1 s after material first becomes unbound. These simulations were computed with our Chimera code employing RbR spectral neutrino transport, special and general relativistic transport effects, and state-of-the-art neutrino interactions. Continuing the evolution beyond 1 s after core bounce allows the explosions to develop more fully and the processes involved in powering the explosions to become more clearly evident. We compute explosion energy estimates, including the negative gravitational binding energy of the stellar envelope outside the expanding shock, of 0.34, 0.88, 0.38, and 0.70 Bethe (B ≡

erg) and increasing at 0.03, 0.15, 0.19, and 0.52

, respectively, for the 12, 15, 20, and 25

models at the endpoint of this report. We examine the growth of the explosion energy in our models through detailed analyses of the energy sources and flows. We discuss how the explosion energies may be subject to stochastic variations as exemplfied by the effect of the explosion geometry of the 20

model in reducing its explosion energy. We compute the proto-neutron star masses and kick velocities. We compare our results for the explosion energies and ejected

masses against some observational standards despite the large error bars in both models and observations.
s-PROCESSING IN AGB STARS REVISITED. II. ENHANCED 13C PRODUCTION THROUGH MHD-INDUCED MIXING
Authors: Trippella O. , Busso M. , Palmerini S. , Maiorca E. , Nucci M. C. 
Published: February 2016

ABSTRACT
Slow neutron captures are responsible for the production of about 50% of elements heavier than iron, mainly occurring during the asymptotic giant branch phase of low-mass stars (1 ≲ M/M
⊙ ≲ 3), where the main neutron source is the 13C(α, n)16O reaction. This last reaction is activated from locally produced 13C, formed by partial mixing of hydrogen into the He-rich layers. We present here the first attempt to describe a physical mechanism for the formation of the 13C reservoir, studying the mass circulation induced by magnetic buoyancy without adding new free parameters to those already involved in stellar modeling. Our approach represents the application to the stellar layers relevant for s-processing of recent exact analytical 2D and 3D models for magneto-hydrodynamic processes at the base of convective envelopes in evolved stars in order to promote downflows of envelope material for mass conservation during the occurrence of a dredge-up phenomenon. We find that the proton penetration is characterized by small concentrations, but is extended over a large fractional mass of the He-layers, thus producing 13C reservoirs of several 10−3
M
⊙. The ensuing 13C-enriched zone has an almost flat profile, while only a limited production of 14N occurs. In order to verify the effects of our new findings we show how the abundances of the main s-component nuclei can be accounted for in solar proportions and how our large 13C-reservoir allows us to solve a few so far unexplained features in the abundance distribution of post-AGB objects.
SIMULATIONS OF THE KELVIN–HELMHOLTZ INSTABILITY DRIVEN BY CORONAL MASS EJECTIONS IN THE TURBULENT CORONA
Authors: Gómez Daniel O. , DeLuca Edward E. , Mininni Pablo D. 
Published: February 2016

ABSTRACT
Recent high-resolution Atmospheric Imaging Assembly/Solar Dynamics Observatory images show evidence of the development of the Kelvin–Helmholtz (KH) instability, as coronal mass ejections (CMEs) expand in the ambient corona. A large-scale magnetic field mostly tangential to the interface is inferred, both on the CME and on the background sides. However, the magnetic field component along the shear flow is not strong enough to quench the instability. There is also observational evidence that the ambient corona is in a turbulent regime, and therefore the criteria for the development of the instability are a priori expected to differ from the laminar case. To study the evolution of the KH instability with a turbulent background, we perform three-dimensional simulations of the incompressible magnetohydrodynamic equations. The instability is driven by a velocity profile tangential to the CME–corona interface, which we simulate through a hyperbolic tangent profile. The turbulent background is generated by the application of a stationary stirring force. We compute the instability growth rate for different values of the turbulence intensity, and find that the role of turbulence is to attenuate the growth. The fact that KH instability is observed sets an upper limit on the correlation length of the coronal background turbulence.
DYNAMICS OF CORONAL RAIN AND DESCENDING PLASMA BLOBS IN SOLAR PROMINENCES. II. PARTIALLY IONIZED CASE
Authors: Oliver R. , Soler R. , Terradas J. , Zaqarashvili T. V. 
Published: February 2016

ABSTRACT
Coronal rain clumps and prominence knots are dense condensations with chromospheric to transition region temperatures that fall down in the much hotter corona. Their typical speeds are in the range 30–150 km s−1 and of the order of 10–30 km s−1, respectively, i.e., they are considerably smaller than free-fall velocities. These cold blobs contain a mixture of ionized and neutral material that must be dynamically coupled in order to fall together, as observed. We investigate this coupling by means of hydrodynamic simulations in which the coupling arises from the friction between ions and neutrals. The numerical simulations presented here are an extension of those of Oliver et al. to the partially ionized case. We find that, although the relative drift speed between the two species is smaller than 1 m s−1 at the blob center, it is sufficient to produce the forces required to strongly couple charged particles and neutrals. The ionization degree has no discernible effect on the main results of our previous work for a fully ionized plasma: the condensation has an initial acceleration phase followed by a period with roughly constant velocity, and, in addition, the maximum descending speed is clearly correlated with the ratio of initial blob to environment density.
CAN LARGE TIME DELAYS OBSERVED IN LIGHT CURVES OF CORONAL LOOPS BE EXPLAINED IN IMPULSIVE HEATING?
Authors: Lionello Roberto , Alexander Caroline E. , Winebarger Amy R. , Linker Jon A. , Mikić Zoran 
Published: February 2016

ABSTRACT
The light curves of solar coronal loops often peak first in channels associated with higher temperatures and then in those associated with lower temperatures. The delay times between the different narrowband EUV channels have been measured for many individual loops and recently for every pixel of an active region observation. The time delays between channels for an active region exhibit a wide range of values. The maximum time delay in each channel pair can be quite large, i.e., >5000 s. These large time delays make-up 3%–26% (depending on the channel pair) of the pixels where a trustworthy, positive time delay is measured. It has been suggested that these time delays can be explained by simple impulsive heating, i.e., a short burst of energy that heats the plasma to a high temperature, after which the plasma is allowed to cool through radiation and conduction back to its original state. In this paper, we investigate whether the largest observed time delays can be explained by this hypothesis by simulating a series of coronal loops with different heating rates, loop lengths, abundances, and geometries to determine the range of expected time delays between a set of four EUV channels. We find that impulsive heating cannot address the largest time delays observed in two of the channel pairs and that the majority of the large time delays can only be explained by long, expanding loops with photospheric abundances. Additional observations may rule out these simulations as an explanation for the long time delays. We suggest that either the time delays found in this manner may not be representative of real loop evolution, or that the impulsive heating and cooling scenario may be too simple to explain the observations, and other potential heating scenarios must be explored.
ON GALACTIC DENSITY MODELING IN THE PRESENCE OF DUST EXTINCTION
Authors: Bovy Jo , Rix Hans-Walter , Green Gregory M. , Schlafly Edward F. , Finkbeiner Douglas P. 
Published: February 2016

ABSTRACT
Inferences about the spatial density or phase-space structure of stellar populations in the Milky Way require a precise determination of the effective survey volume. The volume observed by surveys such as Gaia or near-infrared spectroscopic surveys, which have good coverage of the Galactic midplane region, is highly complex because of the abundant small-scale structure in the three-dimensional interstellar dust extinction. We introduce a novel framework for analyzing the importance of small-scale structure in the extinction. This formalism demonstrates that the spatially complex effect of extinction on the selection function of a pencil-beam or contiguous sky survey is equivalent to a low-pass filtering of the extinction-affected selection function with the smooth density field. We find that the angular resolution of current 3D extinction maps is sufficient for analyzing Gaia sub-samples of millions of stars. However, the current distance resolution is inadequate and needs to be improved by an order of magnitude, especially in the inner Galaxy. We also present a practical and efficient method for properly taking the effect of extinction into account in analyses of Galactic structure through an effective selection function. We illustrate its use with the selection function of red-clump stars in APOGEE using and comparing a variety of current 3D extinction maps.
PROBING THE OUTSKIRTS OF THE EARLY-STAGE GALAXY CLUSTER MERGER A1750
Authors: Bulbul Esra , Randall Scott W. , Bayliss Matthew , Miller Eric , Andrade-Santos Felipe , Johnson Ryan , Bautz Mark , Blanton Elizabeth L. , Forman William R. , Jones Christine , Paterno-Mahler Rachel , Murray Stephen S. , Sarazin Craig L. , Smith Randall K. , Ezer Cemile 
Published: February 2016

ABSTRACT
We present results from recent Suzaku and Chandra X-ray and Multiple Mirrior Telescope optical observations of the strongly merging “double cluster” A1750 out to its virial radius, both along and perpendicular to a putative large-scale structure filament. Some previous studies of individual clusters have found evidence for ICM entropy profiles that flatten at large cluster radii, as compared with the self-similar prediction based on purely gravitational models of hierarchical cluster formation, and gas fractions that rise above the mean cosmic value. Weakening accretion shocks and the presence of unresolved cool gas clumps, both of which are expected to correlate with large-scale structure filaments, have been invoked to explain these results. In the outskirts of A1750, we find entropy profiles that are consistent with self-similar expectations, and gas fractions that are consistent with the mean cosmic value, both along and perpendicular to the putative large-scale filament. Thus, we find no evidence for gas clumping in the outskirts of A1750, in either direction. This may indicate that gas clumping is less common in lower temperature (kT ≈ 4 keV), less massive systems, consistent with some (but not all) previous studies of low-mass clusters and groups. Cluster mass may, therefore, play a more important role in gas clumping than dynamical state. Finally, we find evidence for diffuse, cool (<1 keV) gas at large cluster radii (R
200) along the filament, which is consistent with the expected properties of the denser, hotter phase of the warm–hot intergalactic medium.
QUANTIFYING DISCORDANCE IN THE 2015 PLANCK CMB SPECTRUM
Authors: Addison G. E. , Huang Y. , Watts D. J. , Bennett C. L. , Halpern M. , Hinshaw G. , Weiland J. L. 
Published: February 2016

ABSTRACT
We examine the internal consistency of the Planck 2015 cosmic microwave background (CMB) temperature anisotropy power spectrum. We show that tension exists between cosmological constant cold dark matter (

) model parameters inferred from multipoles

(roughly those accessible to Wilkinson Microwave Anisotropy Probe), and from

, particularly the CDM density,

, which is discrepant at

for a Planck -motivated prior on the optical depth,

. We find some parameter tensions to be larger than previously reported because of inaccuracy in the code used by the Planck Collaboration to generate model spectra. The Planck

constraints are also in tension with low-redshift data sets, including Planck ’s own measurement of the CMB lensing power spectrum (

), and the most precise baryon acoustic oscillation scale determination (

). The Hubble constant predicted by Planck from

,

km s

Mpc−1, disagrees with the most precise local distance ladder measurement of

km s

Mpc−1 at the

level, while the Planck value from

,

km s

Mpc−1, is consistent within

. A discrepancy between the Planck and South Pole Telescope high-multipole CMB spectra disfavors interpreting these tensions as evidence for new physics. We conclude that the parameters from the Planck high-multipole spectrum probably differ from the underlying values due to either an unlikely statistical fluctuation or unaccounted-for systematics persisting in the Planck data.
RADIATION PRESSURE ON FLUFFY SUBMICRON-SIZED GRAINS
Authors: Silsbee Kedron , Draine Bruce T. 
Published: February 2016

ABSTRACT
We investigate the claim that the ratio β of radiation pressure force to gravitational force on a dust grain in our solar system can substantially exceed unity for some grain sizes, provided that grain porosity is high enough. For model grains consisting of random aggregates of silicate spherules, we find that the maximum value of β is almost independent of grain porosity, but for small (

) grains, β actually decreases with increasing porosity. We also investigate the effect of metallic iron and amorphous carbon inclusions in the dust grains and find that while these inclusions do increase the radiation pressure cross-section, β remains below unity for grains with 3 pg of silicate material. These results affect the interpretation of the grain trajectories estimated from the Stardust mission, which were modeled assuming β values exceeding one. We find that radiation pressure effects are not large enough for particles Orion and Hylabrook captured by Stardust to be of interstellar origin given their reported impact velocities. We also consider the effects of solar radiation on transverse velocities and grain spin, and show that radiation pressure introduces both transverse velocities and equatorial spin velocities of several hundred meters per second for incoming interstellar grains at 2 au. These transverse velocities are not important for modeling trajectories, but such spin rates may result in centrifugal disruption of aggregates.