bluuebunny/crossref_metadata_2025_split huggingface dataset:
HbA1c and the Prediction of Type 2 Diabetes in Children and Adults
Authors: Vijayakumar Pavithra , Nelson Robert G. , Hanson Robert L. , Knowler William C. , Sinha Madhumita 
Published: November 2016

OBJECTIVE
Long-term data validating glycated hemoglobin (HbA1c) in assessing the risk of type 2 diabetes in children are limited. HbA1c, fasting plasma glucose (FPG), and 2-h postload plasma glucose (2hPG) concentrations were measured in a longitudinal study of American Indians to determine their utility in predicting incident diabetes, all of which is thought to be type 2 in this population.

RESEARCH DESIGN AND METHODS
Incident diabetes (FPG ≥126 mg/dL [7.0 mmol/L], 2hPG ≥200 mg/dL [11.1 mmol/L], HbA1c ≥6.5% [8 mmol/mol], or clinical diagnosis) was determined in 2,095 children without diabetes ages 10–19 years monitored through age 39, and in 2,005 adults ages 20–39 monitored through age 59. Areas under the receiver operating characteristic (ROC) curve for HbA1c, FPG, and 2hPG in predicting diabetes within 10 years were compared.

RESULTS
During long-term follow-up of children and adolescents who did not initially have diabetes, the incidence rate of subsequent diabetes was fourfold (in boys) as high and more than sevenfold (in girls) as high in those with HbA1c ≥5.7% as in those with HbA1c ≤5.3%—greater rate ratios than experienced by adults in the same HbA1c categories. Analyses of ROCs revealed no significant differences between HbA1c, FPG, and 2hPG in sensitivity and specificity for identifying children and adolescents who later developed diabetes.

CONCLUSIONS
HbA1c is a useful predictor of diabetes risk in children and can be used to identify prediabetes in children with other type 2 diabetes risk factors with the same predictive value as FPG and 2hPG.
Flow diversion in the treatment of aneurysms: a randomized care trial and registry
Authors: Raymond Jean , Gentric Jean-Christophe , Darsaut Tim E. , Iancu Daniela , Chagnon Miguel , Weill Alain , Roy Daniel 
Published: November 2016

OBJECTIVEThe Flow Diversion in the Treatment of Intracranial Aneurysm Trial (FIAT) was designed to guide the clinical use of flow diversion, an innovative method to treat intracranial aneurysms, within a care trial and to study safety and efficacy.METHODSFIAT, conducted in 3 Canadian hospitals, proposed randomized allocation to flow diversion or standard management options (observation, coil embolization, parent vessel occlusion, or clip placement), and a registry of non-randomized patients treated with flow diversion. The primary safety outcome was death or dependency (modified Rankin Scale score > 2) at 3 months, to be determined for all patients who received flow diversion at any time. The primary efficacy outcome was angiographic occlusion at 3–12 months combined with an independent clinical outcome.RESULTSOf 112 participating patients recruited between May 2, 2011, and February 25, 2015, 78 were randomized (39 in each arm), and 34 received flow diversion within the registry. The study was halted due to safety concerns. Twelve (16%) of 75 patients (95% CI 8.9%–26.7%) who were allocated to or received flow diversion at any time were dead (n = 8) or dependent (n = 4) at 3 months or more, crossing a predefined safety boundary. Death or dependency occurred in 5 (13.2%) of 38 patients randomly allocated and treated by flow diversion (95% CI 5.0%–28.9%) and in 5 (12.8%) of 39 patients allocated to standard treatment (95% CI 4.8%–28.2%). Efficacy was below expectations of the trial hypothesis: 16 (42.1%) of 38 patients (95% CI 26.7%–59.1%) randomly allocated to flow diversion failed to reach the primary outcome, as compared with 14 (35.9%) of 39 patients allocated to standard treatment (95% CI 21.7%–52.9%).CONCLUSIONSFlow diversion was not as safe and effective as hypothesized. More randomized trials are needed to determine the role of flow diversion in the management of aneurysms.Clinical trial registration no.: NCT01349582 (clinicaltrials.gov)
A systematic review of overall survival in pediatric primary glioblastoma multiforme of the spinal cord
Authors: Konar Subhas K. , Bir Shyamal C. , Maiti Tanmoy K. , Nanda Anil 
Published: November 2016

OBJECTIVE
The incidence of primary spinal cord glioblastoma multiforme (GBM) in the pediatric age group is very rare. Only a few case series and case reports have been published in the literature; therefore, overall survival (OS) outcome and the as-yet poorly defined management options are not discussed in detail. The authors performed a cumulative survival analysis of all reported cases of pediatric spinal cord GBM to identify the predictive factors related to final survival outcome.

METHODS
A comprehensive search for relevant articles was performed on PubMed's electronic database MEDLINE for the period from 1950 to 2015 using the search words “malignant spinal cord tumor” and “spinal glioblastoma multiforme.” This study was limited to patients younger than 18 years of age. Survival rates for children with various tumor locations and treatments were collected from the published articles and analyzed.

RESULTS
After an extensive literature search, 29 articles met the study inclusion criteria. From the detailed information in these articles, the authors found 53 children eligible for the survival analysis. The majority (45%) of the children were more than 12 years old. Thirty-four percent of the cases were between 7 and 12 years of age, and 21% were younger than 7 years. In the Kaplan-Meier survival analysis, children younger than 7 years of age had better survival (13 months) than the children older than 7 years (7–12 years: 10 months, > 12 years: 9 months; p = 0.01, log-rank test). Fifty-five percent of the children were female and 45% were male. A cervical tumor location (32%) was the most common, followed by thoracic (28.3%). Cervicothoracic (18.9%) and conus (18.8%) tumor locations shared the same percentage of cases. Cervical tumors had a worse outcome than tumors in other locations (p = 0.003, log-rank test). The most common presenting symptom was limb weakness (53%), followed by sensory disturbances (25%). Median OS was 10 months. The addition of adjuvant therapy (radiotherapy [RT] and/or chemotherapy [CT]) after surgery significantly improved OS (p = 0.01, log-rank test). Children who underwent gross-total resection and RT had better outcomes than those who underwent subtotal resection and RT (p = 0.04, log-rank test). Cerebrospinal fluid spread, hydrocephalus, brain metastasis, and spinal metastasis were not correlated with OS in primary spinal GBM.

CONCLUSIONS
Adjuvant therapy after surgery had a beneficial effect on overall outcome of spinal GBM in the pediatric age group. Gross-total resection followed by RT produced a better outcome than subtotal resection with RT. Further large-scale prospective study is required to establish the genetic and molecular factors related to OS in primary GBM of the spinal cord in pediatric patients.
Lokale Anpassung bei Waldbaumarten: genetische Prozesse und Bedeutung im Klimawandel
Authors: Rellstab Christian , Pluess Andrea R. , Gugerli Felix 
Published: November 2016

Local adaptation in forest trees: genetic processes and relevance under climate change
Forest trees will have to adapt to future climatic changes, a process that will comprise genetic changes as a key component. Owing to technological advances it is now possible to identify the signature of natural selection and local adaptation in the genome. Environmental association analyses aim at associating adaptive genetic patterns with environmental parameters describing the local habitat. On the basis of such studies – including own investigations using oak and beech in Switzerland –, we show that forest trees are genetically differentiated along various environmental gradients, especially temperature and precipitation. Numerous genes could be found that presumably play a role in the adaptation to such environmental factors. Based on these findings, one could identify trees or stands that are adapted to future local conditions, and respective seed material could be considered in silviculture. Because such approaches are still in their infancy and because genome-environment interactions are complex, management strategies should focus on the preservation of (adaptive) genetic diversity, natural regeneration, and connectivity among stands. This would set the basis for the local adaptation of forest stands to altered environmental conditions by natural processes.
Identification of Legionella from clinically diagnosed pneumonia patients and environmental samples
Authors: Jahan Rownak , Tarafder Shirin , Saleh Ahmed Abu , Miah Ruhul Amin 
Published: November 2016

Legionnaires disease is a multisystem disease with life-threatening acute and severe form of pneumonia which is responsible for 2-9% pneumonia with high mortality. Eighty six respiratory tract samples and urine were collected from clinically diagnosed pneumonia patients and 12 water samples were collected from different environment. Identification of Legionella was done by culture and Polymerase Chain Reaction (PCR) of respiratory tract samples and environmental samples and Legionella Antigen (Ag) in urine was detected by Immunochromatographic test (ICT). Legionella was identified from 4 (4.65%) clinically diagnosed pneumonia patients of which 1 (1.16%) case was culture positive, 1 (1.16%) case was urine ICT positive and PCR was positive in all four cases. Of the 12 water samples tested, 4 (33.33%) samples were Legionella positive by PCR but culture results of these samples were negative. Identification of Legionella should be done by PCR in parallel with culture and urine ICT. Detection of Legionella in environmental samples is also needed to explore possible links between the water sources and disease transmission in population.
LOW-FREQUENCY RADIO OBSERVATIONS OF THE SOLAR CORONA WITH ARCMINUTE ANGULAR RESOLUTION: IMPLICATIONS FOR CORONAL TURBULENCE AND WEAK ENERGY RELEASES
Authors: Mugundhan V. , Ramesh R. , Barve Indrajit V. , Kathiravan C. , Gireesh G. V. S. , Kharb P. , Misra Apurva 
Published: November 2016

ABSTRACT
We report on the first long baseline interferometer (length ≈8 km) observations of the solar corona at 37 MHz that were carried out recently with an angular resolution of

. The results indicate that, (1) discrete radio sources of the aforesaid angular size or even lesser are present in the solar corona from where radiation at the above frequency originates. This constrains the angular broadening of radio sources at low frequencies due to scattering by density turbulence in the solar corona; and (2) the observed sources in the present case correspond to the weakest energy releases in the solar atmosphere reported so far.
WHAT IS THE SOURCE OF QUIET SUN TRANSITION REGION EMISSION?
Authors: Schmit D. J. , De Pontieu Bart 
Published: November 2016

ABSTRACT
Dating back to the first observations of the on-disk corona, there has been a qualitative link between the photosphere’s magnetic network and enhanced transition-temperature plasma emission. These observations led to the development of a general model that describes emission structures through the partitioning of the atmospheric volume with different magnetic loop geometries that exhibit different energetic equilibria. Does the internetwork produce transition-temperature emission? What fraction of network flux connects to the corona? How does quiet Sun emission compare with low-activity Sun-like stars? In this work, we revisit the canonical model of the quiet Sun, with high-resolution observations from the Interface Region Imaging Spectrograph (IRIS) and HMI in hand, to address those questions. We use over 900 deep exposures of Si iv 1393 Å from IRIS along with nearly simultaneous HMI magnetograms to quantify the correlation between transition-temperature emission structures and magnetic field concentrations through a number of novel statistics. Our observational results are coupled with analysis of the Bifrost MHD model and a large-scale potential field model. Our results paint a complex portrait of the quiet Sun. We measure an emission signature in the distant internetwork that cannot be attributed to network contribution. We find that the dimmest regions of emission are not linked to the local vertical magnetic field. Using the MHD simulation, we categorize the emission contribution from cool mid-altitude loops and high-altitude coronal loops and discuss the potential emission contribution of spicules. Our results provide new constraints on the coupled solar atmosphere so that we can build on our understanding of how dynamic thermal and magnetic structures generate the observed phenomena in the transition region.
A UNIFIED MODEL OF GRAIN ALIGNMENT: RADIATIVE ALIGNMENT OF INTERSTELLAR GRAINS WITH MAGNETIC INCLUSIONS
Authors: Hoang Thiem , Lazarian A. 
Published: November 2016

ABSTRACT
The radiative torque (RAT) alignment of interstellar grains with ordinary paramagnetic susceptibilities has been supported by earlier studies. The alignment of such grains depends on the so-called RAT parameter q
max, which is determined by the grain shape. In this paper, we elaborate on our model of RAT alignment for grains with enhanced magnetic susceptibility due to iron inclusions, such that RAT alignment is magnetically enhanced, which we term the MRAT mechanism. Such grains can be aligned with high angular momentum at the so-called high-J attractor points, achieving a high degree of alignment. Using our analytical model of RATs, we derive the critical value of the magnetic relaxation parameter δ
m to produce high-J attractor points as functions of q
max and the anisotropic radiation angle relative to the magnetic field ψ. We find that if about 10% of the total iron abundance present in silicate grains is forming iron clusters, this is sufficient to produce high-J attractor points for all reasonable values of q
max. To calculate the degree of grain alignment, we carry out numerical simulations of MRAT alignment by including stochastic excitations from gas collisions and magnetic fluctuations. We show that large grains can achieve perfect alignment when the high-J attractor point is present, regardless of the values of q
max. Our obtained results pave the way for the physical modeling of polarized thermal dust emission as well as magnetic dipole emission. We also find that millimeter-sized grains in accretion disks may be aligned with the magnetic field if they are incorporated with iron nanoparticles.
PONDEROMOTIVE ACCELERATION IN CORONAL LOOPS
Authors: Dahlburg R. B. , Laming J. M. , Taylor B. D. , Obenschain K. 
Published: November 2016

ABSTRACT
Ponderomotive acceleration has been asserted to be a cause of the first ionization potential (FIP) effect, the well-known enhancement in abundance by a factor of 3–4 over photospheric values of elements in the solar corona with FIP less than about 10 eV. It is shown here by means of numerical simulations that ponderomotive acceleration occurs in solar coronal loops, with the appropriate magnitude and direction, as a “by-product” of coronal heating. The numerical simulations are performed with the HYPERION code, which solves the fully compressible three-dimensional magnetohydrodynamic equations including nonlinear thermal conduction and optically thin radiation. Numerical simulations of coronal loops with an axial magnetic field from 0.005 to 0.02 T and lengths from 25,000 to 75,000 km are presented. In the simulations the footpoints of the axial loop magnetic field are convected by random, large-scale motions. There is a continuous formation and dissipation of field-aligned current sheets, which act to heat the loop. As a consequence of coronal magnetic reconnection, small-scale, high-speed jets form. The familiar vortex quadrupoles form at reconnection sites. Between the magnetic footpoints and the corona the reconnection flow merges with the boundary flow. It is in this region that the ponderomotive acceleration occurs. Mirroring the character of the coronal reconnection, the ponderomotive acceleration is also found to be intermittent.
OCULAR SHOCK FRONT IN THE COLLIDING GALAXY IC 2163
Authors: Kaufman Michele , Elmegreen Bruce G. , Struck Curtis , Elmegreen Debra Meloy , Bournaud Frédéric , Brinks Elias , Juneau Stephanie , Sheth Kartik 
Published: November 2016

ABSTRACT
ALMA observations in the 12CO

line of the interacting galaxy pair IC 2163 and NGC 2207 at 2″ × 1.″5 resolution reveal how the encounter drives gas to pile up in narrow, ∼1 kpc wide, “eyelids” in IC 2163. IC 2163 and NGC 2207 are involved in a grazing encounter, which has led to the development in IC 2163 of an eye-shaped (ocular) structure at mid-radius and two tidal arms. The CO data show that there are large velocity gradients across the width of each eyelid, with a mixture of radial and azimuthal streaming of gas at the outer edge of the eyelid relative to its inner edge. The sense of the radial streaming in the eyelids is consistent with the idea that gas from the outer part of IC 2163 flows inward until its radial streaming slows down abruptly and the gas piles up in the eyelids. The radial compression at the eyelids causes an increase in the gas column density by direct radial impact and also leads to a high rate of shear. A linear regression of the molecular column density

on the magnitude of

across the width of the eyelid at fixed values of azimuth finds a strong correlation between

and

. Substantial portions of the eyelids have high velocity dispersion in CO, indicative of elevated turbulence there.
THE INTERNAL STRUCTURE AND PROPAGATION OF MAGNETOHYDRODYNAMICAL THERMONUCLEAR FLAMES
Authors: Remming Ian S. , Khokhlov Alexei M. 
Published: November 2016

ABSTRACT
We present general equations for non-ideal, reactive flow magnetohydrodynamics (RFMHD) in the form best suited for describing thermonuclear combustion in high-density degenerate matter of SNe Ia. The relative importance of various non-ideal effects is analyzed as a function of characteristic spatial and temporal scales of the problem. From the general RFMHD equations, we derive the one-dimensional ordinary differential equations describing the steady-state propagation of a planar thermonuclear flame front in a magnetic field. The physics of the flame is first studied qualitatively using a simple case of one-step Arrhenius kinetics, a perfect gas equation of state (EOS), and constant thermal conductivity coefficients. After that, the equations are solved, the internal flame front structure is calculated, and the flame velocity, S

l
, and flame thickness, δ

l
, are found for carbon–oxygen degenerate material of supernovae using a realistic EOS, transport properties, and detailed nuclear kinetics. The magnetic field changes the flame behavior significantly, both qualitatively and quantitatively, as compared to the non-magnetic case of classical combustion. (1) The magnetic field influences the evolutionarity of a flame front and makes it impossible for a flame to propagate steadily in a wide range of magnetic field strengths and orientations relative to the front. (2) When the flame moves steadily, it can propagate in several distinct modes, the most important being the slow C

S
and super-Alfvénic C
sup modes. (3) The speed of the flame can be diminished or enhanced by up to several factors relative to the non-magnetic laminar flame speed.
ELUCID—EXPLORING THE LOCAL UNIVERSE WITH RECONSTRUCTED INITIAL DENSITY FIELD. III. CONSTRAINED SIMULATION IN THE SDSS VOLUME
Authors: Wang Huiyuan , Mo H. J. , Yang Xiaohu , Zhang Youcai , Shi JingJing , Jing Y. P. , Liu Chengze , Li Shijie , Kang Xi , Gao Yang 
Published: November 2016

ABSTRACT
A method we developed recently for the reconstruction of the initial density field in the nearby universe is applied to the Sloan Digital Sky Survey Data Release 7. A high-resolution N-body constrained simulation (CS) of the reconstructed initial conditions, with 30723 particles evolved in a

box, is carried out and analyzed in terms of the statistical properties of the final density field and its relation with the distribution of Sloan Digital Sky Survey galaxies. We find that the statistical properties of the cosmic web and the halo populations are accurately reproduced in the CS. The galaxy density field is strongly correlated with the CS density field, with a bias that depends on both galaxy luminosity and color. Our further investigations show that the CS provides robust quantities describing the environments within which the observed galaxies and galaxy systems reside. Cosmic variance is greatly reduced in the CS so that the statistical uncertainties can be controlled effectively, even for samples of small volumes.
DISENTANGLING THE VIRGO OVERDENSITY WITH RR LYRAE STARS
Authors: Vivas A. Katherina , Zinn Robert , Farmer John , Duffau Sonia , Ping Yiding 
Published: November 2016

ABSTRACT
We use a combination of spatial distribution and radial velocity to search for halo substructures in a sample of 412 RR Lyrae stars (RRLSs) that covers a region of ∼525 square degrees of the Virgo overdensity (VOD) and spans distances from the Sun from 4 to 75 kpc. With a friends-of-friends algorithm we identified six high-significance groups of RRLSs in phase space, which we associate mainly with the VOD and with the Sagittarius stream. Four other groups were also flagged as less significant overdensities. Three high-significance and three lower-significance groups have distances between ∼10 and 20 kpc, which places them in the distance range attributed by others to the VOD. The largest of these is the Virgo stellar stream at 19 kpc, which has 18 RRLSs, a factor of two increase over the number known previously. While these VOD groups are distinct according to our selection criteria, their overlap in position and distance and, in a few cases, similarity in radial velocity are suggestive that they may not all stem from separate accretion events. Even so, the VOD appears to be caused by more than one overdensity. The Sagittarius (Sgr) stream is a very obvious feature in the background of the VOD at a mean distance of 44 kpc. Two additional high-significance groups were detected at distances

. Their radial velocities and locations differ from the expected path of the Sgr debris in this part of the sky, and they are likely to be remnants of other accretion events.