bluuebunny/crossref_metadata_2025_split huggingface dataset:
The Association between Glucose Exposure and the Risk of Peritonitis in Peritoneal Dialysis Patients
Authors: van Diepen Anouk T.N. , van Esch Sadie , Struijk Dirk G. , Krediet Raymond T. 
Published: April 2016

Background and objective Little or no clinical evidence is available on the association between glucose exposure and peritoneal host defense in peritoneal dialysis (PD) patients. The objective of the present study was to quantify the exposure to glucose during the first year on PD and investigate the association with subsequent peritonitis. Methods We analyzed prospectively collected demographic and peritonitis data from incident adult PD patients between 1990 and 2010. For the present study, we conducted a review of both in- and outpatient medical records of all patients to obtain their day-to-day dialysis schemes during the first year on PD. From these data, the average exposure to glucose was quantified. The exposure was stratified into low- and high-glucose groups based on the median, analyzed per standard deviation and in quartiles. Cox proportional hazard models were used to calculate crude and adjusted hazard ratios (HRs) and 95% confidence intervals for the association between glucose exposure and peritonitis. Adjustments were made for age, sex, primary kidney disease, diabetes mellitus, Davies comorbidity score and the treatment period. Results In total, 230 patients were included in the study of whom 151 (66%) experienced a first peritonitis episode. The median follow-up time was 2.6 years (interquartile range [IQR]: 1.9 – 3.8) in the low-glucose group and 3.1 (IQR: 2.1 – 4.2) in the high-glucose group. After adjustment for confounding factors, no association between high glucose exposure and the risk of peritonitis was found (HR: 0.81; 0.55 – 1.17). No association was present when glucose exposure was analyzed per standard deviation (SD) (HR: 0.98; 0.79 – 1.21) or patient quartiles were applied. No association was identified between glucose exposure and severe peritonitis, Staphylococcus aureus peritonitis, or a peritonitis episode that lasted more than 14 days. Conclusions Exposure to glucose is not associated with an increased risk of peritonitis. The equilibrium between glycemic harm to peritoneal host defense and detrimental effects of glucose on invading microorganisms may determine the susceptibility to peritoneal infection.
Comparison of Early Mechanical and Infective Complications in First Time Blind, Bedside, Midline Percutaneous Tenckhoff Catheter Insertion with Ultra-Short Break-in Period in Diabetics and Non-Diabetics: Setting New Standards
Authors: George Ninoo , Alexander Suceena , David Vinoi George , Basu Gopal , Mohapatra Anjali , Valson Anna T. , Jacob Shibu , Pathak Harish K. , Devasia Antony , Tamilarasi Veerasamy , Varughese Santosh 
Published: April 2016

Background There are no large studies that have examined ultra-short break-in period with a blind, bedside, midline approach to Tenckhoff catheter insertion. Methods Observational cohort study of 245 consecutive adult patients who underwent percutaneous catheter insertion for chronic peritoneal dialysis (PD) at our center from January 2009 to December 2013. There were 132 (53.9%) diabetics and 113 (46.1%) non-diabetics in the cohort. Results The mean break-in period for the percutaneous group was 2.68 ± 2.6 days. There were significantly more males among the diabetics (103 [78%] vs 66 [58.4%], p = 0.001). Diabetics had a significantly higher body mass index (BMI) (23.9 ± 3.7 kg/m2 vs 22.2 ± 4 kg/m2, p < 0.001) and lower serum albumin (33.1 ± 6.3 g/L vs 37 ± 6 g/L, p < 0.001) compared with non-diabetics. Poor catheter outflow was present in 6 (4.5%) diabetics and 16 (14.2%) non-diabetics ( p = 0.009). Catheter migration was also significantly more common in the non-diabetic group (11 [9.7%] vs 2 [1.5%], p = 0.004). Primary catheter non-function was present in 17(15%) of the non-diabetics and in 7(5.3%) of the diabetics ( p = 0.01). There were no mortality or major non-procedural complications during the catheter insertions. Among patients with 1 year of follow-up data, catheter survival (93/102 [91.2%] vs 71/82 [86.6%], p = 0.32) and technique survival (93/102 [91.2%] vs 70/82 [85.4%], p = 0.22) at 1 year was comparable between diabetics and non-diabetics, respectively. Conclusions Percutaneous catheter insertion by practicing nephrologists provides a short break-in period with very low mechanical and infective complications. Non-diabetic status emerged as a significant risk factor for primary catheter non-function presumed to be due to more patients with lower BMI and thus smaller abdominal cavities. This is the first report that systematically compares diabetic and non-diabetic patients.
Estimation of the Center Effect on Early Peritoneal Dialysis Failure: A Multilevel Modelling Approach
Authors: Guillouët Sonia , Veniez Ghislaine , Verger Christian , Béchade Clémence , Ficheux Maxence , Uteza Juliette , Lobbedez Thierry 
Published: April 2016

Introduction This study was carried out to investigate the center effect on the risk of peritoneal dialysis (PD) failure within the first 6 months of therapy using a multilevel approach. Methods This was a retrospective cohort study based on data from the French Language Peritoneal Dialysis Registry. We analyzed 5,406 incident patients starting PD between January 2008 and December 2012 in 128 PD centers. The end of the observation period was December 31, 2013. Results Of the 5,406 patients, 415 stopped PD within the first 6 months. There was a significant heterogeneity between centers (variance of the random effect: 0.10). Only 3% of the variance of the event of interest was attributable to differences between centers. At the individual level, only treatment before PD (odds ratio [OR]: 1.93 for hemodialysis and OR: 2.29 for renal transplantation) and underlying nephropathy ( p < 0.01) were associated with early PD failure. At the center level, only center experience was associated (OR: 0.78) with the risk of PD failure. Center effect accounted for 52% of the disparities between centers. Conclusion Center effect on early PD failure is significant. Center experience is associated with a lower risk of transfer to hemodialysis.
Rate of Decline of Residual Kidney Function before and after the Start of Peritoneal Dialysis
Authors: He Lian , Liu Xihui , Li Zi , Abreu Zita , Malavade Tushar , Lok Charmaine E. , Bargman Joanne M. 
Published: April 2016

Background There is a paucity of information on whether peritoneal dialysis (PD) slows the decline of residual kidney function (RKF) compared to the natural slope of RKF decline prior to dialysis start. Our aim was to analyze the RKF decline before and after initiating PD, and to determine the principal factors affecting this decline during the PD period. Methods We determined individual glomerular filtration rates (GFR) for approximately 12 months before and after PD in 77 new PD patients in a large academic medical center (2008 – 2012). The GFR was estimated by the Modification of Diet in Renal Disease (MDRD) equation in the predialysis period and by averaging 24-hour urine creatinine and urea clearances in the PD period. The rate of RKF decline was calculated using unadjusted linear regression analysis. Wilcoxon signed rank test was used to compare RKF decline before and after PD initiation. Multivariate linear regression was used to identify independent risk factors for RKF decline in the PD phase. Results A significantly slower mean rate of RKF decline was observed in the PD period compared with the predialysis period (-0.21 ± 0.30 vs -0.59 ± 0.55 mL/min/1.73 m2/month, p < 0.01). Higher baseline RKF, higher serum phosphate, and older age were independently associated with faster decline of RKF (all p < 0.01). Conclusions In patients with advanced chronic kidney disease, initiating PD was associated with a slower rate of RKF decline compared to the rate in the predialysis period.
COMPOSITIONAL SIMILARITIES AND DISTINCTIONS BETWEEN TITAN’S EVAPORITIC TERRAINS
Authors: MacKenzie S. M. , Barnes Jason W. 
Published: April 2016

ABSTRACT
We document the similarities in composition between the equatorial basins Tui Regio, Hotei Regio, and other 5-μm-bright materials, notably the north polar evaporites, by investigating the presence and extent of an absorption feature at 4.92 μm. In most observations, Woytchugga Lacuna, Ontario Lacus, MacKay Lacus, deposits near Fensal, some of the lakes and dry lake beds south of Ligeia, and the southern shores of Kraken Mare share the absorption feature at 4.92 μm observed in the spectra of Tui and Hotei. Besides Woytchugga and at Fensal, these 5-μm-bright deposits are geomorphologically substantiated evaporites. Thus, the similarity in composition strengthens the hypothesis that Tui and Hotei once contained liquid. Other evaporite deposits, however, do not show the 4.92 μm absorption, notably Muggel Lacus and the shores of Ligeia Mare at the north pole. This difference in composition suggests that there is more than one kind of soluble material in Titan’s lakes that can create evaporite and/or that the surface properties at the Visual and Infrared Mapping Spectrometer wavelength scale are not uniform between the different deposits (crystal size, abundance, etc.). Our results indicate that the surface structure, composition, and formation history of Titan’s evaporites may be at least as dynamic and complex as their Earth counterparts.
ON THE MASS AND ORIGIN OF CHARIKLO’S RINGS
Authors: Pan Margaret , Wu Yanqin 
Published: April 2016

ABSTRACT
Observations in 2013 and 2014 of the Centaur 10199 Chariklo and its ring system consistently indicated that the radial width of the inner, more massive ring varies with longitude. That strongly suggests that this ring has a finite eccentricity despite the fast differential precession that Chariklo’s large quadrupole moment should induce. If the inferred apse alignment is maintained by the ring’s self-gravity, as it is for the Uranian rings, we estimate a ring mass of a few times 1016 g and a typical particle size of a few meters. These values imply a collisional spreading time of ∼105 years, which is somewhat shorter than the typical Centaur dynamical lifetime of a few million years and much shorter than the age of the solar system. In light of this time constraint, we evaluate previously suggested ring formation pathways including collisional ejection and satellite disruption. We also investigate in detail a contrasting formation mechanism, the lofting of dust particles off Chariklo’s surface into orbit via outflows of sublimating CO and/or N2 triggered after Chariklo was scattered inward by giant planets. This alternate scenario predicts that rings should be common among 100 km class Centaurs but rare among Kuiper Belt objects and smaller Centaurs. It also predicts that Centaurs should show seasonal variations in cometary activity with activity maxima occurring shortly after equinox.
EVOLUTION OF THE DUST SIZE DISTRIBUTION OF COMET 67P/CHURYUMOV–GERASIMENKO FROM 2.2 au TO PERIHELION
Authors: Fulle M. , Marzari F. , Della Corte V. , Fornasier S. , Sierks H. , Rotundi A. , Barbieri C. , Lamy P. L. , Rodrigo R. , Koschny D. , Rickman H. , Keller H. U. , López-Moreno J. J. , Accolla M. , Agarwal J. , A’Hearn M. F. , Altobelli N. , Barucci M. A. , Bertaux J.-L. , Bertini I. , Bodewits D. , Bussoletti E. , Colangeli L. , Cosi M. , Cremonese G. , Crifo J.-F. , Da Deppo V. , Davidsson B. , Debei S. , De Cecco M. , Esposito F. , Ferrari M. , Giovane F. , Gustafson B. , Green S. F. , Groussin O. , Grün E. , Gutierrez P. , Güttler C. , Herranz M. L. , Hviid S. F. , Ip W. , Ivanovski S. L. , Jerónimo J. M. , Jorda L. , Knollenberg J. , Kramm R. , Kührt E. , Küppers M. , Lara L. , Lazzarin M. , Leese M. R. , López-Jiménez A. C. , Lucarelli F. , Mazzotta Epifani E. , McDonnell J. A. M. , Mennella V. , Molina A. , Morales R. , Moreno F. , Mottola S. , Naletto G. , Oklay N. , Ortiz J. L. , Palomba E. , Palumbo P. , Perrin J.-M. , Rietmeijer F. J. M. , Rodríguez J. , Sordini R. , Thomas N. , Tubiana C. , Vincent J.-B. , Weissman P. , Wenzel K.-P. , Zakharov V. , Zarnecki J. C. 
Published: April 2016

ABSTRACT
The Rosetta probe, orbiting Jupiter-family comet 67P/Churyumov–Gerasimenko, has been detecting individual dust particles of mass larger than 10−10 kg by means of the GIADA dust collector and the OSIRIS Wide Angle Camera and Narrow Angle Camera since 2014 August and will continue until 2016 September. Detections of single dust particles allow us to estimate the anisotropic dust flux from 67P, infer the dust loss rate and size distribution at the surface of the sunlit nucleus, and see whether the dust size distribution of 67P evolves in time. The velocity of the Rosetta orbiter, relative to 67P, is much lower than the dust velocity measured by GIADA, thus dust counts when GIADA is nadir-pointing will directly provide the dust flux. In OSIRIS observations, the dust flux is derived from the measurement of the dust space density close to the spacecraft. Under the assumption of radial expansion of the dust, observations in the nadir direction provide the distance of the particles by measuring their trail length, with a parallax baseline determined by the motion of the spacecraft. The dust size distribution at sizes >1 mm observed by OSIRIS is consistent with a differential power index of −4, which was derived from models of 67P’s trail. At sizes <1 mm, the size distribution observed by GIADA shows a strong time evolution, with a differential power index drifting from −2 beyond 2 au to −3.7 at perihelion, in agreement with the evolution derived from coma and tail models based on ground-based data. The refractory-to-water mass ratio of the nucleus is close to six during the entire inbound orbit and at perihelion.
INFRARED SUPERNOVA REMNANTS AND THEIR INFRARED-TO-X-RAY FLUX RATIOS
Authors: Koo Bon-Chul , Lee Jae-Joon , Jeong Il-Gyo , Seok Ji Yeon , Kim Hyun-Jeong 
Published: April 2016

ABSTRACT
Recent high-resolution infrared space missions have revealed supernova remnants (SNRs) of diverse morphology in infrared (IR) dust emission that are often very different from their X-ray appearance. The observed range of infrared-to-X-ray (IRX) flux ratios of SNRs is also wide. For a sample of 20 Galactic SNRs, we obtain their IR and X-ray properties and investigate the physical causes for such large differences. We find that the observed IRX flux ratios (

R

IRX,obs

) are related to the IRX morphology, with SNRs with the largest

R

IRX,obs

showing anticorrelated IRX morphology. By analyzing the relation of

R

IRX,obs

to X-ray and IR parameters, we show that the

R

IRX,obs

of some SNRs agrees with theoretical ratios of SNR shocks in which dust grains are heated and destroyed by collisions with plasma particles. For the majority of SNRs, however,

R

IRX,obs

values are either significantly smaller or significantly larger than the theoretical ratios. The latter SNRs have relatively low dust temperatures. We discuss how the natural and/or environmental properties of SNRs could have affected the IRX flux ratios and the IRX morphology of these SNRs. We conclude that the SNRs with largest

R

IRX,obs

are probably located in a dense environment and that their IR emission is from dust heated by shock radiation rather than by collisions. Our result suggests that the IRX flux ratio, together with dust temperature, can be used to infer the nature of unresolved SNRs in external galaxies.
A TECHNIQUE FOR CONSTRAINING THE DRIVING SCALE OF TURBULENCE AND A MODIFIED CHANDRASEKHAR–FERMI METHOD
Authors: Cho Jungyeon , Yoo Hyunju 
Published: April 2016

ABSTRACT
The Chandrasekhar–Fermi (CF) method is a powerful technique for estimating the strength of the mean magnetic field projected on the plane of the sky. In this paper, we present a technique for improving the CF method in which we take into account the averaging effect arising from independent eddies along the line of sight (LOS). In the conventional CF method, the strength of fluctuating magnetic field divided by

4
π

ρ

¯

, where

ρ

¯

is average density, is assumed to be comparable to the LOS velocity dispersion. However, this is not true when the driving scale of turbulence L

f
, i.e., the outer scale of turbulence, is smaller than the size of the system along the LOS L
los. In fact, the conventional CF method overestimates the strength of the mean plane-of-the-sky magnetic field by a factor of

∼

L

los

/

L

f

.

We show that the standard deviation of centroid velocities divided by the average LOS velocity dispersion is a good measure of

L

los

/

L

f

,

which enables us to propose a modified CF method.
OPTICAL TRANSIENTS POWERED BY MAGNETARS: DYNAMICS, LIGHT CURVES, AND TRANSITION TO THE NEBULAR PHASE
Authors: Wang Ling-Jun , Wang S. Q. , Dai Z. G. , Xu Dong , Han Yan-Hui , Wu X. F. , Wei Jian-Yan 
Published: April 2016

ABSTRACT
Millisecond magnetars can be formed via several channels: core collapse of massive stars, accretion-induced collapse of white dwarfs (WDs), double WD mergers, double neutron star (NS) mergers, and WD-NS mergers. Because the mass of ejecta from these channels could be quite different, their light curves are also expected to be diverse. We evaluate the dynamic evolution of optical transients powered by millisecond magnetars. We find that the magnetar with a short spin-down timescale converts its rotational energy mostly into the kinetic energy of the transient, while the energy of a magnetar with a long spin-down timescale goes into radiation of the transient. This leads us to speculate that hypernovae could be powered by magnetars with short spin-down timescales. At late times the optical transients will gradually evolve into a nebular phase because of the photospheric recession. We treat the photosphere and nebula separately because their radiation mechanisms are different. In some cases the ejecta could be light enough that the magnetar can accelerate it to a relativistic speed. It is well known that the peak luminosity of a supernova (SN) occurs when the luminosity is equal to the instantaneous energy input rate, as shown by Arnett. We show that photospheric recession and relativistic motion can modify this law. The photospheric recession always leads to a delay of the peak time

relative to the time

at which the SN luminosity equals the instantaneous energy input rate. Relativistic motion, however, may change this result significantly.
X-RAY SPECTRA OF THE HIGH-MASS X-RAY BINARY 4U 1700-37 USING BEPPOSAX, SUZAKU, AND RXTE OBSERVATIONS
Authors: Seifina Elena , Titarchuk Lev , Shaposhnikov Nikolai 
Published: April 2016

ABSTRACT
We present an X-ray spectral analysis of the high-mass binary 4U 1700-37 during its hard-soft state evolution. We use BeppoSAX, Suzaku, and Rossi X-ray Timing Explorer observations for this investigation. We argue that the X-ray broadband spectra during all of the spectral states can be adequately reproduced by a model consisting of a low-temperature blackbody component, two Comptonized components which are both due to the presence of a Compton cloud (CC) that up-scatters seed photons of T

s1 ≲ 1.4 keV and T

s2 < 1 keV, and an iron-line component. Using this model, we find that the photon power-law index is almost constant, Γ1 ∼ 2 for all spectral states. However, Γ2 shows behavior that is dependent on the spectral state. Namely, Γ2 is quasi-constant at the level of Γ2 ∼ 2 while the CC plasma temperature

kT

e

(
2
)

is less than 40 keV; on the other hand, Γ2 is in the range of 1.3 < Γ2 < 2 when

kT

e

(
2
)

is greater than 40 keV. We explain this quasi-stability of Γ during most of the hard-soft transitions of 4U 1700-37 in the framework of a model in which the resulting spectrum is described by two Comptonized components. We find that these Comptonized spectral components of the high-mass X-ray binaries 4U 1700-37 are similar to those previously found in neutron star (NS) sources. This index dependence versus both the mass accretion rate and kT

e
revealed in 4U 1700-37 is universal observational evidence for the presence of an NS in 4U 1700-37.
DISCOVERY OF THE CANDIDATE OFF-NUCLEAR ULTRASOFT HYPER-LUMINOUS X-RAY SOURCE 3XMM J141711.1+522541
Authors: Lin Dacheng , Carrasco Eleazar R. , Webb Natalie A. , Irwin Jimmy A. , Dupke Renato , Romanowsky Aaron J. , Ramirez-Ruiz Enrico , Strader Jay , Homan Jeroen , Barret Didier , Godet Olivier 
Published: April 2016

ABSTRACT
We report the discovery of an off-nuclear ultrasoft hyper-luminous X-ray source candidate 3XMM J141711.1+522541 in the inactive S0 galaxy SDSS J141711.07+522540.8 (z = 0.41827, d

L
= 2.3 Gpc) in the Extended Groth Strip. It is located at a projected offset of ∼1.″0 (5.2 kpc) from the nucleus of the galaxy and was serendipitously detected in five XMM-Newton observations in 2000 July. Two observations have enough counts and can be fitted with a standard thermal disk with an apparent inner disk temperature

kT

MCD

∼
0.13

keV

and a 0.28–14.2 keV unabsorbed luminosity L
X ∼ 4 × 1043 erg s−1 in the source rest frame. The source was still detected in three Chandra observations in 2002 August, with similarly ultrasoft but fainter spectra (kT
MCD ∼ 0.17 keV, L
X ∼ 0.5 × 1043 erg s−1). It was not detected in later observations, including two by Chandra in 2005 October, one by XMM-Newton in 2014 January, and two by Chandra in 2014 September–October, implying a long-term flux variation factor of >14. Therefore the source could be a transient with an outburst in 2000–2002. It has a faint optical counterpart candidate, with apparent magnitudes of m
F606W = 26.3 AB mag and m
F814W = 25.5 AB mag in 2004 December (implying an absolute V-band magnitude of ∼−15.9 AB mag). We discuss various explanations for the source and find that it is best explained as a massive black hole (BH) embedded in the nucleus of a possibly stripped satellite galaxy, with the X-ray outburst due to tidal disruption of a surrounding star by the BH. The BH mass is ∼105
M
⊙, assuming the peak X-ray luminosity at around the Eddington limit.
CONSTRAINING WHITE DWARF STRUCTURE AND NEUTRINO PHYSICS IN 47 TUCANAE
Authors: Goldsbury R. , Heyl J. , Richer H. B. , Kalirai J. S. , Tremblay P. E. 
Published: April 2016

ABSTRACT
We present a robust statistical analysis of the white dwarf cooling sequence in 47 Tucanae. We combine Hubble Space Telescope UV and optical data in the core of the cluster, Modules for Experiments in Stellar Evolution (MESA) white dwarf cooling models, white dwarf atmosphere models, artificial star tests, and a Markov Chain Monte Carlo sampling method to fit white dwarf cooling models to our data directly. We use a technique known as the unbinned maximum likelihood to fit these models to our data without binning. We use these data to constrain neutrino production and the thickness of the hydrogen layer in these white dwarfs. The data prefer thicker hydrogen layers

(

q

H

=
3.2
×

10

−
5

)

and we can strongly rule out thin layers

(

q

H

=

10

−
6

)

. The neutrino rates currently in the models are consistent with the data. This analysis does not provide a constraint on the number of neutrino species.