bluuebunny/crossref_metadata_2025_split huggingface dataset:
Two‐way Interaction Effects of Perioperative Complications on 30‐Day Mortality in General Surgery
Authors: Kim Minjae , Li Guohua 
Published: July 2017

AbstractBackgroundMultiple perioperative complications increase mortality risk, and certain complications synergistically increase this risk to a greater degree than might be expected if the complications were independent, but these effects are not well established.MethodsThis is a retrospective cohort study of 422,827 intraabdominal general surgery patients (American College of Surgeons National Surgical Quality Improvement Program 2005–2011). Eight complications were evaluated: acute respiratory failure (ARF), acute kidney injury (AKI), sepsis/septic shock, stroke, cardiac arrest (CA), myocardial infarction (MI), deep vein thrombosis/pulmonary embolus, and transfusion. Each combination of two complications (28 total) was modeled using a Cox model for 30‐day mortality, with adjustment for preoperative comorbidities and risk factors. Additive interaction was determined with the relative excess risk due to interaction (RERI). A positive RERI indicates that the mortality risk with both complications is greater than the sum of the individual mortality risks. Bonferroni correction was applied (α= 0.05/28 = 0.0018).ResultsSeven combinations demonstrated positive interaction: sepsis‐CA (RERI 88.1;p< 0.0001), ARF–AKI (RERI 50.5;p< 0.0001), AKI–sepsis (RERI 33.9;p< 0.0001), sepsis–stroke (RERI 33.9;p< 0.0001), ARF–stroke (RERI 32.3;p< 0.0001), AKI–MI (RERI 24.5;p= 0.0013), and ARF–sepsis (RERI 19.2;p< 0.0001). Two combinations demonstrated negative interaction: ARF–CA (RERI −65.1;p= 0.0017) and CA‐transfusion (RERI −52.0,p< 0.0001).ConclusionsInteraction effects exist between certain complications to increase the risk of short‐term mortality. ARF, AKI, sepsis, and stroke were most likely to be involved in positive interactions. Further research into the mechanisms for these effects will be necessary to develop strategies to minimize the compounding effects of multiple complications in the perioperative period.
An introduction to computational tools for differential binding analysis with ChIP‐seq data
Authors: Tu Shiqi , Shao Zhen 
Published: July 2017

BackgroundGene transcription in eukaryotic cells is collectively controlled by a large panel of chromatin associated proteins and ChIP‐seq is now widely used to locate their binding sites along the whole genome. Inferring the differential binding sites of these proteins between biological conditions by comparing the corresponding ChIP‐seq samples is of general interest, yet it is still a computationally challenging task.ResultsHere, we briefly review the computational tools developed in recent years for differential binding analysis with ChIP‐seq data. The methods are extensively classified by their strategy of statistical modeling and scope of application. Finally, a decision tree is presented for choosing proper tools based on the specific dataset.ConclusionsComputational tools for differential binding analysis with ChIP‐seq data vary significantly with respect to their applicability and performance. This review can serve as a practical guide for readers to select appropriate tools for their own datasets.
Multifaceted roles of complementary sequences on circRNA formation
Authors: Yang Qin , Wang Ying , Yang Li 
Published: July 2017

BackgroundCircular RNAs (circRNAs) from back‐spliced exon(s) are characterized by the covalently closed loop feature with neither 5′ to 3′ polarity nor polyadenylated tail. By using specific computational approaches that identify reads mapped to back‐splice junctions with a reversed genomic orientation, ten thousands of circRNAs have been recently re‐identified in various cell lines/tissues and across different species. Increasing lines of evidence suggest that back‐splicing is catalyzed by the canonical spliceosomal machinery and modulated by cis‐elements and trans‐factors.ResultsIn this mini‐review, we discuss our current understanding of circRNA biogenesis regulation, mainly focusing on the complex regulation of complementary sequences, especially Alus in human, on circRNA formation.ConclusionsBack‐splicing can be significantly facilitated by RNA pair formed by orientation‐opposite complementary sequences that juxtapose flanking introns of circularized exon(s). RNA pair formed within individual introns competes with RNA pair formed across flanking introns in the same gene locus, leading to distinct choices for either canonical splicing or back‐splicing. Multiple RNA pairs that bracket different circle‐forming exons compete for alternative back‐splicing selection, resulting in multiple circRNAs generated in a single gene locus.
A Historical Review of Gender-Affirming Medicine: Focus on Genital Reconstruction Surgery
Authors: Frey Jordan D. , Poudrier Grace , Thomson Jennifer E. , Hazen Alexes 
Published: July 2017

AbstractGender dysphoria (Diagnostic and Statistical Manual of Mental Disorders, Fifth Edition) is characterized by a marked discrepancy between one’s birth-assigned sex and one’s gender identity and is sometimes addressed by gender-affirming surgery. As public visibility and institutional support for the transgender and gender non-conforming population continue to increase, the demand for competent multidisciplinary teams of medical professionals equipped to care for this population is expected to rise—including plastic surgeons, urologists, gynecologists, endocrinologists, and breast surgeons, among others. Genital reconstruction procedures for the male-to-female and female-to-male transgender patient present unique surgical challenges that continue to evolve from their respective origins in the 19th and 20th centuries. A historical review of surgical techniques and standards of care attendant to gender-affirming medicine is presented, with foremost emphasis placed on how techniques for genital reconstruction in particular continue to evolve and advance. In addition, the current status of transition-related health care in the United States, including research gaps and contemporary clinical challenges, is reviewed.
Magnitude, numerosity, and development of number: Implications for mathematics disabilities
Authors: Jordan Nancy C. , Rinne Luke , Resnick Ilyse M. 
Published: July 2017

AbstractLeibovich et al. challenge the prevailing view that non-symbolic number sense (e.g., sensing number the same way one might sense color) is innate, that detection of numerosity is distinct from detection of continuous magnitude. In the present commentary, the authors' viewpoint is discussed in light of the integrative theory of numerical development along with implications for understanding mathematics disabilities.
What is the precise role of cognitive control in the development of a sense of number?
Authors: Merkley Rebecca , Scerif Gaia , Ansari Daniel 
Published: July 2017

AbstractThe theory put forward by Leibovich et al. of how children acquire a sense of number does not specify the mechanisms through which cognitive control plays a role in this process. We argue that visual attention and number word knowledge influence each other over development and contribute to the development of the concept of number.
The contributions of non-numeric dimensions to number encoding, representations, and decision-making factors
Authors: Odic Darko 
Published: July 2017

AbstractLeibovich et al. suggest that congruency effects in number perception (biases towards smaller, denser, etc., dots) are evidence for the number's dependence on these dimensions. I argue that they fail to differentiate between effects at three distinct levels of number perception – encoding, representations, and decision making – and that differentiating between these allows the number to be independent from, but correlated with, non-numeric dimensions.
Population genetic structure and gene flow of Adélie penguins (Pygoscelis adeliae) breeding throughout the western Antarctic Peninsula
Authors: Gorman Kristen B. , Talbot Sandra L. , Sonsthagen Sarah A. , Sage George K. , Gravely Meg C. , Fraser William R. , Williams Tony D. 
Published: July 2017

AbstractAdélie penguins (Pygoscelis adeliae) are responding to ocean–climate variability throughout the marine ecosystem of the western Antarctic Peninsula (WAP) where some breeding colonies have declined by 80%. Nuclear and mitochondrial DNA (mtDNA) markers were used to understand historical population genetic structure and gene flow given relatively recent and continuing reductions in sea ice habitats and changes in numbers of breeding adults at colonies throughout the WAP. Genetic diversity, spatial genetic structure, genetic signatures of fluctuations in population demography and gene flow were assessed in four regional Adélie penguin colonies. The analyses indicated little genetic structure overall based on bi-parentally inherited microsatellite markers (FST=-0.006–0.004). No significant variance was observed in overall haplotype frequency (mtDNAΦST=0.017;P=0.112). Some comparisons with Charcot Island were significant, suggestive of female-biased philopatry. Estimates of gene flow based on a two-population coalescent model were asymmetrical from the species’ regional core to its northern range. Breeding Adélie penguins of the WAP are a panmictic population and hold adequate genetic diversity and dispersal capacity to be resilient to environmental change.
Destruction of Be star disk by large scale magnetic fields
Authors: ud-Doula Asif , Owocki Stanley , Kee Nathaniel (Dylan) , Vanyo Michael 
Published: July 2017

AbstractClassical Be stars are rapidly rotating stars with circumstellar disks that come and go on time scale of years. Recent observational data strongly suggests that these stars lack the 10% incidence of global magnetic fields observed in other main-sequence B stars. Such an apparent lack of magnetic fields may indicate that Be disks are fundamentally incompatible with a significant large scale magnetic field. In this work, using numerical magnetohydrodynamics (MHD) simulations, we show that a dipole field of only 100G can lead to the quick disruption of a Be disk. Such a limit is in line with the observational upper limits for these objects.
Wind-embedded shocks in FASTWIND: X-ray emission and K-shell absorption
Authors: Carneiro L. P. , Puls J. , Sundqvist J. O. , Hoffmann T. L. 
Published: July 2017

AbstractEUV and X-ray radiation emitted from wind-embedded shocks can affect the ionization balance in the outer atmospheres of massive stars, and can also be the mechanism responsible for producing highly ionized atoms detected in the wind UV spectra. To investigate these processes, we implemented the emission from wind-embedded shocks and related physics into our atmosphere/spectrum synthesis code FASTWIND. We also account for the high energy absorption of the cool wind, by adding important K-shell opacities. Various tests justfying our approach have been described by Carneiro+(2016, A&A 590, A88).In particular, we studied the impact of X-ray emission on the ionization balance of important elements. In almost all the cases, the lower ionization stages (O iv, N iv, P v) are depleted and the higher stages (N v, O v, O vi) become enhanced. Moreover, also He lines (in particular He ii 1640 and He ii 4686) can be affected as well.Finally, we carried out an extensive discussion of the high-energy mass absorption coefficient, κν, regarding its spatial variation and dependence on Teff. We found that (i) the approximation of a radially constant κν can be justified for r ⩾ 1.2R* and λ ⩽ 18 Å, and also for many models at longer wavelengths. (ii) In order to estimate the actual value of this quantity, however, the He ii background needs to be considered from detailed modeling.
Mass of dust in core-collapse supernovae as viewed from energy balance in the ejecta
Authors: Nozawa Takaya 
Published: July 2017

AbstractRecent far-infrared (FIR) observations have revealed the presence of freshly formed dust with the masses exceeding 0.1 M⊙ in young remnants of core-collapse supernovae (CCSNe) such as SN 1987A and Cassiopeia A. Meanwhile, dust masses derived from near- to mid-infrared (N/MIR) observations of CCSNe a few years after explosions are on the order of 10−5–10−3M⊙. Here, we demonstrate that such small dust masses as seen from N/MIR observations would not necessarily reflect the formation history of dust but could be just limited by the luminosity of the SN that can heat up dust formed in the ejecta.
A new sample of red supergiants in the Inner Galaxy
Authors: Messineo M. , Zhu Q. , Figer D. F. , Menten K. M. , Ivanov V. D. , Kudritzki R.-P. , Chen C.-H. Rosie 
Published: July 2017

AbstractWe carried out a pivot experiment to select distant luminous late-type stars on the basis on their 2MASS and GLIMPSE photometry. Low-resolution infrared spectra enabled us to measure the equivalent widths (EWs) of their CO band-heads at 2.293 μm, and to confirm an extraordinarily high detection rate of red supergiants (RSGs), i.e. 61% (Messineo et al. (2016)).
Taking the Measure of Massive Stars and their Environments with the CHARA Array Long-baseline Interferometer
Authors: Gies Douglas R. 
Published: July 2017

AbstractMost massive stars are so distant that their angular diameters are too small for direct resolution. However, the observational situation is now much more favorable, thanks to new opportunities available with optical/IR long-baseline interferometry. The Georgia State University Center for High Angular Resolution Astronomy Array at Mount Wilson Observatory is a six-telescope instrument with a maximum baseline of 330 meters, which is capable of resolving stellar disks with diameters as small as 0.2 milliarcsec. The distant stars are no longer out of range, and many kinds of investigations are possible. Here we summarize a number of studies involving angular diameter measurements and effective temperature estimates for OB stars, binary and multiple stars (including the σ Orionis system), and outflows in Luminous Blue Variables. An enlarged visitors program will begin in 2017 that will open many opportunities for new programs in high angular resolution astronomy.
There Are (super)Giants in the Sky: Searching for Misidentified Massive Stars in Algorithmically-Selected Quasar Catalogs
Authors: Dorn-Wallenstein Trevor Z. , Levesque Emily 
Published: July 2017

AbstractThanks to incredible advances in instrumentation, surveys like the Sloan Digital Sky Survey have been able to find and catalog billions of objects, ranging from local M dwarfs to distant quasars. Machine learning algorithms have greatly aided in the effort to classify these objects; however, there are regimes where these algorithms fail, where interesting oddities may be found. We present here an X-ray bright quasar misidentified as a red supergiant/X-ray binary, and a subsequent search of the SDSS quasar catalog for X-ray bright stars misidentified as quasars.
Stellar Winds in Massive X-ray Binaries
Authors: Kretschmar Peter , Martínez-Núñez Silvia , Bozzo Enrico , Oskinova Lidia M. , Puls Joachim , Sidoli Lara , Sundqvist Jon Olof , Blay Pere , Falanga Maurizio , Fürst Felix , Gímenez-García Angel , Kreykenbohm Ingo , Kühnel Matthias , Sander Andreas , Torrejón José Miguel , Wilms Jörn , Podsiadlowski Philipp , Manousakis Antonios 
Published: July 2017

AbstractStrong winds from massive stars are a topic of interest to a wide range of astrophysical fields. In High-Mass X-ray Binaries the presence of an accreting compact object on the one side allows to infer wind parameters from studies of the varying properties of the emitted X-rays; but on the other side the accretor’s gravity and ionizing radiation can strongly influence the wind flow. Based on a collaborative effort of astronomers both from the stellar wind and the X-ray community, this presentation attempts to review our current state of knowledge and indicate avenues for future progress.
Observational signatures of hot-star magnetospheres
Authors: Oksala Mary E. 
Published: July 2017

AbstractMagnetic fields play an important role in shaping the circumstellar environment of hot, massive stars. Observational diagnostics give clues to the presence of magnetism across the entire electromagnetic spectrum. Infrared features can show more complex structure, indicating they may probe deeper opacities than optical features. Optical and infrared features mimic each other, with identical blue and red peak variations and identical peak velocity of material. These comparisons indicate the location of the infrared and optical emitting material is similar. Longer wavelength diagnostics are currently being developed and tested. IR spectroscopy is a viable tool to detect magnetic candidates in the Galactic center and star forming regions.
The Tarantula Nebula as a template for extragalactic star forming regions from VLT/MUSE and HST/STIS
Authors: Crowther Paul A. , Caballero-Nieves Saida M. , Castro Norberto , Evans Christopher J. 
Published: July 2017

AbstractWe present VLT/MUSE observations of NGC 2070, the dominant ionizing nebula of 30 Doradus in the LMC, plus HST/STIS spectroscopy of its central star cluster R136. Integral Field Spectroscopy (MUSE) and pseudo IFS (STIS) together provides a complete census of all massive stars within the central 30×30 parsec2 of the Tarantula. We discuss the integrated far-UV spectrum of R136, of particular interest for UV studies of young extragalactic star clusters. Strong He iiλ1640 emission at very early ages (1–2 Myr) from very massive stars cannot be reproduced by current population synthesis models, even those incorporating binary evolution and very massive stars. A nebular analysis of the integrated MUSE dataset implies an age of ~4.5 Myr for NGC 2070. Wolf-Rayet features provide alternative age diagnostics, with the primary contribution to the integrated Wolf-Rayet bumps arising from R140 rather than the more numerous H-rich WN stars in R136. Caution should be used when interpreting spatially extended observations of extragalactic star-forming regions.
Massive stars in advanced evolutionary stages, and the progenitor of GW150914
Authors: Hamann Wolf-Rainer , Oskinova Lidia , Todt Helge , Sander Andreas , Hainich Rainer , Shenar Tomer , Ramachandran Varsha 
Published: July 2017

AbstractThe recent discovery of a gravitational wave from the merging of two black holes of about 30 solar masses each challenges our incomplete understanding of massive stars and their evolution. Critical ingredients comprise mass-loss, rotation, magnetic fields, internal mixing, and mass transfer in close binary systems. The imperfect knowledge of these factors implies large uncertainties for models of stellar populations and their feedback. In this contribution we summarize our empirical studies of Wolf-Rayet populations at different metallicities by means of modern non-LTE stellar atmosphere models, and confront these results with the predictions of stellar evolution models. At the metallicity of our Galaxy, stellar winds are probably too strong to leave remnant masses as high as ~30 M⊙, but given the still poor agreement between evolutionary tracks and observation even this conclusion is debatable. At the low metallicity of the Small Magellanic Cloud, all WN stars which are (at least now) single are consistent with evolving quasi-homogeneously. O and B-type stars, in contrast, seem to comply with standard evolutionary models without strong internal mixing. Close binaries which avoided early merging could evolve quasi-homogeneously and lead to close compact remnants of relatively high masses that merge within a Hubble time.
The circumstellar environments of B[e] Supergiants
Authors: Maravelias G. , Kraus M. , Cidale L. , Arias M. L. , Aret A. , Fernandes M. Borges 
Published: July 2017

AbstractThe evolution of massive stars encompasses short-lived transition phases in which mass-loss is more enhanced and usually eruptive. A complex environment, combining atomic, molecular and dust regions, is formed around these stars. In particular, the circumstellar environment of B[e] Supergiants is not well understood. To address that, we have initiated a campaign to investigate their environments for a sample of Galactic and Magellanic Cloud sources. Using high-resolution optical and near-infrared spectra (MPG-ESO/FEROS, GEMINI/Phoenix and VLT/CRIRES, respectively), we examine a set of emission features ([OI], [CaII], CO bandheads) to trace the physical conditions and kinematics in their formation regions. We find that the B[e] Supergiants are surrounded by a series of rings of different temperatures and densities, a probable result of previous mass-loss events. In many cases the CO forms very close to the star, while we notice also an alternate mixing of densities and temperatures (which give rise to the different emission features) along the equatorial plane.
The wind-wind collision hole in eta Car
Authors: Damineli A. , Teodoro M. , Richardson N. D. , Gull T. R. , Corcoran M. F. , Hamaguchi K. , Groh J. H. , Weigelt G. , Hillier D. J. , Russell C. , Moffat A. , Pollard K. R. , Madura T. I. 
Published: July 2017

AbstractEta Carinae is one of the most massive observable binaries. Yet determination of its orbital and physical parameters is hampered by obscuring winds. However the effects of the strong, colliding winds changes with phase due to the high orbital eccentricity. We wanted to improve measures of the orbital parameters and to determine the mechanisms that produce the relatively brief, phase-locked minimum as detected throughout the electromagnetic spectrum. We conducted intense monitoring of the He ii λ4686 line in η Carinae for 10 months in the year 2014, gathering ~300 high S/N spectra with ground- and space-based telescopes. We also used published spectra at the FOS4 SE polar region of the Homunculus, which views the minimum from a different direction. We used a model in which the He ii λ4686 emission is produced by two mechanisms: a) one linked to the intensity of the wind-wind collision which occurs along the whole orbit and is proportional to the inverse square of the separation between the companion stars; and b) the other produced by the ‘bore hole’ effect which occurs at phases across the periastron passage. The opacity (computed from 3D SPH simulations) as convolved with the emission reproduces the behavior of equivalent widths both for direct and reflected light. Our main results are: a) a demonstration that the He ii λ4686 light curve is exquisitely repeatable from cycle to cycle, contrary to previous claims for large changes; b) an accurate determination of the longitude of periastron, indicating that the secondary star is ‘behind’ the primary at periastron, a dispute extended over the past decade; c) a determination of the time of periastron passage, at ~4 days after the onset of the deep light curve minimum; and d) show that the minimum is simultaneous for observers at different lines of sight, indicating that it is not caused by an eclipse of the secondary star, but rather by the immersion of the wind-wind collision interior to the inner wind of the primary.
The evolution of magnetic hot massive stars: Implementation of the quantitative influence of surface magnetic fields in modern models of stellar evolution
Authors: Keszthelyi Zsolt , Wade Gregg A. , Petit Véronique 
Published: July 2017

AbstractLarge-scale dipolar surface magnetic fields have been detected in a fraction of OB stars, however only few stellar evolution models of massive stars have considered the impact of these fossil fields. We are performing 1D hydrodynamical model calculations taking into account evolutionary consequences of the magnetospheric-wind interactions in a simplified parametric way. Two effects are considered: i) the global mass-loss rates are reduced due to mass-loss quenching, and ii) the surface angular momentum loss is enhanced due to magnetic braking. As a result of the magnetic mass-loss quenching, the mass of magnetic massive stars remains close to their initial masses. Thus magnetic massive stars - even at Galactic metallicity - have the potential to be progenitors of ‘heavy’ stellar mass black holes. Similarly, at Galactic metallicity, the formation of pair instability supernovae is plausible with a magnetic progenitor.