bluuebunny/crossref_metadata_2025_split huggingface dataset:
Effect of aminocaproic acid on clot strength and clot lysis of canine blood determined by use of an in vitro model of hyperfibrinolysis
Authors: Brown Jamie C. , Brainard Benjamin M. , Fletcher Daniel J. , Nie Ben , Arnold Robert D. , Schmiedt Chad W. 
Published: November 2016

Abstract
OBJECTIVE To determine pharmacodynamic and pharmacokinetic profiles of aminocaproic acid (ACA) by use of a thromboelastography (TEG)-based in vitro model of hyperfibrinolysis and high-performance liquid chromatography–mass spectrometry.
ANIMALS 5 healthy adult dogs.
PROCEDURES A single dose of injectable ACA (20, 50, or 100 mg/kg) or an ACA tablet (approximately 100 mg/kg) was administered orally. Blood samples were collected at 0, 15, 30, 45, 60, 90, 120, and 240 minutes after ACA administration for pharmacokinetic analysis. Samples were obtained at 0, 60, and 240 minutes for pharmacodynamic analysis by use of a TEG model of hyperfibrinolysis.
RESULTS No adverse effects were detected. In the hyperfibrinolysis model, after all doses, a significantly higher TEG maximum amplitude (clot strength), compared with baseline, was detected at 60 and 240 minutes. Additionally, the percentage of fibrinolysis was reduced from the baseline value at 60 and 240 minutes, with the greatest reduction at 60 minutes. At 240 minutes, there was significantly less fibrinolysis for the 100 mg/kg dose than the 20 mg/kg dose. Maximum plasma ACA concentration was dose dependent. There was no significant difference in pharmacokinetic parameters between 100 mg/kg formulations.
CONCLUSIONS AND CLINICAL RELEVANCE In an in vitro model of hyperfibrinolysis, ACA inhibited fibrinolysis at all doses tested. At 240 minutes after administration, the 100 mg/kg dose inhibited fibrinolysis more effectively than did the 20 mg/kg dose. Thus, ACA may be useful for in vivo prevention of fibrinolysis in dogs.
IMPACT FOR HUMAN MEDICINE These data may improve research models of hyperfibrinolytic diseases.
Population pharmacokinetics of enrofloxacin in purple sea stars (Pisaster ochraceus) following an intracoelomic injection or extended immersion
Authors: Rosenberg Justin F. , Haulena Martin , Phillips Brianne E. , Harms Craig A. , Lewbart Gregory A. , Lahner Lesanna L. , Papich Mark G. 
Published: November 2016

Abstract
OBJECTIVE To determine population pharmacokinetics of enrofloxacin in purple sea stars (Pisaster ochraceus) administered an intracoelomic injection of enrofloxacin (5 mg/kg) or immersed in an enrofloxacin solution (5 mg/L) for 6 hours.
ANIMALS 28 sea stars of undetermined age and sex.
PROCEDURES The study had 2 phases. Twelve sea stars received an intracoelomic injection of enrofloxacin (5 mg/kg) or were immersed in an enrofloxacin solution (5 mg/L) for 6 hours during the injection and immersion phases, respectively. Two untreated sea stars were housed with the treated animals following enrofloxacin administration during both phases. Water vascular system fluid samples were collected from 4 sea stars and all controls at predetermined times during and after enrofloxacin administration. The enrofloxacin concentration in those samples was determined by high-performance liquid chromatography. For each phase, noncompartmental analysis of naïve averaged pooled samples was used to obtain initial parameter estimates; then, population pharmacokinetic analysis was performed that accounted for the sparse sampling technique used.
RESULTS Injection phase data were best fit with a 2-compartment model; elimination half-life, peak concentration, area under the curve, and volume of distribution were 42.8 hours, 18.9 μg/mL, 353.8 μg•h/mL, and 0.25 L/kg, respectively. Immersion phase data were best fit with a 1-compartment model; elimination half-life, peak concentration, and area under the curve were 56 hours, 36.3 μg•h/mL, and 0.39 μg/mL, respectively.
CONCLUSIONS AND CLINICAL RELEVANCE Results suggested that the described enrofloxacin administration resulted in water vascular system fluid drug concentrations expected to exceed the minimum inhibitory concentration for many bacterial pathogens.
Use of manual alveolar recruitment maneuvers to eliminate atelectasis artifacts identified during thoracic computed tomography of healthy neonatal foals
Authors: Lascola Kara M. , Clark-Price Stuart C. , Joslyn Stephen K. , Mitchell Mark A. , O'Brien Robert T. , Hartman Susan K. , Kline Kevin H. 
Published: November 2016

Abstract
OBJECTIVE To evaluate use of single manual alveolar recruitment maneuvers (ARMs) to eliminate atelectasis during CT of anesthetized foals.
ANIMALS 6 neonatal Standardbred foals.
PROCEDURES Thoracic CT was performed on spontaneously breathing anesthetized foals positioned in sternal (n = 3) or dorsal (3) recumbency when foals were 24 to 36 hours old (time 1), 4 days old (time 2), 7 days old (time 3), and 10 days old (time 4). The CT images were collected without ARMs (all times) and during ARMs with an internal airway pressure of 10, 20, and 30 cm H2O (times 2 and 3). Quantitative analysis of CT images measured whole lung and regional changes in attenuation or volume with ARMs.
RESULTS Increased attenuation and an alveolar pattern were most prominent in the dependent portion of the lungs. Subjectively, ARMs did not eliminate atelectasis; however, they did incrementally reduce attenuation, particularly in the nondependent portion of the lungs. Quantitative differences in lung attenuation attributable to position of foal were not identified. Lung attenuation decreased significantly (times 2 and 3) and lung volume increased significantly (times 2 and 3) after ARMs. Changes in attenuation and volume were most pronounced in the nondependent portion of the lungs and at ARMs of 20 and 30 cm H2O.
CONCLUSIONS AND CLINICAL RELEVANCE Manual ARMs did not eliminate atelectasis but reduced attenuation in nondependent portions of the lungs. Positioning of foals in dorsal recumbency for CT may be appropriate when pathological changes in the ventral portion of the lungs are suspected.
Femoral Fracture Following Acute Trauma in a Female Collegiate Swimmer
Authors: Hernandez Jonathan , Gamradt Seth , Morcos Drew 
Published: November 2016

The patient was a 20-year-old Division I female collegiate swimmer who presented to the athletic training room following a traumatic onset of right knee pain. She was immediately transferred to the hospital for diagnostic imaging. Knee radiographs revealed a minimally displaced fracture of her right distal femur that extended from her intercondylar notch to the lateral aspect of her distal femoral metaphysis, while computed tomography and magnetic resonance imaging scans revealed the intra-articular nature of the fracture. J Orthop Sports Phys Ther 2016;46(11):1010. doi:10.2519/jospt.2016.0418
Giant Cell Tumor of the Distal Femur
Authors: Hannah Mary Kay C. , Easterling Emmanuel J. , Woodson Cheryl Ann 
Published: November 2016

A 24-year-old woman presented to a physical therapy clinic reporting a 4-month history of constant left knee pain of insidious onset. In the setting of nonlocalized, nontraumatic chronic knee pain, the physical therapist ordered radiographs, which revealed an osteolytic lesion along the distal anterolateral femur, suggesting a giant cell tumor. The radiologist then recommended computed tomography for better appreciation of the lesion and magnetic resonance imaging to investigate any soft tissue abnormality. J Orthop Sports Phys Ther 2016;46(11):1011. doi:10.2519/jospt.2016.0419
Unraveling the Complexity of Low Back Pain
Authors: O'Sullivan Peter , Caneiro Joao Paulo , O'Keeffe Mary , O'Sullivan Kieran 
Published: November 2016

Low back pain (LBP) is the leading cause of disability worldwide. Various approaches to diagnose and manage LBP have arisen, leading to an exponential increase in health care costs. Paradoxically, this trend has been associated with a concurrent increase in disability and chronicity. The health care system faces enormous challenges, with both the disability burden and financial impact relating to LBP escalating. Growing evidence suggests that current practice is discordant with contemporary evidence, and is in fact often exacerbating the problem. Change will demand a cultural shift in LBP beliefs and practice. J Orthop Sports Phys Ther 2016;46(11):932–937. doi:10.2519/jospt.2016.0609
Effects of diffusion alloying on the microstructure and properties of TiC-reinforced Fe-based PM materials
Authors: Liu Zili , Zhang Haohan , Liu Xiqin , Zheng Yong , Huang Xin , Zou Dehua 
Published: November 2016

Abstract
The effects of diffusion alloying on the microstructure and properties of TiC-reinforced Fe-based powder metallurgy materials were investigated via X-ray diffraction, scanning electron microscopy, energy dispersive spectroscopy, and mechanical testing. The results show that the distribution of Ti in diffusion-alloyed particles becomes more uniform with increasing diffusion time. The TiC particles formed in-situ during sintering, and the microstructure of Fe-based powder metallurgy materials prepared from diffusion-alloyed powders became rounder, more uniform and refined with increasing diffusion alloying time. The apparent hardness and the bending strength increased with increasing diffusion time. The fracture mode of the samples prepared from diffusion-alloyed powders had brittle and ductile characteristics.
A CONSTRAINT ON THE FORMATION TIMESCALE OF THE YOUNG OPEN CLUSTER NGC 2264: LITHIUM ABUNDANCE OF PRE-MAIN SEQUENCE STARS
Authors: Lim Beomdu , Sung Hwankyung , Kim Jinyoung S. , Bessell Michael S. , Hwang Narae , Park Byeong-Gon 
Published: November 2016

ABSTRACT
The timescale of cluster formation is an essential parameter in order to understand the formation process of star clusters. Pre-main sequence (PMS) stars in nearby young open clusters reveal a large spread in brightness. If the spread were considered to be a result of a real spread in age, the corresponding cluster formation timescale would be about 5–20 Myr. Hence it could be interpreted that star formation in an open cluster is prolonged for up to a few tens of Myr. However, difficulties in reddening correction, observational errors, and systematic uncertainties introduced by imperfect evolutionary models for PMS stars can result in an artificial age spread. Alternatively, we can utilize Li abundance as a relative age indicator of PMS star to determine the cluster formation timescale. The optical spectra of 134 PMS stars in NGC 2264 have been obtained with MMT/Hectochelle. The equivalent widths have been measured for 86 PMS stars with a detectable Li line (

). Li abundance under the condition of local thermodynamic equilibrium (LTE) was derived using the conventional curve of growth method. After correction for non-LTE effects, we find that the initial Li abundance of NGC 2264 is

. From the distribution of the Li abundances, the underlying age spread of the visible PMS stars is estimated to be about 3–4 Myr and this, together with the presence of embedded populations in NGC 2264, suggests that the cluster formed on a timescale shorter than 5 Myr.
ON THE STAR FORMATION PROPERTIES OF VOID GALAXIES
Authors: Moorman Crystal M. , Moreno Jackeline , White Amanda , Vogeley Michael S. , Hoyle Fiona , Giovanelli Riccardo , Haynes Martha P. 
Published: November 2016

ABSTRACT
We measure the star formation properties of two large samples of galaxies from the SDSS in large-scale cosmic voids on timescales of 10 and 100 Myr, using Hα emission line strengths and GALEX FUV fluxes, respectively. The first sample consists of 109,818 optically selected galaxies. We find that void galaxies in this sample have higher specific star formation rates (SSFRs; star formation rates per unit stellar mass) than similar stellar mass galaxies in denser regions. The second sample is a subset of the optically selected sample containing 8070 galaxies with reliable H i detections from ALFALFA. For the full H i detected sample, SSFRs do not vary systematically with large-scale environment. However, investigating only the H i detected dwarf galaxies reveals a trend toward higher SSFRs in voids. Furthermore, we estimate the star formation rate per unit H i mass (known as the star formation efficiency; SFE) of a galaxy, as a function of environment. For the overall H i detected population, we notice no environmental dependence. Limiting the sample to dwarf galaxies still does not reveal a statistically significant difference between SFEs in voids versus walls. These results suggest that void environments, on average, provide a nurturing environment for dwarf galaxy evolution allowing for higher specific star formation rates while forming stars with similar efficiencies to those in walls.
QUASI-PERIODIC ACCELERATION OF ELECTRONS IN THE FLARE ON 2012 JULY 19
Authors: Huang Jing , Kontar Eduard P. , Nakariakov Valery M. , Gao Guannan 
Published: November 2016

ABSTRACT
Quasi-periodic pulsations (QPPs) of nonthermal emission in an M7.7 class flare on 2012 July 19 are investigated with spatially resolved observations at microwave and HXR bands and with spectral observations at decimetric, metric waves. Microwave emission at 17 GHz of two footpoints, HXR emission at 20–50 keV of the north footpoint and loop top, and type III bursts at 0.7–3 GHz show prominent in-phase oscillations at 270 s. The microwave emission of the loop leg has less pulsation but stronger emission. Through the estimation of plasma density around the loop top from EUV observations, we find that the local plasma frequency would be 1.5 GHz or even higher. Thus, type III bursts at 700 MHz originate above the loop top. Quasi-periodic acceleration or injection of energetic electrons is proposed to dominate these in-phase QPPs of nonthermal emission from footpoints, loop top, and above. In the overlying region, drifting pulsations (DPS) at 200–600 MHz oscillate at a distinct period (200 s). Its global structure drifts toward lower frequency, which is closely related to upward plasmoids observed simultaneously from EUV emission. Hence, nonthermal emission from overlying plasmoids and underlying flaring loops show different oscillating periods. Two individual systems of quasi-periodic acceleration of electrons are proposed to coincide in the bi-direction outflows from the reconnection region.
PROTOPLANETARY DISK HEATING AND EVOLUTION DRIVEN BY SPIRAL DENSITY WAVES
Authors: Rafikov Roman R. 
Published: November 2016

ABSTRACT
Scattered light imaging of protoplanetary disks often reveals prominent spiral arms, likely excited by massive planets or stellar companions. Assuming that these arms are density waves, evolving into spiral shocks, we assess their effect on the thermodynamics, accretion, and global evolution of the disk. We derive analytical expressions for the direct (irreversible) heating, angular momentum transport, and mass accretion rate induced by disk shocks of arbitrary amplitude. These processes are very sensitive to the shock strength. We show that waves of moderate strength (density jump at the shock ΔΣ/Σ ∼ 1) result in negligible disk heating (contributing at the ∼1% level to the energy budget) in passive, irradiated protoplanetary disks on ∼100 au scales, but become important within several au. However, shock heating is a significant (or even dominant) energy source in disks of cataclysmic variables, stellar X-ray binaries, and supermassive black hole binaries, heated mainly by viscous dissipation. Mass accretion induced by the spiral shocks is comparable to (or exceeds) the mass inflow due to viscous stresses. Protoplanetary disks featuring prominent global spirals must be evolving rapidly, in ≲0.5 Myr at ∼100 au. A direct upper limit on the evolution timescale can be established by measuring the gravitational torque due to the spiral arms from the imaging data. We find that, regardless of their origin, global spiral waves must be important agents of the protoplanetary disk evolution. They may serve as an effective mechanism of disk dispersal and could be related to the phenomenon of transitional disks.
A STEEPER THAN LINEAR DISK MASS–STELLAR MASS SCALING RELATION
Authors: Pascucci I. , Testi L. , Herczeg G. J. , Long F. , Manara C. F. , Hendler N. , Mulders G. D. , Krijt S. , Ciesla F. , Henning Th. , Mohanty S. , Drabek-Maunder E. , Apai D. , Szűcs L. , Sacco G. , Olofsson J. 
Published: November 2016

ABSTRACT
The disk mass is among the most important input parameter for every planet formation model to determine the number and masses of the planets that can form. We present an ALMA 887 μm survey of the disk population around objects from ∼2 to 0.03 M
⊙ in the nearby ∼2 Myr old Chamaeleon I star-forming region. We detect thermal dust emission from 66 out of 93 disks, spatially resolve 34 of them, and identify two disks with large dust cavities of about 45 au in radius. Assuming isothermal and optically thin emission, we convert the 887 μm flux densities into dust disk masses, hereafter M
dust. We find that the

relation is steeper than linear and of the form M
dust ∝ (M
*)1.3–1.9, where the range in the power-law index reflects two extremes of the possible relation between the average dust temperature and stellar luminosity. By reanalyzing all millimeter data available for nearby regions in a self-consistent way, we show that the 1–3 Myr old regions of Taurus, Lupus, and Chamaeleon I share the same

relation, while the 10 Myr old Upper Sco association has a steeper relation. Theoretical models of grain growth, drift, and fragmentation reproduce this trend and suggest that disks are in the fragmentation-limited regime. In this regime millimeter grains will be located closer in around lower-mass stars, a prediction that can be tested with deeper and higher spatial resolution ALMA observations.
FIRST DETECTION OF A PULSAR BOW SHOCK NEBULA IN FAR-UV: PSR J0437–4715∗
Authors: Rangelov Blagoy , Pavlov George G. , Kargaltsev Oleg , Durant Martin , Bykov Andrei M. , Krassilchtchikov Alexandre 
Published: November 2016

ABSTRACT
Pulsars traveling at supersonic speeds are often accompanied by cometary bow shocks seen in Hα. We report on the first detection of a pulsar bow shock in the far-ultraviolet (FUV). We detected it in FUV images of the nearest millisecond pulsar J0437−4715 obtained with the Hubble Space Telescope. The images reveal a bow-like structure positionally coincident with part of the previously detected Hα bow shock, with an apex at 10″ ahead of the moving pulsar. Its FUV luminosity,

erg s−1, exceeds the Hα luminosity from the same area by a factor of 10. The FUV emission could be produced by the shocked interstellar medium matter or, less likely, by relativistic pulsar wind electrons confined by strong magnetic field fluctuations in the bow shock. In addition, in the FUV images we found a puzzling extended (≃3″ in size) structure overlapping with the limb of the bow shock. If related to the bow shock, it could be produced by an inhomogeneity in the ambient medium or an instability in the bow shock. We also report on a previously undetected X-ray emission extending for about 5″ ahead of the pulsar, possibly a pulsar wind nebula created by shocked pulsar wind, with a luminosity L(0.5–8 keV) ∼ 3 × 1028 erg s−1.
GAS-PHASE ABSORPTIONS OF C+
60: A NEW COMPARISON WITH ASTRONOMICAL MEASUREMENTS*

†
Authors: Walker G. A. H. , Campbell E. K. , Maier J. P. , Bohlender D. , Malo L. 
Published: November 2016

ABSTRACT
Campbell et al. recently revised, by a few tenths of an Å, the wavelengths for their low-temperature laboratory measurements of fullerene

bands. This accounts for the perturbation caused by the He atom to the

spectrum. Here, we demonstrate that the revised laboratory wavelengths improve coincidence with the 9632, 9577, 9428, 9365, and 9348 diffuse interstellar bands detected towards the stars HD 46711, HD 169454, and HD 183143.
THE TRENDS HIGH-CONTRAST IMAGING SURVEY. VI. DISCOVERY OF A MASS, AGE, AND METALLICITY BENCHMARK BROWN DWARF
Authors: Crepp Justin R. , Gonzales Erica J. , Bechter Eric B. , Montet Benjamin T. , Johnson John Asher , Piskorz Danielle , Howard Andrew W. , Isaacson Howard 
Published: November 2016

ABSTRACT
The mass and age of substellar objects are degenerate parameters leaving the evolutionary state of brown dwarfs ambiguous without additional information. Theoretical models are normally used to help distinguish between old, massive brown dwarfs and young, low-mass brown dwarfs but these models have yet to be properly calibrated. We have carried out an infrared high-contrast imaging program with the goal of detecting substellar objects as companions to nearby stars to help break degeneracies in inferred physical properties such as mass, age, and composition. Rather than using imaging observations alone, our targets are pre-selected based on the existence of dynamical accelerations informed from years of stellar radial velocity (RV) measurements. In this paper, we present the discovery of a rare benchmark brown dwarf orbiting the nearby (d = 18.69 ± 0.19 pc), solar-type (G9V) star HD 4747 ([Fe/H] = −0.22 ± 0.04) with a projected separation of only ρ = 11.3 ± 0.2 au (θ = 0.″6). Precise Doppler measurements taken over 18 years reveal the companion’s orbit and allow us to place strong constraints on its mass using dynamics (

). Relative photometry (ΔK

s
= 9.05 ± 0.14,

,

) indicates that HD 4747 B is most likely a late-type L-dwarf and, if near the L/T transition, an intriguing source for studying cloud physics, variability, and polarization. We estimate a model-dependent mass of

for an age of

Gyr based on gyrochronology. Combining astrometric measurements with RV data, we calculate the companion dynamical mass (

) and orbit (e = 0.740 ± 0.002) directly. As a new mass, age, and metallicity benchmark, HD 4747 B will serve as a laboratory for precision astrophysics to test theoretical models that describe the emergent radiation of brown dwarfs.
Reporting on the Prevalence of Antiretroviral Drug Resistance in a Regional HIV Population over 20 Years: A Word of Caution
Authors: Gill Victoria C , Lynch Tarah , Ramazani Soheil , Krentz Hartmut B 
Published: November 2016

Background Failure to achieve complete viral suppression with antiretroviral drugs (ARV) may lead to uncontrolled HIV replication, ARV resistance and negative outcomes. Monitoring and reporting of HIV resistance trends is important but problematic. We examined prevalent resistance rates in an HIV population over 20 years and document how rates may appear to vary greatly based solely on which parameters are utilized. Methods We determined the annual use of geno-typic antiretroviral resistance testing (GART) from 1995 to 2014 for all patients receiving HIV care in southern Alberta, Canada, and the presence of resistance mutations in those tested. The impact on prevalent resistance rates of using cumulative or latest GART was also determined. Results Between 1995 and 2014, the number of patients with GART increased from <1% to 71%. Prevalent resistance in patients with GART decreased from a high of 52% in 2003 to 25.8% in 2014. However, if prevalence rates were reported using all active patients as denominator, including those without GART, prevalence increased from 0.7% to 18.5%. Prevalence rates were 7% to 9% higher in any given year if cumulative GART rather than latest GART results were used. Conclusions While prevalence resistance rates are decreasing, the precise rates being reported may vary due to increasing number of patients tested annually, using either the entire population as denominator or only patients with GART, and using either last or cumulative GART. Defining these parameters is critical if prevalence is to be compared over time or between HIV populations.