bluuebunny/crossref_metadata_2025_split huggingface dataset:
Reliability assessment of the Biffl Scale for blunt traumatic cerebrovascular injury as detected on computer tomography angiography
Authors: Foreman Paul M. , Griessenauer Christoph J. , Kicielinski Kimberly P. , Schmalz Philip G. R. , Rocque Brandon G. , Fusco Matthew R. , Sullivan Joseph C. , Deveikis John P. , Harrigan Mark R. 
Published: October 2016

OBJECTIVEBlunt traumatic cerebrovascular injury (TCVI) represents structural injury to a vessel due to high-energy trauma. The Biffl Scale is a widely accepted grading scheme for these injuries that was developed using digital subtraction angiography. In recent years, screening CT angiography (CTA) has been used to identify patients with TCVI. The reliability of this scale, with injuries assessed using CTA, has not yet been determined.METHODSSeven independent raters, including 2 neurosurgeons, 2 neuroradiologists, 2 neurosurgical residents, and 1 neurosurgical vascular fellow, independently reviewed each presenting CTA of the neck performed in 40 patients with confirmed TCVI and assigned a Biffl grade. Ten images were repeated to assess intrarater reliability, for a total of 50 CTAs. Fleiss' multirater kappa (κ) and interclass correlation were calculated as a measure of interrater reliability. Weighted Cohen's κ was used to assess intrarater reliability.RESULTSFleiss' multirater κ was 0.65 (95% CI 0.61–0.69), indicating substantial agreement as to the Biffl grade assignment among the 7 raters. Interclass correlation was 0.82, demonstrating excellent agreement among the raters. Intrarater reliability was perfect (weighted Cohen's κ = 1) in 2 raters, and near perfect (weighted Cohen's κ > 0.8) in the remaining 5 raters.CONCLUSIONSGrading of TCVI with CTA using the Biffl Scale is reliable.
Diet-induced weight loss is sufficient to reduce senescent cell number in white adipose tissue of weight-cycled mice
Authors: List Edward O. , Jensen Elizabeth , Kowalski Jesse , Buchman Mathew , Berryman Darlene E. , Kopchick John J. 
Published: October 2016

Previously, our laboratory reported that weight-cycled mice outlive their obese counterparts. To gain a better mechanistic understanding of these results, we evaluated cellular senescence in white adipose tissue (WAT) of lean, obese, and weight cycled mice. Our results show that at the end of a 28 day weight loss cycle cellular senescence is significantly reduced in multiple WAT depots compared to obese mice, which also corresponds to a reduction in circulating activin A (a marker of senescence). These findings suggest that a previously undescribed benefit to weight loss may be a reduction of cellular senescence in WAT.
Enhanced detection rate of typhoid fever among clinically suspected patients in a tertiary referral hospital in Dhaka, Bangladesh using nested polymerase chain reaction technology
Authors: Khan Shafinaz , Mia Ruhul Amin , Khatun Sumaiya 
Published: October 2016

A nested polymerase chain reaction (PCR) specific for Salmonella enterica subspecies enteric serovar Typhi was used for the detection of the pathogen in blood. This study was done during the period of March 2013 to February 2014. A total of 80 clinically suspected cases of typhoid fever were included in the study. Blood was collected from all participating individuals. Nested PCR targeting the flagellin gene (fliC) of Salmonella Typhi & blood culture were done for each of the cases. The positivity rate of PCR & blood culture was 70%& 20% respectively. The positivity rate of PCR was significantly higher than blood culture (P< 0.05). With the nested PCR, S. Typhi DNAs were detected from blood specimens of 67.2% (43/64) patients among the suspected typhoid fever cases on the basis of clinical features but with negative cultures. We conclude that the PCR technique could be used as a novel diagnostic method of typhoid fever, particularly in culture-negative cases in an endemic country like Bangladesh.
Timing of rapid diversification and convergent origins of active pollination within Agavoideae (Asparagaceae)
Authors: McKain Michael R. , McNeal Joel R. , Kellar P. Roxanne , Eguiarte Luis E. , Pires J. Chris , Leebens‐Mack Jim 
Published: October 2016

PREMISE OF THE STUDY:Yucca species are ideal candidates for the study of coevolution due to the obligate mutualism they form with yucca moth pollinators (genera Tegeticula and Parategeticula). Yuccas are not the only species to exhibit a mutualism with yucca moths; the genus Hesperoyucca is pollinated by the California yucca moth (Tegeticula maculata). Relationships among yuccas, Hesperoyucca, and other members of subfamily Agavoideae are necessary to understand the evolution of this unique pollination syndrome. Here, we investigate evolutionary relationships of yuccas and closely related genera looking at the timing and origin of yucca moth pollination.METHODS:In this study, we sequenced the chloroplast genomes of 20 species in the subfamily Agavoideae (Asparagaceae) and three confamilial outgroup taxa to resolve intergeneric phylogenetic relationships of Agavoideae. We estimated divergence times using protein‐coding genes from 67 chloroplast genomes sampled across monocots to determine the timing of the yucca moth pollination origin.KEY RESULTS:We confidently resolved intergeneric relationships in Agavoideae, demonstrating the origin of the yucca–yucca moth mutualism on two distinct lineages that diverged 27 million years ago. Comparisons of Yucca and Hesperoyucca divergence time to those of yucca moths (Tegeticula and Parategeticula, Prodoxidae) indicate overlapping ages for the origin of pollinating behavior in the moths and pollination by yucca moths in the two plant lineages.CONCLUSION:Whereas pollinating yucca moths have been shown to have a single origin within the Prodoxidae, there were independent acquisitions of active pollination on lineages leading to Yucca and Hesperoyucca within the Agavoideae.
The impact of hybridization on long‐term persistence of polyploid Dactylorhiza species
Authors: Jacquemyn Hans , van der Meer Sascha , Brys Rein 
Published: October 2016

PREMISE OF THE STUDY:Hybridization may pose severe threats to the long‐term survival of the parental taxa through introgression and the formation of hybrid swarms. However, when the resulting hybrids show strong male and female sterility, backcrossing and introgression are unlikely to occur, but the parental species may suffer from reduced male and female fitness.METHODS:We assessed the impact of hybridization on the long‐term persistence of two food‐deceptive orchids in the genus Dactylorhiza (the common Dactylorhiza maculata and the rare D. sphagnicola). The extent of hybridization was investigated using both molecular markers and morphometric measurements. To determine the strength of postmating reproductive isolation, hand pollinations were conducted between pure and hybrid individuals. Finally, fruit set and seed viability of open‐pollinated plants were determined in sympatric and allopatric populations to investigate the impact of hybridization on the reproductive output of the pure parental species.KEY RESULTS:Our results showed that postmating reproductive isolation was weak and that hybridization occurred frequently within the studied sympatric population. Although hybrids were characterized by very low female fitness, mainly because of strongly reduced seed viability, backcrossing appeared to occur and was asymmetric toward the rare D. sphagnicola. Fruit set and seed viability of open‐pollinated plants were also significantly lower in the sympatric population than in the allopatric populations, indicating that hybridization and ongoing introgression incurred fitness costs in the pure parental species.CONCLUSIONS:Overall, our results suggest that extensive hybridization can affect the long‐term viability of the parental species through the combined effect of introgression following interspecific hybrid fertilization and reduced fitness of the parental species.
Complex pollination of a tropical Asian rainforest canopy tree by flower‐feeding thrips and thrips‐feeding predators
Authors: Kondo Toshiaki , Nishimura Sen , Tani Naoki , Ng Kevin Kit Siong , Lee Soon Leong , Muhammad Norwati , Okuda Toshinori , Tsumura Yoshihiko , Isagi Yuji 
Published: October 2016

PREMISE OF THE STUDY:In tropical rainforests of Southeast Asia, a highly fecund thrips (Thrips spp.) responds rapidly to the mass flowering at multiple‐year intervals characteristic of certain species such as the canopy tree studied here, Shorea acuminata, by feeding on flower resources. However, past DNA analyses of pollen adherent to thrips bodies revealed that the thrips promoted a very high level of self‐pollination. Here, we identified the pollinator that contributes to cross‐pollination and discuss ways that the pollination system has adapted to mass flowering.METHODS:By comparing the patterns of floral visitation and levels of genetic diversity in adherent pollen loads among floral visitors, we evaluated the contribution of each flower visitor to pollination.KEY RESULTS:The big‐eyed bug, Geocoris sp., a major thrips predator, was an inadvertent pollinator, and importantly contributed to cross‐pollination. The total outcross pollen adhering to thrips was approximately 30% that on the big‐eyed bugs. Similarly, 63% of alleles examined in S. acuminata seeds and seedlings occurred in pollen adhering to big‐eyed bugs; about 30% was shared with pollen from thrips.CONCLUSIONS:During mass flowering, big‐eyed bugs likely travel among flowering S. acuminata trees, attracted by the abundant thrips. Floral visitation patterns of big‐eyed bugs vs. other insects suggest that these bugs can maintain their population size between flowering by preying upon another thrips (Haplothrips sp.) that inhabits stipules of S. acuminata throughout the year and quickly respond to mass flowering. Thus, thrips and big‐eyed bugs are essential components in the pollination of S. acuminata.
K2-31B, A GRAZING TRANSITING HOT JUPITER ON A 1.26-DAY ORBIT AROUND A BRIGHT G7V STAR
Authors: Grziwa Sascha , Gandolfi Davide , Csizmadia Szilard , Fridlund Malcolm , Parviainen Hannu , Deeg Hans J. , Cabrera Juan , Djupvik Amanda A. , Albrecht Simon , Palle Enric B. , Pätzold Martin , Béjar Victor J. S. , Prieto-Arranz Jorge , Eigmüller Philipp , Erikson Anders , Fynbo Johan P. U. , Guenther Eike W. , Hatzes Artie P. , Kiilerich Amanda , Korth Judith , Kuutma Teet , Montañés-Rodríguez Pilar , Nespral David , Nowak Grzegorz , Rauer Heike , Saario Joonas , Sebastian Daniel , Slumstrup Ditte 
Published: October 2016

ABSTRACT
We report the discovery of K2-31b, the first confirmed transiting hot Jupiter detected by the K2 space mission. We combined K2 photometry with FastCam lucky imaging and FIES and HARPS high-resolution spectroscopy to confirm the planetary nature of the transiting object and derived the system parameters. K2-31b is a 1.8-Jupiter-mass planet on a 1.26-day orbit around a G7 V star (

M
⊙,

R
⊙). The planetary radius is poorly constrained (0.7 < R
p < 1.4 R
Jup),15
owing to the grazing transit and the low sampling rate of the K2 photometry.16
TRACKING NEPTUNE’S MIGRATION HISTORY THROUGH HIGH-PERIHELION RESONANT TRANS-NEPTUNIAN OBJECTS
Authors: Kaib Nathan A. , Sheppard Scott S. 
Published: October 2016

ABSTRACT
Recently, Sheppard et al. presented the discovery of seven new trans-Neptunian objects with moderate eccentricities, perihelia beyond 40 au, and semimajor axes beyond 50 au. Like the few previously known objects on similar orbits, these objects’ semimajor axes are just beyond the Kuiper Belt edge and clustered around Neptunian mean motion resonances (MMRs). These objects likely obtained their observed orbits while trapped within MMRs, when the Kozai–Lidov mechanism raised their perihelia and weakened Neptune’s dynamical influence. Using numerical simulations that model the production of this population, we find that high-perihelion objects near Neptunian MMRs can constrain the nature and timescale of Neptune’s past orbital migration. In particular, the population near the 3:1 MMR (near 62 au) is especially useful due to its large population and short dynamical evolution timescale. If Neptune finishes migrating within ∼100 Myr or less, we predict that over 90% of high-perihelion objects near the 3:1 MMR will have semimajor axes within 1 au of each other, very near the modern resonance’s center. On the other hand, if Neptune’s migration takes ∼300 Myr, we expect ∼50% of this population to reside in dynamically fossilized orbits over ∼1 au closer to the Sun than the modern resonance. We highlight 2015 KH162 as a likely member of this fossilized 3:1 population. Under any plausible migration scenario, nearly all high-perihelion objects in resonances beyond the 4:1 MMR (near 76 au) reach their orbits well after Neptune stops migrating and compose a recently generated, dynamically active population.
EXPLAINING INVERTED-TEMPERATURE LOOPS IN THE QUIET SOLAR CORONA WITH MAGNETOHYDRODYNAMIC WAVE-MODE CONVERSION
Authors: Schiff Avery J. , Cranmer Steven R. 
Published: October 2016

ABSTRACT
Coronal loops trace out bipolar, arch-like magnetic fields above the Sun’s surface. Recent measurements that combine rotational tomography, extreme-ultraviolet imaging, and potential-field extrapolation have shown the existence of large loops with inverted-temperature profiles, i.e., loops for which the apex temperature is a local minimum, not a maximum. These “down loops” appear to exist primarily in equatorial quiet regions near solar minimum. We simulate both these and the more prevalent large-scale “up loops” by modeling coronal heating as a time-steady superposition of (1) dissipation of incompressible Alfvén wave turbulence and (2) dissipation of compressive waves formed by mode conversion from the initial population of Alfvén waves. We found that when a large percentage (>99%) of the Alfvén waves undergo this conversion, heating is greatly concentrated at the footpoints and stable “down loops” are created. In some cases we found loops with three maxima that are also gravitationally stable. Models that agree with the tomographic temperature data exhibit higher gas pressures for “down loops” than for “up loops,” which is consistent with observations. These models also show a narrow range of Alfvén wave amplitudes: 3 to 6 km s−1 at the coronal base. This is low in comparison to typical observed amplitudes of 20–30 km s−1 in bright X-ray loops. However, the large-scale loops we model are believed to compose a weaker diffuse background that fills much of the volume of the corona. By constraining the physics of loops that underlie quiescent streamers, we hope to better understand the formation of the slow solar wind.
THE AGE AND DISTANCE OF THE KEPLER OPEN CLUSTER NGC 6811 FROM AN ECLIPSING BINARY, TURNOFF STAR PULSATION, AND GIANT ASTEROSEISMOLOGY∗
Authors: Sandquist Eric L. , Jessen-Hansen J. , Shetrone Matthew D. , Brogaard Karsten , Meibom Søren , Leitner Marika , Stello Dennis , Bruntt Hans , Antoci Victoria , Orosz Jerome A. , Grundahl Frank , Frandsen Søren 
Published: October 2016

ABSTRACT
We present the analysis of an eccentric, partially eclipsing long-period (P = 19.23 days) binary system KIC 9777062 that contains main-sequence stars near the turnoff of the intermediate-age open cluster NGC 6811. The primary is a metal-lined Am star with a possible convective blueshift to its radial velocities, and one star (probably the secondary) is likely to be a γ Dor pulsator. The component masses are 1.603 ± 0.006(stat.) ± 0.016(sys.) and 1.419 ± 0.003 ± 0.008

, and the radii are 1.744 ± 0.004 ± 0.002 and 1.544 ± 0.002 ± 0.002

. The isochrone ages of the stars are mildly inconsistent: the age from the mass–radius combination for the primary (1.05 ± 0.05 ± 0.09 Gyr, where the last quote was systematic uncertainty from models and metallicity) is smaller than that from the secondary (1.21 ± 0.05 ± 0.15 Gyr) and is consistent with the inference from the color–magnitude diagram (1.00 ± 0.05 Gyr). We have improved the measurements of the asteroseismic parameters Δν and ν
max for helium-burning stars in the cluster. The masses of the stars appear to be larger (or alternately, the radii appear to be smaller) than predicted from isochrones using the ages derived from the eclipsing stars. The majority of stars near the cluster turnoff are pulsating stars: we identify a sample of 28 δ Sct, 15 γ Dor, and 5 hybrid types. We used the period–luminosity relation for high-amplitude δ Sct stars to fit the ensemble of the strongest frequencies for the cluster members, finding

. This is larger than most previous determinations, but smaller than values derived from the eclipsing binary (10.47 ± 0.05).
URCA COOLING PAIRS IN THE NEUTRON STAR OCEAN AND THEIR EFFECT ON SUPERBURSTS
Authors: Deibel Alex , Meisel Zach , Schatz Hendrik , Brown Edward F. , Cumming Andrew 
Published: October 2016

ABSTRACT
An accretion outburst onto a neutron star deposits hydrogen-rich and/or helium-rich material into the neutron star’s envelope. Thermonuclear burning of accreted material robustly produces Urca pairs—pairs of nuclei that undergo cycles of

-capture and

-decay. The strong T
5 dependence of the Urca cooling neutrino luminosity means that Urca pairs in the neutron star interior potentially remove heat from accretion-driven nuclear reactions. In this study, we identify Urca pairs in the neutron star’s ocean—a plasma of ions and electrons overlaying the neutron star crust—and demonstrate that Urca cooling occurs at all depths in the ocean. We find that Urca pairs in the ocean and crust lower the ocean’s steady-state temperature during an accretion outburst and that unstable carbon ignition, which is thought to trigger superbursts, occurs deeper than it would otherwise. Cooling superburst light curves, however, are only marginally impacted by cooling from Urca pairs because the superburst peak radiative luminosity

is always much greater than the Urca pair neutrino luminosity

in the hot post-superburst ocean.
A PORTRAIT OF COLD GAS IN GALAXIES AT 60 pc RESOLUTION AND A SIMPLE METHOD TO TEST HYPOTHESES THAT LINK SMALL-SCALE ISM STRUCTURE TO GALAXY-SCALE PROCESSES
Authors: Leroy Adam K. , Hughes Annie , Schruba Andreas , Rosolowsky Erik , Blanc Guillermo A. , Bolatto Alberto D. , Colombo Dario , Escala Andres , Kramer Carsten , Kruijssen J. M. Diederik , Meidt Sharon , Pety Jerome , Querejeta Miguel , Sandstrom Karin , Schinnerer Eva , Sliwa Kazimierz , Usero Antonio 
Published: October 2016

ABSTRACT
The cloud-scale density, velocity dispersion, and gravitational boundedness of the interstellar medium (ISM) vary within and among galaxies. In turbulent models, these properties play key roles in the ability of gas to form stars. New high-fidelity, high-resolution surveys offer the prospect to measure these quantities across galaxies. We present a simple approach to make such measurements and to test hypotheses that link small-scale gas structure to star formation and galactic environment. Our calculations capture the key physics of the Larson scaling relations, and we show good correspondence between our approach and a traditional “cloud properties” treatment. However, we argue that our method is preferable in many cases because of its simple, reproducible characterization of all emission. Using, low-J
12CO data from recent surveys, we characterize the molecular ISM at 60 pc resolution in the Antennae, the Large Magellanic Cloud (LMC), M31, M33, M51, and M74. We report the distributions of surface density, velocity dispersion, and gravitational boundedness at 60 pc scales and show galaxy-to-galaxy and intragalaxy variations in each. The distribution of flux as a function of surface density appears roughly lognormal with a 1σ width of ∼0.3 dex, though the center of this distribution varies from galaxy to galaxy. The 60 pc resolution line width and molecular gas surface density correlate well, which is a fundamental behavior expected for virialized or free-falling gas. Varying the measurement scale for the LMC and M31, we show that the molecular ISM has higher surface densities, lower line widths, and more self-gravity at smaller scales.
DETECTION OF SOLAR-LIKE OSCILLATIONS, OBSERVATIONAL CONSTRAINTS, AND STELLAR MODELS FOR θ CYG, THE BRIGHTEST STAR OBSERVED BY THE KEPLER MISSION
Authors: Guzik J. A. , Houdek G. , Chaplin W. J. , Smalley B. , Kurtz D. W. , Gilliland R. L. , Mullally F. , Rowe J. F. , Bryson S. T. , Still M. D. , Antoci V. , Appourchaux T. , Basu S. , Bedding T. R. , Benomar O. , Garcia R. A. , Huber D. , Kjeldsen H. , Latham D. W. , Metcalfe T. S. , Pápics P. I. , White T. R. , Aerts C. , Ballot J. , Boyajian T. S. , Briquet M. , Bruntt H. , Buchhave L. A. , Campante T. L. , Catanzaro G. , Christensen-Dalsgaard J. , Davies G. R. , Doğan G. , Dragomir D. , Doyle A. P. , Elsworth Y. , Frasca A. , Gaulme P. , Gruberbauer M. , Handberg R. , Hekker S. , Karoff C. , Lehmann H. , Mathias P. , Mathur S. , Miglio A. , Molenda-Żakowicz J. , Mosser B. , Murphy S. J. , Régulo C. , Ripepi V. , Salabert D. , Sousa S. G. , Stello D. , Uytterhoeven K. 
Published: October 2016

ABSTRACT

θ Cygni is an F3 spectral type magnitude V = 4.48 main-sequence star that was the brightest star observed by the original Kepler spacecraft mission. Short-cadence (58.8 s) photometric data using a custom aperture were first obtained during Quarter 6 (2010 June–September) and subsequently in Quarters 8 and 12–17. We present analyses of solar-like oscillations based on Q6 and Q8 data, identifying angular degree l = 0, 1, and 2 modes with frequencies of 1000–2700 μHz, a large frequency separation of 83.9 ± 0.4 μHz, and maximum oscillation amplitude at frequency ν
max = 1829 ± 54 μHz. We also present analyses of new ground-based spectroscopic observations, which, combined with interferometric angular diameter measurements, give T
eff = 6697 ± 78 K, radius 1.49 ± 0.03 R
⊙, [Fe/H] = −0.02 ± 0.06 dex, and log g = 4.23 ± 0.03. We calculate stellar models matching these constraints using the Yale Rotating Evolution Code and the Asteroseismic Modeling Portal. The best-fit models have masses of 1.35–1.39 M
⊙ and ages of 1.0–1.6 Gyr. θ Cyg’s T
eff and log g place it cooler than the red edge of the γ Doradus instability region established from pre-Kepler ground-based observations, but just at the red edge derived from pulsation modeling. The pulsation models show γ Dor gravity modes driven by the convective blocking mechanism, with frequencies of 1–3 cycles per day (11 to 33 μHz). However, gravity modes were not seen in Kepler data; one signal at 1.776 cycles per day (20.56 μHz) may be attributable to a faint, possibly background, binary.