bluuebunny/crossref_metadata_2025_split huggingface dataset:
Effect of a high-fat–high-cholesterol diet on gallbladder bile acid composition and gallbladder motility in dogs
Authors: Kakimoto Toshiaki , Kanemoto Hideyuki , Fukushima Kenjiro , Ohno Koichi , Tsujimoto Hajime 
Published: November 2017

Abstract
OBJCTIVE To investigate the effects of dietary lipid overload on bile acid metabolism and gallbladder motility in healthy dogs.
ANIMALS 7 healthy Beagles.
PROCEDURES In a crossover study, dogs were fed a high-fat–high-cholesterol diet (HFCD) or a low-fat diet (LFD) for a period of 2 weeks. After a 4-month washout period, dogs were fed the other diet for 2 weeks. Before and at the end of each feeding period, the concentrations of each of the gallbladder bile acids, cholecystokinin (CCK)-induced gallbladder motility, and bile acid metabolism–related hepatic gene expression were examined in all dogs.
RESULTS The HFCD significantly increased plasma total cholesterol concentrations. The HFCD also increased the concentration of taurochenodeoxycholic acid and decreased the concentration of taurocholic acid in bile and reduced gallbladder contractility, whereas the LFD significantly decreased the concentration of taurodeoxycholic acid in bile. Gene expression analysis revealed significant elevation of cholesterol 7α-hydroxylase mRNA expression after feeding the HFCD for 2 weeks, but the expression of other genes was unchanged.
CONCLUSIONS AND CLINICAL RELEVANCE Feeding the HFCD and LFD for 2 weeks induced changes in gallbladder bile acid composition and gallbladder motility in dogs. In particular, feeding the HFCD caused an increase in plasma total cholesterol concentration, an increase of hydrophobic bile acid concentration in bile, and a decrease in gallbladder sensitivity to CCK. These results suggested that similar bile acid compositional changes and gallbladder hypomotility might be evident in dogs with hyperlipidemia.
A Longitudinal Journey with BYOD Classrooms: Issues of Access, Capability and Outcome Divides
Authors: Adhikari Janak , Mathrani Anuradha , Scogings Chris 
Published: November 2017

Bring Your Own Devices (BYOD) classrooms is the latest addition to the ongoing quest for transforming pedagogical practices and driving educational development outcomes. Governments and policymakers around the world are embracing the idea of integrating digital learning technologies into educational settings backed by research on the benefits offered like the lifelong development of individual learners. While technological interventions open up unlimited possibilities for accessing information and improving collaboration, thereby engaging learners with more interactive learning activities, a new type of gap between individuals could also take shape as the penetration of technologies and adoption stages advance. Results from past projects of similar nature within educational settings have indicated the possible rise in the gap among individuals based on digital access (i.e., equity in access/ownership of digital learning technologies), digital capability (i.e., equity in digital/information literacy skills and usage) and digital outcome (i.e., equity in knowledge acquisition and progression).Therefore, we have conducted a longitudinal study to investigate a BYOD initiative by a New Zealand School. This study shares rich insights in the context of technology-mediated pedagogies and specifically BYOD classroom, as to how digital divides moved beyond access and skills to ensure inclusive learning outcomes. As a part of the five-year study of the technology-mediated teaching and learning initiative, we have been able to explain some of the unanswered questions around the issue of digital divides in the learning process. We investigated issues pertaining to digital divide in the context of BYOD classrooms to make the following revelations. First, the BYOD classroom initiative did not end up accentuating existing gaps in access to digital tools and technologies, despite earlier studies indicating towards increase in gaps. Second, our analysis strongly indicated the changing nature of digital divides with the presence of gaps in terms of information literacy and critical thinking ability, as the BYOD classroom progressed to mature stage. This was eventually bridged in the later stage, as students slowly adjusted to the classroom curricular structures in the BYOD classroom. Third, learner self-efficacy has been identified as a determinant of learning outcomes. In the earlier phase of ICT adoption, learner self-efficacy is influenced by a combination of information literacy, critical thinking ability, and positive motivation; however subsequently, self-efficacy influences affordances in various aspects of social cognitive abilities related to individual’s learning activities affecting how learners engage and apply technology to achieve learning outcomes.
The 2017 AANS Presidential Address. A world of innovation
Authors: Boop Frederick A. 
Published: December 2017

The 2016 scientific meeting of the American Association of Neurological Surgeons (AANS) focused on the theme “A World of Innovation.” In his presidential address, 2016 AANS President Frederick Boop compared the historical development of the specialty of neurological surgery with that of the development of global communications. In the early years, general surgeons training in the United States would spend post-residency time abroad learning from surgical masters in Europe and other places. Since Harvey Cushing’s day, neurosurgeons from around the world continue to travel abroad, with many now coming to America for training at centers of excellence.Current clinical practice is defined by multi-national, multi-center clinical trials, and the AANS subsidiary NeuroPoint Alliance has positioned itself to serve as an international center for the oversight of such trials. The Neurosurgery Research & Education Foundation and the Journal of Neurosurgery Publishing Group have made it possible for a neurosurgeon anywhere with Internet access to learn relevant surgical anatomy, learn new neurosurgical procedures, and watch masters in the field perform operations via high-definition surgical videos at no cost via learning platforms such as the Rhoton Collection, the Neurosurgical Atlas, and Neurosurgical Focus video supplements. At the same time, patients are now traveling abroad to seek medical specialty care. Although the globalization of health care poses certain threats, it also presents neurosurgeons with a world of opportunities.
Four Weeks of Off-Season Training Improves Peak Oxygen Consumption in Female Field Hockey Players
Authors: Funch Lindsey , Lind Erik , True Larissa , Van Langen Deborah , Foley John , Hokanson James 
Published: November 2017

The purpose of the study was to examine the changes in peak oxygen consumption	( V ˙O2peak) and running economy (RE) following four-weeks of high intensity training and concurrent strength and conditioning during the off-season in collegiate female field hockey players. Fourteen female student-athletes (age 19.29 ± 0.91 years) were divided into two training groups, matched from baseline V ˙O2peak: High Intensity Training (HITrun; n = 8) and High Intensity Interval Training (HIIT; n = 6). Participants completed 12 training sessions. HITrun consisted of 30 min of high-intensity running, while HIIT consisted of a series of whole-body high intensity Tabata-style intervals (75–85% of age predicted maximum heart rate) for a total of four minutes. In addition to the interval training, the off-season training included six resistance training sessions, three team practices, and concluded with a team scrimmage. V ˙O2peak was measured pre- and post-training to determine the effectiveness of the training program. A two-way mixed (group × time) ANOVA showed a main effect of time with a statistically significant difference in V ˙O2peak from pre- to post-testing, F(1, 12) = 12.657, p = 0.004, partial η2 = 0.041. Average (±SD) V ˙O2peak increased from 44.64 ± 3.74 to 47.35 ± 3.16 mL·kg−1·min−1 for HIIT group and increased from 45.39 ± 2.80 to 48.22 ± 2.42 mL·kg−1·min−1 for HITrun group. Given the similar improvement in aerobic power, coaches and training staff may find the time saving element of HIIT-type conditioning programs attractive.
Nanolensed Fast Radio Bursts
Authors: Eichler David 
Published: November 2017

Abstract
It is suggested that fast radio bursts can probe gravitational lensing by clumpy dark matter objects that range in mass from 10−3
M
⊙–102
M
⊙. They may provide a more sensitive probe than observations of lensings of objects in the Magellanic Clouds, and could find or rule out clumpy dark matter with an extended mass spectrum.
The Effects of Protostellar Disk Turbulence on CO Emission Lines: A Comparison Study of Disks with Constant CO Abundance versus Chemically Evolving Disks
Authors: Yu Mo , Evans Neal J. , Dodson-Robinson Sarah E. , Willacy Karen , Turner Neal J. 
Published: November 2017

Abstract
Turbulence is the leading candidate for angular momentum transport in protoplanetary disks and therefore influences disk lifetimes and planet formation timescales. However, the turbulent properties of protoplanetary disks are poorly constrained observationally. Recent studies have found turbulent speeds smaller than what fully-developed MRI would produce (Flaherty et al.). However, existing studies assumed a constant CO/H2 ratio of 10−4 in locations where CO is not frozen-out or photo-dissociated. Our previous studies of evolving disk chemistry indicate that CO is depleted by incorporation into complex organic molecules well inside the freeze-out radius of CO. We consider the effects of this chemical depletion on measurements of turbulence. Simon et al. suggested that the ratio of the peak line flux to the flux at line center of the CO J = 3–2 transition is a reasonable diagnostic of turbulence, so we focus on that metric, while adding some analysis of the more complex effects on spatial distribution. We simulate the emission lines of CO based on chemical evolution models presented in Yu et al., and find that the peak-to-trough ratio changes as a function of time as CO is destroyed. Specifically, a CO-depleted disk with high turbulent velocity mimics the peak-to-trough ratios of a non-CO-depleted disk with lower turbulent velocity. We suggest that disk observers and modelers take into account the possibility of CO depletion when using line profiles or peak-to-trough ratios to constrain the degree of turbulence in disks. Assuming that

at all disk radii can lead to underestimates of turbulent speeds in the disk by at least 0.2 km s−1.
Bow Ties in the Sky. II. Searching for Gamma-Ray Halos in the Fermi Sky Using Anisotropy
Authors: Tiede Paul , Broderick Avery E. , Shalaby Mohamad , Pfrommer Christoph , Puchwein Ewald , Chang Philip , Lamberts Astrid 
Published: November 2017

Abstract
Many-degree-scale gamma-ray halos are expected to surround extragalactic high-energy gamma-ray sources. These arise from the inverse Compton emission of an intergalactic population of relativistic electron/positron pairs generated by the annihilation of

gamma rays on the extragalactic background light. These are typically anisotropic due to the jetted structure from which they originate (in the case of radio galaxies) or are oriented perpendicular to a large-scale intergalactic magnetic field (for blazar geometries). Here, we propose a novel method for detecting these inverse Compton gamma-ray halos based on this anisotropic structure that is centered on the active galactic nucleus (AGN). By marginalizing over the radial distribution of halo photons, we demonstrate that the angular power spectrum shows a characteristic sawtooth pattern with a dominant dipolar power and elevated even multipoles. Specifically, we show that by stacking those angular power spectra instead of images, it is possible to robustly detect gamma-ray halos with existing Fermi Large Area Telescope (LAT) observations for a broad class of intergalactic magnetic fields. Importantly, by testing a large number of systematics, our suggested power spectrum statistics appears to be robust and unbiased with respect to systematic uncertainties within the LAT instrumental response and associated with contaminating astronomical sources.
Phase Offsets and the Energy Budgets of Hot Jupiters
Authors: Schwartz Joel C. , Kashner Zane , Jovmir Diana , Cowan Nicolas B. 
Published: November 2017

Abstract
Thermal phase curves of short-period planets on circular orbits provide joint constraints on the fraction of incoming energy that is reflected (Bond albedo) and the fraction of absorbed energy radiated by the night hemisphere (heat recirculation efficiency). Many empirical studies of hot Jupiters have implicitly assumed that the dayside is the hottest hemisphere and the nightside is the coldest hemisphere. For a given eclipse depth and phase amplitude, an orbital lag between a planet’s peak brightness and its eclipse—a phase offset—implies that planet’s nightside emits greater flux. To quantify how phase offsets impact the energy budgets of short-period planets, we compile all infrared observations of the nine planets with multi-band eclipse depths and phase curves. Accounting for phase offsets shifts planets to lower Bond albedo and greater day–night heat transport, usually by ≲1σ. For WASP-12b, the published phase variations have been analyzed in two different ways, and the inferred energy budget depends sensitively on which analysis one adopts. Our fiducial scenario supports a Bond albedo of

, significantly higher than the published optical geometric albedo, and a recirculation efficiency of

, following the trend of larger day–night temperature contrast with greater stellar irradiation. If instead we adopt the alternative analysis, then WASP-12b has a Bond albedo consistent with zero and a much higher recirculation efficiency. To definitively determine the energy budget of WASP-12b, new observational analyses will be necessary.
An Observationally Constrained 3D Potential-field Source-surface Model for the Evolution of Longitude-dependent Coronal Structures
Authors: Everson Rosa Wallace , Dikpati Mausumi 
Published: November 2017

Abstract
The improvement of techniques for realistically modeling the solar magnetic field has been a priority in solar physics for decades. The challenge of creating synoptic maps of the photosphere that reliably reflect conditions at all locations concurrently is a major limitation to progress in this area. White-light coronal images, which contain morphological information about the 3D corona at the solar limb, have been largely overlooked as a resource for constraining or correcting synoptic maps. We explore a complementary approach to traditional magnetogram-based coronal field solutions that makes use of these images. Applying a modified 3D potential-field source-surface (PFSS) model, we investigate the use of MLSO white-light coronal images for deriving 3D coronal morphology by empirically fitting model solutions with observations only. Applying an iterative technique to coronal image data from the solar minima preceding Cycles 22, 23, and 24, and the ascending phase of Cycle 23, we obtain model solutions as linear combinations of low order and degree spherical harmonics. We find that the 3D morphology produced by our method agrees qualitatively with traditional magnetogram-based PFSS approaches for coronas that are dipole dominated. For more complex coronas, additional constraints are needed to account for polarity and correct interpretation of coronal structures. Estimates of the relative strength of dipoles versus multipoles in the coronal field also agree with traditional methods, but the contributions of specific multipoles do not, revealing nonuniqueness in our results. Future work will incorporate magnetogram-based solutions prior to applying the iterative technique.
NuSTAR View of the Black Hole Wind in the Galaxy Merger IRAS F11119+3257
Authors: Tombesi F. , Veilleux S. , Meléndez M. , Lohfink A. , Reeves J. N. , Piconcelli E. , Fiore F. , Feruglio C. 
Published: November 2017

Abstract
Galactic winds driven by active galactic nuclei (AGNs) have been invoked to play a fundamental role in the co-evolution between supermassive black holes and their host galaxies. Finding observational evidence of such feedback mechanisms is of crucial importance and it requires a multi-wavelength approach in order to compare winds at different scales and phases. In Tombesi et al., we reported the detection of a powerful ultra-fast outflow (UFO) in the Suzaku X-ray spectrum of the ultra-luminous infrared galaxy IRAS F11119+3257. The comparison with a galaxy-scale OH molecular outflow observed with Herschel in the same source supported the energy-conserving scenario for AGN feedback. The main objective of this work is to perform an independent check of the Suzaku results using the higher sensitivity and wider X-ray continuum coverage of NuSTAR. We clearly detect a highly ionized Fe K UFO in the 100 ks NuSTAR spectrum with parameters N
H = (3.2 ± 1.5) × 1024 cm−2, log ξ =

erg s−1 cm, and

. The launching radius is likely at a distance of r ≥ 16r

s
from the black hole. The mass outflow rate is in the range of

≃ 0.5–2 M
⊙ yr−1. The UFO momentum rate and power are

≃ 0.5–2 L
AGN/c and

≃ 7%–27% L
AGN, respectively. The UFO parameters are consistent between the 2013 Suzaku and the 2015 NuSTAR observations. Only the column density is found to be variable, possibly suggesting a clumpy wind. The comparison with the energetics of molecular outflows estimated in infrared and millimeter wavelengths support a connection between the nuclear and galaxy-scale winds in luminous AGNs.
Observations of the GRB Afterglow ATLAS17aeu and Its Possible Association with GW 170104
Authors: Stalder B. , Tonry J. , Smartt S. J. , Coughlin M. , Chambers K. C. , Stubbs C. W. , Chen T.-W. , Kankare E. , Smith K. W. , Denneau L. , Sherstyuk A. , Heinze A. , Weiland H. , Rest A. , Young D. R. , Huber M. E. , Flewelling H. , Lowe T. , Magnier E. A. , Schultz A. S. B. , Waters C. , Wainscoat R. , Willman M. , Wright D. E. , Chu J. , Sanders D. , Inserra C. , Maguire K. , Kotak R. 
Published: November 2017

Abstract
We report the discovery and multiwavelength data analysis of the peculiar optical transient, ATLAS17aeu. This transient was identified in the sky map of the LIGO gravitational wave event GW 170104 by our ATLAS and Pan-STARRS coverage. ATLAS17aeu was discovered 23.1 hr after GW 170104 and rapidly faded over the next three nights, with a spectrum revealing a blue featureless continuum. The transient was also detected as a fading X-ray source by Swift and in the radio at 6 and 15 GHz. The gamma-ray burst GRB 170105A was detected by three satellites 19.04 hr after GW 170104 and 4.10 hr before our first optical detection. We analyze the multiwavelength fluxes in the context of the known GRB population and discuss the observed sky rates of GRBs and their afterglows. We find it statistically likely that ATLAS17aeu is an afterglow associated with GRB 170105A, with a chance coincidence ruled out at the 99% confidence or 2.6σ. A long, soft GRB within a redshift range of

would be consistent with all the observed multiwavelength data. The Poisson probability of a chance occurrence of GW 170104 and ATLAS17aeu is p = 0.04. This is the probability of a chance coincidence in 2D sky location and in time. These observations indicate that ATLAS17aeu is plausibly a normal GRB afterglow at significantly higher redshift than the distance constraint for GW 170104 and therefore a chance coincidence. However, if a redshift of the faint host were to place it within the GW 170104 distance range, then physical association with GW 170104 should be considered.
HST/COS Far-ultraviolet Spectroscopic Analysis of U Geminorum Following a Wide Outburst*
Authors: Godon Patrick , Shara Michael M. , Sion Edward M. , Zurek David 
Published: November 2017

Abstract
We used the Cosmic Origins Spectrograph (COS) on the Hubble Space Telescope (HST) to obtain a series of four far-ultraviolet (FUV; 915–2148 Å) spectroscopic observations of the prototypical dwarf nova U Geminorum during its cooling following a two-week outburst. Our FUV spectral analysis of the data indicates that the white dwarf (WD) cools from a temperature of ∼41,500 K, 15 days after the peak of the outburst, to ∼36,250 K, 56 days after the peak of the outburst, assuming a massive WD (log(g) = 8.8) and a distance of 100.4 ± 3.7 pc. These results are self-consistent with a ∼1.1 M
⊙ WD with a 5000 ± 200 km radius. The spectra show absorption lines of H i, He ii, C ii iii iv, N iii iv, O vi, S iv, Si ii iii iv, Al iii, Ar iii, and Fe ii, but no emission features. We find suprasolar abundances of nitrogen, confirming the anomalous high N/C ratio. The FUV light curve reveals a ±5% modulation with the orbital phase, showing dips near phases 0.25 and ∼0.75, where the spectra exhibit an increase in the depth of some absorption lines and in particular strong absorption lines from Si ii, Al iii, and Ar iii. The phase dependence we observe is consistent with material overflowing the disk rim at the hot spot, reaching a maximum elevation near phase 0.75, falling back at smaller radii near phase 0.5 where it bounces off the disk surface, and again rising above the disk near phase ∼0.25. There is a large scatter in the absorption lines’ velocities, especially for the silicon lines, while the carbon lines seem to match more closely the orbital velocity of the WD. This indicates that many absorption lines are affected by—or form in—the overflowing stream material veiling the WD, making the analysis of the WD spectra more difficult.
Evolution of Proton and Alpha Particle Velocities through the Solar Cycle
Authors: Ďurovcová T. , Šafránková J. , Němeček Z. , Richardson J. D. 
Published: November 2017

Abstract
Relative properties of solar wind protons and α particles are often used as indicators of a source region on the solar surface, and analysis of their evolution along the solar wind path tests our understanding of physics of multicomponent magnetized plasma. The paper deals with the comprehensive analysis of the difference between proton and α particle bulk velocities at 1 au with a special emphasis on interplanetary coronal mass ejections (ICMEs). A comparison of about 20 years of Wind observations at 1 au with Helios measurements closer to the Sun (0.3–0.7 au) generally confirms the present knowledge that (1) the differential speed between both species increases with the proton speed; (2) the differential speed is lower than the local Alfvén speed; (3) α particles are faster than protons near the Sun, and this difference decreases with the increasing distance. However, we found a much larger portion of observations with protons faster than α particles in Wind than in Helios data and attributed this effect to a preferential acceleration of the protons in the solar wind. A distinct population characterized by a very small differential velocity and nearly equal proton and α particle temperatures that is frequently observed around the maximum of solar activity was attributed to ICMEs. Since this population does not exhibit any evolution with increasing collisional age, we suggest that, by contrast to the solar wind from other sources, ICMEs are born in an equilibrium state and gradually lose this equilibrium due to interactions with the ambient solar wind.