bluuebunny/crossref_metadata_2025_split huggingface dataset:
Comparison of two ultrasound-guided injection techniques targeting the sacroiliac joint region in equine cadavers
Authors: Bergamino Chiara , Sanders Ruth , Fogarty Ursula , Puggioni Antonella , Kearney Clodagh , David Florent , David Stack John 
Published: July 2016

Summary
Objectives: To compare the accuracy and distribution of injectate for cranial (CR) and caudomedial (CM) ultrasound-guided injections of equine sacroiliac joints.
Methods: Both sacroiliac joints from 10 lumbo sacropelvic specimens were injected using cranial parasagittal (CR; curved 18 gauge, 25 cm spinal needles) and caudomedial (CM; straight 18 gauge, 15 cm spinal needles) ultrasound-guided approaches. Injectate consisted of 4 ml iodinated contrast and 2 ml methylene blue. Computed tomo-graphical (CT) scans were performed before and after injections. Time for needle guidance and repositioning attempts were recorded. The CT sequences were analysed for accuracy and distribution of contrast.
Results: Intra-articular contrast was detected in sacroiliac joints following 15/40 injections. The CR and CM approaches deposited injectate ≤ 2 cm from sacroiliac joint margins following 17/20 and 20/20 injections, respectively. Median distance of closest contrast to the sacroiliac joint was 0.4 cm (interquartile range [IQR]: 1.5 cm) for CR approaches and 0.6 cm (IQR: 0.95 cm) for CM approaches. Cranial injections resulted in injectate contacting lumbosacral intertrans-verse joints 15/20 times. Caudomedial injections were perivascular 16/20 times.
Limitations: Safety and efficacy could not be established.
Clinical relevance: Cranial and CM ultra-sound-guided injections targeting sacroiliac joints were very accurate for periarticular injection, but accuracy was poor for intra- articular injection. Injectate was frequently found in contact with interosseous sacroiliac ligaments, as well as neurovascular and synovial structures in close vicinity of sacroiliac joints.
New development and validation of 50 SSR markers in breadfruit (Artocarpus altilis, Moraceae) by next‐generation sequencing
Authors: De Bellis Fabien , Malapa Roger , Kagy Valérie , Lebegin Stéphane , Billot Claire , Labouisse Jean‐Pierre 
Published: July 2016

Premise of the study:Using next‐generation sequencing technology, new microsatellite loci were characterized in Artocarpus altilis (Moraceae) and two congeners to increase the number of available markers for genotyping breadfruit cultivars.Methods and Results:A total of 47,607 simple sequence repeat loci were obtained by sequencing a library of breadfruit genomic DNA with an Illumina MiSeq system. Among them, 50 single‐locus markers were selected and assessed using 41 samples (39 A. altilis, one A. camansi, and one A. heterophyllus). All loci were polymorphic in A. altilis, 44 in A. camansi, and 21 in A. heterophyllus. The number of alleles per locus ranged from two to 19.Conclusions:The new markers will be useful for assessing the identity and genetic diversity of breadfruit cultivars on a small geographical scale, gaining a better understanding of farmer management practices, and will help to optimize breadfruit genebank management.
THE CORRELATION BETWEEN METALLICITY AND DEBRIS DISK MASS
Authors: Gáspár András , Rieke George H. , Ballering Nicholas 
Published: July 2016

ABSTRACT
We find that the initial dust masses in planetary debris disks are correlated with the metallicities of their central stars. We compiled a large sample of systems, including Spitzer, the Herschel DUNES and DEBRIS surveys, and WISE debris disk candidates. We also merged 33 metallicity catalogs to provide homogeneous [Fe/H] and

values. We analyzed this merged sample, including 222 detected disks (74 warm and 148 cold) around a total of 187 systems (some with multiple components) and 440 disks with only upper limits (125 warm and 315 cold) around a total of 360 systems. The disk dust masses at a common early evolutionary point in time were determined using our numerical disk evolutionary code, evolving a unique model for each of the 662 disks backward to an age of 1 Myr. We find that disk-bearing stars seldom have metallicities less than

and that the distribution of warm component masses lacks examples with large mass around stars of low metallicity (

). Previous efforts to find a correlation have been largely unsuccessful; the primary improvements supporting our result are (1) basing the study on dust masses, not just infrared excess detections; (2) including upper limits on dust mass in a quantitative way; (3) accounting for the evolution of debris disk excesses as systems age; (4) accounting fully for the range of uncertainties in metallicity measurements; and (5) having a statistically large enough sample.
ON THE RELATIONSHIP BETWEEN SUNSPOT STRUCTURE AND MAGNETIC FIELD CHANGES ASSOCIATED WITH SOLAR FLARES
Authors: Song Y. L. , Zhang M. 
Published: July 2016

ABSTRACT
Many previous studies have shown that magnetic fields and sunspot structures present rapid and irreversible changes associated with solar flares. In this paper, we first use five X-class flares observed by Solar Dynamics Observatory/Helioseismic and Magnetic Imager to show that not only do magnetic fields and sunspot structures show rapid, irreversible changes, but also that these changes are closely related both spatially and temporally. The magnitudes of the correlation coefficients between the temporal variations of the horizontal magnetic field and sunspot intensity are all larger than 0.90, with a maximum value of 0.99 and an average value of 0.96. Then, using four active regions during quiescent periods, three observed and one simulated, we show that in sunspot penumbra regions there also exists a close correlation between sunspot intensity and horizontal magnetic field strength in addition to the well-known correlation between sunspot intensity and the normal magnetic field strength. By connecting these two observational phenomena, we show that the sunspot structure change and magnetic field change are two facets of the same phenomena of solar flares; one change might be induced by the change of the other due to a linear correlation between sunspot intensity and magnetic field strength out of a local force balance.
IGRINS SPECTROSCOPY OF CLASS I SOURCES: IRAS 03445+3242 AND IRAS 04239+2436
Authors: Lee Seokho , Lee Jeong-Eun , Park Sunkyung , Lee Jae-Joon , Kidder Benjamin , Mace Gregory N. , Jaffe Daniel T. 
Published: July 2016

ABSTRACT
We have detected molecular and atomic line emission from the hot and warm disks of two Class I sources, IRAS 03445+3242 and IRAS 04239+2436, using the high-resolution Immersion GRating INfrared Spectrograph (IGRINS). CO overtone band transitions and near-IR lines of Na i and Ca i, all in emission, trace the hot inner disk, while CO rovibrational absorption spectra of the first overtone transition trace the warm gas within the inner few AU of the disk. The emission-line profiles for both sources show evidence for Keplerian disks. A thin Keplerian disk with power-law temperature and column density profiles with a projected rotational velocity of ∼60–75 km s−1 and a gas temperature of ∼3500 K at the innermost annulus can reproduce the CO overtone band emission. Na i and Ca i emission lines also arise from this disk, but they show complicated line features possibly affected by photospheric absorption lines. Multi-epoch observations show asymmetric variations of the line profiles on one-year (CO overtone bandhead and atomic lines for IRAS 03445+3242) or on one-day (atomic lines for IRAS 04239+2436) timescales, implying non-axisymmetric features in disks. The narrow CO rovibrational absorption spectra (v = 0

→

2) indicate that both warm (>150 K) and cold (∼20–30 K) CO gas are present along the line of sight to the inner disk. This study demonstrates the power of IGRINS as a tool for studies of the sub-AU-scale hot and AU-scale warm protoplanetary disks with its simultaneous coverage of the full H and K bands with high spectral resolution (R = 45,000) allowing many aspects of the sources to be investigated at once.
DID THE CRAB PULSAR UNDERGO A SMALL GLITCH IN 2006 LATE MARCH/EARLY APRIL?
Authors: Vivekanand M. 
Published: July 2016

ABSTRACT
On 2006 August 23 the Crab Pulsar underwent a glitch, which was reported by the Jodrell Bank and the Xinjiang radio observatories. Neither data are available to the public. However, the Jodrell group publishes monthly arrival times of the Crab Pulsar pulse (their actual observations are done daily), and using these, it is shown that about 5 months earlier the Crab Pulsar probably underwent a small glitch, which has not been reported before. Neither observatory discusses the detailed analysis of data from 2006 March to August; either they may not have detected this small glitch, or they may have attributed it to timing noise in the Crab Pulsar. The above result is verified using X-ray data from RXTE. If this is indeed true, this is probably the smallest glitch observed in the Crab Pulsar so far, whose implications are discussed. This work addresses the confusion possible between small-magnitude glitches and timing noise in pulsars.
MULTIPLE OUTFLOWS IN THE GIANT ERUPTION OF A MASSIVE STAR*
Authors: Humphreys Roberta M. , Martin John C. , Gordon Michael S. , Jones Terry J. 
Published: July 2016

ABSTRACT
The supernova impostor PSN J09132750+7627410 in NGC 2748 reached a maximum luminosity of ≈−14 mag. It was quickly realized that it was not a true supernova, but another example of a nonterminal giant eruption. PSN J09132750+7627410 is distinguished by multiple P Cygni absorption minima in the Balmer emission lines that correspond to outflow velocities of −400, −1100, and −1600 km s−1. Multiple outflows have been observed in only a few other objects. In this paper we describe the evolution of the spectrum and the P Cygni profiles for 3 months past maximum, the post-maximum formation of a cool, dense wind, and the identification of a possible progenitor. One of the possible progenitors is an infrared source. Its pre-eruption spectral energy distribution suggests a bolometric luminosity of −8.3 mag and a dust temperature of 780 K. If it is the progenitor, it is above the AGB limit, unlike the intermediate-luminosity red transients. The three P Cygni profiles could be due to ejecta from the current eruption, the wind of the progenitor, or previous mass-loss events. We suggest that they were all formed as part of the same high-mass-loss event and are due to material ejected at different velocities or energies. We also suggest that multiple outflows during giant eruptions may be more common than reported.
PROBABILITY OF CME IMPACT ON EXOPLANETS ORBITING M DWARFS AND SOLAR-LIKE STARS
Authors: Kay C. , Opher M. , Kornbleuth M. 
Published: July 2016

ABSTRACT
Solar coronal mass ejections (CMEs) produce adverse space weather effects at Earth. Planets in the close habitable zone of magnetically active M dwarfs may experience more extreme space weather than at Earth, including frequent CME impacts leading to atmospheric erosion and leaving the surface exposed to extreme flare activity. Similar erosion may occur for hot Jupiters with close orbits around solar-like stars. We have developed a model, Forecasting a CME's Altered Trajectory (ForeCAT), which predicts a CME's deflection. We adapt ForeCAT to simulate CME deflections for the mid-type M dwarf V374 Peg and hot Jupiters with solar-type hosts. V374 Peg's strong magnetic fields can trap CMEs at the M dwarfs's Astrospheric Current Sheet, that is, the location of the minimum in the background magnetic field. Solar-type CMEs behave similarly, but have much smaller deflections and do not become trapped at the Astrospheric Current Sheet. The probability of planetary impact decreases with increasing inclination of the planetary orbit with respect to the Astrospheric Current Sheet: 0.5–5 CME impacts per day for M dwarf exoplanets, 0.05–0.5 CME impacts per day for solar-type hot Jupiters. We determine the minimum planetary magnetic field necessary to shield a planet's atmosphere from CME impacts. M dwarf exoplanets require values between tens and hundreds of Gauss. Hot Jupiters around a solar-type star, however, require a more reasonable <30 G. These values exceed the magnitude required to shield a planet from the stellar wind, suggesting that CMEs may be the key driver of atmospheric losses.
THE IBEX RIBBON AND THE PICKUP ION RING STABILITY IN THE OUTER HELIOSHEATH. II. MONTE-CARLO AND PARTICLE-IN-CELL MODEL RESULTS
Authors: Niemiec J. , Florinski V. , Heerikhuisen J. , Nishikawa K.-I. 
Published: July 2016

ABSTRACT
The nearly circular ribbon of energetic neutral atom (ENA) emission discovered by NASA’s Interplanetary Boundary EXplorer satellite (IBEX), is most commonly attributed to the effect of charge exchange of secondary pickup ions (PUIs) gyrating about the magnetic field in the outer heliosheath (OHS) and the interstellar space beyond. The first paper in the series (Paper I) presented a theoretical analysis of the pickup process in the OHS and hybrid-kinetic simulations, revealing that the kinetic properties of freshly injected proton rings depend sensitively on the details of their velocity distribution. It was demonstrated that only rings that are not too narrow (parallel thermal spread above a few km s−1) and not too wide (parallel temperature smaller than the core plasma temperature) could remain stable for a period of time long enough to generate ribbon ENAs. This paper investigates the role of electron dynamics and the extra spatial degree of freedom in the ring ion scattering process with the help of two-dimensional full particle-in-cell (PIC) kinetic simulations. A good agreement is observed between ring evolution under unstable conditions in hybrid and PIC models, and the dominant modes are found to propagate parallel to the magnetic field. We also present more realistic ribbon PUI distributions generated using Monte Carlo simulations of atomic hydrogen in the global heliosphere and examine the effect of both the cold ring-like and the hot “halo” PUIs produced from heliosheath ENAs on the ring stability. It is shown that the second PUI population enhances the fluctuation growth rate, leading to faster isotropization of the solar-wind-derived ring ions.
THE HYDROGEN EPOCH OF REIONIZATION ARRAY DISH. I. BEAM PATTERN MEASUREMENTS AND SCIENCE IMPLICATIONS
Authors: Neben Abraham R. , Bradley Richard F. , Hewitt Jacqueline N. , DeBoer David R. , Parsons Aaron R. , Aguirre James E. , Ali Zaki S. , Cheng Carina , Ewall-Wice Aaron , Patra Nipanjana , Thyagarajan Nithyanandan , Bowman Judd , Dickenson Roger , Dillon Joshua S. , Doolittle Phillip , Egan Dennis , Hedrick Mike , Jacobs Daniel C. , Kohn Saul A. , Klima Patricia J. , Moodley Kavilan , Saliwanchik Benjamin R. B. , Schaffner Patrick , Shelton John , Taylor H. A. , Taylor Rusty , Tegmark Max , Wirt Butch , Zheng Haoxuan 
Published: July 2016

ABSTRACT
The Hydrogen Epoch of Reionization Array (HERA) is a radio interferometer aiming to detect the power spectrum of 21 cm fluctuations from neutral hydrogen from the epoch of reionization (EOR). Drawing on lessons from the Murchison Widefield Array and the Precision Array for Probing the EOR, HERA is a hexagonal array of large (14 m diameter) dishes with suspended dipole feeds. The dish not only determines overall sensitivity, but also affects the observed frequency structure of foregrounds in the interferometer. This is the first of a series of four papers characterizing the frequency and angular response of the dish with simulations and measurements. In this paper, we focus on the angular response (i.e., power pattern), which sets the relative weighting between sky regions of high and low delay and thus apparent source frequency structure. We measure the angular response at 137 MHz using the ORBCOMM beam mapping system of Neben et al. We measure a collecting area of 93 m2 in the optimal dish/feed configuration, implying that HERA-320 should detect the EOR power spectrum at z ∼ 9 with a signal-to-noise ratio of 12.7 using a foreground avoidance approach with a single season of observations and 74.3 using a foreground subtraction approach. Finally, we study the impact of these beam measurements on the distribution of foregrounds in Fourier space.
NONUNIVERSAL STAR FORMATION EFFICIENCY IN TURBULENT ISM
Authors: Semenov Vadim A. , Kravtsov Andrey V. , Gnedin Nickolay Y. 
Published: July 2016

ABSTRACT
We present a study of a star formation prescription in which star formation efficiency (SFE) depends on local gas density and turbulent velocity dispersion, as suggested by direct simulations of SF in turbulent giant molecular clouds (GMCs). We test the model using a simulation of an isolated Milky-Way-sized galaxy with a self-consistent treatment of turbulence on unresolved scales. We show that this prescription predicts a wide variation of local SFE per free-fall time,

∼ 0.1%–10%, and gas depletion time,

∼ 0.1–10 Gyr. In addition, it predicts an effective density threshold for star formation due to suppression of

in warm diffuse gas stabilized by thermal pressure. We show that the model predicts star formation rates (SFRs) in agreement with observations from the scales of individual star-forming regions to the kiloparsec scales. This agreement is nontrivial, as the model was not tuned in any way and the predicted SFRs on all scales are determined by the distribution of the GMC-scale densities and turbulent velocities σ in the cold gas within the galaxy, which is shaped by galactic dynamics. The broad agreement of the star formation prescription calibrated in the GMC-scale simulations with observations both gives credence to such simulations and promises to put star formation modeling in galaxy formation simulations on a much firmer theoretical footing.
Open Modular Hardware and Software Kit for Creations of Remote Experiments Accessible from PC and Mobile Devices
Authors: Lustig Frantisek , Dvorak Jiri , Kuriscak Pavel , Brom Pavel 
Published: July 2016

The goal of this paper is to introduce open modular hardware and software system “iSES Remote Lab SDK” (iSES – internet School Experimental Studio) designed for easy creation of real remotely controlled laboratories (RCL) that are accessible from PC, tablets and mobile phones. Open modular system “iSES Remote Lab SDK” consists of approx. 20 freely distributable JavaScript objects in a commented source code. Widgets are highly configurable and provide many well documented options and allow to build a complex measurement and control interface with data and video transfer. Open modular system “iSES Remote Lab SDK” can communicate with different measurement platforms (ISES, Arduino are ready; CMA CoachLab, Vernier etc. are tested), and also common universal measurement devices with a COM or USB port, further universal rotation and linear motion stepper motors, etc.). We will introdukce our 18 online advanced remote labs. Any user may have an access to the RCL on PC and mobile devices (iPad, smart phone, etc.) as well. Even non-programmers can build up a simple RCL and publish it in 15 minutes on the Internet! System “iSES Remote Lab SDK“ has obtained the GOLC Online Laboratory Award 2016 in the category Remote Controlled Lab [1].
L’étranger à la cour de France selon l’ambassade espagnole auprès du Roi très chrétien (1re moitié du XVIIe siècle)
Authors: Hugon Alain 
Published: July 2016

La question de la perception des étrangers se pose de manière singulière pour les diplomates du roi d’Espagne à la cour de France car ils étaient issus d’un Empire qui agrégeait de nombreuses possessions et de nombreux peuples, et eux-mêmes n’étaient pas toujours de la nationalité de leur souverain. De ce fait, les ambassadeurs du Roi catholique percevaient-ils la nationalité et la naturalité différemment des sujets du roi de France en sa cour ? L’hostilité de celle-ci à leur égard et le contexte de rivalité expliquent l’attention que mettaient les diplomates à s’observer les uns les autres, bien qu’ils fussent tous étrangers. Ils se trouvaient confrontés à un espace curial qui délimitait de plus en plus nettement les espaces de pouvoir, favorisant les concurrences diplomatiques. Par ailleurs, une tendance à l’institutionnalisation des fonctions de contrôle des agents apparaissait à la cour de France, à laquelle ils étaient sensibles.
Les séries historiques entre la fiction et le réel : quand les scénaristes rivalisent avec les historiens
Authors: Deroide Ioanis 
Published: July 2016

Cet article explore les liens entre les récits que construisent les historiens dans leurs livres et ceux que nous proposent les séries télévisées historiques afin de mettre en lumière comment les seconds peuvent concurrencer les premiers. Sa première partie montre les atouts dont disposent les auteurs de fictions télévisées pour traiter du passé de manière particulièrement vivante et riche, plus encore qu’au cinéma. Sa deuxième partie établit que les séries dites historiques relèvent davantage d’un travail de mémoire que d’histoire puisque justement le passé est saisi comme vivant dans une démarche où l’affect l’emporte sur la raison. Sa troisième partie essaie de définir ce que serait une série véritablement « historienne », c’est-à-dire construite selon un regard similaire à celui que l’historien porte sur l’objet de son étude.
Rome : un péplum enfin réaliste ?
Authors: Bessières Vivien 
Published: July 2016

Nous aimerions nous demander si la forme sérielle ne conduit pas à repenser les termes du débat sur le réalisme et la mimesis. La question de la réalité est-elle la même au cinéma et dans une série télévisée ? La série Rome (HBO, 2005-7) participe d’un genre à prétention réaliste : le péplum, ou plutôt l’epic aux États-Unis. Passant d’un art à l’autre, le genre modifie-t-il son rapport au réel ? Il semble bien que, du film à la série, le réalisme de l’espace-temps ne cesse pas de se trouver confronté aux exigences génériques. Chaque genre réaliste constitue ainsi un vraisemblable propre. Sous ce rapport, une série n’est pas plus « vraie » qu’un film, et la réalité historique est toujours plus ou moins déformée au service de la fiction. Seul change le choix opéré dans le matériau historique – d’un art de l’événement à un art du quotidien. Le topos du combat de gladiateurs, par exemple, connaît un traitement tout différent sur le grand écran et sur le petit. Dans Gladiator, c’est un événement exceptionnel, qui a lieu dans l’immense amphithéâtre du Colisée, et auquel assistent l’empereur et sa cour. Dans Rome, c’est une manière habituelle de rendre la justice. Le combat se déroule dans une construction provisoire en bois, et seule la plèbe est présente. Films et séries font leur choix dans le matériau historique selon deux logiques différentes : la grande histoire événementielle pour les premiers ; le quotidien des petites gens pour les secondes. Cette nouvelle découpe du réel rejoint finalement l’évolution récente de la discipline historique.