bluuebunny/crossref_metadata_2025_split huggingface dataset:
UKIRT MICROLENSING SURVEYS AS A PATHFINDER FOR WFIRST: THE DETECTION OF FIVE HIGHLY EXTINGUISHED LOW-
EVENTS
Authors: Shvartzvald Y. , Bryden G. , Gould A. , Henderson C. B. , Howell S. B. , Beichman C. 
Published: January 2017

ABSTRACT
Optical microlensing surveys are restricted from detecting events near the Galactic plane and center, where the event rate is thought to be the highest due to the high optical extinction of these fields. In the near-infrared (NIR), however, the lower extinction leads to a corresponding increase in event detections and is a primary driver for the wavelength coverage of the WFIRST microlensing survey. During the 2015 and 2016 bulge observing seasons, we conducted NIR microlensing surveys with UKIRT in conjunction with and in support of the Spitzer and Kepler microlensing campaigns. Here, we report on five highly extinguished (

), low-Galactic latitude (

) microlensing events discovered from our 2016 survey. Four of them were monitored with an hourly cadence by optical surveys but were not reported as discoveries, likely due to the high extinction. Our UKIRT surveys and suggested future NIR surveys enable the first measurement of the microlensing event rate in the NIR. This wavelength regime overlaps with the bandpass of the filter in which the WFIRST microlensing survey will conduct its highest-cadence observations, making this event rate derivation critically important for optimizing its yield.
CONSEQUENCES OF A DISTANT MASSIVE PLANET ON THE LARGE SEMIMAJOR AXIS TRANS-NEPTUNIAN OBJECTS
Authors: Shankman C. , Kavelaars J. J. , Lawler S. M. , Gladman B. J. , Bannister M. T. 
Published: January 2017

Abstract
We explore the distant giant planet hypothesis by integrating the large-semimajor-axis, large-pericenter trans-Neptunian objects (TNOs) in the presence of the giant planets and an external perturber whose orbit is consistent with the proposed distant, eccentric, and inclined giant planet, so-called planet 9. We find that TNOs with semimajor axes greater than 250 au experience some longitude of perihelion shepherding, but that a generic outcome of such evolutions is that the TNOs evolve to larger pericenter orbits and commonly get raised to retrograde inclinations. This pericenter and inclination evolution requires a massive disk of TNOs (tens of

) in order to explain the detection of the known sample today. Some of the highly inclined orbits produced by the examined perturbers will be inside of the orbital parameter space probed by prior surveys, implying a missing signature of the ninth-planet scenario. The distant giant planet scenarios explored in this work do not reproduce the observed signal of simultaneous clustering in argument of pericenter, longitude of the ascending node, and longitude of perihelion in the region of the known TNOs.
DHIGLS: DRAO H i INTERMEDIATE GALACTIC LATITUDE SURVEY
Authors: Blagrave K. , Martin P. G. , Joncas G. , Kothes R. , Stil J. M. , Miville-Deschênes M. A. , Lockman Felix J. , Taylor A. R. 
Published: January 2017

ABSTRACT
Observations of Galactic H i gas for seven targeted regions at intermediate Galactic latitude are presented at

angular resolution using data from the DRAO Synthesis Telescope (ST) and the Green Bank Telescope (GBT). The DHIGLS data are the most extensive arcminute-resolution measurements of the diffuse atomic interstellar medium beyond those in the Galactic plane. The acquisition, reduction, calibration, and mosaicking of the DRAO ST data and the cross calibration and incorporation of the short-spacing information from the GBT are described. The high quality of the resulting DHIGLS products enables a variety of new studies in directions of low Galactic column density. We analyze the angular power spectra of maps of the integrated H i emission (column density) from the data cubes for several distinct velocity ranges. In fitting power-spectrum models based on a power law, but including the effects of the synthesized beam and noise at high spatial frequencies, we find exponents ranging from −2.5 to −3.0. Power spectra of maps of the centroid velocity for these components give similar results. These exponents are interpreted as being representative of the three-dimensional density and velocity fields of the atomic gas, respectively. We find evidence for dramatic changes in the H i structures in channel maps over even small changes in velocity. This narrow line emission has counterparts in absorption spectra against bright background radio sources, quantifying that the gas is cold and dense and can be identified as the cold neutral medium phase. Fully reduced DHIGLS H i data cubes and other data products are available at www.cita.utoronto.ca/DHIGLS.
RADIO MEASUREMENTS OF THE STELLAR PROPER MOTIONS IN THE CORE OF THE ORION NEBULA CLUSTER
Authors: Dzib Sergio A. , Loinard Laurent , Rodríguez Luis F. , Gómez Laura , Forbrich Jan , Menten Karl M. , Kounkel Marina A. , Mioduszewski Amy J. , Hartmann Lee , Tobin John J. , Rivera Juana L. 
Published: January 2017

ABSTRACT
Using multi-epoch Very Large Array observations, covering a time baseline of 29.1 years, we have measured the proper motions of 88 young stars with compact radio emission in the core of the Orion Nebula Cluster (ONC) and the neighboring BN/KL region. Our work increases the number of young stars with measured proper motion at radio frequencies by a factor of 2.5 and enables us to perform a better statistical analysis of the kinematics of the region than was previously possible. Most stars (79 out of 88) have proper motions consistent with a Gaussian distribution centered on

mas yr−1, and

mas yr−1, with velocity dispersions of

mas yr−1,

mas yr−1. We looked for organized movements of these stars but found no clear indication of radial expansion/contraction or rotation. The remaining nine stars in our sample show peculiar proper motions that differ from the mean proper motions of the ONC by more than 3σ. One of these stars, V 1326 Ori, could have been expelled from the Orion Trapezium 7000 years ago. Two could be related to the multi-stellar disintegration in the BN/KL region, in addition to the previously known sources BN, I and n. The others either have high uncertainties (so their anomalous proper motions are not firmly established) or could be foreground objects.
THE PROPER MOTIONS OF THE DOUBLE RADIO SOURCE n IN THE ORION BN/KL REGION
Authors: Rodríguez Luis F. , Dzib Sergio A. , Loinard Laurent , Zapata Luis , Gómez Laura , Menten Karl M. , Lizano Susana 
Published: January 2017

ABSTRACT
We have extended the time baseline for observations of the proper motions of radio sources in the Orion BN/KL region from 14.7 to 22.5 years. We present improved determinations for the sources BN and I. In addition, we address the proper motions of the double radio source n, that have been questioned in the literature. We confirm that all three sources are moving away at transverse velocities of tens of kilometers per second from a region in-between them, where they were located about 500 years ago. Source n exhibits a new component that we interpret as due to a one-sided ejection of free–free emitting plasma that took place after 2006.36. We used the highly accurate relative proper motions between sources BN and I to determine that their closest separation took place in the year 1475 ± 6, when they were within ∼100 au or less from each other in the plane of the sky.
THE HIGHLY IONIZED CIRCUMGALACTIC MEDIUM IS KINEMATICALLY UNIFORM AROUND GALAXIES
Authors: Nielsen Nikole M. , Kacprzak Glenn G. , Muzahid Sowgat , Churchill Christopher W. , Murphy Michael T. , Charlton Jane C. 
Published: January 2017

ABSTRACT
The circumgalactic medium (CGM) traced by O vi

doublet absorption has been found to concentrate along the projected major and minor axes of the host galaxies. This suggests that O vi traces accreting and outflowing gas, respectively, which are key components of the baryon cycle of galaxies. We investigate this further by examining the kinematics of 29 O vi absorbers associated with galaxies at

as a function of galaxy color, inclination, and azimuthal angle. Each galaxy was imaged with the Hubble Space Telescope (HST), and the absorption was detected in COS/HST spectra of nearby (

kpc) background quasars. We use the pixel-velocity two-point correlation function to characterize the velocity spread of the absorbers, which is a method used previously for a sample of Mg ii absorber–galaxy pairs. The absorption velocity spread for O vi is more extended than Mg ii, which suggests that the two ions trace differing components of the CGM. Again, in contrast to Mg ii, the O vi absorption velocity spreads are similar regardless of galaxy color, inclination, and azimuthal angle. This indicates that the kinematics of the high-ionization gas is not strongly influenced by the current star formation activity in the galaxy. The kinematic homogeneity of O vi absorption and its tendency to be observed mainly along the projected galaxy major and minor axes is likely due to varying ionization conditions and gas densities about the galaxy. Gas in intermediate azimuthal angles may be ionized out of the O vi phase, possibly resulting in an azimuthal angle dependence of the distribution of gas in higher ionization states.
THE EVOLUTION OF GAS GIANT ENTROPY DURING FORMATION BY RUNAWAY ACCRETION
Authors: Berardo David , Cumming Andrew , Marleau Gabriel-Dominique 
Published: January 2017

ABSTRACT
We calculate the evolution of gas giant planets during the runaway gas accretion phase of formation, to understand how the luminosity of young giant planets depends on the accretion conditions. We construct steady-state envelope models, and run time-dependent simulations of accreting planets with the code Modules for Experiments in Stellar Astrophysics. We show that the evolution of the internal entropy depends on the contrast between the internal adiabat and the entropy of the accreted material, parametrized by the shock temperature T
0 and pressure P
0. At low temperatures (

–

, depending on model parameters), the accreted material has a lower entropy than the interior. The convection zone extends to the surface and can drive a high luminosity, leading to rapid cooling and cold starts. For higher temperatures, the accreted material has a higher entropy than the interior, giving a radiative zone that stalls cooling. For

, the surface–interior entropy contrast cannot be accommodated by the radiative envelope, and the accreted matter accumulates with high entropy, forming a hot start. The final state of the planet depends on the shock temperature, accretion rate, and starting entropy at the onset of runaway accretion. Cold starts with

require low accretion rates and starting entropy, and the temperature of the accreting material needs to be maintained close to the nebula temperature. If instead the temperature is near the value required to radiate the accretion luminosity,

, as suggested by previous work on radiative shocks in the context of star formation, gas giant planets form in a hot start with

.
A STATISTICAL STUDY OF FLARE PRODUCTIVITY ASSOCIATED WITH SUNSPOT PROPERTIES IN DIFFERENT MAGNETIC TYPES OF ACTIVE REGIONS
Authors: Yang Ya-Hui , Hsieh Min-Shiu , Yu Hsiu-Shan , Chen P. F. 
Published: January 2017

ABSTRACT
It is often believed that intense flares preferentially originate from the large-size active regions (ARs) with strong magnetic fields and complex magnetic configurations. This work investigates the dependence of flare activity on the AR properties and clarifies the influence of AR magnetic parameters on the flare productivity, based on two data sets of daily sunspot and flare information as well as the GOES soft X-ray measurements and HMI vector magnetograms. By considering the evolution of magnetic complexity, we find that flare behaviors are quite different in the short- and long-lived complex ARs and the ARs with more complex magnetic configurations are likely to host more impulsive and intense flares. Furthermore, we investigate several magnetic quantities and perform the two-sample Kolmogorov–Smirnov test to examine the similarity/difference between two populations in different types of ARs. Our results demonstrate that the total source field strength on the photosphere has a good correlation with the flare activity in complex ARs. It is noted that intense flares tend to occur at the regions of strong source field in combination with an intermediate field-weighted shear angle. This result implies that the magnetic free energy provided by a complex AR could be high enough to trigger a flare eruption even with a moderate magnetic shear on the photosphere. We thus suggest that the magnetic free energy represented by the source field rather than the photospheric magnetic complexity is a better quantity to characterize the flare productivity of an AR, especially for the occurrence of intense flares.
THE RADIAL DISTRIBUTIONS OF THE TWO MAIN-SEQUENCE COMPONENTS IN THE YOUNG MASSIVE STAR CLUSTER NGC 1856
Authors: Li Chengyuan , de Grijs Richard , Deng Licai , Milone Antonino P. 
Published: January 2017

ABSTRACT
The recent discovery of double main sequences in the young, massive star cluster NGC 1856 has caught significant attention. The observations can be explained by invoking two stellar generations with different ages and metallicities or by a single generation of stars composed of two populations characterized by different rotation rates. We analyzed the number ratios of stars belonging to both main-sequence components in NGC 1856 as a function of radius. We found that their number ratios remain approximately unchanged from the cluster’s central region to its periphery, indicating that both components are homogeneously distributed in space. Through a comparison of the loci of the best-fitting isochrones with the ridge lines of both stellar components, we found that both multiple stellar populations and rapid stellar rotation can potentially explain the observed main-sequence bifurcation in NGC 1856. However, if NGC 1856 were a young representative of the old globular clusters, then the multiple stellar populations model would not be able to explain the observed homogeneity in the spatial distributions of these two components, since all relevant scenarios would predict that the second stellar generation should be formed in a more compact configuration than that of the first stellar generation, while NGC 1856 is too young for both stellar generations to have been fully mixed dynamically. We speculate that the rapid stellar rotation scenario would be the favored explanation of the observed multiple stellar sequences in NGC 1856.
PERIOD–COLOR AND AMPLITUDE–COLOR RELATIONS AT MAXIMUM AND MINIMUM LIGHT FOR RR LYRAE STARS IN THE SDSS STRIPE 82 REGION
Authors: Ngeow Chow-Choong , Kanbur Shashi M. , Bhardwaj Anupam , Schrecengost Zachariah , Singh Harinder P. 
Published: January 2017

ABSTRACT
Investigation of period–color (PC) and amplitude–color (AC) relations at the maximum and minimum light can be used to probe the interaction of the hydrogen ionization front (HIF) with the photosphere and the radiation hydrodynamics of the outer envelopes of Cepheids and RR Lyraes. For example, theoretical calculations indicated that such interactions would occur at minimum light for RR Lyrae and result in a flatter PC relation. In the past, the PC and AC relations have been investigated by using either the (V − R)MACHO or (V − I) colors. In this work, we extend previous work to other bands by analyzing the RR Lyraes in the Sloan Digital Sky Survey Stripe 82 Region. Multi-epoch data are available for RR Lyraes located within the footprint of the Stripe 82 Region in five (ugriz) bands. We present the PC and AC relations at maximum and minimum light in four colors: (u − g)0, (g − r)0, (r − i)0, and (i − z)0, after they are corrected for extinction. We found that the PC and AC relations for this sample of RR Lyraes show a complex nature in the form of flat, linear or quadratic relations. Furthermore, the PC relations at minimum light for fundamental mode RR Lyrae stars are separated according to the Oosterhoff type, especially in the (g − r)0 and (r − i)0 colors. If only considering the results from linear regressions, our results are quantitatively consistent with the theory of HIF-photosphere interaction for both fundamental and first overtone RR Lyraes.
PARTICLE SCATTERING OFF OF RIGHT-HANDED DISPERSIVE WAVES
Authors: Schreiner C. , Kilian P. , Spanier F. 
Published: January 2017

ABSTRACT
Resonant scattering of fast particles off low frequency plasma waves is a major process determining transport characteristics of energetic particles in the heliosphere and contributing to their acceleration. Usually, only Alfvén waves are considered for this process, although dispersive waves are also present throughout the heliosphere. We investigate resonant interaction of energetic electrons with dispersive, right-handed waves. For the interaction of particles and a single wave a variable transformation into the rest frame of the wave can be performed. Here, well-established analytic models derived in the framework of magnetostatic quasi-linear theory can be used as a reference to validate simulation results. However, this approach fails as soon as several dispersive waves are involved. Based on analytic solutions modeling the scattering amplitude in the magnetostatic limit, we present an approach to modify these equations for use in the plasma frame. Thereby we aim at a description of particle scattering in the presence of several waves. A particle-in-cell code is employed to study wave–particle scattering on a micro-physically correct level and to test the modified model equations. We investigate the interactions of electrons at different energies (from 1 keV to 1 MeV) and right-handed waves with various amplitudes. Differences between model and simulation arise in the case of high amplitudes or several waves. Analyzing the trajectories of single particles we find no microscopic diffusion in the case of a single plasma wave, although a broadening of the particle distribution can be observed.
Functional Conversion and Dominance of γδ T Subset in Mouse Experimental Autoimmune Uveitis
Authors: Liang Dongchun , Nian Hong , Shao Hui , Kaplan Henry J. , Sun Deming 
Published: January 2017

Abstract
We have previously shown that activated γδ T cells have a much stronger proinflammatory effect in the development of experimental autoimmune uveitis than their nonactivated counterparts. Our present study explored γδ T cell subsets are functionally distinct in autoimmune pathogenesis and determined the pathogenic contribution of biased Vγ4+ γδ T cell activation in this disease. By systematically comparing two major peripheral γδ T cell subsets, the Vγ1+ and the Vγ4+ cells, we found that the Vγ4+ cells were readily activated in B6 mice during experimental autoimmune uveitis development, whereas Vγ1+ cells remained nonactivated. Cytokines that were abundantly found in the serum of immunized mice activated Vγ4+, but did not activate Vγ1+, cells. The Vγ4+ cells had a strong proinflammatory activity, whereas the Vγ1+ cells remained nonactivated when tested immediately after isolation from immunized mice. However, when the Vγ1+ cells were activated in vitro, they promoted inflammation. Our results demonstrated that activation is a major factor in switching the enhancing and inhibiting effects of both Vγ1+ and Vγ4+ γδ T cell subsets, and that γδ T cell subsets differ greatly in their activation requirements. Whether the enhancing or inhibiting function of γδ T cells is dominant is mainly determined by the proportion of the γδ T cells that are activated versus the proportion not activated.
Concussion Baseline Testing: Preexisting Factors, Symptoms, and Neurocognitive Performance
Authors: Cottle Jordan E. , Hall Eric E. , Patel Kirtida , Barnes Kenneth P. , Ketcham Caroline J. 
Published: January 2017

Context:Neurocognitive test scores are often considered an important aspect of concussion management. To best use these data, clinicians must understand potential factors that may influence baseline performance on these tests.Objective:To determine preexisting factors that may influence performance on the Immediate Post-Concussion Assessment and Cognitive Test (ImPACT).Design:Cross-sectional study.Setting:Research laboratory.Patients or Other Participants:A total of 486 National Collegiate Athletic Association Division I collegiate student-athletes.Main Outcome Measure(s):To determine neurocognitive functioning and total symptom score at baseline, ImPACT was administered. Outcomes were verbal memory, visual memory, visual motor speed, reaction time, and total symptom score. A self-report demographic section at the beginning of ImPACT was used to gather information concerning previous treatment for headaches, migraines, and psychiatric conditions; diagnosis of attention-deficit/hyperactivity disorder; and exposure to previous strenuous exercise. We conducted multivariate analyses of variance to determine if the ImPACT composite and total symptom scores differed according to preexisting factors (P &lt; .0083).Results:Sex showed an effect on verbal memory (P = .001), visual motor speed (P &lt; .001), and reaction time (P = .006), with women performing better than men. A previous diagnosis of attention-deficit/hyperactivity disorder affected visual motor speed (P = .008). Previous treatment for headaches (P &lt; .001), migraines (P = .001), a psychiatric condition (P &lt; .001), or a diagnosis of attention-deficit/hyperactivity disorder (P &lt; .001) all showed effects on the total symptom score. Strenuous exercise did not affect neurocogntive performance or total symptom score.Conclusions:Based on our findings and the previous literature, we suggest that many preexisting factors influence baseline neurocognitive data. Baseline testing is an important aspect of concussion management. Sports medicine professionals should be cognizant of these factors when developing concussion-management protocols.
Prosthetic Management of Total Glossectomy Patients
Authors: Yarramaneni Varun , Balakrishnan Dhanasekar , Aparna IN , Kapoor Saumya 
Published: January 2017

ABSTRACT

Background
Total glossectomy impairs various functions of tongue, such as mastication, speech, swallowing, and also results in psychological breach for the patient during social activities. In a glossectomy patient, the new size of the oral cavity often produces a change in the resonance associated with certain sounds. Also, due to the decrease in size and function of the tongue, interruption occurs in articulation patterns between the tongue, the hard and soft palate, and the teeth.

Materials and methods
We performed a review with a bibliographic search in Scopus, Web of Science along with the PubMed/Medline, Google scholar and internet. We included the articles with major contribution toward management of total glossectomy, excluded articles and works about surgical treatments in anatomical locations other than the oral cavity.

Conclusion
To obtain maximum rehabilitation for these patients, the dentist must have a thorough knowledge of the physiologic processes involved in oral functions. The present article is an overview of various objectives and design concepts for rehabilitation of a total glossectomized patient.

How to cite this article
Yarramaneni V, Balakrishnan D, Aparna IN, Kapoor S. Prosthetic Management of Total Glossectomy Patients. Int J Prosthodont Restor Dent 2016;6(3):66-68.