bluuebunny/crossref_metadata_2025_split huggingface dataset:
Numerical Analysis of Historic Structural Elements Using 3D Point Cloud Data
Authors: Almac Umut , Pekmezci Isıl Polat , Ahunbay Metin 
Published: June 2016

The 3D laser scanner has become a common instrument in numerous field applications such as structural health monitoring, assessment and documentation of structural damages, volume and dimension control of excavations, geometrical recording of built environment, and construction progress monitoring in different fields. It enables capture of millions of points from the surface of objects with high accuracy and in a very short time. These points can be employed to extrapolate the shape of the elements. In this way, the collected data can be developed to construct three-dimensional digital models that can be used in structural FEM analysis.
This paper presents structural evaluation of a historic building through FE models with the help of a 3D point cloud. The main focus of the study is on the stone columns of a historic cistern. These deteriorated load bearing elements have severe non-uniform erosion, which leads to formation of significant stress concentrations. At this point, the 3D geometric data becomes crucial in revealing the stress distribution of severely eroded columns due to material deterioration.
According to the results of static analysis using real geometry, maximum stress in compression increased remarkably on the columns in comparison with the geometrically idealized models. These values seem to approach the compressive strength of the material, which was obtained from the point load test results. Moreover, the stress distribution of the analysis draws attention to the section between columns and their capitals. According to the detailed 3D documentation, there is a reduced contact surface between columns and capitals to transfer loads.
Seismic Design of Box-Type Unreinforced Masonry Buildings Through Direct Displacement-Based Approach
Authors: Parisi Fulvio 
Published: June 2016

In the last decade, displacement-based seismic design procedures have been recognised to be effective alternatives to force-based design (FBD) methods. Indeed, displacement based design (DBD) may allow the structural engineer to get more realistic predictions of local and global deformations of the structure, and hence damage, under design earthquakes. This facilitates the achievement of performance objectives and loss mitigation in the lifetime of the structure. Nonetheless, DBD needs further investigation for some structural types such as masonry buildings.
In this paper, a direct displacement based design (DDBD) procedure for unreinforced masonry (URM) buildings is presented and critically compared to FBD. The procedure is proposed for box-type URM buildings with reinforced concrete slabs, bond beams and lintels above openings, which have shown acceptable seismic performance in severe earthquakes preventing out-of-plane failure modes. Seismic design of a three storey brick masonry building in a high seismicity region is discussed as a case study. The effects of ordinary and near-field design earthquakes, as well as load combinations and accidental eccentricity prescribed by current codes, were investigated. Finally, design solutions provided by FBD and DDBD were optimised and their construction costs were estimated. It was found that, particularly at small epicentral distances, neglecting the combination of horizontal seismic actions and accidental eccentricity may induce significant underestimation and an ideally more uniform distribution of strength demands on URM walls. In addition, construction costs resulting from DDBD may be significantly lower than those related to code based FBD procedures.
Static Analysis of Cross Vaults: The Case of the Cathedral of Casertavecchia
Authors: Contestabile M. , Babilio E. , Fortunato A. , Guerriero L. , Lippiello M. , Pasquino M. , Angelillo M. 
Published: June 2016

In the present paper, on assuming that the material has infinite friction and no cohesion,i.e. it is No-Tension in the sense of Heyman, we study the equilibrium of cross vaults of unequal rise, such as those of some Romanesque and Gothic churches. In particular the case study of the lateral cross vaults of the Cathedral of the old town of Caserta is analyzed. The scope of the paper is not to study in detail and quantitatively any particular vault, rather we give a compressive equilibrium solution (compatible with the unilateral material assumption) for the general case of cross vaults, constructed on arches of unequal rise, and loaded by a uniform load.For the purpose of the structural analysis, the vault is modelled as a thin shell made of Rigid No-Tension material. The webs of the vault that we consider, are supported on two crossing ribs. To obtain the axial force inside the ribs, equilibrated and singular stress fields (that is stress fields concentrated on curves and balanced with the loads) are constructed.An estimate of the thrust forces transmitted by the vault to the peripheral arches and walls is also obtained, so that the stability of these structures can be checked.
Multi Organ Dysfunction in Term Neonates with Perinatal Asphyxia
Authors: Vemuri Aditya , Lalwani Sanjay 
Published: June 2016

Introduction: Multiorgan dysfunction (MOD) is one of the four consensus based criteria for the diagnosis of intrapartum asphyxia. The theoretical concept behind MOD is the diving reflex -conservation of blood flow to vital organs at the cost of non-vital organs. The objective of this study was to assess the patterns of involvement of each major organ/system in term asphyxiated neonates.Material and Methods: This was a hospital based prospective study. Sixty term neonates who had suffered perinatal asphyxia were assessed for central nervous system, kidney, cardiovascular system, gastrointestinal system and liver dysfunction. Results: Out of 60 eligible neonates, 57 (95%) had evidence of at least one organ dysfunction. Cardiovascular system involvement (95%) was most common, followed by renal system (37%), hepatic system (22%), central nervous system and hematological system (20% each) and finally, gastrointestinal tract (8%).Conclusion: MOD is frequently associated with perinatal asphyxia with cardiovascular system being the most commonly affected.J Nepal Paediatr Soc 2015;35(3):307-311.
Effects of <i>Alchemilla mollis</i> and <i>Alchemilla persica</i> on the wound healing process
Authors: Ergene Öz Burçin , Ilhan Mert , Ozbilgin Serkan , Küpeli Akkol Esra , Bahadır Acıkara Özlem , Saltan Gülçin , Keleş Hikmet , Süntar Ipek 
Published: June 2016

<p class="Abstract"><em>Alchemilla mollis</em>, is used in traditional medicine for the treatment of wounds and excessive menstruation. Aqueous methanol extracts of<em> A. mollis</em> and <em>A. persica</em> were evaluated for wound healing acivity by using linear incision and circular excision wound models along with hydroxyproline estimation and histopathological analysis. Anti-inflammatory effect was determined according to Whittle method. The extracts prepared from the aerial parts of <em>A. mollis</em> and <em>A. persica</em> exerted significant wound healing activity with the tensile strength values of 39.3% and 33.3%, respectively, and with the contraction values of 51.4% and 43.5%, respectively. Hydroxyproline estimation and histopathological analysis also confirmed the results. The extracts of <em>A. mollis</em> and <em>A. persica</em> showed significant anti-inflammatory activity with the values of 30.6% and 26.6% respectively. These results showed that <em>A. mollis</em> and <em>A. persica</em> possess significant wound healing and anti-inflammatory activities.</p><p class="Abstract"><strong>Video Clip</strong></p><p class="Subheading"><a href="https://youtube.com/v/k2Hz7f1e4SI">Circular excision wound model</a>: 2 min</p><p> </p>
Extraction, isolation and purification of exopolysaccharide from lactic acid bacteria using ethanol precipitation method
Authors: Bajpai Vivek K. , Majumder Rajib , Rather Irfan A. , Kim Kangmin 
Published: June 2016

<p>Lactic acid bacteria are classified ‘Generally Recognized As Safe’ (GRAS) with most effective potential to divert significant amount of fermentable sugars towards the biosynthesis of functional exopolysaccharide. Exopolysaccharides from lactic acid bacteria are receiving a renewed interest due to the claims of human health benefits, such as modulation of immune response system and more importantly in food and pharma industries as a texturizer, viscosifer, emulsifier and syneresis-lowering agent. Its purification methodology involves: a) Extraction of cell-free supernatant from lactic acid bacteria; b) Denature of protein using trichloroacetic acid; c) Ethanol precipitation; d) Dialysis; and e) Freeze drying. However, depending on nature of research, compounds can be further purified using scanning electron microscopy (SEM), infrared spectrum (IR); and nuclear magnetic resonance (NMR) spectral analyses.</p><p><strong>Video Clips</strong></p><p><a href="https://www.youtube.com/v/PGDyHPEk5jY">Part 1</a>: 7 min 42 sec</p><p><a href="https://youtube.com/v/G8ZMZ4z1DMs">Part 2</a>: 3 min 36 sec</p>
STELLAR VARIABILITY AND FLARE RATES FROM DOME A, ANTARCTICA, USING 2009 AND 2010 CSTAR OBSERVATIONS
Authors: Oelkers Ryan J. , Macri Lucas M. , Wang Lifan , Ashley Michael C. B. , Cui Xiangqun , Feng Long-Long , Gong Xuefei , Lawrence Jon S. , Qiang Liu , Luong-Van Daniel , Pennypacker Carl R. , Yuan Xiangyan , York Donald G. , Zhou Xu , Zhu Zhenxi 
Published: June 2016

ABSTRACT
The Chinese Small Telescope Array (CSTAR) carried out high-cadence time-series observations of ∼20.1 square degrees centered on the South Celestial Pole during the 2008, 2009, and 2010 winter seasons from Dome A in Antarctica. The nearly continuous six months of dark conditions during each observing season allowed for

>

10

6

images to be collected through gri and clear filters, resulting in the detection of

>

10

4

sources over the course of three years of operation. The nearly space-like conditions in the Antarctic plateau are an ideal testbed for the suitability of very small-aperture (

<
20

cm) telescopes to detect transient events, variable stars, and stellar flares. We present the results of a robust search for such objects using difference image analysis of the data obtained during the 2009 and 2010 winter seasons. While no transients were found, we detected 29 flaring events and find a normalized flaring rate of 5 ± 4 × 10−7 flare hr−1 for late-K dwarfs, 1 ± 1 × 10−6 flare hr−1 for M dwarfs and 7 ± 1 × 10−7 flare hr−1 for all other stars in our sample. We suggest future small-aperture telescopes planned for deployment at Dome A would benefit from a tracking mechanism, to help alleviate effects from ghosting, and a finer pixel scale, to increase the telescope's sensitivity to faint objects. We find that the light curves of non-transient sources have excellent photometric qualities once corrected for systematics, and are limited only by photon noise and atmospheric scintillation.
THE ARAUCARIA PROJECT: ON THE TIP OF THE RED GIANT BRANCH DISTANCE DETERMINATION TO THE MAGELLANIC CLOUDS
Authors: Górski Marek , Pietrzyński Grzegorz , Gieren Wolfgang , Catelan Márcio , Pilecki Bogumił , Karczmarek Paulina , Suchomska Ksenia , Graczyk Dariusz , Konorski Piotr , Zgirski Bartłomiej , Wielgórski Piotr 
Published: June 2016

ABSTRACT
We present a precise optical and near-infrared determination of the tip of the red giant branch (TRGB) brightness in the Large and Small Magellanic Clouds (respectively, LMC and SMC). The commonly used calibrations of the absolute magnitude of the TRGB lead to an overestimation of the distance to the LMC and SMC in the K band, and an underestimation of the distance in the optical I band for both galaxies. Reported discrepancies are at the level of 0.2 mag, with respect to the very accurate distance determinations to both MCs based on late-type eclipsing binaries. The differential distances between the LMC and SMC obtained in the J and K bands, and for the bolometric brightness are consistent with each other, and with the results obtained from eclipsing binaries and other distance indicators.
TWO HOT JUPITERS FROM K2 CAMPAIGN 4
Authors: Johnson Marshall C. , Gandolfi Davide , Fridlund Malcolm , Csizmadia Szilard , Endl Michael , Cabrera Juan , Cochran William D. , Deeg Hans J. , Grziwa Sascha , Ramírez Ivan , Hatzes Artie P. , Eigmüller Philipp , Barragán Oscar , Erikson Anders , Guenther Eike W. , Korth Judith , Kuutma Teet , Nespral David , Pätzold Martin , Palle Enric , Prieto-Arranz Jorge , Rauer Heike , Saario Joonas 
Published: June 2016

ABSTRACT
We confirm the planetary nature of two transiting hot Jupiters discovered by the Kepler spacecraft’s K2 extended mission in its Campaign 4, using precise radial velocity measurements from FIES@NOT, HARPS-N@TNG, and the coudé spectrograph on the McDonald Observatory 2.7 m telescope. K2-29 b (EPIC 211089792b) transits a K1V star with a period of 3.2589263 ± 0.0000015 days; its orbit is slightly eccentric (

e
=

0.084

−
0.023

+
0.032

). It has a radius of

R

P

=

1.000

−
0.067

+
0.071

R
J and a mass of

M

P

=

0.613

−
0.026

+
0.027

M
J. Its host star exhibits significant rotational variability, and we measure a rotation period of

P

rot

=
10.777
±
0.031

days. K2-30 b (EPIC 210957318 b) transits a G6V star with a period of 4.098503 ± 0.000011 days. It has a radius of

R

P

=

1.039

−
0.051

+
0.050

R
J and a mass of

M

P

=

0.579

−
0.027

+
0.028

M
J. The star has a low metallicity for a hot Jupiter host,

[
Fe

/

H
]
=
−
0.15
±
0.05

.
LATE POP III STAR FORMATION DURING THE EPOCH OF REIONIZATION: RESULTS FROM THE RENAISSANCE SIMULATIONS
Authors: Xu Hao , Norman Michael L. , O’Shea Brian W. , Wise John H. 
Published: June 2016

ABSTRACT
We present results on the formation of Population III (Pop III) stars at redshift 7.6 from the Renaissance Simulations, a suite of extremely high-resolution and physics-rich radiation transport hydrodynamics cosmological adaptive-mesh refinement simulations of high-redshift galaxy formation performed on the Blue Waters supercomputer. In a survey volume of about 220 comoving Mpc3, we found 14 Pop III galaxies with recent star formation. The surprisingly late formation of Pop III stars is possible due to two factors: (i) the metal enrichment process is local and slow, leaving plenty of pristine gas to exist in the vast volume; and (ii) strong Lyman–Werner radiation from vigorous metal-enriched star formation in early galaxies suppresses Pop III formation in (“not so”) small primordial halos with mass less than ∼3 × 107
M
⊙. We quantify the properties of these Pop III galaxies and their Pop III star formation environments. We look for analogs to the recently discovered luminous Ly α emitter CR7, which has been interpreted as a Pop III star cluster within or near a metal-enriched star-forming galaxy. We find and discuss a system similar to this in some respects, however, the Pop III star cluster is far less massive and luminous than CR7 is inferred to be.
ROTATING STARS AND THE FORMATION OF BIPOLAR PLANETARY NEBULAE. II. TIDAL SPIN-UP
Authors: García-Segura G. , Villaver E. , Manchado A. , N. Langer  , Yoon S.-C. 
Published: June 2016

ABSTRACT
We present new binary stellar evolution models that include the effects of tidal forces, rotation, and magnetic torques with the goal of testing planetary nebulae (PNs) shaping via binary interaction. We explore whether tidal interaction with a companion can spin-up the asymptotic giant brach (AGB) envelope. To do so, we have selected binary systems with main-sequence masses of 2.5 M
⊙ and 0.8 M
⊙ and evolve them allowing initial separations of 5, 6, 7, and 8 au. The binary stellar evolution models have been computed all the way to the PNs formation phase or until Roche lobe overflow (RLOF) is reached, whatever happens first. We show that with initial separations of 7 and 8 au, the binary avoids entering into RLOF, and the AGB star reaches moderate rotational velocities at the surface (∼3.5 and ∼2 km s−1, respectively) during the inter-pulse phases, but after the thermal pulses it drops to a final rotational velocity of only ∼0.03 km s−1. For the closest binary separations explored, 5 and 6 au, the AGB star reaches rotational velocities of ∼6 and ∼4 km s−1, respectively, when the RLOF is initiated. We conclude that the detached binary models that avoid entering the RLOF phase during the AGB will not shape bipolar PNs, since the acquired angular momentum is lost via the wind during the last two thermal pulses. This study rules out tidal spin-up in non-contact binaries as a sufficient condition to form bipolar PNs.
z ≳ 7 GALAXIES WITH RED SPITZER/IRAC [3.6]–[4.5] COLORS IN THE FULL CANDELS DATA SET: THE BRIGHTEST-KNOWN GALAXIES AT z ∼ 7–9 AND A PROBABLE SPECTROSCOPIC CONFIRMATION AT z = 7.48
Authors: Roberts-Borsani G. W. , Bouwens R. J. , Oesch P. A. , Labbe I. , Smit R. , Illingworth G. D. , Dokkum P. van , Holden B. , Gonzalez V. , Stefanon M. , Holwerda B. , Wilkins S. 
Published: June 2016

ABSTRACT
We identify four unusually bright (H

< 25.5) galaxies from Hubble Space Telescope (HST) and Spitzer CANDELS data with probable redshifts z ∼ 7–9. These identifications include the brightest-known galaxies to date at z ≳ 7.5. As Y-band observations are not available over the full CANDELS program to perform a standard Lyman-break selection of z > 7 galaxies, we employ an alternate strategy using deep Spitzer/IRAC data. We identify z ∼ 7.1–9.1 galaxies by selecting z ≳ 6 galaxies from the HST CANDELS data that show quite red IRAC [3.6]−[4.5] colors, indicating strong [O iii]+Hβ lines in the 4.5 μm band. This selection strategy was validated using a modest sample for which we have deep Y-band coverage, and subsequently used to select the brightest z ≥ 7 sources. Applying the IRAC criteria to all HST-selected optical dropout galaxies over the full ∼900 arcmin2 of the CANDELS survey revealed four unusually bright z ∼ 7.1, 7.6, 7.9, and 8.6 candidates. The median [3.6]−[4.5] color of our selected z ∼ 7.1–9.1 sample is consistent with rest-frame [O iii]+Hβ EWs of ∼1500 Å in the [4.5] band. Keck/MOSFIRE spectroscopy has been independently reported for two of our selected sources, showing Lyα at redshifts of 7.7302 ± 0.0006 and

, respectively. We present similar Keck/MOSFIRE spectroscopy for a third selected galaxy with a probable 4.7σ Lyα line at z
spec = 7.4770 ± 0.0008. All three have H160-band magnitudes of ∼25 mag and are ∼0.5 mag more luminous (M
1600 ∼ −22.0) than any previously discovered z ∼ 8 galaxy, with important implications for the UV luminosity function (LF). Our three brightest and highest redshift z > 7 galaxies all lie within the CANDELS-EGS field, providing a dramatic illustration of the potential impact of field-to-field variance.
SEARCHING FOR THE HR 8799 DEBRIS DISK WITH HST/STIS
Authors: Gerard B. , Lawler S. , Marois C. , Tannock M. , Matthews B. , Venn K. 
Published: June 2016

ABSTRACT
We present a new algorithm for space telescope high contrast imaging of close-to-face-on planetary disks called Optimized Spatially Filtered (OSFi) normalization. This algorithm is used on HR 8799 Hubble Space Telescope (HST) Space Telescope Imaging Spectrograph (STIS) coronagraphic archival data, showing an over-luminosity after reference star point-spread function (PSF) subtraction that may be from the inner disk and/or planetesimal belt components of this system. The PSF-subtracted radial profiles in two separate epochs from 2011 and 2012 are consistent with one another, and self-subtraction shows no residual in both epochs. We explore a number of possible false-positive scenarios that could explain this residual flux, including telescope breathing, spectral differences between HR 8799 and the reference star, imaging of the known warm inner disk component, OSFi algorithm throughput and consistency with the standard spider normalization HST PSF subtraction technique, and coronagraph misalignment from pointing accuracy. In comparison to another similar STIS data set, we find that the over-luminosity is likely a result of telescope breathing and spectral difference between HR 8799 and the reference star. Thus, assuming a non-detection, we derive upper limits on the HR 8799 dust belt mass in small grains. In this scenario, we find that the flux of these micron-sized dust grains leaving the system due to radiation pressure is small enough to be consistent with measurements of other debris disk halos.
THE ABSOLUTE RATE OF LGRB FORMATION
Authors: Graham J. F. , Schady P. 
Published: June 2016

ABSTRACT
We estimate the long-duration gamma-ray burst (LGRB) progenitor rate using our recent work on the effects of environmental metallically on LGRB formation in concert with supernovae (SNe) statistics via an approach patterned loosely off the Drake equation. Beginning with the cosmic star formation history, we consider the expected number of broad-line Type Ic events (the SNe type associated with LGRBs) that are in low-metallicity host environments adjusted by the contribution of high-metallicity host environments at a much reduced rate. We then compare this estimate to the observed LGRB rate corrected for instrumental selection effects to provide a combined estimate of the efficiency fraction of these progenitors to produce LGRBs and the fraction of which are beamed in our direction. From this we estimate that an aligned LGRB occurs for approximately every 4000 ± 2000 low-metallically broad-lined SNe Ic. Therefore, if one assumes a semi-nominal beaming factor of 100, then only about one such supernova out of 40 produce an LGRB. Finally, we propose an off-axis LGRB search strategy of targeting only broad-line Type Ic events that occur in low-metallicity hosts for radio observation.
MIGRATION AND GROWTH OF PROTOPLANETARY EMBRYOS. III. MASS AND METALLICITY DEPENDENCE FOR FGKM MAIN-SEQUENCE STARS
Authors: Liu Beibei , Zhang Xiaojia , Lin Douglas N. C. 
Published: June 2016

ABSTRACT
Radial velocity and transit surveys have found that the fraction of FGKM stars with close-in super-Earth(s) (η
⊕) is around 30%–50%, independent of the stellar mass M
* and metallicity Z
*. In contrast, the fraction of solar-type stars harboring one or more gas giants (η
J) with masses M
p > 100 M
⊕ is nearly 10%–15%, and it appears to increase with both M
* and Z
*. Regardless of the properties of their host stars, the total mass of some multiple super-Earths systems exceeds the core mass of Jupiter and Saturn. We suggest that both super-Earths and supercritical cores of gas giants were assembled from a population of embryos that underwent convergent type I migration from their birthplaces to a transition location between viscously heated and irradiation-heated disk regions. We attribute the cause for the η
⊕–η
J dichotomy to conditions required for embryos to merge and to acquire supercritical core mass (

) for the onset of efficient gaseous envelope accretion. We translate this condition into a critical disk accretion rate, and our analysis and simulation results show that it weakly depends on M
* and decreases with metallicity of disk gas Z
d. We find that embryos are more likely to merge into supercritical cores around relatively massive and metal-rich stars. This dependence accounts for the observed η
J–M
*. We also consider the

dispersed relationship and reproduce the observed η
J–Z
* correlation.