bluuebunny/crossref_metadata_2025_split huggingface dataset:
Feasibility of a Natural Surfactant as a Stabilizer for Cosmetics with Liposome-Encapsulated Plant Stem Cells: Pre-Formulation and Formulation Through Stability Studies
Authors: Filipović Mila , Lukić Milica , Krstonošić Veljko , Đorđević Sanela , Pantelić Ivana , Gledović Ana , Vuleta Gordana , Savić Snežana 
Published: May 2016

Abstract
During the formulation of liposome-containing products different problems can occur and the selection of a suitable carrier remains the greatest challenge. To estimate feasibility of a novel alkyl polyglucoside surfactant (hydroxystearyl alcohol and hydroxystearyl glucoside) as an emulsifier for cosmetics with liposome-encapsulated plant stem cells, we performed a two-phase study. In the first, the pre-formulation phase, the emulsifier's critical micelle concentration (CMC) and liposome-encapsulated active-emulsifier interactions were determined. The second phase was carried out to develop and characterize a cosmetic emulsion suitable to serve as a carrier for liposomes. The investigated emulsifier, with the obtained CMC value of 0.0085 wt.%, could be classified as liposome-friendly and can be used to develop stable and aesthetically acceptable cosmetics or even prospective pharmaceutical liposome-containing emulsions.
Transition from Micelle to Vesicle of a Novel Sugar-Based Surfactant Containing Trisiloxane
Authors: Zhou Xiyang , Zhang Dianlong 
Published: May 2016

Abstract
Vesicles form spontaneously in aqueous solution of a novel sugar-based surfactant containing trisiloxane [Si(3)N-GHA]. The transition was monitored among the monomer, micelle and vesicle through the variation of surface tension, accompanied by surface tension measurements. The vesicles of a trisiloxane containing sugar-based surfactant have been characterized by dynamic light scattering (DLS) and negative-stained transmission electron microscopy (TEM). The vesicle aggregation can be explained by the critical packing parameter derived from an analysis of chemical structure.
Wrought aluminium–magnesium alloys subjected to SPD processing
Authors: Snopiński Przemysław , Tański Tomasz , Labisz Krzysztof , Rusz Stanislav , Jonsta Petr , Król Mariusz 
Published: May 2016

Abstract
The article presents the influence of stationary plastic deformation, using the equal channel angular pressing (ECAP) method, on the structure and properties of an aluminium alloy with 3 % magnesium content. In order to investigate changes in the structure and substructure, light microscopy and transmission electron microscopy were used. The influence of plastic deformation was determined by hardness measurement using the Vickers method. The results of the investigation show that, even after one ECAP, it is possible to decrease grain size to a range of 30 – 70 nm, and increase the mechanical properties by nearly 90 %. It was also found that the additional twist angle of the die has a minor effect on the properties and structure of the investigated alloy.
Friction and wear of diamond-like carbon film deposited on CoCrMo alloy under different lubrication
Authors: Luo Yong , Yang Ting , Liu Qiuzhen 
Published: May 2016

Abstract
CoCrMo alloys are widely used as artificial joint implants due to their excellent mechanical properties, good wear resistance and outstanding corrosion resistance. However, the risks of release of cobalt and chromium ions urge researchers to improve the wear resistance of implants further by using surface modification technology. Diamond-like carbon film with 3.0 μm thickness was deposited on the surface of CoCrMo alloy using ion-source-assisted magnetron sputtering. The friction coefficients of the CoCrMo alloy decreased remarkably under different conditions after the formation of diamond-like carbon film. After the deposition of diamond-like carbon film the wear rates of the CoCrMo alloy decreased by 52.4 %, 47.1 % and 49.4 %, under dry friction, physiological saline, and bovine serum lubrication, respectively.
A COHERENT STUDY OF EMISSION LINES FROM BROADBAND PHOTOMETRY: SPECIFIC STAR FORMATION RATES AND [O iii]/Hβ RATIO AT 3 < z < 6
Authors: Faisst A. L. , Capak P. , Hsieh B. C. , Laigle C. , Salvato M. , Tasca L. , Cassata P. , Davidzon I. , Ilbert O. , Le Fèvre O. , Masters D. , McCracken H. J. , Steinhardt C. , Silverman J. D. , de Barros S. , Hasinger G. , Scoville N. Z. 
Published: May 2016

ABSTRACT
We measure the Hα and [O iii] emission line properties as well as specific star formation rates (sSFRs) of spectroscopically confirmed 3 < z < 6 galaxies in COSMOS from their observed colors versus redshift evolution. Our model describes consistently the ensemble of galaxies including intrinsic properties (age, metallicity, star formation history), dust attenuation, and optical emission lines. We forward-model the measured Hα equivalent widths (EW) to obtain the sSFR out to z ∼ 6 without stellar mass fitting. We find a strongly increasing rest-frame Hα EW that is flattening off above z ∼ 2.5 with average EWs of 300–600 Å at z ∼ 6. The sSFR is increasing proportionally to

(
1
+
z
)

2.4

at z < 2.2 and to

(
1
+
z
)

1.5

at higher redshifts, indicative of a fast build-up of mass in high-z galaxies within e-folding times of 100–200 Myr at z ∼ 6. The redshift evolution at z > 3 cannot be fully explained in a picture of growth driven by cold accretion. We find a progressively increasing [O iii]λ5007/Hβ ratio out to z ∼ 6, consistent with the ratios in local galaxies selected by increasing Hα EW (i.e., sSFR). This demonstrates the potential of using “local high-z analogs” to investigate the spectroscopic properties and relations of galaxies in the re-ionization epoch.
THE DISTANCE DUALITY RELATION FROM STRONG GRAVITATIONAL LENSING
Authors: Liao Kai , Li Zhengxiang , Cao Shuo , Biesiada Marek , Zheng Xiaogang , Zhu Zong-Hong 
Published: May 2016

ABSTRACT
Under very general assumptions of the metric theory of spacetime, photons traveling along null geodesics and photon number conservation, two observable concepts of cosmic distance, i.e., the angular diameter and the luminosity distances are related to each other by the so-called distance duality relation (DDR)

. Observational validation of this relation is quite important because any evidence of its violation could be a signal of new physics. In this paper we introduce a new method to test the DDR based on strong gravitational lensing systems and type Ia supernovae (SNe Ia) under a flat universe. The method itself is worth attention because unlike previously proposed techniques, it does not depend on all other prior assumptions concerning the details of cosmological model. We tested it using a new compilation of strong lensing (SL) systems and JLA compilation of SNe Ia and found no evidence of DDR violation. For completeness, we also combined it with previous cluster data and showed its power on constraining the DDR. It could become a promising new probe in the future in light of forthcoming massive SL surveys and because of expected advances in galaxy cluster modeling.
REFLECTED LIGHT CURVES, SPHERICAL AND BOND ALBEDOS OF JUPITER- AND SATURN-LIKE EXOPLANETS*
Authors: Dyudina Ulyana , Zhang Xi , Li Liming , Kopparla Pushkar , Ingersoll Andrew P. , Dones Luke , Verbiscer Anne , Yung Yuk L. 
Published: May 2016

ABSTRACT
Reflected light curves observed for exoplanets indicate that a few of them host bright clouds. We estimate how the light curve and total stellar heating of a planet depends on forward and backward scattering in the clouds based on Pioneer and Cassini spacecraft images of Jupiter and Saturn. We fit analytical functions to the local reflected brightnesses of Jupiter and Saturn depending on the planet’s phase. These observations cover broadbands at 0.59–0.72 and 0.39–0.5 μm, and narrowbands at 0.938 (atmospheric window), 0.889 (CH4 absorption band), and 0.24–0.28 μm. We simulate the images of the planets with a ray-tracing model, and disk-integrate them to produce the full-orbit light curves. For Jupiter, we also fit the modeled light curves to the observed full-disk brightness. We derive spherical albedos for Jupiter and Saturn, and for planets with Lambertian and Rayleigh-scattering atmospheres. Jupiter-like atmospheres can produce light curves that are a factor of two fainter at half-phase than the Lambertian planet, given the same geometric albedo at transit. The spherical albedo is typically lower than for a Lambertian planet by up to a factor of ∼1.5. The Lambertian assumption will underestimate the absorption of the stellar light and the equilibrium temperature of the planetary atmosphere. We also compare our light curves with the light curves of solid bodies: the moons Enceladus and Callisto. Their strong backscattering peak within a few degrees of opposition (secondary eclipse) can lead to an even stronger underestimate of the stellar heating.
ON THE ABSENCE OF EUV EMISSION FROM COMET C/2012 S1 (ISON)
Authors: Bryans Paul , Pesnell W. Dean 
Published: May 2016

ABSTRACT
When the sungrazing comet C/2012 S1 (ISON) made its perihelion passage within two solar radii of the Sun’s surface, it was expected to be a bright emitter at extreme ultraviolet (EUV) wavelengths. However, despite solar EUV telescopes repointing to track the orbit of the comet, no emission was detected. This “null result” is interesting in its own right, offering the possibility of placing limits on the size and composition of the nucleus. We explain the lack of detection by considering the properties of the comet and the solar atmosphere that determine the intensity of EUV emission from sungrazing comets. By comparing these properties with those of sungrazing comet C/2011 W3 (Lovejoy), which did emit in the EUV, we conclude that the primary factor resulting in non-detectable EUV emission from C/2012 S1 (ISON) was an insufficiently large nucleus. We conclude that the radius of C/2012 S1 (ISON) was at least a factor of four less than that of C/2011 W3 (Lovejoy). This is consistent with white-light observations in the days before perihelion that suggested the comet was dramatically reducing in size on approach.
THE INTERMEDIATE-MASS STAR-FORMING REGION LYNDS 1340. AN OPTICAL VIEW
Authors: Kun Mária , Moór Attila , Szegedi-Elek Elza , Reipurth Bo 
Published: May 2016

ABSTRACT
We have performed an optical spectroscopic and photometric search for young stellar objects associated with the molecular cloud Lynds 1340, and examined the structure of the cloud by constructing an extinction map, based on SDSS data. The new extinction map suggests a shallow, strongly fragmented cloud, having a mass of some 3700 M
☉. Longslit spectroscopic observations of the brightest stars over the area of L1340 revealed that the most massive star associated with L1340 is a B4-type, ∼5 M
☉ star. The new spectroscopic and photometric data of the intermediate-mass members led to a revised distance of

pc, and revealed seven members of the young stellar population with M ≳ 2 M
☉. Our search for Hα emission line stars, conducted with the Wide Field Grism Spectrograph 2 on the 2.2 m telescope of the University of Hawaii and covering a 30′ × 40′ area, resulted in the detection of 75 candidate low-mass pre-main sequence stars, 58 of which are new. We constructed spectral energy distributions (SEDs) of our target stars, based on SDSS, 2MASS, Spitzer, and WISE photometric data, derived their spectral types, extinctions, and luminosities from BVRIJ fluxes, estimated masses by means of pre-main sequence evolutionary models, and examined the disk properties utilizing the 2–24 μm interval of the SED. We measured the equivalent width of the Hα lines and derived accretion rates. The optically selected sample of pre-main sequence stars has a median effective temperature of 3970 K, a stellar mass of 0.7 M
☉, and an accretion rate of 7.6 × 10−9
M
☉ yr−1.
WHY ARE RAPIDLY ROTATING M DWARFS IN THE PLEIADES SO (INFRA)RED? NEW PERIOD MEASUREMENTS CONFIRM ROTATION-DEPENDENT COLOR OFFSETS FROM THE CLUSTER SEQUENCE
Authors: Covey Kevin R. , Agüeros Marcel A. , Law Nicholas M. , Liu Jiyu , Ahmadi Aida , Laher Russ , Levitan David , Sesar Branimir , Surace Jason 
Published: May 2016

ABSTRACT
Stellar rotation periods (P
rot) measured in open clusters have proved to be extremely useful for studying stars’ angular momentum content and rotationally driven magnetic activity, which are both age- and mass-dependent processes. While P
rot measurements have been obtained for hundreds of solar-mass members of the Pleiades, measurements exist for only a few low-mass (<0.5 M
⊙) members of this key laboratory for stellar evolution theory. To fill this gap, we report P
rot for 132 low-mass Pleiades members (including nearly 100 with M ≤ 0.45 M
⊙), measured from photometric monitoring of the cluster conducted by the Palomar Transient Factory in late 2011 and early 2012. These periods extend the portrait of stellar rotation at 125 Myr to the lowest-mass stars and re-establish the Pleiades as a key benchmark for models of the transport and evolution of stellar angular momentum. Combining our new P
rot with precise BVIJHK photometry reported by Stauffer et al. and Kamai et al., we investigate known anomalies in the photometric properties of K and M Pleiades members. We confirm the correlation detected by Kamai et al. between a star's P
rot and position relative to the main sequence in the cluster's color–magnitude diagram. We find that rapid rotators have redder (V − K) colors than slower rotators at the same V, indicating that rapid and slow rotators have different binary frequencies and/or photospheric properties. We find no difference in the photometric amplitudes of rapid and slow rotators, indicating that asymmetries in the longitudinal distribution of starspots do not scale grossly with rotation rate.
INSTABILITY OF NON-UNIFORM TOROIDAL MAGNETIC FIELDS IN ACCRETION DISKS
Authors: Hirabayashi Kota , Hoshino Masahiro 
Published: May 2016

ABSTRACT
We present a new type of instability that is expected to drive magnetohydrodynamic (MHD) turbulence from a purely toroidal magnetic field in an accretion disk. It is already known that in a differentially rotating system, the uniform toroidal magnetic field is unstable due to magnetorotational instability (MRI) under a non-axisymmetric and vertical perturbation, while it is stable under a purely vertical perturbation. Contrary to the previous study, this paper proposes an unstable mode completely confined to the equatorial plane, driven by the expansive nature of the magnetic pressure gradient force under a non-uniform toroidal field. The basic nature of this growing eigenmode, which we name “magneto-gradient driven instability,” is studied using linear analysis, and the corresponding nonlinear evolution is then investigated using two-dimensional ideal MHD simulations. Although a single localized magnetic field channel alone cannot provide sufficient Maxwell stress to contribute significantly to the angular momentum transport, we find that the mode coupling between neighboring toroidal fields under multiple localized magnetic field channels drastically generates a highly turbulent state and leads to the enhanced transport of angular momentum, which is comparable to the efficiency seen in previous studies on MRIs. This horizontally confined mode may play an important role in the saturation of an MRI through complementray growth with the toroidal MRIs and coupling with magnetic reconnection.
STOCHASTIC PARTICLE ACCELERATION IN TURBULENCE GENERATED BY MAGNETOROTATIONAL INSTABILITY
Authors: Kimura Shigeo S. , Toma Kenji , Suzuki Takeru K. , Inutsuka Shu-ichiro 
Published: May 2016

ABSTRACT
We investigate stochastic particle acceleration in accretion flows. It is believed that magnetorotational instability (MRI) generates turbulence inside accretion flows and that cosmic rays (CRs) are accelerated by the turbulence. We calculate equations of motion for CRs in the turbulent fields generated by MRI with the shearing box approximation and without back reaction to the field. Our results show that the CRs randomly gain or lose their energy through interaction with the turbulent fields. The CRs diffuse in the configuration space anisotropically: the diffusion coefficient in the direction of the unperturbed flow is about 20 times higher than the Bohm coefficient, while those in the other directions are only a few times higher than the Bohm. The momentum distribution is isotropic and its evolution can be described by the diffusion equation in momentum space where the diffusion coefficient is a power-law function of the CR momentum. We show that the shear acceleration works efficiently for energetic particles. We also cautiously note that in the shearing box approximation, particles that cross the simulation box many times along the radial direction undergo unphysical runaway acceleration by the Lorentz transformation, which needs to be taken into account with special care.
THE EFFECTS OF ANGULAR MOMENTUM ON HALO PROFILES
Authors: Lentz Erik W , Quinn Thomas R , Rosenberg Leslie J 
Published: May 2016

ABSTRACT
The near universality of DM halo density profiles provided by N-body simulations proved to be robust against changes in total mass density, power spectrum, and some forms of initial velocity dispersion. Here we study the effects of coherently spinning up an isolated DM-only progenitor on halo structure. Halos with spins within several standard deviations of the simulated mean (λ ≲ 0.20) produce profiles with negligible deviations from the universal form. Only when the spin becomes quite large (λ ≳ 0.20) do departures become evident. The angular momentum distribution also exhibits a near universal form, which is also independent of halo spin up to λ ≲ 0.20. A correlation between these epidemic profiles and the presence of a strong bar in the virialized halo is also observed. These bar structures bear resemblance to the radial orbit instability in the rotationless limit.
GALAXY LUMINOSITY FUNCTION OF THE DYNAMICALLY YOUNG ABELL 119 CLUSTER: PROBING THE CLUSTER ASSEMBLY
Authors: Lee Youngdae , Rey Soo-Chang , Hilker Michael , Sheen Yun-Kyeong , Yi Sukyoung K. 
Published: May 2016

ABSTRACT
We present the galaxy luminosity function (LF) of the Abell 119 cluster down to

mag based on deep images in the u, g, and r bands taken by using MOSAIC II CCD mounted on the Blanco 4 m telescope at the CTIO. The cluster membership was accurately determined based on the radial velocity information and on the color–magnitude relation for bright galaxies and the scaling relation for faint galaxies. The overall LF exhibits a bimodal behavior with a distinct dip at

mag (

mag), which is more appropriately described by a two-component function. The shape of the LF strongly depends on the clustercentric distance and on the local galaxy density. The LF of galaxies in the outer, low-density region exhibits a steeper slope and more prominent dip compared with that of counterparts in the inner, high-density region. We found evidence for a substructure in the projected galaxy distribution in which several overdense regions in the Abell 119 cluster appear to be closely associated with the surrounding, possible filamentary structure. The combined LF of the overdense regions exhibits a two-component function with a distinct dip, while the LF of the central region is well described by a single Schechter function. We suggest that, in the context of the hierarchical cluster formation scenario, the observed overdense regions are the relics of galaxy groups, retaining their two-component LFs with a dip, which acquired their shapes through a galaxy merging process in group environments, before they fall into a cluster.
THE POPULATION OF COMPACT RADIO SOURCES IN THE ORION NEBULA CLUSTER
Authors: Forbrich J. , Rivilla V. M. , Menten K. M. , Reid M. J. , Chandler C. J. , Rau U. , Bhatnagar S. , Wolk S. J. , Meingast S. 
Published: May 2016

ABSTRACT
We present a deep centimeter-wavelength catalog of the Orion Nebula Cluster (ONC), based on a 30 hr single-pointing observation with the Karl G. Jansky Very Large Array in its high-resolution A-configuration using two 1 GHz bands centered at 4.7 and 7.3 GHz. A total of 556 compact sources were detected in a map with a nominal rms noise of 3 μJy bm−1, limited by complex source structure and the primary beam response. Compared to previous catalogs, our detections increase the sample of known compact radio sources in the ONC by more than a factor of seven. The new data show complex emission on a wide range of spatial scales. Following a preliminary correction for the wideband primary-beam response, we determine radio spectral indices for 170 sources whose index uncertainties are less than ±0.5. We compare the radio to the X-ray and near-infrared point-source populations, noting similarities and differences.
L’hégémonie politique à l’épreuve des musiques urbaines à Luanda, Angola
Authors: Buire Chloé 
Published: May 2016

Fondé sur un travail d’immersion ethnographique à Luanda et sur une analyse de la culture populaire urbaine, cet article interroge la réception des musiques actuelles par la jeunesse luandaise. Il part d’un fait d’actualité : en juin 2015, quinze jeunes activistes qui débattaient des principes de résistance pacifique ont été arrêtés et accusés de préparer un coup d’État. L’article défend l’idée que ces arrestations sont emblématiques des mécanismes de domination du parti au pouvoir et surtout de leur ambivalence. Sans annoncer la fin du régime autoritaire en Angola, l’émergence d’une scène musicale underground , depuis la fin de la guerre civile, illustre en effet les contradictions d’un système hégémonique qui, pour entretenir le consentement populaire, ouvre malgré lui des espaces de contestation qui redéfinissent l’espace public angolais depuis la chute des prix du pétrole en 2014.
Long-term Visual and Refractive Outcomes After LASIK for High Myopia and Astigmatism From −8.00 to −14.25 D
Authors: Reinstein Dan Z. , Carp Glenn I. , Archer Timothy J. , Lewis Tariq A. , Gobbe Marine , Moore Johnny , Moore Tara 
Published: May 2016

PURPOSE:
To evaluate outcomes of high myopic LASIK using the MEL 80 excimer laser (Carl Zeiss Meditec, Jena, Germany).

METHODS:

Retrospective analysis of 479 consecutive high myopic LASIK procedures (318 patients) using the MEL 80 excimer laser and VisuMax femtosecond laser (Carl Zeiss Meditec) in 77% of cases or zero compression Hansatome microkeratome (Bausch & Lomb, Rochester, NY) in 23% of cases. Inclusion criteria were preoperative spherical equivalent refraction (SEQ) of between −8.00 and −14.25 diopters (D) and corrected distance visual acuity (CDVA) of 20/20 or better. Patients were observed for a minimum of 1 year. Flap thickness was between 80 and 160
µ
m and optical zone was between 5.75 and 6.50 mm. Standard outcomes analysis was performed.

RESULTS:

Mean attempted SEQ was −9.39 ± 1.22 D (range: −8.00 to −14.18 D) and mean cylinder was −1.03 ± 0.84 D (range: 0.00 to −4.50 D). Mean age was 37 ± 9 years (range: 21 to 60 years) with 54% female patients. Postoperative SEQ was ±0.50 D in 55% and ±1.00 D in 83% of eyes after primary treatment. After re-treatment, 69% of eyes were within ±0.50 D and 95% were within ±1.00 D. UDVA was 20/20 or better in 89% of eyes after final treatment. One line of CDVA was lost in 3% of eyes and no eyes lost two or more lines. Statistically significant increases (
P
< .001) were measured in contrast sensitivity (CSV-1000) at 12 and 18 cycles per degree.

CONCLUSIONS:
The MEL 80 excimer laser was found to achieve high efficacy and safety for treatment of high myopia between −8.00 and −14.25 D and up to −4.50 D of cylinder.

[
J Refract Surg.
2016;32(5):290–297.]