bluuebunny/crossref_metadata_2025_split huggingface dataset:
Influence of storage conditions on in vitro stability of atrial natriuretic peptide and of anesthesia on plasma atrial natriuretic peptide concentration in cats
Authors: Heishima Yasuhiro , Hori Yasutomo , Chikazawa Seishiro , Kanai Kazutaka , Hoshi Fumio , Itoh Naoyuki 
Published: July 2016

Abstract
OBJECTIVE To investigate the in vitro stability of atrial natriuretic peptide (ANP) in plasma samples under various storage conditions and the influence of anesthesia on plasma ANP concentration in cats.
ANIMALS 1 cat with congestive heart failure and 5 healthy adult mixed-breed cats.
PROCEDURES A plasma sample from the cat with heart failure was serially diluted, and dilutional parallelism of ANP concentration was evaluated. Plasma samples containing aprotinin or serum samples from the 5 healthy cats were kept at room temperature (27°C) for ≤ 12 hours. Plasma samples from the same healthy cats were stored at −70°, −20°, or 4°C for ≤ 14 days. Plasma samples were obtained from the healthy cats before and during isoflurane anesthesia. Plasma ANP concentrations were measured at a commercial laboratory by use of a human ANP chemiluminescence assay.
RESULTS Intra- and interassay coefficients of variation were 1.5% and 2.5%, respectively, and dilutional parallelism was established. Although ANP concentration decreased by 82.4 ± 13.6% (mean ± SD) after sample storage for 12 hours at room temperature, this decrease was prevented by aprotinin. Plasma ANP concentrations were stable for 7 days at −20°C and for 14 days at −70°C. However, concentrations decreased markedly to 57.6 ± 6.9% at −20°C and to 18.0 ± 3.0% at 4°C after 14 days. Plasma ANP concentration decreased significantly in cats during anesthesia and was correlated with blood pressure.
CONCLUSIONS AND CLINICAL RELEVANCE Results suggested that aprotinin should be added routinely in preparation of plasma samples from cats for measurement of ANP concentration, and those samples, if stored, should be frozen immediately at ≤ −20°C. General anesthesia or systemic blood pressure may affect plasma ANP concentration in cats.
High Sensitization to House-Dust Mites in Patients with Allergic Rhinitis in the Eastern Black Sea Region of Turkey: A Retrospective Study
Authors: Coskun Zerrin Ozergin , Erdivanlı Ozlem Celebi , Kazıkdas Kadir Çagdas , Terzi Suat , Sahin Unal , Ozgur Abdulkadir , Demirci Munir , Dursun Engin , Cingi Cemal 
Published: July 2016

Objectives Identification of the most common aeroallergens to which patients are sensitized in a specific area is important in the diagnosis and treatment of allergic rhinitis (AR). We determined the distribution of aeroallergens, detected by skin-prick tests (SPT), in adult patients with AR in the Eastern Black Sea region of Turkey and compared the results with the other regions of Turkey and in the world. Methods The medical records of SPT performed on 1457 patients with symptoms of AR (with regard to the Allergic Rhinitis and its Impact on Asthma 2008 guidelines) between March 2010 and March 2013 were analyzed retrospectively. SPT were carried out with the same panel, which included grass; weeds; trees; mold; epidermal mixtures; and with two house-dust mite (HDM) extracts, Dermatophagoides pteronyssinus and Dermatophagoides farinae. Results In 1229 of 1457 patients (84.4%), there were positive reactions for at least one aeroallergen on the SPT. The most common aeroallergen was the HDM D. pteronyssinus (84% [n = 1033]) followed by D. farinae (78.2% [n = 962]). Grass pollen sensitivity (70.8% [n = 871]) was higher than tree or weed pollen sensitivity in this region. Conclusions The most common aeroallergens in AR are HDMs of D. pteronyssinus and D. farinae in the Eastern Black Sea region in Turkey. Our study may help in developing environmental control strategies for AR.
Treating Allergic Conjunctivitis: A Once-daily Medication that Provides 24-hour Symptom Relief
Authors: Carr Warner , Schaeffer Jack , Donnenfeld Eric 
Published: July 2016

Background Allergic conjunctivitis (AC) is a common ocular inflammatory manifestation of allergen exposure in sensitized individuals. Signs and symptoms of AC can decrease quality of life, interfere with productivity, and lead to considerable economic burden. Consistent suppression of conjunctival inflammation is necessary for managing AC, but currently available medications require frequent administration and exhibit limited duration of action. Methods In this review, we summarized AC pathogenesis, diagnosis, and current treatment options as well as their limitations. Findings from the literature were discussed in the context of the unmet need for a once-daily medication with sustained 24-hour effectiveness. Results Topical pharmacologic treatments are the most common approach for managing extant AC; however, most available medications require multiple daily instillations. Dual-acting antihistamine-mast cell stabilizing agents are currently considered first-line therapeutics for AC because they provide acute relief of signs and symptoms and block persistent inflammation to promote regression of AC. Recent studies of a newly-developed, higher-concentration formulation of a dual-acting antihistamine-mast cell stabilizer have demonstrated that this formulation provides a 24-hour duration of action with once-daily dosing. Conclusions Dual-acting AC medications exhibit a high degree of overall effectiveness and are well tolerated for chronic use. A newly available once-daily medication that manages signs and symptoms of AC for a full 24 hours may be considered a treatment of choice for patients experiencing seasonal or perennial AC. ClinicalTrials.gov NCT01743027 and NCT01479374
Azithromycin for the Treatment of Eosinophilic Nasal Polyposis: Clinical and Histologic Analysis
Authors: de Oliveira Isamara Simas , Crosara Paulo Fernando Tormin Borges , Cassali Geovanni Dantas , dos Reis Diego Carlos , Rodrigues Danilo Santana , Nunes Flavio Barbosa , Guimarães Roberto Eustáquio Santos 
Published: July 2016

Introduction Macrolides used as immunomodulators are a promising tool for chronic inflammatory airway diseases. Eosinophilic nasal polyposis (ENP) is still considered a disease that is difficult to control with the currently standardized treatments. Objectives To evaluate prolonged treatment with low-dose azithromycin for ENP based on clinical and histopathologic variables. Methods The present investigation was a self-paired case study of 33 patients with ENP. A comparison was performed between patients before and after treatment with azithromycin for 8 weeks. The patients were subjected to clinical examinations, staging (three-dimensional imaging by endoscopy), application of the questionnaire, and biopsy of nasal polyps at the beginning and at the end of the treatment. Results The treatment yielded a clinical improvement regarding the two variables studied: polyposis staging (69.7%) and questionnaire (57.6%). We did not find significant differences in the inflammatory pattern and in the percentage or absolute number of eosinophils per field between samples obtained before and after the treatment (p > 0.05). There was no difference between the answers obtained from groups with and without asthma and/or aspirin intolerance (p > 0.3). The patients with advanced initial staging exhibited lower subjective improvement index and staging reduction (p = 0.031 and p = 0.012, respectively). Conclusion Based on this study, azithromycin may be considered as another therapeutic option for ENP. However, further studies are necessary to define the real mechanism of action involved.
SUPRATHERMAL ELECTRONS IN TITAN’S SUNLIT IONOSPHERE: MODEL–OBSERVATION COMPARISONS
Authors: Vigren E. , Galand M. , Wellbrock A. , Coates A. J. , Cui J. , Edberg N. J. T. , Lavvas P. , Sagnières L. , Snowden D. , Vuitton V. , Wahlund J.-E. 
Published: July 2016

ABSTRACT
The dayside ionosphere of the Saturnian satellite Titan is generated mainly from photoionization of N2 and CH4. We compare model-derived suprathermal electron intensities with spectra measured by the Cassini Plasma Spectrometer/Electron Spectrometer (CAPS/ELS) in Titan's sunlit ionosphere (altitudes of 970–1250 km) focusing on the T40, T41, T42, and T48 Titan flybys by the Cassini spacecraft. The model accounts only for photoelectrons and associated secondary electrons, with a main input being the impinging solar EUV spectra as measured by the Thermosphere Ionosphere Mesosphere Energy and Dynamics/Solar EUV Experiment and extrapolated to Saturn. Associated electron-impact electron production rates have been derived from ambient number densities of N2 and CH4 (measured by the Ion Neutral Mass Spectrometer/Closed Source Neutral mode) and related energy-dependent electron-impact ionization cross sections. When integrating up to electron energies of 60 eV, covering the bulk of the photoelectrons, the model-based values exceed the observationally based values typically by factors of ∼3 ± 1. This finding is possibly related to current difficulties in accurately reproducing the observed electron number densities in Titan's dayside ionosphere. We compare the utilized dayside CAPS/ELS spectra with ones measured in Titan's nightside ionosphere during the T55–T59 flybys. The investigated nightside locations were associated with higher fluxes of high-energy (>100 eV) electrons than the dayside locations. As expected, for similar neutral number densities, electrons with energies <60 eV give a higher relative contribution to the total electron-impact ionization rates on the dayside (due to the contribution from photoelectrons) than on the nightside.
MULTI-SPACECRAFT OBSERVATIONS AND TRANSPORT MODELING OF ENERGETIC ELECTRONS FOR A SERIES OF SOLAR PARTICLE EVENTS IN AUGUST 2010
Authors: Dröge W. , Kartavykh Y. Y. , Dresing N. , Klassen A. 
Published: July 2016

ABSTRACT
During 2010 August a series of solar particle events was observed by the two STEREO spacecraft as well as near-Earth spacecraft. The events, occurring on August 7, 14, and 18, originated from active regions 11093 and 11099. We combine in situ and remote-sensing observations with predictions from our model of three-dimensional anisotropic particle propagation in order to investigate the physical processes that caused the large angular spreads of energetic electrons during these events. In particular, we address the effects of the lateral transport of the electrons in the solar corona that is due to diffusion perpendicular to the average magnetic field in the interplanetary medium. We also study the influence of two coronal mass ejections and associated shock waves on the electron propagation, and a possible time variation of the transport conditions during the above period. For the August 18 event we also utilize electron observations from the MESSENGER spacecraft at a distance of 0.31 au from the Sun for an attempt to separate between radial and longitudinal dependencies in the transport process. Our modelings show that the parallel and perpendicular diffusion mean free paths of electrons can vary significantly not only as a function of the radial distance, but also of the heliospheric longitude. Normalized to a distance of 1 au, we derive values of λ
∥ in the range of 0.15–0.6 au, and values of λ
⊥ in the range of 0.005–0.01 au. We discuss how our results relate to various theoretical models for perpendicular diffusion, and whether there might be a functional relationship between the perpendicular and the parallel mean free path.
DOUBLE DYNAMO SIGNATURES IN A GLOBAL MHD SIMULATION AND MEAN-FIELD DYNAMOS
Authors: Beaudoin Patrice , Simard Corinne , Cossette Jean-François , Charbonneau Paul 
Published: July 2016

ABSTRACT
The 11 year solar activity cycle is the most prominent periodic manifestation of the magnetohydrodynamical (MHD) large-scale dynamo operating in the solar interior, yet longer and shorter (quasi-) periodicities are also present. The so-called “quasi-biennial” signal appearing in many proxies of solar activity has been gaining increasing attention since its detection in p-mode frequency shifts, which suggests a subphotospheric origin. A number of candidate mechanisms have been proposed, including beating between co-existing global dynamo modes, dual dynamos operating in spatially separated regions of the solar interior, and Rossby waves driving short-period oscillations in the large-scale solar magnetic field produced by the 11 year activity cycle. In this article, we analyze a global MHD simulation of solar convection producing regular large-scale magnetic cycles, and detect and characterize shorter periodicities developing therein. By constructing kinematic mean-field α
2Ω dynamo models incorporating the turbulent electromotive force (emf) extracted from that same simulation, we find that dual-dynamo behavior materializes in fairly wide regions of the model’s parameters space. This suggests that the origin of the similar behavior detected in the MHD simulation lies with the joint complexity of the turbulent emf and differential rotation profile, rather that with dynamical interactions such as those mediated by Rossby waves. Analysis of the simulation also reveals that the dual dynamo operating therein leaves a double-period signature in the temperature field, consistent with a dual-period helioseismic signature. Order-of-magnitude estimates for the magnitude of the expected frequency shifts are commensurate with helioseismic measurements. Taken together, our results support the hypothesis that the solar quasi-biennial oscillations are associated with a secondary dynamo process operating in the outer reaches of the solar convection zone.
THE NUCLEUS OF THE PLANETARY NEBULA EGB 6 AS A POST-MIRA BINARY*
Authors: Bond Howard E. , Ciardullo Robin , Esplin Taran L. , Hawley Steven A. , Liebert James , Munari Ulisse 
Published: July 2016

ABSTRACT
EGB 6 is a faint, large, ancient planetary nebula (PN). Its central star, a hot DAOZ white dwarf (WD), is a prototype of a rare class of PN nuclei associated with dense, compact emission-line knots. The central star also shows excess fluxes in both the near-infrared (NIR) and mid-infrared (MIR). In a 2013 paper, we used Hubble Space Telescope (HST) images to show that the compact nebula is a point-like source, located 0.″16 (∼118 AU) from the WD. We attributed the NIR excess to an M dwarf companion star, which appeared to coincide with the dense emission knot. We now present new ground-based NIR spectroscopy, showing that the companion is actually a much cooler source with a continuous spectrum, apparently a dust-enshrouded low-luminosity star. New HST images confirm common proper motion of the emission knot and red source with the WD. The I-band, NIR, and MIR fluxes are variable, possibly on timescales as short as days. We can fit the spectral energy distribution (SED) with four blackbodies (the WD, a ∼1850 K NIR component, and MIR dust at 385 and 175 K). Alternatively, we show that the NIR/MIR SED is very similar to that of Class 0/I young stellar objects. We suggest a scenario in which the EGB 6 nucleus is descended from a wide binary similar to the Mira system, in which a portion of the wind from an AGB star was captured into an accretion disk around a companion star; a remnant of this disk has survived to the present time and is surrounded by gas photoionized by UV radiation from the WD.
SUPERNOVA DRIVING. III. SYNTHETIC MOLECULAR CLOUD OBSERVATIONS
Authors: Padoan Paolo , Juvela Mika , Pan Liubin , Haugbølle Troels , Nordlund Åke 
Published: July 2016

ABSTRACT
We present a comparison of molecular clouds (MCs) from a simulation of supernova (SN) driven interstellar medium (ISM) turbulence with real MCs from the Outer Galaxy Survey. The radiative transfer calculations to compute synthetic CO spectra are carried out assuming that the CO relative abundance depends only on gas density, according to four different models. Synthetic MCs are selected above a threshold brightness temperature value, T
B,min = 1.4 K, of the J = 1 − 0 12CO line, generating 16 synthetic catalogs (four different spatial resolutions and four CO abundance models), each containing up to several thousands MCs. The comparison with the observations focuses on the mass and size distributions and on the velocity–size and mass–size Larson relations. The mass and size distributions are found to be consistent with the observations, with no significant variations with spatial resolution or chemical model, except in the case of the unrealistic model with constant CO abundance. The velocity–size relation is slightly too steep for some of the models, while the mass–size relation is a bit too shallow for all models only at a spatial resolution dx ≈ 1 pc. The normalizations of the Larson relations show a clear dependence on spatial resolution, for both the synthetic and the real MCs. The comparison of the velocity–size normalization suggests that the SN rate in the Perseus arm is approximately 70% or less of the rate adopted in the simulation. Overall, the realistic properties of the synthetic clouds confirm that SN-driven turbulence can explain the origin and dynamics of MCs.
THE BLACK HOLE CENTRAL ENGINE FOR ULTRA-LONG GAMMA-RAY BURST 111209A AND ITS ASSOCIATED SUPERNOVA 2011KL
Authors: Gao He , Lei Wei-Hua , You Zhi-Qiang , Xie Wei 
Published: July 2016

ABSTRACT
Recently, the first association between an ultra-long gamma-ray burst (GRB) and a supernova was reported, i.e., GRB 111209A/SN 2011kl, enabling us to investigate the physics of central engines or even progenitors for ultra-long GRBs. In this paper, we inspect the broadband data of GRB 111209A/SN 2011kl. The late-time X-ray light curve exhibits a GRB 121027A-like fallback bump, suggesting a black hole (BH) central engine. We thus propose a collapsar model with fallback accretion for GRB 111209A/SN 2011kl. The required model parameters, such as the total mass and radius of the progenitor star, suggest that the progenitor of GRB 111209A is more likely a Wolf–Rayet star instead of a blue supergiant, and the central engine of this ultra-long burst is a BH. The implications of our results are discussed.
GAS LOSS BY RAM PRESSURE STRIPPING AND INTERNAL FEEDBACK FROM LOW-MASS MILKY WAY SATELLITES
Authors: Emerick Andrew , Low Mordecai-Mark Mac , Grcevich Jana , Gatto Andrea 
Published: July 2016

ABSTRACT
The evolution of dwarf satellites in the Milky Way (MW) is affected by a combination of ram pressure stripping (RPS), tidal stripping, and internal feedback from massive stars. We investigate gas loss processes in the smallest satellites of the MW using three-dimensional, high-resolution, idealized wind tunnel simulations, accounting for gas loss through both ram pressure stripping and expulsion by supernova feedback. Using initial conditions appropriate for a dwarf galaxy like Leo T, we investigate whether or not environmental gas stripping and internal feedback can quench these low-mass galaxies on the expected timescales, shorter than 2 Gyr. We find that supernova feedback contributes negligibly to the stripping rate for these low star formation rate galaxies. However, we also find that RPS is less efficient than expected in the stripping scenarios we consider. Our work suggests that although RPS can eventually completely strip these galaxies, other physics is likely at play to reconcile our computed stripping times with the rapid quenching timescales deduced from observations of low-mass MW dwarf galaxies. We discuss the roles additional physics may play in this scenario, including host-satellite tidal interactions, cored versus cuspy dark matter profiles, reionization, and satellite preprocessing. We conclude that a proper accounting of these physics together is necessary to understand the quenching of low-mass MW satellites.
ON THE OPTICAL–X-RAY CORRELATION FROM OUTBURST TO QUIESCENCE IN LOW-MASS X-RAY BINARIES: THE REPRESENTATIVE CASES OF V404 CYG AND CEN X-4
Authors: Bernardini F. , Russell D. M. , Kolojonen K. I. I. , Stella L. , Hynes R. I. , Corbel S. 
Published: July 2016

ABSTRACT
Low-mass X-ray binaries (LMXBs) show evidence of a global correlation of debated origin between X-ray and optical luminosity. We study for the first time this correlation in two transient LMXBs, the black hole (BH) V404 Cyg and the neutron star Cen X-4, over six orders of magnitude in X-ray luminosity, from outburst to quiescence. After subtracting the contribution from the companion star, the Cen X-4 data can be described by a single power-law correlation of the form

, consistent with disk reprocessing. We find a similar correlation slope for V404 Cyg in quiescence (0.46) and a steeper one (0.56) in the outburst hard state of 1989. However, V404 Cyg is about 160–280 times optically brighter, at a given 3–9 keV X-ray luminosity, compared to Cen X-4. This ratio is a factor of 10 smaller in quiescence, where the normalization of the V404 Cyg correlation also changes. Once the bolometric X-ray emission is considered and the known main differences between V404 Cyg and Cen X-4 are taken into account (a larger compact object mass, accretion disk size, and the presence of a strong jet contribution in the hard state for the BH system), the two systems lie on the same correlation. In V404 Cyg, the jet dominates spectrally at optical–infrared frequencies during the hard state but makes a negligible contribution in quiescence, which may account for the change in its correlation slope and normalization. These results provide a benchmark to compare with data from the 2015 outburst of V404 Cyg and, potentially, other transient LMXBs as well.
FERROMAGNETISM AND PARTICLE COLLISIONS: APPLICATIONS TO PROTOPLANETARY DISKS AND THE METEORITICAL RECORD
Authors: Hubbard Alexander 
Published: July 2016

ABSTRACT
The meteoritical record shows both iron partitioning and tungsten isotopic partitioning between the matrix and chondrules. Tungsten is not abundant enough to have driven its own isotopic partitioning, but if tungsten were correlated with iron then ferromagnetic interaction grains could help explain both observations. We derive a practical parameterization for the increase in particle–particle collision rates caused by mutually attracting particle magnetic dipole moments. While the appropriate magnetic parameters remain uncertain, we show that ambient magnetic fields in protoplanetary disks are expected to be strong enough to magnetize iron metal bearing dust grains sufficiently to drive large increases in their collision rates. Such increased collision rates between iron-metal-rich grains could help preserve primordial iron and W isotopic inhomogeneities, and would help explain why the meteoritical record shows their partitioning in the solar nebula. The importance of magnetic interactions for larger grains whose growth is balanced by fragmentation is less clear and will require future laboratory or numerical studies.
L’idée régulatrice du temps absolu et son rôle dans la théorie kantienne de l’expérience
Authors: Beydoun Zaki 
Published: July 2016

Nous tentons ici de démontrer que le concept du temps absolu, tel qu’il intervient dans le texte des « Analogies de l’expérience », renvoie à une idée régulatrice de la raison qui joue, dans la théorie kantienne de l’expérience, un rôle parallèle à celui qu’attribue Kant à l’idée régulatrice de l’espace absolu dans les Premiers principes métaphysiques de la science de la nature. Dans ce cadre, il s’agit d’établir une distinction nette entre l’idée du temps absolu et l’intuition pure du temps, ainsi que de démontrer que les principes dynamiques de l’entendement pur et, corrélativement, la possibilité de l’expérience, reposent sur cette idée.