bluuebunny/crossref_metadata_2025_split huggingface dataset:
Formulation and Evaluation of Microsponge Based Nicorandil Sustained Released Tablet
Authors: Patel S. S. , Patel M. R. , Patel M. J. 
Published: September 2017

The aim of the present work was to develop once-daily sustained release microsponges formulations of Nicorandil, a potent potassium channel opener used in cardiovascular diseases and it has low oral bioavailability (70%) and half-life 1 h. So, it is good candidate for sustained release formulations based on microsponge technology. The microsponges were prepared by using quasi-emulsion solvent diffusion method. Scanning Electron Microscopy (SEM) revealed that the microsponges of nicorandil with Eudragit - RSPO and HPMC K100M were smooth, porous, glossy and discrete spherical. The actual drug content and encapsulation efficiency of batch M1 to M9 were obtained in range of 62.05 ± 0.31 to 80.69 ± 0.43 and 64.41 ± 1.71 to 70.58 ± 1.12, respectively. The microsponges formulations were subjected to in-vitro release studies and the results were evaluated kinetically and statically. The best fitted model was found to be Korsmeyer - Peppas model (R2 = 0.9992) for M6 batch. The n value for Korsmeyer - Peppas model was between 0.5 and 1.0 which is indicative of non-Fickian diffusion. Statistical analysis using ANOVA yielded a p value of 0.572 for all the formulations, indicating that there was no significant difference among them.
A New Orbit for the Eclipsing Binary V577 Oph
Authors: Jeffery Elizabeth J. , Barnes Thomas G. , Skillen Ian , Montemayor Thomas J. 
Published: September 2017

Abstract
Pulsating stars in eclipsing binary systems are unique objects for providing constraints on stellar models. To fully leverage the information available from the binary system, full orbital radial velocity curves must be obtained. We report 23 radial velocities for components of the eclipsing binary V577 Oph, whose primary star is a δ Sct variable. The velocities cover a nearly complete orbit and a time base of 20 years. We computed orbital elements for the binary and compared them to the ephemeris computed by Creevey et al. The comparison shows marginally different results. In particular, a change in the systemic velocity by −2 km s−1 is suggested by our results. We compare this systemic velocity difference to that expected due to reflex motion of the binary in response to the third body in the system. The systemic velocity difference is consistent with reflex motion, given our mass determination for the eclipsing binary and the orbital parameters determined by Volkov & Volkova for the three-body orbit. We see no evidence for the third body in our spectra, but we do see strong interstellar Na D lines that are consistent in strength with the direction and expected distance of V577 Oph.
Exploring the Inner Acceleration Region of Solar Wind: A Study Based on Coronagraphic UV and Visible Light Data
Authors: Bemporad A. 
Published: September 2017

Abstract
This work combined coronagraphic visible light (VL) and UV data to provide with an unprecedented view of the inner corona where the nascent solar wind is accelerated. The UV (H i Lyα) and VL (polarized brightness) images (reconstructed with SOHO/UVCS, LASCO, and Mauna Loa data) have been analyzed with the Doppler dimming technique to provide for the first time daily 2D images of the radial wind speed between 1 and 6 R
⊙ over 1 month of observations. Results show that both polar and equatorial regions are characterized at the base of the corona by plasma outflows at speeds

km s−1. The plasma is then decelerated within ∼1.5 R
⊙ at the poles and ∼2.0 R
⊙ at the equator, where local minima of the expansion speeds are reached, and gently reaccelerated higher up, reaching speeds typical of fast and slow wind components. The mass flux is highly variable with latitude and time at the equator and more uniform and stable over the poles. The polar flow is asymmetric, with speeds above the south pole lower than those above the north pole. A correlation (anticorrelation) between the wind speed and its density is found below (above) ∼1.8 R
⊙. The 2D distribution of forces responsible for deceleration and reacceleration of solar wind is provided and interpreted in terms of Alfvén waves. These results provide a possible connection between small-scale outflows reported with other instruments at the base of the corona and bulk wind flows measured higher up.
Experimental Phase Functions of Millimeter-sized Cosmic Dust Grains
Authors: Muñoz O. , Moreno F. , Vargas-Martín F. , Guirado D. , Escobar-Cerezo J. , Min M. , Hovenier J. W. 
Published: September 2017

Abstract
We present the experimental phase functions of three types of millimeter-sized dust grains consisting of enstatite, quartz, and volcanic material from Mount Etna, respectively. The three grains present similar sizes but different absorbing properties. The measurements are performed at 527 nm covering the scattering angle range from 3° to 170°. The measured phase functions show two well-defined regions: (i) soft forward peaks and (ii) a continuous increase with the scattering angle at side- and back-scattering regions. This behavior at side- and back-scattering regions is in agreement with the observed phase functions of the Fomalhaut and HR 4796A dust rings. Further computations and measurements (including polarization) for millimeter-sized grains are needed to draw some conclusions about the fluffy or compact structure of the dust grains.
Satellitesimal Formation via Collisional Dust Growth in Steady Circumplanetary Disks
Authors: Shibaike Yuhito , Okuzumi Satoshi , Sasaki Takanori , Ida Shigeru 
Published: September 2017

Abstract
The icy satellites around Jupiter are considered to have formed in a circumplanetary disk. While previous models have focused on the formation of the satellites starting from satellitesimals, the question of how satellitesimals themselves form from smaller dust particles has not yet been addressed. In this work, we study the possibility that satellitesimals form in situ in a circumplanetary disk. We calculate the radial distribution of the surface density and representative size of icy dust particles that grow by colliding with each other and drift toward the central planet in a steady circumplanetary disk with a continuous supply of gas and dust from the parent protoplanetary disk. The radial drift barrier is overcome if the ratio of the dust-to-gas accretion rates onto the circumplanetary disk,

, is high and the strength of turbulence, α, is not too low. The collision velocity is lower than the critical velocity of fragmentation when α is low. Taken together, we find that the conditions for satellitesimal formation via dust coagulation are given by

and

. The former condition is generally difficult to achieve, suggesting that the in situ satellitesimal formation via particle sticking is viable only under extreme conditions. We also show that neither satellitesimal formation via the collisional growth of porous aggregates nor via streaming instability is viable as long as

is low.
A Mixture Evolution Scenario of the AGN Radio Luminosity Function. II. Do Low- and High-power Radio-loud AGNs Evolve Differently?
Authors: Yuan Zunli , Wang Jiancheng , Zhou Ming , Qin Longhua , Mao Jirong 
Published: September 2017

Abstract
Following previous work, we further confirm that the cosmic evolution of steep-spectrum radio-loud AGNs (active galactic nuclei) can be reproduced by a simple combination of density evolution (DE) and luminosity evolution (LE). This mixture evolution scenario can naturally explain the luminosity-dependent evolution of radio-loud AGNs. Our models successfully fitted a large amount of data on radio luminosity functions of steep-spectrum sources and multi-frequency source counts. The modeling indicates that the DE slowly increases as

out to

, and then rapidly decreases as

, while the LE rapidly increases as

out to a higher redshift (at least

). We find a high-redshift decline (i.e., redshift cutoff) in the number density of steep-spectrum radio sources, but we cannot conclude whether such a decline is sharp or shallow. We believe that whether a redshift cutoff occurs or not depends mainly on DE, while its steepness is decided by LE, which, however, cannot be well constrained due to the lack of high-redshift samples. Most intriguingly, according to our mixture evolution scenario, there appears to be no need for different evolution for the low- and high-power radio-loud AGNs. Both types of sources experience the same combined evolution of DE and LE.
A Widespread, Clumpy Starburst in the Isolated Ongoing Dwarf Galaxy Merger dm1647+21
Authors: Privon G. C. , Stierwalt S. , Patton D. R. , Besla G. , Pearson S. , Putman M. , Johnson K. E. , Kallivayalil N. , Liss S. ,   (TiNy Titans)
Published: September 2017

Abstract
Interactions between pairs of isolated dwarf galaxies provide a critical window into low-mass hierarchical, gas-dominated galaxy assembly and the build-up of stellar mass in low-metallicity systems. We present the first Very Large Telescope/Multi Unit Spectroscopic Explorer (VLT/MUSE) optical integral field unit (IFU) observations of the interacting dwarf pair dm1647+21 selected from the TiNy Titans survey. The Hα emission is widespread and corresponds to a total unobscured star formation rate (SFR) of 0.44 M
⊙ yr−1, which is 2.7 times higher than the SFR inferred from Sloan Digital Sky Survey (SDSS) data. The implied specific SFR (sSFR) for the system is elevated by more than an order of magnitude above non-interacting dwarfs in the same mass range. This increase is dominated by the lower-mass galaxy, which has a sSFR enhancement of >50. Examining the spatially resolved maps of classic optical line diagnostics, we find that the interstellar medium (ISM) excitation can be fully explained by star formation. The velocity field of the ionized gas is not consistent with simple rotation. Dynamical simulations indicate that the irregular velocity field and the stellar structure is consistent with the identification of this system as an ongoing interaction between two dwarf galaxies. The widespread, clumpy enhancements in the star formation in this system point to important differences in the effect of mergers on dwarf galaxies, compared to massive galaxies; rather than the funneling of gas to the nucleus and giving rise to a nuclear starburst, starbursts in low-mass galaxy mergers may be triggered by large-scale ISM compression, and thus may be more distributed.
A Panchromatic View of Brown Dwarf Aurorae
Authors: Pineda J. Sebastian , Hallinan Gregg , Kao Melodie M. 
Published: September 2017

Abstract
Stellar coronal activity has been shown to persist into the low-mass star regime, down to late M-dwarf spectral types. However, there is now an accumulation of evidence suggesting that at the end of the main sequence, there is a transition in the nature of the magnetic activity from chromospheric and coronal to planet-like and auroral, from local impulsive heating via flares and MHD wave dissipation to energy dissipation from strong large-scale magnetospheric current systems. We examine this transition and the prevalence of auroral activity in brown dwarfs through a compilation of multiwavelength surveys of magnetic activity, including radio, X-ray, and optical. We compile the results of those surveys and place their conclusions in the context of auroral emission as a consequence of large-scale magnetospheric current systems that accelerate energetic electron beams and drive the particles to impact the cool atmospheric gas. We explore the different manifestations of auroral phenomena, like Hα, in brown dwarf atmospheres and define their distinguishing characteristics. We conclude that large-amplitude photometric variability in the near-infrared is most likely a consequence of clouds in brown dwarf atmospheres, but that auroral activity may be responsible for long-lived stable surface features. We report a connection between auroral Hα emission and quiescent radio emission in electron cyclotron maser instability pulsing brown dwarfs, suggesting a potential underlying physical connection between quiescent and auroral emissions. We also discuss the electrodynamic engines powering brown dwarf aurorae and the possible role of satellites around these systems both to power the aurorae and seed the magnetosphere with plasma.
The Formation of Rapidly Rotating Black Holes in High-mass X-Ray Binaries
Authors: Batta Aldo , Ramirez-Ruiz Enrico , Fryer Chris 
Published: September 2017

Abstract
High-mass X-ray binaries (HMXRBs), such as Cygnus X-1, host some of the most rapidly spinning black holes (BHs) known to date, reaching spin parameters

. However, there are several effects that can severely limit the maximum BH spin parameter that could be obtained from direct collapse, such as tidal synchronization, magnetic core-envelope coupling, and mass loss. Here, we propose an alternative scenario where the BH is produced by a failed supernova (SN) explosion that is unable to unbind the stellar progenitor. A large amount of fallback material ensues, whose interaction with the secondary naturally increases its overall angular momentum content, and therefore the spin of the BH when accreted. Through SPH hydrodynamic simulations, we studied the unsuccessful explosion of an

pre-SN star in a close binary with a

companion with an orbital period of ≈1.2 days, finding that it is possible to obtain a BH with a high spin parameter

even when the expected spin parameter from direct collapse is

. This scenario also naturally explains the atmospheric metal pollution observed in HMXRB stellar companions.
Myositis-associated Interstitial Lung Disease: Predictors of Failure of Conventional Treatment and Response to Tacrolimus in a US Cohort
Authors: Sharma Niharika , Putman Michael S. , Vij Rekha , Strek Mary E. , Dua Anisha 
Published: September 2017

Objective.Patients with myositis-associated interstitial lung disease (MA-ILD) are often refractory to conventional treatment, and predicting their response to therapy is challenging. Recent case reports and small series suggest that tacrolimus may be useful in refractory cases.Methods.A retrospective cohort study of patients with MA-ILD comparing clinical characteristics between those who responded to or failed conventional treatment. In those who failed conventional treatment and received adjunctive tacrolimus, response to tacrolimus was measured by the improvement in myositis, ILD, and change in the dose of glucocorticoids.Results.Thirty-one of 54 patients (57%) responded to conventional treatment based on the predefined variables of improvement in myositis and/or ILD. Patients with polymyositis (PM)-ILD were more likely to respond to conventional treatment than those with dermatomyositis (DM)-ILD (67% vs 35%, p = 0.013). Twenty-three patients failed conventional treatment, 18 of whom subsequently received adjunctive tacrolimus. Ninety-four percent had improvements in ILD and 72% showed improvement in both myositis and ILD. The mean doses of prednisone decreased from baseline by 65% at 3–6 months (p = 0.002) and 81% at 1 year (p < 0.001).Conclusion.Patients with PM-ILD were more likely to respond to conventional treatment than patients with DM-ILD, but clinical characteristics and serology did not otherwise predict response to therapy. A majority of patients with MA-ILD refractory to conventional therapy improved while receiving tacrolimus and were able to decrease their dose of both glucocorticoids and other disease-modifying antirheumatic drugs.
Determinants of Nurses’ Use of Physical Restraints in Surgical Intensive Care Unit Patients
Authors: Dolan Jeanne , Dolan Looby Sara E. 
Published: September 2017

Background
Physical restraints are used in intensive care units, particularly among patients at risk for self-terminating necessary treatment interventions, including endotracheal tubes and invasive catheters. Assessments conducted by intensive care unit nurses often influence the collaborative decision to initiate and discontinue restraints in critical care patients. However, little is known about factors that influence the critical thought processes of intensive care unit nurses in determining use of restraints.

Objectives
To describe nurses’ determinants of initiation and discontinuation of restraints in surgical intensive care unit patients.

Methods
Semistructured interviews were conducted to identify and describe determinants of initiation and discontinuation of physical restraints. Demographic and employment data were collected via questionnaire. Interviews were recorded, transcribed, and analyzed by using conventional content analysis to establish categories and identify themes.

Results
A total of 13 nurses (mean age 43 [SD, 12] years, 92% female, mean of 18 [SD, 12] years of practice as a registered nurse, 69% bachelor of science in nursing) participated in the study. Content analysis revealed 3 general categories and 8 themes that indicated the thoughtful reflection processes nurses in a surgical intensive care unit use to determine use of restraints.

Conclusions
Top priorities were ensuring patient safety and comfort. Nurses synthesized factors including practice experience, patient-specific behaviors and risk, and patients’ need for devices in determining use of restraints.
Post–Intensive Care Syndrome in Family Decision Makers of Long-term Acute Care Hospital Patients
Authors: Petrinec Amy 
Published: September 2017

Background
Family members of critically ill patients experience indications of post–intensive care syndrome, including anxiety, depression, and posttraumatic stress disorder. Despite increased use of long-term acute care hospitals for critically ill patients, little is known about the impact of long-term hospitalization on patients’ family members.

Objectives
To examine indications of post–intensive care syndrome, coping strategies, and health-related quality of life among family decision makers during and after patients’ long-term hospitalization.

Methods
A single-center, prospective, longitudinal descriptive study was undertaken of family decision makers of adult patients admitted to long-term acute care hospitals. Indications of post–intensive care syndrome and coping strategies were measured on the day of hospital admission and 30 and 60 days later. Health-related quality of life was measured by using the Short Form-36, version 2, at admission and 60 days later.

Results
The sample consisted of 30 family decision makers. On admission, 27% reported moderate to severe anxiety, and 20% reported moderate to severe depression. Among the decision makers, 10% met criteria for a provisional diagnosis of posttraumatic stress disorder. At admission, the mean physical summary score for quality of life was 47.8 (SD, 9.91) and the mean mental summary score was 48.00 (SD, 10.28). No significant changes occurred during the study period. Problem-focused coping was the most frequently used coping strategy at all time points.

Conclusion
Family decision makers of patients in long-term acute care hospitals have a significant prevalence of indications of post–intensive care syndrome.
Comparison of ozone profiles and influences from the tertiary ozone maximum in the night-to-day ratio above Switzerland
Authors: Moreira Lorena , Hocke Klemens , Kämpfer Niklaus 
Published: September 2017

Abstract. Stratospheric and middle-mesospheric ozone profiles above Bern, Switzerland (46.95° N, 7.44° E; 577 m) have been continually measured by the GROMOS (GROund-based Millimeter-wave Ozone Spectrometer) microwave radiometer since 1994. GROMOS is part of the Network for the Detection of Atmospheric Composition Change (NDACC). A new version of the ozone profile retrievals has been developed with the aim of improving the altitude range of retrieval profiles. GROMOS profiles from this new retrieval version have been compared to coincident ozone profiles obtained by the satellite limb sounder Aura Microwave Limb Sounder (MLS). The study covers the stratosphere and middle mesosphere from 50 to 0.05 hPa (from 21 to 70 km) and extends over the period from July 2009 to November 2016, which results in more than 2800 coincident profiles available for the comparison. On average, GROMOS and MLS comparisons show agreement generally over 20 % in the lower stratosphere and within 2 % in the middle and upper stratosphere for both daytime and nighttime, whereas in the mesosphere the mean relative difference is below 40 % during the daytime and below 15 % during the nighttime. In addition, we have observed the annual variation in nighttime ozone in the middle mesosphere, at 0.05 hPa (70 km), characterized by the enhancement of ozone during wintertime for both ground-based and space-based measurements. This behaviour is related to the middle-mesospheric maximum in ozone (MMM).
Target categorization of aerosol and clouds by continuous multiwavelength-polarization lidar measurements
Authors: Baars Holger , Seifert Patric , Engelmann Ronny , Wandinger Ulla 
Published: September 2017

Abstract. Absolute calibrated signals at 532 and 1064 nm and the depolarization ratio from a multiwavelength lidar are used to categorize primary aerosol but also clouds in high temporal and spatial resolution. Automatically derived particle backscatter coefficient profiles in low temporal resolution (30 min) are applied to calibrate the lidar signals. From these calibrated lidar signals, new atmospheric parameters in temporally high resolution (quasi-particle-backscatter coefficients) are derived. By using thresholds obtained from multiyear, multisite EARLINET (European Aerosol Research Lidar Network) measurements, four aerosol classes (small; large, spherical; large, non-spherical; mixed, partly non-spherical) and several cloud classes (liquid, ice) are defined. Thus, particles are classified by their physical features (shape and size) instead of by source. The methodology is applied to 2 months of continuous observations (24 h a day, 7 days a week) with the multiwavelength-Raman-polarization lidar PollyXT during the High-Definition Clouds and Precipitation for advancing Climate Prediction (HD(CP)2) Observational Prototype Experiment (HOPE) in spring 2013. Cloudnet equipment was operated continuously directly next to the lidar and is used for comparison. By discussing three 24 h case studies, it is shown that the aerosol discrimination is very feasible and informative and gives a good complement to the Cloudnet target categorization. Performing the categorization for the 2-month data set of the entire HOPE campaign, almost 1 million pixel (5 min  ×  30 m) could be analysed with the newly developed tool. We find that the majority of the aerosol trapped in the planetary boundary layer (PBL) was composed of small particles as expected for a heavily populated and industrialized area. Large, spherical aerosol was observed mostly at the top of the PBL and close to the identified cloud bases, indicating the importance of hygroscopic growth of the particles at high relative humidity. Interestingly, it is found that on several days non-spherical particles were dispersed from the ground into the atmosphere.