bluuebunny/crossref_metadata_2025_split huggingface dataset:
Antimicrobial and Biofilm Inhibitory Activity of Nanoparticles Against Clinical Isolates from Urinary Tract Infection
Authors: Ashwak Jasim Kzar  
Published: January 2021

At these days nanoparticles (NPs) are used as antibacterial due to its have chemical-physical addition to
biological effect. A big group of microbial cells adhering to a surface are called biofilm. Exposure to nano
particles such as (Ag, Al2O3, Ni) may prevent colonization of new bacteria onto the biofilm. In the present
research we have analyze whether the biofilm formation of some isolates of pathogenic bacteria could be
influenced by NPs. Also we examined the susceptibility of the isolates to some antibiotics in combination
with Ag, Al2O3 and Ni nanoparticles. (50) Strains of isolated K. pneumonia have been examine from patients
with urinary tract infection were collected from Education of Baghdad hospitals in Iraq. Serial dilution of
Tube method to determination of MIC and MBEC for Nanoparticles against isolates was done. Biofilm
formation was evaluated by micro titer plates. Additionally. disc diffusion method was used to assay the
various antibiotics and combinations for bactericidal activity against the isolates. The results showed that
about 97% of the strains were capable to form of structure biofilms. More than 82% about of strains showed
resistance to commonly used antibiotics. Antibiotics and antimicrobials from mixed nanoparticles were
higher than compared to nanoparticles alone. Therefore, a synergistic effect was observed between silver -
Nickel nanoparticles and silver - aluminum oxide nanoparticles in to inhibiting the growth of K. pneumonia
strains. Furthermore, cytotoxicity activity of Ag NPs against Neuro-2a cells was higher than Al2O3 NPs. The
results suggest that nanoparticles can be used as antimicrobial agents for therapeutic to treat urinary tract
infections caused by K. pneumoniae.
Study of Pedestrian Injuries and Fatalities in Maharashtra Population
Authors: Mohammed Abdul Mateen  
Published: January 2021

Background- Pedestrians are the common road users India, with increasing traffic on road has lead to
injuries and fatalities. The incidences of fatalities are higher than drivers of four wheelers or motor cyclist.
Method- Out of 734 Injuries and 213 fatalities were recorded in medico-legal records. The causes, types of
injuries age group, causes of fatalities were also studied.
Results- The major age group was between 10-20 had 210(28.6%) followed by age group 61-70 had
142(19.3%). The major history of pedestrian were 210(28.6%) alcoholic, followed by 173(23.5%) were
busy in mobile speaking. The major fractures were 69(9.40%) fractions of sternum, 176(23.9%) fracture
of skull. 185(25.2%) intra-cranial hemorrhage. The major causes of fatalities were hemorrhage and shock
138(64.7%), followed by head injuries57(26.7%).
Effect of Different Shoe Lacing Pattern on Different Types of Foot in Recreational Runners
Authors: Rushikesh Rajendra Mangale, Amrutkuvar Rayjade  
Published: January 2021

Background: There has been an increase in the overall prevalence of obesity in India. There has been a
26% rise in the obesity among the young adults of India. At the same time, an awareness about fitness and
health has also been on a rise in our country.Jogging and running have been on a rise in popularity among
the youth of India. Heel-to-toe drop, styles of running, brand, fit and shoe lacing are some other factors that
affect running. Out of these shoe lacing is one of the simplest factors to modify. It can be done by anybody
and is an extremely cost effective measure.
Methodology: An experimental study is being conducted with a sample size of 33 subject in karad. The
population under study is Recreational runners age group of 20-40 years both male and female subjects. VAS
and Foot Posture Index were the outcome measures used.
Result: There was a significant effect of modifying shoe lacing patterns on FFI scores. (p=<0.001) There was
also a significant effect on FPS (p <0.001) and FDS (p <0.001) subscales whereas there was no significant
effect on ALS subscale (p >0.05). A significant decrease in pain was also noted. (p <0.05)
Conclusion On the basis of the results of the study, it was concluded that there was a significant effect of
modifying shoe lacing patterns on amateur runners.
Bipolar Disorder: A Major Setback in Substance Abuse
Authors: Jeetendra Kumar Gupta  
Published: January 2021

Substance abuse refers to harmful or precarious use of psychoactive substances, including alcohol, cannabis
and illicit drugs. It is directly and indirectly responsible for millions of morbidities each year. It is a
crucial snag of present generation. Illegitimate use of psychoactive drugs can lead to lunatic illnesses. The
prevalence of psychotic disorders among patients with substance abuse has attended noticeable magnitude.
This study indicates that bipolar disorder is more likely to occur in patients with substance abuse. Chronic
substance abuse can lead to down-regulation of concerned receptors as well as erosion of gray matter in the
prefrontal cortex of brain. Hence, it would be imperative to address bipolar disorder from the perspective of
potential and progressive adverse effect of substance abuse. The observation of study indicates that bipolar
disorder is more prevalent in cannabis, alcohol and cocaine abuse cases. Drug abuse disorders are associated
with impaired outcome of manic depression maladies that brings severe high or low moods, thinking and
behavior.
Assessment of Patient’s Knowledge Regarding Hemodialysis Therapy at Imam Hussein Medical City in Holly Karbala Governorate
Authors: Hussam Abbas Dawood  
Published: January 2021

Background: Descriptive and analytical study in which evaluation approach applied in order to achieve
the objectives of the study mentioned at the beginning of the search. The study began in 2 April 2016 to
21 June 2017,The research was conducted in order to identify hemodialysis patients knowledge regarding
hemodialysis therapy at Imam Hussein medical city in holly Karbala Governorate
Objectives: to assess hemodialysis patients knowledge about hemodialysis therapy, To find out the
relationship between hemodialysis knowledge and some variables such as: age, gender, level of education.
Methods: This Descriptive and analytical study was conducted at Imam Hussein medical city in the province
of Karbala, Iraq, from 1 October 2017 to 1 April 2018, use to to identify hemodialysis patients knowledge
regarding hemodialysis therapy. SPSS 21 was used for statistical analysis.
Results: shown on Results of the study that Highest percent of the study samples was samples age (50 or
more) years old, According to the gender, the study sample were male and female, equal percent and number
was (50-50%), Most of the study sample low educational levels, Most of them had married, Finally the
general knowledge level of Imam Hussein medical city regarding hemodialysis therapy is High.
Conclusion: Highest percent of the study samples was samples age (50 or more) years old, According to
the gender, the study sample were male and female, equal percent and number was (50-50%), Finally the
general knowledge level of Imam Hussein medical city regarding hemodialysis therapy is High.
Study of Immunological Parameters, Hematologic Outcomes And Epidemiology Features of Renal Dysfunction Frequently in Karbala Province, Iraq
Authors: Alyaa Aziz Gubiar Al-Nasrallah  
Published: January 2021

Renal failure or dysfunction: A disease occurs by a severe weakness in one kidney or both, they lose ability
to do their functions effectively, resulting in the body’s inability to remove waste and fluids, Leading to a
significant changes in chemistry of blood and body fluid.
The study occurred in Karbala province where study samples were collected, which included (124). Samples
divided in (64) patients and (60) control, patients had another division according to sex (44) male and (20)
female. Immunologic parameters include (kidney injury molecules (KIM-1), pro-inflammatory TNF-?, IgG
antibodies) Elabscience Kit, concentration in serum was massacred by (ELISA) Technique and hematologic
test measured automatically by (Humlate plus-1 Device).
The results showed increase in kidney injury in age groups beyond the age of 40 years. A significantly higher
incidence of disease among males more than females. Results show significant statically variations in serum
levels:
1- kidney injury molecules (KIM-1) levels was increased in serum in patients significantly compare with
control.
2- (TNF-?) levels was increased in patients than control.
3- IgG levels decreased in patients than control.
Another routine tests occurs to patients to know the effects of disease on blood variations, the test was
included CBC count the results show CBC tests: (WBC, MHC, MCHC, RDWS, RDWC, PLT, PCT, PDWS,
PDWC, P-LCC and P-LCR) have no significant differentials while CBC tests: (LYM., MON., GRA., RBC.,
HGB., HCT., MCV, MPV) which decrease in patient compare with control significantly.
Increase kidney injury and inflammatory in serum patients with disease, by measured some parameters levels
in sera as indicators for disease progression and decrease in some antibodies such as IgG concentration of in
sera, as well as the hematologic tests referrer to disease may associated with anemia.
Three-dimensional Structure and Dust Extinction in the Small Magellanic Cloud
Authors: Yanchulova Merica-Jones Petia , Sandstrom Karin M. , Johnson L. Clifton , Dolphin Andrew E. , Dalcanton Julianne J. , Gordon Karl , Roman-Duval Julia , Weisz Daniel R. , Williams Benjamin F. 
Published: January 2021

Abstract
We examine the three-dimensional structure and dust extinction properties in a ∼200 pc × 100 pc region in the southwest bar of the Small Magellanic Cloud (SMC). We model a deep Hubble Space Telescope optical color–magnitude diagram (CMD) of red clump and red giant branch stars in order to infer the dust extinction and galactic structure. We model the distance distribution of the stellar component with a Gaussian and find a centroid distance of 65.2 kpc (distance modulus μ = 19.07 mag) with an FWHM ≈ 11.3 kpc. This large extent along the line of sight reproduces results from previous studies using variable stars and red clump stars. Additionally, we find an offset between the stellar and dust distributions, with the dust on the near side relative to the stars by 3.22

kpc, resulting in a 73% reddened fraction of stars. Modeling the dust layer with a log-normal A

V
distribution indicates a mean extinction 〈A

V
〉 = 0.41 ± 0.09 mag. We also calculate A

V
/N

H
= 3.2–4.2 × 10−23 mag cm2 H−1, which is significantly lower than the Milky Way value but is comparable to previous SMC dust-to-gas ratio measurements. Our results yield the first joint dust extinction and 3D geometry properties in a key region in the SMC. This study demonstrates that CMD modeling can be a powerful tool to simultaneously constrain dust extinction and geometry properties in nearby galaxies.
Scintillation Arcs in Pulsar B0450–18
Authors: Rickett Barney J. , Stinebring Dan R. , Zhu Hengrui , Minter Anthony H. 
Published: January 2021

Abstract
We report on Green Bank Telescope observations of interstellar scintillation from the pulsar B0450−18 at 340 and 825 MHz, revealing prominent arcs in the secondary spectra at both frequencies. The arcs are successfully modeled by one-dimensional angular brightness distributions, estimated by two independent techniques. The distributions do not follow the expected shape for a Kolmogorov plasma density spectrum, and their overall angular widths follow a scaling law, versus frequency, that is slightly slower than the inverse square law expected from plasma dispersion. They also exhibit discrete peaks that are the cause of the occasional reverse sub-arcs. Over a narrow (5%) frequency range these peaks do not participate in the overall spreading, having angular positions that are fixed on the sky. However, the peaks do evolve over a wider range of frequencies and cannot be traced from 825 to 340 MHz. Our conclusions add further evidence for a widespread distribution of highly localized regions of interstellar plasma with small-scale structure that is either elongated or flattened.
The First Mid-infrared Detection of HNC in the Interstellar Medium: Probing the Extreme Environment toward the Orion Hot Core
Authors: Nickerson Sarah , Rangwala Naseem , Colgan Sean W. J. , DeWitt Curtis , Huang Xinchuan , Acharyya Kinsuk , Drozdovskaya Maria , Fortenberry Ryan C. , Herbst Eric , Lee Timothy J. 
Published: January 2021

Abstract
We present the first mid-infrared (MIR) detections of HNC and

in the interstellar medium, and numerous resolved HCN rovibrational transitions. Our observations span 12.8–22.9 μm toward the hot core Orion IRc2, obtained with the Echelon-Cross-Echelle Spectrograph aboard the Stratospheric Observatory for Infrared Astronomy (SOFIA). In particular, ∼5 km s−1 resolution distinguishes individual rovibrational transitions of the HNC and HCN P, Q, and R branches; and the

R branch. This allows direct measurement of the species’ excitation temperatures, column densities, and relative abundances. HNC and

exhibit a local standard of rest velocity of −7 km s−1 that may be associated with an outflow from nearby radio source I and an excitation temperature of about 100 K. We resolve two velocity components for HCN, the primary component also being at −7 km s−1 with a temperature of 165 K. The hottest component, which had never before been observed, is at 1 km s−1 with a temperature of 309 K. This is the closest component to the hot core’s center measured to date. The derived

is below expectation for Orion’s Galactocentric distance, but the derived HCN/HNC = 72 ± 7 is expected for this extreme environment. Compared to previous sub-millimeter and millimeter observations, our SOFIA line survey of this region shows that the resolved MIR molecular transitions are probing a distinct physical component and isolating the chemistry closest to the hot core.
The Early Discovery of SN 2017ahn: Signatures of Persistent Interaction in a Fast-declining Type II Supernova
Authors: Tartaglia L. , Sand D. J. , Groh J. H. , Valenti S. , Wyatt S. D. , Bostroem K. A. , Brown P. J. , Yang S. , Burke J. , Chen T.-W. , Davis S. , Förster F. , Galbany L. , Haislip J. , Hiramatsu D. , Hosseinzadeh G. , Howell D. A. , Hsiao E. Y. , Jha S. W. , Kouprianov V. , Kuncarayakti H. , Lyman J. D. , McCully C. , Phillips M. M. , Rau A. , Reichart D. E. , Shahbandeh M. , Strader J. 
Published: January 2021

Abstract
We present high-cadence, comprehensive data on the nearby (D ≃ 33 Mpc) Type II supernova (SN II) 2017ahn, discovered within about one day of the explosion, from the very early phases after explosion to the nebular phase. The observables of SN 2017ahn show a significant evolution over the ≃470 days of our follow-up campaign, first showing prominent, narrow Balmer lines and other high-ionization features purely in emission (i.e., flash spectroscopy features), which progressively fade and lead to a spectroscopic evolution similar to that of more canonical SNe II. Over the same period, the decline of the light curves in all bands is fast, resembling the photometric evolution of linearly declining H-rich core-collapse SNe. The modeling of the light curves and early flash spectra suggests that a complex circumstellar medium surrounds the progenitor star at the time of explosion, with a first dense shell produced during the very late stages of its evolution that is swept up by the rapidly expanding ejecta within the first ∼6 days of the SN evolution, while signatures of interaction are observed also at later phases. Hydrodynamical models support the scenario in which linearly declining SNe II are predicted to arise from massive yellow super- or hypergiants depleted of most of their hydrogen layers.
Classification of High-resolution Solar Hα Spectra Using t-distributed Stochastic Neighbor Embedding
Authors: Verma Meetu , Matijevič Gal , Denker Carsten , Diercke Andrea , Dineva Ekaterina , Balthasar Horst , Kamlah Robert , Kontogiannis Ioannis , Kuckein Christoph , Pal Partha S. 
Published: January 2021

Abstract
The Hα spectral line is a well-studied absorption line revealing properties of the highly structured and dynamic solar chromosphere. Typical features with distinct spectral signatures in Hα include filaments and prominences, bright active-region plages, superpenumbrae around sunspots, surges, flares, Ellerman bombs, filigree, and mottles and rosettes, among others. This study is based on high-spectral resolution Hα spectra obtained with the Echelle spectrograph of the Vacuum Tower Telescope (VTT) located at Observatorio del Teide, Tenerife, Spain. The t-distributed stochastic neighbor embedding (t-SNE) is a machine-learning algorithm, which is used for nonlinear dimensionality reduction. In this application, it projects Hα spectra onto a two-dimensional map, where it becomes possible to classify the spectra according to results of cloud model (CM) inversions. The CM parameters optical depth, Doppler width, line-of-sight velocity, and source function describe properties of the cloud material. Initial results of t-SNE indicate its strong discriminatory power to separate quiet-Sun and plage profiles from those that are suitable for CM inversions. In addition, a detailed study of various t-SNE parameters is conducted, the impact of seeing conditions on the classification is assessed, results for various types of input data are compared, and the identified clusters are linked to chromospheric features. Although t-SNE proves to be efficient in clustering high-dimensional data, human inference is required at each step to interpret the results. This exploratory study provides a framework and ideas on how to tailor a classification scheme toward specific spectral data and science questions.
Unveiling the Architecture of a Pulsar–Binary Black Hole Triple System with Pulsar Arrival Time Analysis
Authors: Hayashi (林 利憲) Toshinori , Suto (須藤 靖) Yasushi 
Published: January 2021

Abstract
A large number of binary black holes (BBHs) with longer orbital periods are supposed to exist as progenitors of BBH mergers recently discovered with gravitational wave (GW) detectors. In our previous papers, we proposed to search for such BBHs in triple systems through the radial velocity modulation of the tertiary orbiting star. If the tertiary is a pulsar, high-precision and high-cadence observations of its arrival time enable an unambiguous characterization of the pulsar–BBH triples located at several kiloparsecs, which are inaccessible with the radial velocity of stars. The present paper shows that such inner BBHs can be identified through the short-term Rømer delay modulation, on the order of 10 ms for our fiducial case, a triple consisting of a 20 M
⊙ BBH and 1.4 M
⊙ pulsar with P
in = 10 days and P
out = 100 days. If the relativistic time delays are measured as well, one can determine basically all the orbital parameters of the triple. For instance, this method is applicable to inner BBHs of down to ∼1 hr orbital periods if the orbital period of the tertiary pulsar is around several days. Inner BBHs with ≲1 hr orbital period emit the GW detectable by future space-based GW missions, including LISA, DECIGO, and BBO, and very short inner BBHs with subsecond orbital period can be even probed by the existing ground-based GW detectors. Therefore, our proposed methodology provides a complementary technique to search for inner BBHs in triples, if they exist at all, in the near future.
Difference in Chemical Composition between the Bright and Faint Red Clump Stars in the Milky Way Bulge
Authors: Lim Dongwook , Lee Young-Wook , Koch Andreas , Hong Seungsoo , Johnson Christian I. , Kim Jaeyeon , Chung Chul , Mateo Mario , Bailey John I. 
Published: January 2021

Abstract
The double red clump (RC) observed in color–magnitude diagrams of the Milky Way bulge is at the heart of the current debate on the structure and formation origin of the bulge. This feature can be explained by the difference between the two RCs either in distance (“X-shaped scenario”) or in chemical composition (“multiple-population scenario”). Here we report our high-resolution spectroscopy for the RC and red giant branch stars in a high-latitude field (b ∼ −8.5°) of the bulge. We find a difference in [Fe/H] between the stars in the bright and faint RC regimes, in the sense that the bright stars are enhanced in [Fe/H] with respect to the faint stars by 0.149 ± 0.036 dex. The stars on the bright RC are also enhanced in [Na/Fe] but appear to be depleted in [Al/Fe] and [O/Fe], although more observations are required to confirm the significance of these differences. Interestingly, these chemical patterns are similar to those observed among multiple stellar populations in the metal-rich bulge globular cluster Terzan 5. In addition, we find a number of Na-rich stars, which would corroborate the presence of multiple populations in the bulge. Our results support an origin of the double RC from dissolved globular clusters that harbor multiple stellar populations. Thus, our study suggests that a substantial fraction of the outer bulge stars would have originated from the assembly of such stellar systems in the early phase of the Milky Way formation.
Non-Boussinesq Low-Prandtl-number Convection with a Temperature-dependent Thermal Diffusivity
Authors: Pandey Ambrish , Schumacher Jörg , Sreenivasan Katepalli R. 
Published: January 2021

Abstract
In an attempt to understand the role of the strong radial dependence of thermal diffusivity on the properties of convection in Sun-like stars, we mimic that effect in non-Oberbeck–Boussinesq convection in a horizontally extended rectangular domain (aspect ratio 16) by allowing the thermal diffusivity κ to increase with the temperature (as in the case of stars). Direct numerical simulations (i.e., numerical solutions of the governing equations by resolving up to the smallest scales without requiring any modeling) show that, in comparison with Oberbeck–Boussinesq simulations (two of which we perform for comparison purposes), the symmetry of the temperature field about the mid-horizontal plane is broken, whereas the velocity and heat flux profiles remain essentially symmetric. Our choice of κ(T), which resembles the variation in stars, results in a temperature field that loses its fine structures toward the hotter part of the computational domain, but the characteristic large scale of the turbulent thermal “superstructures,” which are structures whose size is typically larger than the depth of the convection domain, continues to be largely independent of the depth.
Removing Astrophysics in 21 cm Maps with Neural Networks
Authors: Villanueva-Domingo Pablo , Villaescusa-Navarro Francisco 
Published: January 2021

Abstract
Measuring temperature fluctuations in the 21 cm signal from the epoch of reionization and the cosmic dawn is one of the most promising ways to study the universe at high redshifts. Unfortunately, the 21 cm signal is affected by both cosmology and astrophysics processes in a nontrivial manner. We run a suite of 1000 numerical simulations with different values of the main astrophysical parameters. From these simulations we produce tens of thousands of 21 cm maps at redshifts 10 ≤ z ≤ 20. We train a convolutional neural network to remove the effects of astrophysics from the 21 cm maps and output maps of the underlying matter field. We show that our model is able to generate 2D matter fields not only that resemble the true ones visually but whose statistical properties agree with the true ones within a few percent down to scales ≃2 Mpc−1. We demonstrate that our neural network retains astrophysical information that can be used to constrain the value of the astrophysical parameters. Finally, we use saliency maps to try to understand which features of the 21 cm maps the network is using in order to determine the value of the astrophysical parameters.