bluuebunny/crossref_metadata_2025_split huggingface dataset:
Sample Processing and Stability for Urine Biomarker Studies
Authors: Chang Crystal , Obeid Wassim , Thiessen-Philbrook Heather , Parikh Chirag R 
Published: June 2021

Abstract

Background
Current methods of processing and storing urine samples have not been compared systematically to determine optimal conditions for advancing research on urinary biomarkers. Often, preanalytical handling is nonideal, especially considering the COVID-19 pandemic; consequently, we compared the effects of different short-term storage and processing methods on urinary biomarker measurements.

Methods
Spot urine samples were collected via a Foley catheter from 20 hospitalized patients from the Yale New Haven Hospital within 48 hours postcardiac surgery. The effects of 3 urine storage and processing methods on biomarkers were tested: (a) 48-hour temporary storage at 4 °C prior to freezing at −80 °C, (b) 48-hour temporary storage at 25 °C prior to freezing at −80 °C, and (c) no centrifugation and immediate storage at −80 °C. Established Meso-Scale Device assay methods were used to measure the urine concentrations of 18 biomarkers: interferon gamma (IFN-ɣ), interleukin (IL)-10, IL-12p70, IL-13, IL-1β, IL-2, IL-4, IL-6, IL-8, IL-18, tumor necrosis factor alpha (TNF-α), epidermal growth factor (EGF), neutrophil gelatinase-associated lipocalin (NGAL), osteopontin (OPN), uromodulin (UMOD), kidney injury molecule-1 (KIM-1), monocyte chemoattractant protein-1 (MCP-1), and chitinase-3-like protein 1 (YKL-40).

Results
Measurements of most biomarkers investigated remained stable after temporary storage at 4 °C. IL-6, IL-8, KIM-1, MCP-1, YKL-40, EGF, and NGAL were stable across all 3 processing conditions. IL-12p70 and IL-4 demonstrated significant differences in all tested conditions compared to the reference standard.

Conclusions
We identified several notable biomarkers that are robust to variations in preanalytical techniques and can be reliably investigated with nonideal handling conditions.
An Experimental Evaluation of Alternative Methods for Case Prioritization in Responsive Survey Design
Authors: West Brady T , Chang Wen , Zmich Alexa 
Published: June 2021

Abstract
Growing reluctance of households to participate in surveys has led to a variety of methodological efforts to combat this phenomenon. Several organizations employ case prioritization in a responsive survey design framework, dedicating increased effort to specific subgroups of sampled cases during certain data collection phases. For example, some surveys may prioritize subgroups defined by age and/or race/ethnicity if balanced response rates across these subgroups are important for minimizing nonresponse bias. Unfortunately, no methodological studies to date have identified optimal approaches for applying this increased effort to prioritized cases. This study experimentally examined three alternative methods for case prioritization in the National Survey of Family Growth: simply flagging the cases to receive increased effort in the sample management system (a “standard” method), developing tailored approaches to working the prioritized cases, and no prioritization (a “control” method). In the “tailored” method, which was designed to provide the interviewers with more guidance than simple “flagging,” interviewers worked with their supervisors to develop tailored strategies for how to best work each case within the prioritized subgroup. We find that both prioritization methods improved response rates and led to significant reductions in calling effort per completed case, with the “flagging” approach working particularly well. Given the additional costs associated with the “tailored” method, the results of our experiment provide support for a “hybrid” case prioritization approach that combines optimal features of these two methods.
The development of central nociceptive processing and descending modulation of pain
Authors: Fitzgerald Maria 
Published: June 2021

Abstract
Newborn mammals display robust responses to noxious or tissue-damaging stimulation. These nociceptive or “pain” responses arise from neural activity at different levels of the central nervous system. Protective reflex movements and physiological reactions mediated by spinal cord and brainstem circuits are essential for the preservation of life and well-being but should not be equated with pain awareness. The unique sensation of pain and its unpleasant, threatening quality requires activity in the cortical and subcortical regions of the brain. These brain regions also have the potential to actively increase or decrease pain experience by exerting top-down control of spinal cord and brainstem nociceptive circuits. This chapter summarizes our current knowledge of the development of central nociceptive pathways in the young mammalian brain and the postnatal maturation of top-down pain control. It aims to provide a scientific, mechanistic understanding of infant and childhood pain experience, and their ability to cope with painful events.
Coronal properties of low-mass Population III stars and the radiative feedback in the early universe
Authors: Washinoue Haruka , Suzuki Takeru K 
Published: June 2021

ABSTRACT
We systematically investigated the heating of coronal loops on metal-free stars with various stellar masses and magnetic fields by magnetohydrodynamic simulations. It is found that the coronal property is dependent on the coronal magnetic field strength Bc because it affects the difference of the non-linearity of the Alfvénic waves. Weaker Bc leads to cooler and less dense coronae because most of the input waves dissipate in the lower atmosphere on account of the larger non-linearity. Accordingly EUV and X-ray luminosities also correlate with Bc, while they are emitted in a wide range of the field strength. Finally, we extend our results to evaluating the contribution from low-mass Population III coronae to the cosmic reionization. Within the limited range of our parameters on magnetic fields and loop lengths, the EUV and X-ray radiations give a weak impact on the ionization and heating of the gas at high redshifts. However, there still remains a possibility of the contribution to the reionization from energetic flares involving long magnetic loops.
Short gamma-ray burst jet propagation in binary neutron star merger environments
Authors: Pavan Andrea , Ciolfi Riccardo , Kalinani Jay V , Mignone Andrea 
Published: June 2021

ABSTRACT
The multimessenger event GW170817/GRB 170817A confirmed that binary neutron star (BNS) mergers can produce short gamma-ray burst (SGRB) jets. This evidence promoted new investigations on the mechanisms through which a BNS merger remnant can launch such a powerful relativistic outflow and on the propagation of the latter across the surrounding post-merger environment. In particular, great strides have been made in jet propagation models, establishing connections between the initial jet launching conditions, including the incipient jet launching time (with respect to merger) and the injection parameters, and the observable SGRB prompt and afterglow emission. However, present semi-analytical models and numerical simulations (with one notable exception) adopt simple handmade prescriptions to account for the post-merger environment, lacking a direct association with any specific merging BNS system. Here, we present the first three-dimensional relativistic hydrodynamics simulations of incipient SGRB jets propagating through a post-merger environment that is directly imported from the outcome of a previous general relativistic BNS merger simulation. Our results show that the evolution and final properties of the jet can be largely affected by the anisotropies and the deviations from axisymmetry and homologous expansion characterizing more realistic BNS merger environments. In addition, we find that the inclusion of the gravitational pull from the central compact object, often overlooked, can have a major impact. Finally, we consider different jet launching times referred to the same BNS merger model and discuss the consequences for the ultimate jet properties.
Gravitational waves as a probe of globular cluster formation and evolution
Authors: Romero-Shaw Isobel M , Kremer Kyle , Lasky Paul D , Thrane Eric , Samsing Johan 
Published: June 2021

ABSTRACT
Globular clusters are considered to be likely breeding grounds for compact binary mergers. In this paper, we demonstrate how the gravitational-wave signals produced by compact object mergers can act as tracers of globular cluster formation and evolution. Globular cluster formation is a long-standing mystery in astrophysics, with multiple competing theories describing when and how globular clusters formed. The limited sensitivity of electromagnetic telescopes inhibits our ability to directly observe globular cluster formation. However, with future audio-band detectors sensitive out to redshifts of z ≈ 50 for GW150914-like signals, gravitational-wave astronomy will enable us to probe the Universe when the first globular clusters formed. We simulate a population of binary black hole mergers from theoretically motivated globular cluster formation models, and construct redshift measurements consistent with the predicted accuracy of third-generation detectors. We show that we can locate the peak time of a cluster formation epoch during reionization to within 0.05 Gyr after 1 yr of observations. The peak of a formation epoch that coincides with the Universal star formation rate can be measured to within 0.4–10.5 Gyr after 1 yr of observations, depending on the relative weighting of the model components.
Detection of the LMC-induced sloshing of the Galactic halo
Authors: Erkal Denis , Deason Alis J , Belokurov Vasily , Xue Xiang-Xiang , Koposov Sergey E , Bird Sarah A , Liu Chao , Simion Iulia T , Yang Chengqun , Zhang Lan , Zhao Gang 
Published: June 2021

ABSTRACT
A wealth of recent studies have shown that the LMC is likely massive, with a halo mass &gt;1011 M⊙. One consequence of having such a nearby and massive neighbour is that the inner Milky Way is expected to be accelerated with respect to our Galaxy’s outskirts (beyond ∼30 kpc). In this work, we compile a sample of ∼500 stars with radial velocities in the distant stellar halo, rGC &gt; 50 kpc, to test this hypothesis. These stars span a large fraction of the sky and thus give a global view of the stellar halo. We find that stars in the Southern hemisphere are on average blueshifted, while stars in the North are redshifted, consistent with the expected, mostly downwards acceleration of the inner halo due to the LMC. We compare these results with simulations and find the signal is consistent with the infall of a 1.5 × 1011 M⊙ LMC. We cross-match our stellar sample with Gaia DR2 and find that the mean proper motions are not yet precise enough to discern the LMC’s effect. Our results show that the Milky Way is significantly out of equilibrium and that the LMC has a substantial effect on our Galaxy.
A Dyson sphere around a black hole
Authors: Hsiao Tiger Yu-Yang , Goto Tomotsugu , Hashimoto Tetsuya , Santos Daryl Joe D , On Alvina Y L , Kilerci-Eser Ece , Wong Yi Hang Valerie , Kim Seong Jin , Wu Cossas K-W , Ho Simon C-C , Lu Ting-Yi 
Published: June 2021

ABSTRACT
The search for extraterrestrial intelligence (SETI) has been conducted for nearly 60 yr. A Dyson sphere, a spherical structure that surrounds a star and transports its radiative energy outwards as an energy source for an advanced civilization, is one of the main targets of SETI. In this study, we discuss whether building a Dyson sphere around a black hole is effective. We consider six energy sources: (i) the cosmic microwave background, (ii) the Hawking radiation, (iii) an accretion disc, (iv) Bondi accretion, (v) a corona, and (vi) relativistic jets. To develop future civilizations (for example, a Type II civilization), $4\times 10^{26}\, {\rm W}(1\, {\rm L_{\odot }})$ is expected to be needed. Among (iii) to (vi), the largest luminosity can be collected from an accretion disc, reaching $10^{5}\, {\rm L_{\odot }}$, enough to maintain a Type II civilization. Moreover, if a Dyson sphere collects not only the electromagnetic radiation but also other types of energy (e.g. kinetic energy) from the jets, the total collected energy would be approximately 5 times larger. Considering the emission from a Dyson sphere, our results show that the Dyson sphere around a stellar-mass black hole in the Milky Way ($10\, \rm kpc$ away from us) is detectable in the ultraviolet $(\rm 10{-}400\, {\rm nm)}$, optical $(\rm 400{-}760\, {\rm nm)}$, near-infrared ($\rm 760\, {\rm nm}{-}5\, {\rm \mu m}$), and mid-infrared ($\rm 5{-}40\, {\rm \mu m}$) wavelengths via the waste heat radiation using current telescopes such as Galaxy Evolution Explorer Ultraviolet Sky Surveys. Performing model fitting to observed spectral energy distributions and measuring the variability of radial velocity may help us to identify these possible artificial structures.
Magneto-elastic equilibrium of a neutron star crust
Authors: Kojima Yasufumi , Kisaka Shota , Fujisawa Kotaro 
Published: June 2021

ABSTRACT
We examine the equilibrium of a magnetized neutron star crust. We calculate axially symmetric models in which an elastic force balances solenoidal motion driven by a Lorentz force. A large variety of equilibrium models are allowed by incorporating the elastic shear deformation; in addition, toroidal-magnetic-field-dominated models are available. These results remarkably differ from those in barotropic fluid stars. We demonstrate some models wherein the magnetic energy exceeds the elastic energy. The excess comes from the fact that a large amount of magnetic energy is associated with the irrotational part of the magnetic force, which is balanced with gravity and pressure. It is sufficient for equilibrium models that the minor solenoidal part is balanced by a weak elastic force. We find that the elasticity in the crust plays an important role on the magnetic field confinement. Further, we present the spatial distribution of the shear stress at the elastic limit, by which the crust-fracture location can be identified. The result has useful implications for realistic crust-quake models.
Pulsating iron spectral features in the emission of X-ray pulsar V 0332+53
Authors: Bykov S D , Filippova E V , Gilfanov M R , Tsygankov S S , Lutovinov A A , Molkov S V 
Published: June 2021

ABSTRACT
We present results of phase- and time-resolved study of iron spectral features in the emission of the Be/X-ray transient pulsar V 0332+53 during its type II outburst in 2004 using archival RXTE/PCA data. Coherent pulsations of both fluorescent iron line at ≈6.4 keV and neutral iron K-edge at ≈7.1 keV have been detected throughout the entire outburst. The pulsating iron K-edge is reported for the first time for this object. Near the peak of the outburst, the 3–12 keV pulse profile shows two deep, Fmax/Fmin ∼ 2, and narrow dips of nearly identical shape, separated by exactly Δϕ = 0.5 in phase. The dip spectra are nearly identical to each other and very similar in shape to the spectra outside the dips. The iron K-edge peaks at the phase intervals corresponding to the dips, although its optical depth τK ∼ 0.05 is by far insufficient to explain the dips. The iron line shows pulsations with a complex pulse profile without any obvious correlation with the total flux or optical depth of the K-edge. Accounting for the component associated with reprocessing of the pulsar emission by the surface of the donor star and circumstellar material, we find a very high pulsation amplitude of the iron line flux, Fmax/Fmin ∼ 10. We demonstrate that these properties of V 0332+53 cannot be explained by contemporary emission models for accreting X-ray pulsars and speculate about the origin of the observed iron spectral features.
Simulating cosmic structure formation with the gadget-4 code
Authors: Springel Volker , Pakmor Rüdiger , Zier Oliver , Reinecke Martin 
Published: June 2021

ABSTRACT
Numerical methods have become a powerful tool for research in astrophysics, but their utility depends critically on the availability of suitable simulation codes. This calls for continuous efforts in code development, which is necessitated also by the rapidly evolving technology underlying today’s computing hardware. Here, we discuss recent methodological progress in the gadget code, which has been widely applied in cosmic structure formation over the past two decades. The new version offers improvements in force accuracy, in time-stepping, in adaptivity to a large dynamic range in time-scales, in computational efficiency, and in parallel scalability through a special MPI/shared-memory parallelization and communication strategy, and a more-sophisticated domain decomposition algorithm. A manifestly momentum conserving fast multipole method (FMM) can be employed as an alternative to the one-sided TreePM gravity solver introduced in earlier versions. Two different flavours of smoothed particle hydrodynamics, a classic entropy-conserving formulation and a pressure-based approach, are supported for dealing with gaseous flows. The code is able to cope with very large problem sizes, thus allowing accurate predictions for cosmic structure formation in support of future precision tests of cosmology, and at the same time is well adapted to high dynamic range zoom-calculations with extreme variability of the particle number density in the simulated volume. The gadget-4 code is publicly released to the community and contains infrastructure for on-the-fly group and substructure finding and tracking, as well as merger tree building, a simple model for radiative cooling and star formation, a high dynamic range power spectrum estimator, and an initial condition generator based on second-order Lagrangian perturbation theory.
Binary neutron star merger in common envelope jets supernovae
Authors: Soker Noam 
Published: June 2021

ABSTRACT
I explore a triple-star scenario where a tight neutron star (NS)–NS binary system enters the envelope of a red supergiant (RSG) star and spirals-in towards its core. The two NSs accrete mass through accretion discs and launch jets that power a very luminous and long transient event, a common envelope jets supernova (CEJSN) event. Dynamical friction brings the two NSs to merge either in the RSG envelope or core. The total energy of the event, radiation and kinetic, is $\gtrsim 10^{52} {~\rm erg}$. The light curve stays luminous for months to years and a signal of gravitational waves might be detected. The ejecta contain freshly synthesized r-process elements not only from the NS–NS merger as in kilonova events, but possibly also from the pre-merger jets that the NSs launch inside the core, as in the r-process CEJSN scenario. This scenario shortens the time to NS–NS merger compared with that of kilonovae, and might somewhat ease the problem of the NS–NS r-process scenario to account for r-process nucleosynthesis in the early Universe. I estimate the ratio of NS–NS merger in CEJSN events to core collapse supernova (CCSN) events to be ≲10−6 − 2 × 10−5. However, because they are much more luminous I expect their detection fraction to that of CCSNe to be much larger than this number. This study calls for considering this and similar CEJSN scenarios in binary and in triple-star systems when explaining peculiar and puzzling superluminous supernovae.
Timing and spectral variability of the high-mass X-ray pulsar GX 301−2 over orbital phases observed by Insight-HXMT
Authors: Ding Y Z , Wang W , Epili P R , Liu Q , Ge M Y , Lu F J , Qu J L , Song L M , Zhang S , Zhang S N 
Published: June 2021

ABSTRACT
We report the orbital X-ray variability of the high-mass X-ray binary (HMXB) GX 301−2. GX 301−2 underwent a spin-up process in 2018–2020 with the period evolving from ∼685–670 s. The energy-resolved pulse profiles of the pulsar at 1–60 keV varied from single-peaked and sinusoidal shapes to multipeaked ones across different orbital phases. Pulse fractions evolving over the orbit had negative correlations with the X-ray flux. The broad-band X-ray energy spectrum of the pulsar can be described with a partially covered negative–positive cut-off power-law continuum model. Near the periastron passage of the pulsar we found strong variation in the additional column density ($N_{\mathrm{H}_{2}}$), which correlated with variation of the flux. Curves of growth for both Fe Kα and Fe Kβ lines were plotted to investigate the distribution of matter around the neutron star. We also found evidence for two cyclotron absorption lines in the phase-averaged spectra in GX 301−2, with one line of 30–42 keV and the other line varying over 48–56 keV. The centroid energies of both lines show a similar relationship with X-ray luminosity: positive correlation in the lower luminosity range, and a negative relation above a critical luminosity of $10^{37}\, \rm erg\, s^{-1}$. We estimate the surface magnetic field of the neutron star in GX 301−2 to be ∼(0.5–2) × 1013 G. The two cyclotron line energies have a nearly fixed ratio of ∼1.63 while having a low strength ratio (∼0.05), suggesting that these two features may actually be one line.
The near-UV transit of HD 189733b with the XMM–Newton optical monitor
Authors: King George W , Corrales Lía , Wheatley Peter J , Lavvas Panayotis , Steinrueck Maria E , Bourrier Vincent , Ehrenreich David , Lecavelier des Etangs Alain , Louden Tom 
Published: June 2021

ABSTRACT
We present analysis of XMM–Newton optical monitor observations in the near-ultraviolet of HD 189733, covering 20 primary transits of its hot Jupiter planet. The transit is clearly detected with both the UVW2 and UVM2 filters, and our fits to the data reveal transit depths in agreement with that observed optically. The measured depths correspond to radii of $1.059^{+0.046}_{-0.050}$ and $0.94^{+0.15}_{-0.17}$ times the optically measured radius (1.187 RJ at 4950 Å) in the UVW2 and UVM2 bandpasses, respectively. We also find no statistically significant variation in the transit depth across the 8 yr baseline of the observations. We rule out extended broad-band absorption towards or beyond the Roche lobe at the wavelengths investigated, although observations with higher spectral resolution are required to determine if absorption out to those distances from the planet is present in individual near-UV lines.
The importance of galaxy formation histories in models of reionization
Authors: Mirocha Jordan , La Plante Paul , Liu Adrian 
Published: June 2021

ABSTRACT
Upcoming galaxy surveys and 21-cm experiments targeting high redshifts z ≳ 6 are highly complementary probes of galaxy formation and reionization. However, in order to expedite the large-volume simulations relevant for 21-cm observations, many models of galaxies within reionization codes are entirely subgrid and/or rely on halo abundances only. In this work, we explore the extent to which resolving and modelling individual galaxy formation histories affects predictions both for the galaxy populations detectable by upcoming surveys and the signatures of reionization accessible to upcoming 21-cm experiments. We find that a common approach, in which galaxy luminosity is assumed to be a function of halo mass only, is biased with respect to models in which galaxy properties are evolved through time via semi-analytic modelling and thus reflective of the diversity of assembly histories that naturally arise in N-body simulations. The diversity of galaxy formation histories also results in scenarios in which the brightest galaxies do not always reside in the centres of large-ionized regions, as there are often relatively low-mass haloes undergoing dramatic, but short-term, growth. This has clear implications for attempts to detect or validate the 21-cm background via cross-correlation. Finally, we show that a hybrid approach – in which only haloes hosting galaxies bright enough to be detected in surveys are modelled in detail, with the rest modelled as an unresolved field of haloes with abundance related to large-scale overdensity – is a viable way to generate large-volume ‘simulations‘ well suited to wide-area surveys and current-generation 21-cm experiments targeting relatively large k ≲ 1 h Mpc−1 scales.