bluuebunny/crossref_metadata_2025_split huggingface dataset:
Length of Stay Per Total Body Surface Area Burn: A Validation Study Using the National Burn Registry
Authors: Patterson Kelli N , Onwuka Amanda , Schwartz Dana M , Fabia Renata B , Thakkar Rajan K 
Published: August 2022

Abstract
A length of stay (LOS) of one day per percent total body surface area (TBSA) burn has been generally accepted but not validated in current pediatric burn studies. The primary objective of this study is to validate previous Pediatric Injury Quality Improvement Collaboration (PIQIC) findings by using a national burn registry to evaluate LOS per TBSA burn relative to burn mechanism, sociodemographic characteristics, and clinical factors which influence this ratio. We evaluated patients 0–18 years old who sustained a burn injury and whose demographics were submitted to the National Burn Registry (NBR) dataset from July 2008 through June 2018. Mixed effects generalized additive regression models were performed to identify characteristics associated with the LOS per TBSA burn ratio. Among 51,561 pediatric burn patients, 45% were Non-Hispanic White, 58% were male, and median age was 3.0 years old (IQR: 1.0, 9.0). The most common burn mechanism was scald (55.9%). The median LOS per TBSA burn ratio across all cases was 0.9 (IQR: 0.4, 1.75). In adjusted models, scald burns had a mean predicted LOS per TBSA burn value of 1.2 while chemical burns had the highest ratio (4.8). Non-Hispanic White patients had lower LOS per TBSA burn ratios than all other races and ethnicities (p &lt; .05). These data substantiate evidence on variance in LOS per TBSA burn relative to burn mechanism and race/ethnicity. Knowing these variations can guide expectations in hospital LOS for patients and families and help burn centers benchmark their clinical performance.
Extensive genome introgression between domestic ferret and European polecat during population recovery in Great Britain
Authors: Etherington Graham J , Ciezarek Adam , Shaw Rebecca , Michaux Johan , Croose Elizabeth , Haerty Wilfried , Di Palma Federica 
Published: August 2022

AbstractThe European polecat (Mustela putorius) is a mammalian predator which occurs across much of Europe east to the Ural Mountains. In Great Britain, following years of persecution the range of the European polecat contracted and by the early 1900s was restricted to unmanaged forests of central Wales. The European polecat has recently undergone a population increase due to legal protection and its range now overlaps that of feral domestic ferrets (Mustela putorius furo). During this range expansion, European polecats hybridized with feral domestic ferrets producing viable offspring. Here, we carry out population-level whole-genome sequencing on 8 domestic ferrets, 19 British European polecats, and 15 European polecats from the European mainland. We used a range of population genomics methods to examine the data, including phylogenetics, phylogenetic graphs, model-based clustering, phylogenetic invariants, ABBA-BABA tests, topology weighting, and Fst. We found high degrees of genome introgression in British polecats outside their previous stronghold, even in those individuals phenotyped as “pure” polecats. These polecats ranged from presumed F1 hybrids (gamma = 0.53) to individuals that were much less introgressed (gamma = 0.2). We quantify this introgression and find introgressed genes containing Fst outliers associated with cognitive function and sight.
Dynamic analysis of the single rotor-bearing system considering the comprehensive stiffness and damping
Authors: Ri CholUk , O RyongSik , Zhao Qiang , Chae ChungHyok , Sin YongIl , Sin Yongkon 
Published: August 2022

Abstract
The rotor system supported by the cylindrical roller bearings is widely used in various fields, such as aviation, space and machinery due to its importance. In study of the analysis of the vibration characteristics of the rotor system, it is important to accurately calculate the stiffness and damping of the cylindrical roller bearings. Therefore, in this paper, the dynamic characteristics of the simple rotor-bearing system were analyzed based on the new dynamic model of the rotor system considering the comprehensive stiffness and damping model of the cylindrical roller bearing. In consideration of the radial clearance of the cylindrical roller bearing, the radial load acting on the cylindrical roller bearing is derived and based on this, the Hertz contact stiffness model of the cylindrical roller bearing is obtained. After obtaining the oil film stiffness model of the cylindrical roller bearing according to the EHL theory, the comprehensive stiffness of the cylindrical roller bearing was calculated by combining the Hertz contact stiffness and the oil film stiffness of the cylindrical roller bearing. After a comprehensive damping model of the cylindrical roller bearing considering the radial clearance was created, a dynamic model of the simple rotor-bearing system was created based on the comprehensive stiffness and damping model of the cylindrical roller bearing. The dynamic characteristics of the simple rotor-bearing system were analyzed using the MATLAB program. The amplitude of the simple rotor-bearing system considering the comprehensive stiffness and damping was reduced by 18.2% compared to the case where it was not considered. This shows that the structure of the cylindrical roller bearing has a restraining effect on the unbalanced response of the rotor system.
Doxycycline responding illnesses in returning travellers with undifferentiated non-malaria fever: a European multicentre prospective cohort study
Authors: Camprubí-Ferrer Daniel , Oteo José Antonio , Bottieau Emmanuel , Genton Blaise , Balerdi-Sarasola Leire , Portillo Aránzazu , Cobuccio Ludovico , Van Den Broucke Steven , Santibáñez Sonia , Cadar Dániel , Rodriguez-Valero Natalia , Almuedo-Riera Alex , Subirà Carme , d'Acremont Valérie , Martinez Miguel J , Roldán Montserrat , Navero-Castillejos Jessica , Van Esbroeck Marjan , Muñoz Jose 
Published: August 2022

AbstractBackgroundDiagnosis of undifferentiated non-malaria fevers (NMF) in returning travellers is a great challenge. Currently, there is no consensus about the use of empirical antibiotics in returning travellers with undifferentiated NMF. Although studies in endemic areas showed that a wide range of pathogens implicated in undifferentiated NMF are treatable with doxycycline, the role of doxycycline in returning travellers with fever still has to be explored.MethodsProspective European multicentre cohort study of febrile international travellers (November 2017—November 2019). Immunological and molecular diagnostic techniques for doxycycline responding illnesses (DRI) agents such as Anaplasma phagocytophilum, spotted fever group Rickettsia spp., typhus group Rickettsia spp., Coxiella burnetii, Bartonella spp., Orientia tsutsugamushi, Borrelia miyamotoi, Borrelia recurrentis and Leptospira spp. were systematically performed in all patients with undifferentiated NMF. We estimated the prevalence and predictive factors of DRI in returning travellers with undifferentiated NMF.ResultsAmong 347 travellers with undifferentiated NMF, 106 (30·5%) were finally diagnosed with DRI. Only 57 (53·8%) of the 106 DRI infections were diagnosed by the standard of care. The main causes of DRI were: 55 (51·9%) Rickettsia spp., 16 (15·1%) C. burnetii; 15 (14·2%) Bartonella spp.; 13 (12·3%) Leptospira spp. and 10 (9·5%) A. phagocytophilum. The only predictive factor associated with DRI was presenting an eschar (aOR 39·52, 95%CI 4·85–322·18). Features of dengue such as retro-orbital pain (aOR 0·40, 95%CI 0·21–0·76) and neutropenia (aOR 0·41, 95%CI 0·21–0·79) were negatively associated with DRI.ConclusionsAlthough DRI are responsible for 30% of undifferentiated NMF cases in travellers, those are seldom recognized during the first clinical encounter. Empirical treatment with doxycycline should be considered in returning travellers with undifferentiated fever and negative tests for malaria and dengue, particularly when presenting severe illness, predictive factors for rickettsiosis or no features of dengue.
Revealing the dust grain polarization properties as a function of extinction and distance towards NGC 1893
Authors: Bijas N , Eswaraiah Chakali , Wang Jia-Wei , Jose Jessy , Chen Wen-Ping , Li Di , Lai Shih-Ping , Ojha D K 
Published: August 2022

ABSTRACT
Dust polarization observations at optical wavelengths help us to understand the dust grain properties and trace the plane-of-the-sky component of the magnetic field. In this study, we make use of the I-band polarization data acquired from AIMPOL along with the distances (d) and extinction (AV) data to study the variation of polarization fraction (P) as a function of AV and d towards the star-forming region, NGC 1893. We employ a broken power-law fit and Bayesian analysis on extinction (AV) versus polarization efficiency (P/AV) and distance (d) versus rate of polarization (P/d). We find that P/AV shows a break at an extinction of ∼0.9 mag, whereas P/d exhibits a break at a distance of ∼1.5 kpc. Based on these, we categorize the dust towards NGC 1893 into two populations: (i) foreground dust confined to AV &lt; ∼1 mag and distance up to ∼2 kpc and (ii) Perseus spiral arm dust towards NGC 1893 characterized with AV &gt; ∼1 mag and distance beyond ∼2 kpc. Foreground dust exhibits higher polarization efficiency but a lower polarization rate, whereas Perseus dust shows a lower polarization efficiency but a slightly higher polarization rate. Hence, we suggest that while polarization efficiency reveals the dust grain alignment, the rate of polarization infers about the distribution of dust grains towards NGC 1893. Further, we also shed a light on the spatial variation of intrinsic polarization and magnetic field orientation, and other parameters within the intracluster medium of NGC 1893.
Visualizing the pulsar population using graph theory
Authors: García C R , Torres Diego F , Patruno Alessandro 
Published: August 2022

ABSTRACTThe $P\dot{P}$ diagram is a cornerstone of pulsar research. It is used in multiple ways for classifying the population, understanding evolutionary tracks, identifying issues in our theoretical reach, and more. However, we have been looking at the same plot for more than five decades. A fresh appraisal may be healthy. Is the $P \dot{P}$-diagram the most useful or complete way to visualize the pulsars we know? Here we pose a fresh look at the information we have on the pulsar population. First, we use principal component analysis over magnitudes depending on the intrinsic pulsar’s timing properties (proxies to relevant physical pulsar features), to analyse whether the information contained by the pulsar’s period and period derivative is enough to describe the variety of the pulsar population. Even when the variables of interest depend on P and $\dot{P}$, we show that $P \dot{P}$ are not principal components. Thus, any distance ranking or visualization based only on P and $\dot{P}$ is potentially misleading. Next, we define and compute a properly normalized distance to measure pulsar nearness, calculate the minimum spanning tree of the population, and discuss possible applications. The pulsar tree hosts information about pulsar similarities that go beyond P and $\dot{P}$, and are thus naturally difficult to read from the $P\dot{P}$-diagram. We use this work to introduce the pulsar tree website containing visualization tools and data to allow users to gather information in terms of MST and distance ranking.
Detectability of satellites around directly imaged exoplanets and brown dwarfs
Authors: Lazzoni Cecilia , Desidera Silvano , Gratton Raffaele , Zurlo Alice , Mesa Dino , Ray Shrishmoy 
Published: August 2022

ABSTRACT
Satellites around substellar companions are a heterogeneous class of objects with a variety of different formation histories. Focusing on potentially detectable satellites around exoplanets and brown dwarfs (BDs), we might expect to find objects belonging to two main populations: planet-like satellites similar to Titan or the Galileian Satellites – likely formed within the scope of core accretion; and binary-like objects, formed within different scenarios, such as disc instability. The properties of these potential satellites would be very different from each other. Additionally, we expect that their characterization would provide insightful information about the history of the system. This is particularly important for planets/BDs discovered via direct imaging (DI) with ambiguous origins. In this paper, we review different techniques, applied to DI planets/BDs, that can be used to discover such satellites. This was achieved by simulating a population of satellites around the exoplanet β Pic b, which served as a test case. For each simulated satellite, the amplitude of DI, radial velocity, transit and astrometric signals, with respect to the planet, were retrieved and compared with the detection limits of current and future instruments. Furthermore, we compiled a list of 38 substellar companions discovered via DI to give a preliminary estimate on the probability of finding satellites extracted from the two populations mentioned above, with different techniques. This simplified approach shows that detection of planet-like satellites, though not strictly impossible, is very improbable. On the other hand, the detection of binary-like satellites is within the capabilities of current instrumentation.
The pre-He white dwarfs in eclipsing binaries – IV. WASP 1814+48 with multiperiodic pulsations
Authors: Lee Jae Woo , Hong Kyeongsoo , Kim Hye-Young , Park Jang-Ho 
Published: August 2022

ABSTRACT
For the EL CVn candidate 1SWASPJ181417.43+481117.0 (WASP 1814+48), we secured the first spectroscopic observations between 2015 April and 2021 March. Using the echelle spectra, the radial velocities (RVs) of the primary star were measured with its atmospheric parameters of Teff, 1 = 7770 ± 130 K and $v$1sin i = 47 ± 6 km s−1. We fitted our single-lined RVs and the TESS light curve simultaneously. From the binary modelling, we determined the following fundamental parameters for each component: M1 = 1.659 ± 0.048 M⊙, R1 = 1.945 ± 0.027 R⊙, and L1 = 12.35 ± 0.90 L⊙ for WASP 1814+48 A, and M2 = 0.172 ± 0.005 M⊙, R2 = 0.194 ± 0.005 R⊙, and L2 = 0.69 ± 0.07 L⊙ for WASP 1814+48 B. The surface gravity of log g2 = 5.098 ± 0.026 obtained from M2 and R2 is concurrent with 5.097 ± 0.025 computed directly from the observable quantities. WASP 1814+48 B is well matched with the 0.176-M⊙ white dwarf (WD) evolutionary model for Z = 0.01. The metallicity and our Galactic kinematics indicate that the program target is a thin-disc star. The whole light residuals after the removal of the binary trend were analysed and found to oscillate at a total of 52 frequencies. Among these, most of the low frequencies below 24 d−1 are aliases and orbital harmonics. The five significant frequencies between 32 and 36 d−1 are the pulsation modes of WASP 1814+48 A located in the δ Sct domain on the zero-age main sequence, and the high frequencies of 128–288 d−1 arise from WASP 1814+48 B in the pre-He WD instability strip. Our results reveal that WASP 1814+48 is the fifth EL CVn star that is composed of a δ Sct-type primary and a pre-ELMV (extremely low-mass pre-He WD variable).
A multiwavelength study of the flat-spectrum radio quasar NVSS J141922−083830 covering four flaring episodes
Authors: Buckley D A H , Britto R J , Chandra S , Krushinsky V , Böttcher M , Razzaque S , Lipunov V , Stalin C S , Gorbovskoy E , Tiurina N , Vlasenko D , Kniazev A 
Published: August 2022

ABSTRACT
We present multiwavelength observations and a model for flat-spectrum radio quasar (FSRQ) NVSS J141922−083830, originally classified as a blazar candidate of unknown type (BCU II object) in the Third Fermi-LAT AGN Catalog. Relatively bright flares (&gt;3 magnitudes) were observed on 2015 February 21 (MJD 57074) and 2018 September 8 (MJD 58369) in the optical band with the MASTER Global Robotic Nettelescopes. Optical spectra obtained with the Southern African Large Telescopeon 2015 March 1 (MJD 57082), during outburst, and on 2017 May 30 (MJD 57903), during quiescence, showed emission lines at 5325 Å and at ≈3630 Å that we identified as the Mg ii 2798 Å and C iii] 1909 Å lines, respectively, and hence derived a redshift $z$ = 0.903. Analysis of Fermi-Large Area Telescope (LAT) data was performed in the quiescent regime (5 yr of data) and during four prominent flaring states in 2014 February–April, 2014 October–November, 2015 February–March, and 2018 September. We present spectral and timing analysis with Fermi-LAT. We report a hardening of the gamma-ray spectrum during the last three flaring periods, with a power-law spectral index Γ = 2.0–2.1. The maximum gamma-ray flux level was observed on 2014 October 24 (MJD 56954) at (7.57 ± 1.83) × 10−7 ph cm−2 s−1. The multiwavelength spectral energy distribution (SED) during the 2015 February–March flare supports the earlier evidence of this blazar to belong to the FSRQ class. The SED can be well represented with a single-zone leptonic model with parameters typical of FSRQs, but also a hadronic origin of the high-energy emission cannot be ruled out.
The ‘Giraffe’: discovery of a stripped red giant in an interacting binary with an ∼2 M⊙ lower giant
Authors: Jayasinghe T , Thompson Todd A , Kochanek C S , Stanek K Z , Rowan D M , Martin D V , El-Badry Kareem , Vallely P J , Hinkle J T , Huber D , Isaacson H , Tayar J , Auchettl K , Ilyin I , Howard A W , Badenes C 
Published: August 2022

ABSTRACT
We report the discovery of a stripped giant + lower giant Algol-type binary, 2M04123153+6738486 (2M0412), identified during a search for non-interacting compact object – star binaries. 2M0412 is an evolved (Teff, giant ≃ 4000 K), luminous (Lgiant ≃ 150 L⊙) red giant in a circular P = 81.2 d binary. 2M0412 is a known variable star previously classified as a semiregular variable. The cross-correlation functions of follow-up Keck/HIRES and LBT/Potsdam Echelle Polarimetric and Spectroscopic Instrument (PEPSI) spectra show an radial velocity variable second component with implied mass ratio q = Mgiant/Mcomp ≃ 0.20 ± 0.01. The All-Sky Automated Survey for SuperNovae (ASAS-SN), Asteroid Terrestrial-impact Last Alert System (ATLAS), Transiting Exoplanet Survey Telescope ( TESS), and Zwicky Transient Facility (ZTF) light curves show that the giant is a Roche lobe filling ellipsoidal variable with an inclination of 49.4 ± 0.3°, and a giant mass of Mgiant = 0.38 ± 0.01 M⊙ for a distance of ≃ 3.7 kpc. The mass of the giant indicates that its envelope has been partially stripped. The giant companion on the lower red giant branch has a mass of Mcomp = 1.91 ± 0.03 M⊙ with Teff, comp ≃ 5000 K, Lcomp ≃ 60 L⊙, and Rcomp ≃ 11 R⊙. The lower giant contributes ${\sim }35{{\ \rm per\ cent}}$ of the flux in the V band. We also identify an orbital phase dependent, broad $\rm H\,\alpha$ emission line which could indicate ongoing accretion from the stripped red giant on to the companion.
Effect of radiation drag on the line-force-driven winds
Authors: Wang Bei-Chuan , Yang Xiao-Hong , Bu De-Fu , Huang Shu-Su 
Published: August 2022

ABSTRACT
Ultra-fast outflows (UFOs) with mildly relativistic velocities are measured using the X-ray spectra of radio-quiet and -loud active galactic nuclei. In general, UFOs are believed to be generated from the accretion disc around a black hole. A line-force driving model is suggested to be the mechanism to drive UFOs from the accretion disc. In this paper, we use the non-hydrodynamic approach to examine the influences of radiation-drag effects on the line-force-driven winds generated from the accretion disc. We find that the radiation-drag effects can significantly weaken the line-force-driven winds. Compared with the case without the radiation-drag effects, when the radiation-drag effects are considered, the maximum speed of winds is reduced by ∼60 per cent–70 per cent, the mass outflow rate is reduced by ∼50 per cent–80 per cent, and the kinetic power is reduced by about an order of magnitude. The radiation-drag effects narrow the area where the winds are generated.
Systematic light-curve modelling of TDEs: statistical differences between the spectroscopic classes
Authors: Nicholl Matt , Lanning Daniel , Ramsden Paige , Mockler Brenna , Lawrence Andy , Short Phil , Ridley Evan J 
Published: August 2022

ABSTRACT
With the sample of observed tidal disruption events (TDEs) now reaching several tens, distinct spectroscopic classes have emerged: TDEs with only hydrogen lines (TDE-H), only helium lines (TDE-He), or hydrogen in combination with He ii and often N iii/O iii (TDE-H + He). Here, we model the light curves of 32 optically bright TDEs using the Modular Open Source Fitter for Transients (mosfit) to estimate physical and orbital properties, and look for statistical differences between the spectroscopic classes. For all types, we find a shallow distribution of star masses, compared to a typical initial mass function, in the range ∼0.1–1 M⊙, and no TDEs with very deep encounters. Our main result is that TDE-H events appear to come from less complete disruptions (and possibly lower SMBH masses) than TDE-H+He, with TDE-He events fully disrupted. We also find that TDE-H events have more extended photospheres, in agreement with recent literature, and argue that this could be a consequence of differences in the self-intersection radii of the debris streams. Finally, we identify an approximately linear correlation between black hole mass and radiative efficiency. We suggest that TDE-H may be powered by collision-induced outflows at relatively large radii, while TDE-H + He could result from prompt accretion discs, formed more efficiently in closer encounters around more massive SMBHs.
Cosmological simulations with rare and frequent dark matter self-interactions
Authors: Fischer Moritz S , Brüggen Marcus , Schmidt-Hoberg Kai , Dolag Klaus , Kahlhoefer Felix , Ragagnin Antonio , Robertson Andrew 
Published: August 2022

ABSTRACT
Dark matter (DM) with self-interactions is a promising solution for the small-scale problems of the standard cosmological model. Here we perform the first cosmological simulation of frequent DM self-interactions, corresponding to small-angle DM scatterings. The focus of our analysis lies in finding and understanding differences to the traditionally assumed rare DM (large-angle) self-scatterings. For this purpose, we compute the distribution of DM densities, the matter power spectrum, the two-point correlation function, and the halo and subhalo mass functions. Furthermore, we investigate the density profiles of the DM haloes and their shapes. We find that overall large-angle and small-angle scatterings behave fairly similarly with a few exceptions. In particular, the number of satellites is considerably suppressed for frequent compared to rare self-interactions with the same cross-section. Overall, we observe that while differences between the two cases may be difficult to establish using a single measure, the degeneracy may be broken through a combination of multiple ones. For instance, the combination of satellite counts with halo density or shape profiles could allow discriminating between rare and frequent self-interactions. As a by-product of our analysis, we provide – for the first time – upper limits on the cross-section for frequent self-interactions.