bluuebunny/crossref_metadata_2025_split huggingface dataset:
A Rapid LC–MS-MS Method for the Quantitation of Antiepileptic Drugs in Urine
Authors: Feng Sheng , Bridgewater Brandi , Strickland Erin C , McIntire Gregory 
Published: July 2020

Abstract
Epilepsy is a common neurologic disease that requires treatment with one or more medications. Due to the polypharmaceutical treatments, potential side effects, and drug-drug interactions associated with these medications, therapeutic drug monitoring is important. Therapeutic drug monitoring is typically performed in blood due to established clinical ranges. While blood provides the benefit of determining clinical ranges, urine requires a less invasive collection method, which is attractive for medication monitoring. As urine does not typically have established clinical ranges, it has not become a preferred specimen for monitoring medication adherence. Thus, large urine clinical data sets are rarely published, making method development that addresses reasonable concentration ranges difficult. An initial method developed and validated in-house utilized a universal analytical range of 50–5,000 ng/mL for all antiepileptic drugs and metabolites of interest in this work, namely carbamazepine, carbamazepine-10,11-epoxide, eslicarbazepine, lamotrigine, levetiracetam, oxcarbazepine, phenytoin, 4-hydroxyphenytoin, and topiramate. This upper limit of the analytical range was too low leading to a repeat rate of 11.59% due to concentrations &gt;5,000 ng/mL. Therefore, a new, fast liquid chromatography–tandem mass spectrometry (LC–MS-MS) method with a run time under 4 minutes was developed and validated for the simultaneous quantification of the previously mentioned nine antiepileptic drugs and their metabolites. Urine samples were prepared by solid-phase extraction and analyzed using a Phenomenex Phenyl-Hexyl column with an Agilent 6460 LC–MS-MS instrument system. During method development and validation, the analytical range was optimized for each drug to reduce repeat analysis due to concentrations above the linear range and for carryover. This reduced the average daily repeat rate for antiepileptic testing from 11.59% to 4.82%. After validation, this method was used to test and analyze patient specimens over the course of approximately one year. The resulting concentration data were curated to eliminate specimens that could indicate an individual was noncompliant with their therapy (i.e., positive for illicit drugs) and yielded between 20 and 1,700 concentration points from the patient specimens, depending on the analyte. The resulting raw quantitative urine data set is presented as preliminary reference ranges to assist with interpreting urine drug concentrations for the nine aforementioned antiepileptic medications and metabolites.
Microtremor HVSR analysis of heterogeneous shallow sedimentary structures at Pohang, South Korea
Authors: Kang Su Young , Kim Kwang-Hee , Chiu Jer-Ming , Liu Lanbo 
Published: July 2020

AbstractWe apply the single-station microtremor horizontal-to-vertical spectral ratio (HVSR) method to image the geometry of Pohang Basin, South Korea, which experienced the greatest earthquake damage in Korea during a series of anthropogenic earthquakes between November 2017 and February 2018. We collected and analysed the ambient seismic noise at 124 temporary stations. The resonance frequencies, which vary significantly across the area (0.35–19.86 Hz), were inverted to constrain the depth of the major impedance contrast, which is interpreted to be the sediment–bedrock interface beneath each station. The sedimentary layer thickness is generally thin in the north and thickens to the southern and central parts of the basin, where the depth to bedrock is up to 340 m. We compare the HVSR results with six borehole observations in the area, whose depth to bedrock ranges from 189 to 359 m. The sediment thicknesses obtained via the direct borehole measurements and HVSR method are comparable with each other. The resultant three-dimensional shape of the sedimentary basin provides crucial information for the microzonation of the Pohang area for seismic risk mitigation. It also provides a realistic initial velocity model for three-dimensional tomographic inversions to elucidate the detailed subsurface structure of the region.
Visualization of microstructural change affected by mechanical stimulation in tendon healing with a novel tensionless model
Authors: Oshima Junya , Sasaki Kaoru , Yamamoto Naoto , Kiyosawa Tomoharu , Sekido Mitsuru 
Published: July 2020

Abstract
Since the majority of a tendon’s dry weight is collagen fibers, tendon healing consists mainly of collagen repair and observing three-dimensional networks of collagen fibers with scanning electron microscopy (SEM) is optimal for investigating this process. In this report, a cell-maceration/SEM method was used to investigate extrasynovial tendon (unwrapped tendon in synovial tissue such as the tendon sheath) healing of an injured Achilles tendon in a rat model. In addition, since mechanical stimulation is important for tendon healing, a novel, tensionless, rat lower leg tendon injury model was established and verified by visualizing the structural change of collagen fibers under tensionless conditions by SEM. This new model was created by transplanting the leg of a rat with a tendon laceration to the back, removing mechanical stimulation. We then compared the process of tendon healing with and without tension using SEM. Under tension, collagen at the tendon stump shows axial alignment and repair that subsequently demarcates the paratenon (connective tissue on the surface of an extrasynovial tendon) border. In contrast, under tensionless conditions, the collagen remains randomly arranged. Our findings demonstrate that mechanical stimulation contributes to axial arrangement and reinforces the importance of tendon tension in wound healing.
Music Therapy Private Practice in the United States: Updated Financial and Marketing Recommendations
Authors: Wilhelm Kyle , Knight Andrew 
Published: July 2020

Abstract
More and more music therapists in the United States are entering into private practice. For a private practice to survive, a therapist must make sound financial and marketing decisions that can have wide-ranging implications on the success of the business. Clear and current recommendations from music therapists in private practice can help those wanting to go into private practice as well as those already in private practice. The purpose of this study was to identify a current descriptive profile of music therapists in private practice in the United States as well as marketing and financial recommendations. In addition, comparing this survey with previous surveys can reveal possible trends in the field. Music therapists (N = 745) who self-identified as being self-employed or in private practice were sent a survey designed by the researchers. A total of 193 respondents returned the survey revealing that current therapists in private practice are better educated and value the internet and social media for marketing and session implementation more than respondents of previous surveys. Respondents recommend that music therapists in private practice continually learn by taking business classes and consulting with business experts; diversify funding sources, service options, and populations served; and connect with music therapists and nonmusic therapists in the community.
Comparison of Serum Free and Bioavailable 25-Hydroxyvitamin D Levels in Alzheimer’s Disease and Healthy Control Patients
Authors: Ertilav Esra , Barcin Nur Ebru , Ozdem Sebahat 
Published: July 2020

Abstract

Objective
Many studies have investigated lower 25-hydroxyvitamin D (25[OH]D) levels in patients with Alzheimer’s disease (AD) compared with those in control patients. In the present study, we aimed to evaluate serum free and bioavailable 25(OH)D levels in patients with AD and in healthy control patients.

Methods
The AD group consisted of 85 patients aged &gt;60 years who were diagnosed with possible AD according to National Institute on Aging-Alzheimer’s Association criteria and 85 healthy control patients. Serum levels of total 1,25-dihydroxyvitamin D, total 25(OH)D, vitamin D binding protein (VDBP), parathormone, calcium, phosphorus and albumin, free 25(OH)D, bioavailable 25(OH)D, and the bioavailable 25(OH)D/total 25(OH)D ratio were compared in both groups.

Results
Total 25(OH)D, free 25(OH)D, bioavailable 25(OH)D, and the bioavailable 25(OH)D/total 25(OH)D ratio were significantly lower (P &lt;.001, P &lt;.001, P &lt;.001, P &lt;.05, respectively) in the AD group, whereas the VDBP level was significantly higher (P &lt;.05) in the AD than in the control group.

Conclusion
Free and bioavailable 25(OH)D detected at lower levels in patients with AD limit the target central effects of 25(OH)D; this result suggests that reduced levels of the active free form of vitamin D may be a risk factor for AD and dementia.
Magnetar outburst and spin-down glitch
Authors: Tong H , Huang L 
Published: July 2020

ABSTRACT
The outburst and spin-down glitch of magnetars are modelled from the magnetospheric point of view. We try to discuss the following four questions: (1) Which pulsar on the period and period-derivative diagram are more likely to show magnetar outburst? (2) Which outburst will make the glitch that triggered the outburst to become a spin-down glitch? (3) Can we model the outburst and spin-down glitch in PSR J1119−6127 simultaneously? (4) Why the torque variation is delayed compared with the peak of the X-ray luminosity in 1E 1048.1−5937 and PSR J1119−6127? It is found that both the global and local twisted magnetic field will affect the radiation and timing behaviours of magnetars. Especially, the delay of torque variations may due to the combined effect of increasing twist in the j-bundle and untwisting of the global magnetosphere. A toy model is built for magnetar outburst and torque variations. It can catch the general trend of magnetar outburst: decaying flux, shrinking hotspot, and torque variations.
Jet–ISM interactions near the microquasars GRS 1758−258 and 1E 1740.7−2942
Authors: Tetarenko A J , Rosolowsky E W , Miller-Jones J C A , Sivakoff G R 
Published: July 2020

ABSTRACT
We present Atacama Large Millimeter/Sub-millimeter Array observations of the candidate jet–ISM interaction zones near the black hole X-ray binaries GRS 1758−258 and 1E 1740.7−2942. Using these data, we map the molecular line emission in the regions, detecting emission from the HCN [J = 1−0], HCO+ [J = 1−0], SiO [J = 2−1], CS [J = 2−1], 13CO [J = 1−0], C18O [J = 1−0], HNCO [J = 40,4−30,3], HNCO [J = 50,5−40,4], and CH3OH [J = 21,1−11,0] molecular transitions. Through examining the morphological, spectral, and kinematic properties of this emission, we identify molecular structures that may trace jet-driven cavities in the gas surrounding these systems. Our results from the GRS 1758−258 region in particular, are consistent with recent work, which postulated the presence of a jet-blown cocoon structure in deep radio continuum maps of the region. Using these newly discovered molecular structures as calorimeters, we estimate the time averaged jet power from these systems, finding $(1.1{\!-\!}5.7)\times 10^{36}{\rm erg\, s}^{-1}$ over 0.12−0.31 Myr for GRS 1758−258 and $(0.7{\!-\!}3.5)\times 10^{37}{\rm erg\, s}^{-1}$ over 0.10−0.26 Myr for 1E 1740.7−2942. Additionally, the spectral line characteristics of the detected emission place these molecular structures in the central molecular zone of our Galaxy, thereby constraining the distances to the black hole X-ray binaries to be 8.0 ± 1.0 kpc. Overall, our analysis solidifies the diagnostic capacity of molecular lines, and highlights how astro-chemistry can both identify jet–ISM interaction zones and probe jet feedback from Galactic X-ray binaries.
Constraints on the spin-pole orientation, jet morphology, and rotation of interstellar comet 2I/Borisov with deep HST imaging
Authors: Bolin Bryce T , Lisse Carey M 
Published: July 2020

ABSTRACT
We present high resolution, deep imaging of interstellar comet 2I/Borisov taken with the Hubble Space Telescope/Wide Field Camera 3 (HST/WFC3) on 2019 December 8 UTC and 2020 January 27 UTC (HST GO 16040, PI: Bolin) before and after its perihelion passage in combination with HST/WFC3 images taken on 2019 October 12 UTC and 2019 November 16 UTC (HST GO/DD 16009, PI: Jewitt) before its outburst and fragmentation of 2020 March, thus observing the comet in a relatively undisrupted state. We locate 1–2 arcsec long (2000–3000 km projected length) jet-like structures near the optocentre of 2I that appear to change position angles from epoch to epoch. With the assumption that the jet is located near the rotational pole supported by its stationary appearance on ∼10–100 h time frames in HST images, we determine that 2I’s pole points near α = 322 ± 10° and δ = 37 ± 10° (λ = 341° and β = 48°) and may be in a simple rotation state. Additionally, we find evidence for possible periodicity in the HST time-series light curve on the time-scale of ∼5.3 h with a small amplitude of ∼0.05 mag implying a lower limit on its b/a ratio of ∼1.5 unlike the large ∼2 mag light curve observed for 1I/‘Oumuamua. However, these small light-curve variations may not be the result of the rotation of 2I’s nucleus due to its dust-dominated light-scattering cross-section. Therefore, uniquely constraining the pre-Solar system encounter, pre-outburst rotation state of 2I may not be possible even with the resolution and sensitivity provided by HST observations.
Alkaline exospheres of exoplanet systems: evaporative transmission spectra
Authors: Gebek Andrea , Oza Apurva V 
Published: July 2020

ABSTRACT
Hydrostatic equilibrium is an excellent approximation for the dense layers of planetary atmospheres, where it has been canonically used to interpret transmission spectra of exoplanets. Here, we exploit the ability of high-resolution spectrographs to probe tenuous layers of sodium and potassium gas due to their formidable absorption cross-sections. We present an atmosphere–exosphere degeneracy between optically thick and optically thin mediums, raising the question of whether hydrostatic equilibrium is appropriate for Na i lines observed at exoplanets. To this end we simulate three non-hydrostatic, evaporative, density profiles: (i) escaping, (ii) exomoon, and (iii) torus to examine their imprint on an alkaline exosphere in transmission. By analysing an evaporative curve of growth, we find that equivalent widths of $W_{\mathrm{Na D2}} \sim 1{\!-\!} 10\, \mathrm{m\mathring{\rm A}}$ are naturally driven by evaporation rates ∼103−105 kg s−1 of pure atomic Na. To break the degeneracy between atmospheric and exospheric absorption, we find that if the line ratio is D2/D1 ≳ 1.2 the gas is optically thin on average roughly indicating a non-hydrostatic structure of the atmosphere/exosphere. We show this is the case for Na i observations at hot Jupiters WASP-49b and HD189733b and also simulate their K i spectra. Lastly, motivated by the slew of metal detections at ultra-hot Jupiters, we suggest a toroidal atmosphere at WASP-76b and WASP-121b is consistent with the Na i data at present.
RW Aur B: a modest UX Ori-type companion of the famous primary
Authors: Dodin A , Lamzin S , Petrov P , Safonov B , Takami M , Tatarnikov A 
Published: July 2020

ABSTRACT
The secondary of the famous young binary RW Aur is much less studied than the primary. To rectify this shortcoming, we present here the results of UBVRIJHK photometric, VRI polarimetric and optical spectral observations of RW Aur B. The star demonstrates chaotic brightness variations in the optical band, with irregular, short (∼1-d) dimmings with an amplitude ΔV up to 1.3 mag. The dimmings are accompanied by an increase in the linear polarization (up to 3 per cent in the I band), presumably as a result of the scattering of stellar radiation by dust in the circumstellar disc, which means that RW Aur B can be classified as a UX Ori-type star. We conclude that the observed excess emission at λ ≲ 0.45 μm and longwards of ~2 μm as well as the variability of fluxes and profiles of the H i, He i and Na i D emission lines are due to the accretion process. At the same time, emission components of Ca ii lines indicate that RW Aur B has a powerful chromosphere. Assuming solar elemental abundances, we find the following parameters for the star: Teff = 4100–4200 K, AV = 0.6 ± 0.1 (out of the dimming events), L* ≈ 0.6 ${\rm L}_\odot ,\, R_* \approx 1.5$ ${\rm R}_\odot ,\, M\approx 0.85$ M$_\odot ,\, \dot{M}_{\rm acc}\lt 5\times 10^{-9}$ M⊙ yr−1. Finally, we discuss possible reasons for the different levels of accretion activity of the RW Aur binary components and present arguments in favour of the fact that the components are gravitationally bound.
Linear and non-linear tidal oscillations and mode identification in the eccentric binary system KIC 3858884
Authors: Manzoori Davood 
Published: July 2020

ABSTRACT
The phoebe code was used to analyse the Kepler light-curve and to estimate the physical and geometrical parameters of a rare pulsating binary system, KIC 3858884. The analysis indicated that the system is composed of two detached and very similar main-sequence A-type stars, in a highly eccentric orbit with e = 0.47. After disentangling the binarity effect, the residual data were subjected to Fourier frequency decomposition using period04 software. The resulting frequency spectrum consists of two moderately high-amplitude nearby frequencies, F1 = 7.232199 d−1 and $F2=7.472889\, \mathrm{d}^{-1}$, which were attributed to δ Scuti-type pulsations. In addition, 18 frequencies were identified that were exact harmonics of the orbital frequency $f_{\rm orb}= 0.038533\, \mathrm{d}^{-1}$, and also 53 anharmonics. However, it was found that many of these anharmonic frequencies coupled together non-linearly to give harmonic modes of pulsation. Furthermore, some existing theoretical models of the tidal oscillations were numerically verified in general binary systems through estimations of various modal characteristics, for example mode quantum numbers ${n, l, m,}$ energies Ei, threshold energies Ei,th, damping rates γi, growth rates Γi and stability criteria, etc. The evolution of the stars in the binary system was compared with some similar single pulsating stars on the Hertzsprung–Russell diagram and it was concluded that the evolution of a single star is more rapid. Finally, the observed rate of apsidal line displacement was estimated through eclipse timing variation analysis as Uobs = 74745.2 ± 2566 yr. This was compared with the theoretically calculated rate of the line of apsides motion, UTheo = 73588 ± 2298 yr, and found to be in good agreement within errors, hence verifying general relativity theory once again.
An extensive spectroscopic time series of three Wolf–Rayet stars – II. A search for wind asymmetries in the dust-forming WC7 binary WR137
Authors: St-Louis N , Piaulet C , Richardson N D , Shenar T , Moffat A F J , Eversberg T , Hill G M , Gauza B , Knapen J H , Kubát J , Kubátová B , Sablowski D P , Simón-Díaz S , Bolduan F , Dias F M , Dubreuil P , Fuchs D , Garrel T , Grutzeck G , Hunger T , Küsters D , Langenbrink M , Leadbeater R , Li D , Lopez A , Mauclaire B , Moldenhawer T , Potter M , dos Santos E M , Schanne L , Schmidt J , Sieske H , Strachan J , Stinner E , Stinner P , Stober B , Strandbaek K , Syder T , Verilhac D , Waldschläger U , Weiss D , Wendt A 
Published: July 2020

ABSTRACT
We present the results of a 4-month, spectroscopic campaign of the Wolf–Rayet dust-making binary, WR137. We detect only small-amplitude random variability in the C iii λ5696 emission line and its integrated quantities (radial velocity, equivalent width, skewness, and kurtosis) that can be explained by stochastic clumps in the wind of the WC star. We find no evidence of large-scale periodic variations often associated with Corotating Interaction Regions that could have explained the observed intrinsic continuum polarization of this star. Our moderately high-resolution and high signal-to-noise average Keck spectrum shows narrow double-peak emission profiles in the H α, H β, H γ, He ii λ6678, and He ii λ5876 lines. These peaks have a stable blue-to-red intensity ratio with a mean of 0.997 and a root mean square of 0.004 commensurate with the noise level; no variability is found during the entire observing period. We suggest that these profiles arise in a decretion disc around the O9 companion, which is thus an O9e star. The characteristics of the profiles are compatible with those of other Be/Oe stars. The presence of this disc can explain the constant component of the continuum polarization of this system, for which the angle is perpendicular to the plane of the orbit, implying that the rotation axis of the O9e star is aligned with that of the orbit. It remains to be explained why the disc is so stable within the strong ultraviolet radiation field of the O star. We present a binary evolutionary scenario that is compatible with the current stellar and system parameters.
The Human Face of Naturalism: Putnam and Diamond on Religious Belief and the “Gulfs between Us”
Authors: Miguens Sofia 
Published: July 2020

AbstractHilary Putnam and Cora Diamond both wrote on Wittgenstein’s Three Lectures on Religious Belief. They did it quite differently; my ultimate aim in this article is to explore this difference. Putnam’s view of religion is largely a view of ethical life; I look thus into his writings on ethics and his proposals to face the relativist menace therein. Still, in his incursions into philosophy of religion, describing religious experience through authors such as Rosenzweig, Buber, or Levinas, Putnam deals with what Diamond calls, after Wittgenstein, “the gulfs between us.” Such gulfs, and the threat of relativism they bring, need to be accounted for. With that purpose in mind I complement Putnam’s reading of the Three Lectures with Diamond’s own reading.
Clinical Pearls and Methods for Intraoperative Motor Mapping
Authors: Rossi Marco , Sciortino Tommaso , Conti Nibali Marco , Gay Lorenzo , Viganò Luca , Puglisi Guglielmo , Leonetti Antonella , Howells Henrietta , Fornia Luca , Cerri Gabriella , Riva Marco , Bello Lorenzo 
Published: July 2020

Abstract
Resection of brain tumors involving motor areas and pathways requires the identification and preservation of various cortical and subcortical structures involved in motor control at the time of the procedure, in order to maintain the patient's full motor capacities. The use of brain mapping techniques has now been integrated into clinical practice for many years, as they help the surgeon to identify the neural structures involved in motor functions. A common definition of motor function, as well as knowledge of its neural organization, has been continuously evolving, underlining the need for implementing intraoperative strategies at the time of the procedure. Similarly, mapping strategies have been subjected to continuous changes, enhancing the likelihood of preservation of full motor capacities. As a general rule, the motor mapping strategy should be as flexible as possible and adapted strictly to the individual patient and clinical context of the tumor. In this work, we present an overview of current knowledge of motor organization, indications for motor mapping, available motor mapping, and monitoring strategies, as well as their advantages and limitations. The use of motor mapping improves resection and outcomes in patients harboring tumors involving motor areas and pathways, and should be considered the gold standard in the resection of this type of tumor.