bluuebunny/crossref_metadata_2025_split huggingface dataset:
Current Status of Pain Management in Parkinson’s Disease
Authors: Karnik Vikram , Farcy Nicole , Zamorano Carolina , Bruno Veronica 
Published: January 2020

ABSTRACT:Background:Pain is a non-motor symptom in Parkinson’s disease (PD) which commonly goes underreported. Adequate treatment for pain in PD remains challenging, and to date, no clear guidelines for management are available.Methods:With the goal of understanding and organizing the current status of pain management in PD, we conducted a review of pharmacological and non-pharmacological treatments for pain in patients with PD. Suitable studies cataloged in PubMed and the Cochrane database up to October 31, 2019, were included prioritizing randomized controlled trials.Post-hocanalyses and open-label studies were also included.Results:Treatment with levodopa increases pain thresholds in patients with PD. Apomorphine did not have similar efficacy. Duloxetine provided benefit in an open-label trial. Oxycodone-naloxone PR did not have a significant improvement in pain, but per-protocol analysis showed a reduction in pain when adherence was strong. Rotigotine patch had numerical improvement on pain scales with no statistical significance. Safinamide significantly improved the “bodily discomfort” domain in the PDQ-39 questionnaire. Botulinum toxin A had a non-significant signal toward improving dystonic limb pain in PD. DBS to the subthalamic nucleus may modulate central pain thresholds, and a pilot study of cranioelectric therapy warrants future research in the area.Conclusion:After optimizing dopaminergic therapy, understanding the type of pain a patient is experiencing is essential to optimizing pain control in PD. While recommendations can be made regarding the treatment options in each domain, evidence remains weak and future randomized controlled studies are needed.
Existence, non-existence and blow-up behaviour of minimizers for the mass-critical fractional non-linear Schrödinger equations with periodic potentials
Authors: Dinh Van Duong 
Published: January 2020

AbstractWe consider the minimizing problem for the energy functional with prescribed mass constraint related to the fractional non-linear Schrödinger equation with periodic potentials. Using the concentration-compactness principle, we show a complete classification for the existence and non-existence of minimizers for the problem. In the mass-critical case, under a suitable assumption of the potential, we give a detailed description of blow-up behaviour of minimizers once the mass tends to a critical value.
Age stage, two-sex life table ofHabrobracon hebetor(Braconidae) onSpodoptera exigua(Noctuidae) reared on different sugar beet genotypes
Authors: Fathipour Yaghoub , Talaee Ladan , Bagheri Abdoolnabi , Talebi Ali Asghar , Khajehali Jahangir 
Published: January 2020

AbstractThe present study was carried out to unveil interactive relevance among consecutive and alternate members of a tritrophic system comprised of sugar beet genotypes, beet armyworm,Spodoptera exigua(Hübner), and its parasitoid,Habrobracon hebetor(Say) using demographic parameters. To do so,H. hebetorwas reared onS. exiguafed on 10 sugar beet genotypes, including SB26; SB27; SB29; SB33; SB34; (7112*SB36)*Sh-1-HSF-5; FC220; FC301; SBSI006; and HM 1339RZ in a growth chamber at 25 ± 1 °C, 60 ± 5% RH, and 16:8 (L: D) h photoperiod. The data was analyzed based on the age-stage, two-sex life table theory. Our results revealed high variation in duration of different life stages ofH. hebetoronS. exiguareared on different sugar beet genotypes examined. The shortest (10.605 days) and longest (13.721 days) pre-adult period ofH. hebetorwas onS. exiguareared on SB26 and SB34, respectively. The longest (17.2 days) and shortest adult longevity (7.5 days) was onS. exiguareared on SB26 and SB27, respectively. The highest values of the intrinsic rate of increase (r) (0.209 day−1) and finite rate of increase (λ) (1.233 day−1) were observed onS. exiguareared on SB34 and their lowest values (0.159 and 1.172 day−1, respectively) were recorded on SB27. Resistant and susceptible genotypes toS. exigua, FC301 and (7112*SB36)*Sh-1-HSF-5, respectively, were only genotypes on whichH. hebetorhad greater and approximately equalrcompared withS. exigua. This finding indicates high capability ofH. hebetorto be successfully employed againstS. exiguaon sugar beet genotypes which are extremely different in resistance to this pest.
Adjoint approach to calculating shape gradients for three-dimensional magnetic confinement equilibria. Part 2. Applications
Authors: Paul Elizabeth J. , Antonsen Thomas , Landreman Matt , Cooper W. Anthony 
Published: January 2020

The shape gradient is a local sensitivity function defined on the surface of an object which provides the change in a characteristic quantity, or figure of merit, associated with a perturbation to the shape of the object. The shape gradient can be used for gradient-based optimization, sensitivity analysis and tolerance calculations. However, it is generally expensive to compute from finite-difference derivatives for shapes that are described by many parameters, as is the case for typical stellarator geometry. In an accompanying work (Antonsen, Paul & Landreman J. Plasma Phys., vol. 85 (2), 2019), generalized self-adjointness relations are obtained for magnetohydrodynamic (MHD) equilibria. These describe the relation between perturbed equilibria due to changes in the rotational transform or toroidal current profiles, displacements of the plasma boundary, modifications of currents in the vacuum region or the addition of bulk forces. These are applied to efficiently compute the shape gradient of functions of MHD equilibria with an adjoint approach. In this way, the shape derivative with respect to any perturbation applied to the plasma boundary or coil shapes can be computed with only one additional MHD equilibrium solution. We demonstrate that this approach is applicable for several figures of merit of interest for stellarator configuration optimization: the magnetic well, the magnetic ripple on axis, the departure from quasisymmetry, the effective ripple in the low-collisionality

$1/\unicode[STIX]{x1D708}$

regime

$(\unicode[STIX]{x1D716}_{\text{eff}}^{3/2})$

(Nemov et al. Phys. Plasmas, vol. 6 (12), 1999, pp. 4622–4632) and several finite-collisionality neoclassical quantities. Numerical verification of this method is demonstrated for the magnetic well figure of merit with the VMEC code (Hirshman & Whitson Phys. Fluids, vol. 26 (12), 1983, p. 3553) and for the magnetic ripple with modification of the ANIMEC code (Cooper et al. Comput. Phys. Commun., vol. 72 (1), 1992, pp. 1–13). Comparisons with the direct approach demonstrate that, in order to obtain agreement within several per cent, the adjoint approach provides a factor of

$O(10^{3})$

in computational savings.
What if God commanded something horrible? A pragmatics-based defence of divine command metaethics
Authors: KREMERS PHILIPP 
Published: January 2020

AbstractThe objection of horrible commands claims that divine command metaethics is doomed to failure because it is committed to the extremely counterintuitive assumption that torture of innocents, rape, and murder would be morally obligatory if God commanded these acts. Morriston, Wielenberg, and Sinnott-Armstrong have argued that formulating this objection in terms of counterpossibles is particularly forceful because it cannot be simply evaded by insisting on God's necessary perfect moral goodness. I show that divine command metaethics can be defended even against this counterpossible version of the objection of horrible commands because we can explain the truth-value intuitions about the disputed counterpossibles as the result of conversational implicatures. Furthermore, I show that this pragmatics-based defence of divine command metaethics has several advantages over Pruss'sreductiocounterargument against the counterpossible version of the objection of horrible commands.
Commissioning experience of the X-ray volume imaging system of an image-guided radiotherapy capable linear accelerator
Authors: Raina Payal , Sahoo Susanta Kumar 
Published: January 2020

AbstractAim:An image-guided radiotherapy capable linear accelerator was installed at our hospital which is equipped with an X-ray volumetric imaging (XVI) system. The aim of this study was to describe the results of acceptance tests which were carried out on the XVI facility to verify the manufacturer’s specification.Materials and methods:The commissioning test had six elements: system safety, geometric accuracy, image quality, registration and correction accuracy, X-ray tube and generator performance, and quality assurance (QA) procedures.Results:We had satisfactory results for all the tests. The system passed the safety testes, and the agreement of isocentres was found to be within the tolerance limit. Imaging quality was acceptable. Registration and correction accuracy was tasted with indigenously developed phantom and positioned accurately at isocentre. X-ray tube and generator test results showed that the tube was performing properly.Findings:The described tests represent that the performance of the system is maintained at acceptable levels.
Gravitational fragmentation and formation of giant protoplanets on orbits of tens of AU
Authors: Elbakyan Vardan G. , Vorobyov Eduard I. 
Published: January 2020

AbstractMigration of dense gaseous clumps that form in young protostellar disks via gravitational fragmentation is investigated to determine the likelihood of giant-planet formation. We show that gaseous clumps that form in the outer regions of the disk (> 100 au) through disk fragmentation often migrate toward the central star on timescales from a few thousand to few tens of thousands of years. The tidal mass loss helps the clumps to significantly slow down or even halt their inward migration at a distance of a few tens of AU from the protostar.
Towards Realistic Understandings of Gas Dynamics in Protoplanetary Disks
Authors: Bai Xue-Ning 
Published: January 2020

AbstractThe gas dynamics of protoplanetary disks (PPDs) plays a crucial role in almost all stages of planet formation, yet it is far from being well understood largely due to the complex interplay among various microphysical processes. Primarily, PPD gas dynamics is likely governed by magnetic fields, and their coupling with the weakly ionized gas is described by non-ideal magnetohydrodynamic (MHD) effects. Incorporating these effects, I will present the first fully global simulations of PPDs that include the most realistic disk microphysics. Accretion and disk evolution is primarily driven by magnetized disk winds with significant mass loss comparable to accretion rate. The overall disk gas dynamics strongly depends on the polarity of large-scale poloidal magnetic field threading the disk owing to the Hall effect. The flow structure in the disk is highly unconventional with major implications on planet formation.
Analysis of KOI 2700b, the second exoplanet with a comet-like dusty tail – selected results
Authors: Garai Zoltán , Dolinský Peter 
Published: January 2020

AbstractThe Kepler object KOI 2700b was discovered recently as the second exoplanet with a comet-like dusty tail. We aimed at verifying the disintegrating-planet scenario of KOI 2700b by modeling its light curve and to put constraints on various tail and planet properties, as was done in the case of KIC 12557548b. Here, we describe some selected results of our analysis.
Kinematics of OB-associations in the 3-kpc solar neighborhood
Authors: Melnik Anna M. , Dambis Andrei K. , Glushkova Elena V. , Rautiainen Pertti 
Published: January 2020

AbstractWe use Gaia (DR1, DR2) stellar proper motions to study the kinematics of OB-associations. The average one-dimensional velocity dispersion inside 18 OB-associations with more than 10 Gaia DR1 stars is σv = 3.9 km s−1. The median virial and stellar masses of OB-associations are equal to 7×105 and 9 × 103 solar masses, respectively. The median star-formation efficiency is ε = 2.1%. We have found the expansion in several OB-associations. Models of the Galaxy with a two-component outer ring R1R2 can reproduce the average residual velocities of OB-associations in the Perseus, Sagittarius and Local System complexes.
A physically motivated core definition applied to dust emission observations of the Pipe nebula
Authors: Hasenberger Birgit , Alves João 
Published: January 2020

AbstractDense cores represent a critical stage in the star-formation process, but are not physically well-defined entities. We present a new technique to define core boundaries in observations of molecular clouds based on the physical properties of the cloud medium. Applying this technique to regions in the Pipe nebula, we find that our core boundaries differ from previous analyses, with potentially crucial implications for the statistical properties of the core sample.
Tracing the early planet formation with molecular lines: chemistry of vortex in the protoplanetary disks
Authors: Dzyurkevich Natalia , Lyra Wladimir , Majumdar Liton 
Published: January 2020

AbstractThe millimeter observations of dust in protoplanetary disks show us spectacular structures like numerous gaps, vortices and spirals. In particular, IRS 48 disk demonstrates a large vortex-like structure. Molecular lines provide information about disks that is complementary to dust continuum observations: formaldehyde was found on the inner edge of the IRS 48 vortex, along with detections of SO2 and CS isotopes.We use a reduced chemical network containing main carbon- and sulfur-bearing species to find the molecular species which can be sensitive to the gaps in dust, as well as to accumulation of the dust grains in the vortex. We find that SO molecule is the main reservoir for sulfur in IRS 48, for adopted disk model as in Bruderer et al. 2014. While SO is very sensitive to the gap edge, it cannot trace the vortex as it is weakly responding to the local increase in dust. Instead, SO2 molecule abundance can be expected to drop quickly within the vortex, making it an interesting tracer of dust-trapping structure.
Obliquity Variability of Terrestrial Planets in the Habitable Zone
Authors: Shan Yutong , Li Gongjie 
Published: January 2020

AbstractObliquity (axial tilt) and its variability could play an important role in the climate and habitability of a planet. We explore the spin-axis dynamics of two specific habitable zone exoplanets, Kepler-62f and Kepler-186f, using numerical and analytical techniques. Based on our current understanding of their orbital architecture, we find that, in contrast with the typical conditions in the Solar System, Kepler-62f and 186f should have low obliquity variations except in fine-tuned conditions. Extra undetected planetary companions and/or the existence of a satellite could either stabilize or destabilize obliquities at a variety of values.
Problems with exoplanets around sdBV and sdO stars from primary Kepler field
Authors: Krzesinski Jerzy , Blokesz A. , Ogłoza W. , Dróżdż M. 
Published: January 2020

AbstractThe existence of exoplanets around evolved objects is one of the most interesting subjects from the viewpoint of planetary system evolution and its fate. What happens to the exoplanets engulfed in the host star envelope during red giant branch (RGB) phase? Can planets survive this evolutionary stage of the host star? Here, we are showing that at least some of the exoplanetary candidates recently found around a couple of sdBV stars, KIC 5807616 and KIC 10001893, might not be exoplanets after all. One “exoplanetary signal” visible in the light curve FT of KIC 10001893 can be just a frequency combination of stellar pulsation modes, while others are likely artifacts. Similarly, low frequency signals found in KIC 5807616 light curve FT, are beating frequencies of stellar oscillations, rather than resulting from the exoplanetary radiation. We also analyzed frequency and amplitude changes of the signal around 0.256 c/d (&#x223C;3.9 day) visible in the light curve FT of the KIC 10449976 sdO star. Our simulations show that it is difficult to reproduce the observed signal frequency variations by the weather changes in the exoplanet atmosphere.
Global Protoplanetary Disk Simulations: Dead Zone Formation and FUor Outbursts
Authors: Kadam Kundan , Vorobyov E. , Regály Zs. , Kóspál Á. , Ábráham P. 
Published: January 2020

AbstractWe conducted global hydrodynamic simulations of protoplanetary disk evolution with an adaptive Shakura-Sunyaev &alpha; prescription to represent the layered disk structure, and starting with the collapse phase of the molecular cloud. With the canonical values of model parameters, self-consistent dead zones formed at the scale of a few au. The instabilities associated with the dead zone and corresponding outbursts, similar to FUor eruptions, were also observed in the simulations.
The implications of clustered star formation for (proto)planetary systems and habitability
Authors: Kruijssen J. M. Diederik , Longmore Steven N. 
Published: January 2020

AbstractStar formation is spatially clustered across a range of environments, from dense stellar clusters to unbound associations. As a result, radiative or dynamical interactions with neighbouring stars disrupt (proto)planetary systems and limit their radii, leaving a lasting impact on their potential habitability. In the solar neighbourhood, we find that the vast majority of stars form in unbound associations, such that the interaction of (proto)planetary systems with neighbouring stars is limited to the densest sub-regions. However, the fraction of star formation occurring in compact clusters was considerably higher in the past, peaking at ∼50% in the young Milky Way at redshift z ∼ 2. These results demonstrate that the large-scale star formation environment affects the demographics of planetary systems and the occupation of the habitable zone. We show that planet formation is governed by multi-scale physics, in which Mpc-scale events such as galaxy mergers affect the AU-scale properties of (proto)planetary systems.
Magnetic geometry and activity of cool stars
Authors: Boro Saikia Sudeshna , Lüftinger Theresa , Guedel Manuel 
Published: January 2020

AbstractStellar magnetic field manifestations such as stellar winds and EUV radiation are the key drivers of planetary atmospheric loss and escape. To understand how the central star influences habitability, it is very important to perform detailed investigation of the star’s magnetic field. We investigate the surface magnetic field geometry and chromospheric activity of 51 sun-like stars. The magnetic geometry is reconstructed using Zeeman Doppler imaging. Chromospheric activity is measured using the Ca II H& K lines. We confirm that the Sun’s large-scale geometry is dominantly poloidal, which is also true for slowly rotating stars. Contrary to the Sun, rapidly rotating stars can have a strong toroidal field and a weak poloidal field. This separation in field geometry appears at Ro=1. Our results show that detailed investigation of stellar magnetic field is important to understand its influence on planetary habitability.
Nitrogen-included Carbonaceous Compounds (NCC): Laboratory-synthesized organics as the probable candidate for the carrier of the UIR bands observed in dusty classical novae
Authors: Endo Izumi , Sakon Itsuki , Onaka Takashi , Helton Andrew L. , Lau Ryan M. , Kimura Seiji , Wada Setsuko , Ogawa Nanako , Ohkouchi Naohiko , Kebukawa Yoko 
Published: January 2020

AbstractThe unidentified infrared (UIR) bands have been ubiquitously observed in various astrophysical environments and consist of a series of emission features arising from aromatic and/or aliphatic C-C and C-H bonds [1]. Therefore, their carriers are thought to be related to interstellar organics. However, our knowledge on the true carriers of the UIR bands is still limited. Recently [4] has proposed Mixed Aromatic Aliphatic Organic Nanoparticles, which contains hetero atoms in addition to conventional hydrocarbon models, as a more realistic interpretation of the band carriers. The challenges toward identifying the carriers of the UIR bands are still ongoing. Past studies have shown that the UIR bands observed around classical novae, which characterized by the presence of broad feature around 8&mu;m[2], are somewhat different from those observed in other astrophysical environment. Here we report the success of experimentally synthesizing the organics called Nitrogen-included Carbonaceous Compounds (NCC; [7]) whose infrared properties can reproduce the UIR bands observed in classical novae.
Unveiling the whole from its parts or to see the forest for the trees
Authors: Janot-Pacheco Eduardo , Rachid Marina , Bendjoya Philippe , Domiciano Armando , Antunes-Rosa Caroline , Emilio Marcelo , Lage Claudia 
Published: January 2020

AbstractIf biologically complex molecules as DNA were present in the extraterrestrial targets, their spectral signatures would be rather difficult to be unambiguously identified. As a matter of fact, the molecular array of a single nucleobasis will generate a tangled spectral signature. On the other hand, a part of it, e.g. bands due to the group of HNCO of guanine may have been detected but associated to smaller molecules, e.g. isocianic acid (HNCO). However, if comprised in a nucleobasis, its detection would be misinterpreted. Five key transitions were preliminarly selected for either purines and pyrimidines that should be observed together in the same target. If this happens, it may be that we are detecting the whole from its parts.
Pre- and protostellar cores in the Rosette Nebula
Authors: Bögner R. , Csengeri T. , Wienen M. , Schneider N. , Montillaud J. , Tóth L. V. 
Published: January 2020

AbstractRecent theories on the formation of the Solar System turned the attention to the study of low mass cloud cores in massive star forming regions. The Rosette Molecular Cloud is a well-known star forming area having highly filamentary structure with dense cores covering a wide range of masses. These pre- and protostellar cores were observed by Herschel and key core properties were derived from its data. With the Effelsberg 100m telescope a sample of these cores with masses ranging between 3-40 M⊙ were observed in ammonia inversion lines. In this work we are examining the correlations between these two datasets with the aim of gaining insight of the processes behind the star formation of the region.
Brightness variations of young Sun-like stars from ground-based and space telescopes
Authors: Zsidi G. , Kóspál Á. , Ábrahám P. , Szabó R. , Cseh B. , Sárneczky K. , Sódor Á. , Szakáts R. , Vida K. , Vinkó J. 
Published: January 2020

AbstractYoung stellar objects often show photometric variability, which is well examined at optical wavelengths, but more and more infrared data are also available. The wavelength dependence of the variability carries information on the physical cause of the changing brightness. Here, we examine seven T Tauri-type stars known for their large amplitude variability selected from the Campaign 13 field of the Kepler K2 mission. We complemented the K2 light curves by multifilter optical monitoring observations made with the 90 cm Schmidt telescope of Konkoly Observatory, and by 3.6 and 4.5 μm infrared photometry with a 20 hours cadence using the Spitzer Space Telescope. We found that the wavelength dependence of the observed variability is not consistent with changing interstellar extinction. We suggest that the brightness changes are due to variable accretion, causing a variable illumination of the inner disk.