bluuebunny/crossref_metadata_2025_split huggingface dataset:
A decrease in spontaneous activity in medial prefrontal cortex is associated with sustained hallucinations in chronic schizophrenia: An NIRS study
Authors: Yanagi Masaya , Hosomi Fumiharu , Kawakubo Yoshihiro , Tsuchiya Aki , Ozaki Satoshi , Shirakawa Osamu 
Published: June 2020

AbstractIn functional imaging, accumulating evidence suggests that spontaneous activity decreases during the resting state in the core brain regions of the default-mode network [e.g. medial prefrontal cortex (mPFC)] in schizophrenia. However, the significance of this decreased activity has not been clarified in relation to its clinical symptoms. In this study, near-infrared spectroscopy (NIRS), which is a simple imaging modality suitable for resting state paradigm, was used to evaluate the intensity of the spontaneous activity during the resting state in chronic schizophrenia. Consistent with previous findings of fMRI studies, spontaneous activity decreased in the mPFC of patients with schizophrenia. In addition, the decreased spontaneous activity was associated with severe hallucinations in this region where reality monitoring is fundamentally engaged. These results may encourage additional application of NIRS with the resting state paradigm into daily clinical settings for addressing the broad phenotypes and unstable course of schizophrenia.
Gastroprotective effect of phytoncide extract from Pinus koraiensis pinecone in Helicobacter pylori infection
Authors: Kim Se-eun , Memon Azra , Kim Bae Yong , Jeon Hyelin , Lee Woon Kyu , Kang Se Chan 
Published: June 2020

AbstractFor centuries, herbs have been used by traditional therapists around the world to treat gastrointestinal tract disorders, such as gastritis. We hypothesized that the anti-Helicobacter pylori properties of phytoncide, which is extracted from pinecone waste, would facilitate use as a natural gastroprotective product to treat gastrointestinal tract disorders. Thus, we investigated in vitro antibacterial efficacy against H. pylori by agar diffusion assay. To determine the gastroprotective properties of phytoncide, we conducted hematoxylin and eosin staining, performed assays for the detection of the cytotoxin gene, and evaluated pro-inflammatory cytokine expression in H. pylori-infected C57BL/6 mice. Phytoncide significantly inhibited the survival of H. pylori in the gastrointestinal system of C57BL/6 mice. Reduction of gastric severity in H. pylori-infected mice was associated with reductions in the expression levels of pro-inflammatory cytokines in the gastric mucosa, and of the cytotoxin CagA gene in phytoncide treated groups (P < 0.05 and P < 0.01). In conclusion, phytoncide significantly inhibited the growth of H. pylori in gastro tissue, possibly due to the abundant α-pinene present in the phytoncide as detected by HPLC analysis. Further studies are needed to validate our findings, but we suggest that phytoncide has the potential to be used as a natural ingredient in anti-H. pylori products.
Observational Study of Peritoneal Washing Cytology-Positive Gastric Cancer without Gross Peritoneal Metastasis in Patients who Underwent Radical D2 Gastrectomy
Authors: Shim Hyun-Jeong , Kim Hyeon-Jong , Lee Seung Hyuk , Bae Woo-Kyun , Hwang Eu-Chang , Cho Sang-Hee , Chung Ik-Joo , Bang Hyun-Jin , Hwang Jun Eul 
Published: June 2020

AbstractBackground The clinical features and therapeutic strategies for gastric cancer with positive peritoneal washing cytology but without visible gross peritoneal metastasis have not been defined. The aim of this study was to evaluate the effect and clinical prognostic value of postoperative chemotherapy in gastric cancer patients with positive peritoneal washing cytology without gross peritoneal metastasis who underwent radical D2 gastrectomy in terms of disease-free survival (DFS) and overall survival (OS). Materials and Methods Intraoperative peritoneal washing cytology was performed in 285 patients who underwent radical D2 gastrectomy between April 2004 and May 2016. Of them, 88 patients with positive cytology but without gross peritoneal metastasis were included in the study. In total, 64 patients received postoperative chemotherapy, whereas 24 patients underwent surgery only. Results Most gastric cancer patients with positive cytology without gross peritoneal metastasis demonstrated pT4 and/or pN3 disease. Postoperative chemotherapy improved DFS and OS compared to surgery only in gastric cancer patients with positive cytology without gross peritoneal metastasis (median DFS 11.63 vs. 6.98 months, p < 0.001; median OS 25.50 vs. 12.11 months, p < 0.001). In multivariate analyses of gastric cancer patients with positive cytology without gross peritoneal metastasis, no chemotherapy was the strongest clinical factor for poorer DFS (hazard ratio [HR] 3.76, p < 0.001) or OS (HR 4.37, p < 0.001). Conclusion Postoperative chemotherapy improves the survival outcome compared to surgery alone in gastric cancer patients with positive peritoneal washing cytology but without visible gross peritoneal metastasis who underwent radical D2 gastrectomy.
Amplification of synoptic to annual variability of West African summer monsoon rainfall under global warming
Authors: Akinsanola Akintomide Afolayan , Zhou Wen , Zhou Tianjun , Keenlyside Noel 
Published: June 2020

AbstractIncreased knowledge of future changes in rainfall variability is needed to reduce vulnerability to potential impacts of global warming, especially in highly vulnerable regions like West Africa. While changes in mean and extreme rainfall have been studied extensively, rainfall variability has received less attention, despite its importance. In this study, future changes in West African summer monsoon (WASM) rainfall variability were investigated using data from two regional climate models that participated in the Coordinated Regional Climate Downscaling Experiment (CORDEX). The daily rainfall data were band-pass filtered to isolate variability at a wide range of timescales. Under global warming, WASM rainfall variability is projected to increase by about 10–28% over the entire region and is remarkably robust over a wide range of timescales. We found that changes in mean rainfall significantly explain the majority of intermodel spread in projected WASM rainfall variability. The role of increased atmospheric moisture is examined by estimating the change due to an idealized local thermodynamic enhancement. Analysis reveals that increased atmospheric moisture with respect to warming following the Clausius–Clapeyron relationship can explain the majority of the projected changes in rainfall variability at all timescales.
The planctomycete Stieleria maiorica Mal15T employs stieleriacines to alter the species composition in marine biofilms
Authors: Kallscheuer Nicolai , Jeske Olga , Sandargo Birthe , Boedeker Christian , Wiegand Sandra , Bartling Pascal , Jogler Mareike , Rohde Manfred , Petersen Jörn , Medema Marnix H. , Surup Frank , Jogler Christian 
Published: June 2020

AbstractBacterial strains of the phylum Planctomycetes occur ubiquitously, but are often found on surfaces of aquatic phototrophs, e.g. alga. Despite slower growth, planctomycetes are not outcompeted by faster-growing bacteria in biofilms on such surfaces; however, strategies allowing them to compensate for slower growth have not yet been investigated. Here, we identified stieleriacines, a class of N-acylated tyrosines produced by the novel planctomycete Stieleria maiorica Mal15T, and analysed their effects on growth of the producing strain and bacterial species likely co-occurring with strain Mal15T. Stieleriacines reduced the lag phase of Mal15T and either stimulated or inhibited biofilm formation of two bacterial competitors, indicating that Mal15T employs stieleriacines to specifically alter microbial biofilm composition. The genetic organisation of the putative stieleriacine biosynthetic cluster in strain Mal15T points towards a functional link of stieleriacine biosynthesis to exopolysaccharide-associated protein sorting and biofilm formation.
Drosophila melanogaster behaviour changes in different social environments based on group size and density
Authors: Rooke Rebecca , Rasool Amara , Schneider Jonathan , Levine Joel D. 
Published: June 2020

AbstractMany organisms, when alone, behave differently from when they are among a crowd.Drosophilasimilarly display social behaviour and collective behaviour dynamics within groups not seen in individuals. In flies, these emergent behaviours may be in response to the global size of the group or local nearest-neighbour density. Here we investigate i) which aspect of social life flies respond to: group size, density, or both and ii) whether behavioural changes within the group are dependent on olfactory support cells. Behavioural assays demonstrate that flies adjust their interactive behaviour to group size but otherwise compensate for density by achieving a standard rate of movement, suggesting that individuals are aware of the number of others within their group. We show that olfactory support cells are necessary for flies to behave normally in large groups. These findings shed insight into the subtle and complex life ofDrosophilawithin a social setting.
Misalignment tolerance wireless power transfer system combining inductive and capacitive coupling
Authors: Luo Bo , Zhou Xingyu , Long Tao , Mai Ruikun , He Zhengyou 
Published: June 2020

To resonate with the capacitive power transfer (CPT) system, inductors are usually needed, while additional capacitors are required for the inductive power transfer (IPT) system. To take advantage of the inductance of the IPT system, this study proposes a misalignment tolerance wireless power transfer system that employs the IPT coupler to compensate part of CPT's capacitance for railway applications. In the proposed system, two power transfer paths are formed by the IPT and CPT couplers. Additionally, the system merits a good anti‐misalignment ability by carefully designing the parameters of the proposed system. In a well‐alignment case, only the CPT coupler is utilised to transfer power. While in misalignment case, the IPT coupler is activated to transfer power to improve the misalignment tolerance. Besides, the transfer capability of the combined system can be improved when the misalignment happens. The system coupler, connection method and output power characteristics are presented in detail. Then, the general design procedure is provided with an example system at 1 kW. Experimental results show that the maximum variation of the output is 5.6% when misalignment is up to 250 mm (50%). While the power variation of the system involving single CPT can be as large as 52%.
Numerical simulations of the lower solar atmosphere heating by two-fluid nonlinear Alfvén waves
Authors: Kuźma B. , Wójcik D. , Murawski K. , Yuan D. , Poedts S. 
Published: June 2020

Context. We present new insight into the long-standing problem of plasma heating in the lower solar atmosphere in terms of collisional dissipation caused by two-fluid Alfvén waves.
Aims. Using numerical simulations, we study Alfvén wave propagation and dissipation in a magnetic flux tube and their heating effect.
Methods. We set up 2.5-dimensional numerical simulations with a semi-empirical model of a stratified solar atmosphere and a force-free magnetic field mimicking a magnetic flux tube. We consider a partially ionized plasma consisting of ion + electron and neutral fluids, which are coupled by ion-neutral collisions.
Results. We find that Alfvén waves, which are directly generated by a monochromatic driver at the bottom of the photosphere, experience strong damping. Low-amplitude waves do not thermalize sufficient wave energy to heat the solar atmospheric plasma. However, Alfvén waves with amplitudes greater than 0.1 km s−1 drive through ponderomotive force magneto-acoustic waves in higher atmospheric layers. These waves are damped by ion-neutral collisions, and the thermal energy released in this process leads to heating of the upper photosphere and the chromosphere.
Conclusions. We infer that, as a result of ion-neutral collisions, the energy carried initially by Alfvén waves is thermalized in the upper photosphere and the chromosphere, and the corresponding heating rate is large enough to compensate radiative and thermal-conduction energy losses therein.
Pebble-driven planet formation around very low-mass stars and brown dwarfs
Authors: Liu Beibei , Lambrechts Michiel , Johansen Anders , Pascucci Ilaria , Henning Thomas 
Published: June 2020

We conduct a pebble-driven planet population synthesis study to investigate the formation of planets around very low-mass stars and brown dwarfs in the (sub)stellar mass range between 0.01 M⊙ and 0.1 M⊙. Based on the extrapolation of numerical simulations of planetesimal formation by the streaming instability, we obtain the characteristic mass of the planetesimals and the initial mass of the protoplanet (largest body from the planetesimal populations), in either the early self-gravitating phase or the later non-self-gravitating phase of the protoplanetary disk evolution. We find that the initial protoplanets form with masses that increase with host mass and orbital distance, and decrease with age. Around late M-dwarfs of 0.1 M⊙, these protoplanets can grow up to Earth-mass planets by pebble accretion. However, around brown dwarfs of 0.01 M⊙, planets do not grow to the masses that are greater than Mars when the initial protoplanets are born early in self-gravitating disks, and their growth stalls at around 0.01 Earth-mass when they are born late in non-self-gravitating disks. Around these low-mass stars and brown dwarfs we find no channel for gas giant planet formation because the solid cores remain too small. When the initial protoplanets form only at the water-ice line, the final planets typically have ≳15% water mass fraction. Alternatively, when the initial protoplanets form log-uniformly distributed over the entire protoplanetary disk, the final planets are either very water rich (water mass fraction ≳15%) or entirely rocky (water mass fraction ≲5%).
Interferometric imaging with LOFAR remote baselines of the fine structures of a solar type-IIIb radio burst
Authors: Zhang PeiJin , Zucca Pietro , Sridhar Sarrvesh Seethapuram , Wang ChuanBing , Bisi Mario M. , Dabrowski Bartosz , Krankowski Andrzej , Mann Gottfried , Magdalenic Jasmina , Morosan Diana E. , Vocks Christian 
Published: June 2020

Context. Solar radio bursts originate mainly from high energy electrons accelerated in solar eruptions like solar flares, jets, and coronal mass ejections. A sub-category of solar radio bursts with short time duration may be used as a proxy to understand wave generation and propagation within the corona.
Aims. Complete case studies of the source size, position, and kinematics of short term bursts are very rare due to instrumental limitations. A comprehensive multi-frequency spectroscopic and imaging study was carried out of a clear example of a solar type IIIb-III pair.
Methods. In this work, the source of the radio burst was imaged with the interferometric mode, using the remote baselines of the LOw Frequency ARray (LOFAR). A detailed analysis of the fine structures in the spectrum and of the radio source motion with imaging was conducted.
Results. The study shows how the fundamental and harmonic components have a significantly different source motion. The apparent source of the fundamental emission at 26.56 MHz displaces away from the solar disk center at about four times the speed of light, while the apparent source of the harmonic emission at the same frequency shows a speed of < 0.02 c. The source size of the harmonic emission observed in this case is smaller than that in previous studies, indicating the importance of the use of remote baselines.
New constraints on the location of P9 obtained with the INPOP19a planetary ephemeris
Authors: Fienga A. , Di Ruscio A. , Bernus L. , Deram P. , Durante D. , Laskar J. , Iess L. 
Published: June 2020

Context.We used the new released INPOP19a planetary ephemerides benefiting from Jupiter-updated positions by theJunomission and reanalyzedCassiniobservations.Aims.We test possible locations of the unknown planet P9. To do this, we used the perturbations it produces on the orbits of the outer planets, more specifically, on the orbit of Saturn.Methods.Two statistical criteria were used to identify possible acceptable locations of P9 according to (i) the difference in planetary positions when P9 is included compared with the propagated covariance matrix, and (ii) theχ2likelihood of postfit residuals for ephemerides when P9 is included.Results.No significant improvement of the residuals was found for any of the simulated locations, but we provide zones that induce a significant degradation of the ephemerides.Conclusions.Based on the INPOP19a planetary ephemerides, we demonstrate that if P9 exists, it cannot be closer than 500 AU with a 5M⊕and no closer than 650 AU with a 10M⊕. We also show that there is no clear zone that would indicate the positive existence of planet P9, but there are zones for which the existence of P9 is compatible with the 3σaccuracy of the INPOP planetary ephemerides.
Three short-period Jupiters from TESS
Authors: Nielsen L. D. , Brahm R. , Bouchy F. , Espinoza N. , Turner O. , Rappaport S. , Pearce L. , Ricker G. , Vanderspek R. , Latham D. W. , Seager S. , Winn J. N. , Jenkins J. M. , Acton J. S. , Bakos G. , Barclay T. , Barkaoui K. , Bhatti W. , Briceño C. , Bryant E. M. , Burleigh M. R. , Ciardi D. R. , Collins K. A. , Collins K. I. , Cooke B. F. , Csubry Z. , dos Santos L. A. , Eigmüller Ph. , Fausnaugh M. M. , Gan T. , Gillon M. , Goad M. R. , Guerrero N. , Hagelberg J. , Hart R. , Henning T. , Huang C. X. , Jehin E. , Jenkins J. S. , Jordán A. , Kielkopf J. F. , Kossakowski D. , Lavie B. , Law N. , Lendl M. , de Leon J. P. , Lovis C. , Mann A. W. , Marmier M. , McCormac J. , Mori M. , Moyano M. , Narita N. , Osip D. , Otegi J. F. , Pepe F. , Pozuelos F. J. , Raynard L. , Relles H. M. , Sarkis P. , Ségransan D. , Seidel J. V. , Shporer A. , Stalport M. , Stockdale C. , Suc V. , Tamura M. , Tan T. G. , Tilbrook R. H. , Ting E. B. , Trifonov T. , Udry S. , Vanderburg A. , Wheatley P. J. , Wingham G. , Zhan Z. , Ziegler C. 
Published: June 2020

We report the confirmation and mass determination of three hot Jupiters discovered by the Transiting Exoplanet Survey Satellite (TESS) mission: HIP 65Ab (TOI-129, TIC-201248411) is an ultra-short-period Jupiter orbiting a bright (V = 11.1 mag) K4-dwarf every 0.98 days. It is a massive 3.213 ± 0.078 MJ planet in a grazing transit configuration with an impact parameter of b = 1.17−0.08+0.10. As a result the radius is poorly constrained, 2.03−0.49+0.61RJ. The planet’s distance to its host star is less than twice the separation at which it would be destroyed by Roche lobe overflow. It is expected to spiral into HIP 65A on a timescale ranging from 80 Myr to a few gigayears, assuming a reduced tidal dissipation quality factor of Qs′ = 107 − 109. We performed a full phase-curve analysis of the TESS data and detected both illumination- and ellipsoidal variations as well as Doppler boosting. HIP 65A is part of a binary stellar system, with HIP 65B separated by 269 AU (3.95 arcsec on sky). TOI-157b (TIC 140691463) is a typical hot Jupiter with a mass of 1.18 ± 0.13 MJ and a radius of 1.29 ± 0.02 RJ. It has a period of 2.08 days, which corresponds to a separation of just 0.03 AU. This makes TOI-157 an interesting system, as the host star is an evolved G9 sub-giant star (V = 12.7). TOI-169b (TIC 183120439) is a bloated Jupiter orbiting a V = 12.4 G-type star. It has a mass of 0.79 ±0.06 MJ and a radius of 1.09−0.05+0.08RJ. Despite having the longest orbital period (P = 2.26 days) of the three planets, TOI-169b receives the most irradiation and is situated on the edge of the Neptune desert. All three host stars are metal rich with [Fe / H] ranging from 0.18 to0.24.
Self-scattering of non-spherical dust grains
Authors: Kirchschlager Florian , Bertrang Gesa H.-M. 
Published: June 2020

Context. The understanding of (sub-)millimetre polarisation has made a leap forward since high-resolution imaging with the Atacama Large (sub-)Mm Array (ALMA) became available. Amongst other effects, self-scattering (i.e. the scattering of thermal dust emission on other grains) is thought to be the origin of millimetre polarisation. This opens the first window to a direct measurement of dust grain sizes in regions of optically thick continuum emission as it can be found in protoplanetary discs and star-forming regions. However, the newly derived values of grain sizes are usually around ~100 μm and thus one order of magnitude smaller than those obtained from more indirect measurements, as well as those expected from theory (~1 mm).
Aims. We see the origin of this contradiction in the applied dust model of current self-scattering simulations: a perfect compact sphere. The aim of this study is to test our hypothesis by investigating the impact of non-spherical grain shapes on the self-scattering signal.
Methods. We applied discrete dipole approximation simulations to investigate the influence of the grain shape on self-scattering polarisation in three scenarios: an unpolarised and polarised incoming wave under a fixed and a varying incident polarisation angle.
Results. We find significant deviations of the resulting self-scattering polarisation when comparing non-spherical to spherical grains. In particular, tremendous deviations are found for the polarisation signal of grains when observed outside the Rayleigh regime, that is for >100 μm sized grains observed at the 870 μm wavelength. Self-scattering by oblate grains produces higher polarisation degrees compared to spheres, which challenges the interpretation of the origin of observed millimetre polarisation. A (nearly) perfect alignment of the non-spherical grains is required to account for the observed millimetre polarisation in protoplanetary discs. Furthermore, we find conditions under which the emerging scattering polarisation of non-spherical grains is flipped in orientation by 90°.
Conclusions. These results show clearly that the perfect compact sphere is an oversimplified model, which has reached its limit. Our findings point towards a necessary re-evaluation of the dust grain sizes derived from (sub-)millimetre polarisation.