bluuebunny/crossref_metadata_2025_split huggingface dataset:
Dynamical ejecta of neutron star mergers with nucleonic weak processes – II: kilonova emission
Authors: Just O , Kullmann I , Goriely S , Bauswein A , Janka H-T , Collins C E 
Published: November 2021

ABSTRACT
The majority of existing results for the kilonova (or macronova) emission from material ejected during a neutron-star (NS) merger is based on (quasi-) one-zone models or manually constructed toy-model ejecta configurations. In this study, we present a kilonova analysis of the material ejected during the first $\sim 10\,$ ms of a NS merger, called dynamical ejecta, using directly the outflow trajectories from general relativistic smoothed-particle hydrodynamics simulations, including a sophisticated neutrino treatment and the corresponding nucleosynthesis results, which have been presented in Part I of this study. We employ a multidimensional two-moment radiation transport scheme with approximate M1 closure to evolve the photon field and use a heuristic prescription for the opacities found by calibration with atomic-physics-based reference results. We find that the photosphere is generically ellipsoidal but augmented with small-scale structure and produces emission that is about 1.5–3 times stronger towards the pole than the equator. The kilonova typically peaks after $0.7\!-\!1.5\,$ d in the near-infrared frequency regime with luminosities between $3\!-\!7\times 10^{40}\,$ erg s−1 and at photospheric temperatures of $2.2\!-\!2.8\times 10^3\,$ K. A softer equation of state or higher binary-mass asymmetry leads to a longer and brighter signal. Significant variations of the light curve are also obtained for models with artificially modified electron fractions, emphasizing the importance of a reliable neutrino-transport modelling. None of the models investigated here, which only consider dynamical ejecta, produces a transient as bright as AT2017gfo. The near-infrared peak of our models is incompatible with the early blue component of AT2017gfo.
ACACIA: a new method to produce on-the-fly merger trees in the ramses code
Authors: Ivkovic Mladen , Teyssier Romain 
Published: November 2021

ABSTRACT
The implementation of ACACIA, a new algorithm to generate dark matter halo merger trees with the Adaptive Mesh Refinement code RAMSES, is presented. The algorithm is fully parallel and based on the Message Passing Interface. As opposed to most available merger tree tools, it works on the fly during the course of the N-body simulation. It can track dark matter substructures individually using the index of the most bound particle in the clump. Once a halo (or a sub-halo) merges into another one, the algorithm still tracks it through the last identified most bound particle in the clump, allowing to check at later snapshots whether the merging event was definitive, or whether it was only temporary, with the clump only traversing another one. The same technique can be used to track orphan galaxies that are not assigned to a parent clump anymore because the clump dissolved due to numerical overmerging. We study in detail the impact of various parameters on the resulting halo catalogues and corresponding merger histories. We then compare the performance of our method using standard validation diagnostics, demonstrating that we reach a quality similar to the best available and commonly used merger tree tools. As a proof of concept, we use our merger tree algorithm together with a parametrized stellar-mass-to-halo-mass relation and generate a mock galaxy catalogue that shows good agreement with observational data.
Is the birth of PSR J0538+2817 accompanied by a gamma-ray burst?
Authors: Xu Fan , Geng Jin-Jun , Wang Xu , Li Liang , Huang Yong-Feng 
Published: November 2021

ABSTRACT
Recently, the Five-hundred-meter Aperture Spherical radio Telescope measured the three-dimensional velocity of PSR J0538+2817 with respect to its associated supernova remnant S147 and found a possible spin–velocity alignment for this pulsar. Here, we show that the high velocity and the spin–velocity alignment of this pulsar can be explained by the so-called electromagnetic rocket mechanism. In this framework, the pulsar is kicked in the direction of the spin axis, which naturally explains the spin–velocity alignment. We scrutinize the evolution of the pulsar and show that the kick process can create a highly relativistic jet at the opposite direction of the kick velocity. The lifetime and energetics of the jet is estimated. It is argued that the jet can generate a gamma-ray burst (GRB). The long-term dynamical evolution of the jet is calculated. It is found that the shock radius of the jet should expand to about 32 pc at present, which is well consistent with the observed radius of the supernova remnant S147 (32.1 ± 4.8 pc). Additionally, our calculations indicate that the current velocity of the GRB remnant should be about 440 km s−1, which is also roughly consistent with the observed blast-wave velocity of the remnant of S147 (500 km s−1).
The challenge of simulating the star cluster population of dwarf galaxies with resolved interstellar medium
Authors: Hislop Jessica M , Naab Thorsten , Steinwandel Ulrich P , Lahén Natalia , Irodotou Dimitrios , Johansson Peter H , Walch Stefanie 
Published: November 2021

ABSTRACT
We present results on the star cluster properties from a series of high resolution smoothed particles hydrodynamics (SPH) simulations of isolated dwarf galaxies as part of the griffin project. The simulations at sub-parsec spatial resolution and a minimum particle mass of 4 M⊙ incorporate non-equilibrium heating, cooling, and chemistry processes, and realize individual massive stars. The simulations follow feedback channels of massive stars that include the interstellar-radiation field variable in space and time, the radiation input by photo-ionization and supernova explosions. Varying the star formation efficiency per free-fall time in the range ϵff = 0.2–50${{\ \rm per\ cent}}$ neither changes the star formation rates nor the outflow rates. While the environmental densities at star formation change significantly with ϵff, the ambient densities of supernovae are independent of ϵff indicating a decoupling of the two processes. At low ϵff, gas is allowed to collapse more before star formation, resulting in more massive, and increasingly more bound star clusters are formed, which are typically not destroyed. With increasing ϵff, there is a trend for shallower cluster mass functions and the cluster formation efficiency Γ for young bound clusters decreases from $50 {{\ \rm per\ cent}}$ to $\sim 1 {{\ \rm per\ cent}}$ showing evidence for cluster disruption. However, none of our simulations form low mass (&lt;103 M⊙) clusters with structural properties in perfect agreement with observations. Traditional star formation models used in galaxy formation simulations based on local free-fall times might therefore be unable to capture star cluster properties without significant fine tuning.
On the nature of the X-ray pulsar XTE J1859+083 and its broad-band properties
Authors: Salganik Alexander , Tsygankov Sergey S , Djupvik Anlaug A , Karasev Dmitri I , Lutovinov Alexander A , Buckley David A H , Gromadzki Mariusz , Poutanen Juri 
Published: November 2021

ABSTRACT
This work is devoted to the study of the broad-band 0.8–79 keV spectral and timing properties of the poorly studied X-ray pulsar XTE J1859+083 during its 2015 outburst based on the data from the NuSTAR and Swift observatories. We show that the source pulse profile has complex shape that depends on the energy band. Pulse fraction of XTE J1859+083 has constant value around 35 per cent in the broad energy band, this behaviour is atypical for X-ray pulsars. At the same time its energy spectrum is typical of this class of objects and has a power-law shape with an exponential cutoff at high energies. No cyclotron absorption line was discovered in the source spectrum. On the basis of indirect method and the absence of a cyclotron line, an estimation was made for the magnetic field strength as less than 5 × 1011 G or belonging to the interval from 5 × 1012 to $2.0^{+0.9}_{-1.2}\times 10^{13}$ G. Data from the NOT and SALT telescopes as well as optical and IR sky surveys allowed us also to study the nature of its optical companion. We have proposed and studied new possible candidates for the optical companion of XTE J1859+083 and the most likely candidate was identified. The results of the optical and IR photometry and spectroscopy of these possible companions showed that the system is a Be X-ray binary, showing Brγ, He i, and strong H α spectral lines.
MRI-active inner regions of protoplanetary discs – II. Dependence on dust, disc, and stellar parameters
Authors: Jankovic Marija R , Mohanty Subhanjoy , Owen James E , Tan Jonathan C 
Published: November 2021

ABSTRACT
Close-in super-Earths are the most abundant exoplanets known. It has been hypothesized that they form in the inner regions of protoplanetary discs, out of the dust that may accumulate at the boundary between the inner region susceptible to the magneto-rotational instability (MRI) and an MRI-dead zone further out. In Paper I, we presented a model for the viscous inner disc which includes heating due to both irradiation and MRI-driven accretion; thermal and non-thermal ionization; dust opacities; and dust effects on ionization. Here, we examine how the inner disc structure varies with stellar, disc, and dust parameters. For high accretion rates and small dust grains, we find that: (1) the main sources of ionization are thermal ionization and thermionic and ion emission; (2) the disc features a hot, high-viscosity inner region, and a local gas pressure maximum at the outer edge of this region (in line with previous studies); and (3) an increase in the dust-to-gas ratio pushes the pressure maximum outwards. Consequently, dust can accumulate in such inner discs without suppressing the MRI, with the amount of accumulation depending on the viscosity in the MRI-dead regions. Conversely, for low accretion rates and large dust grains, there appears to be an additional steady-state solution in which: (1) stellar X-rays become the main source of ionization; (2) MRI-viscosity is high throughout the disc; and (3) the pressure maximum ceases to exist. Hence, if planets form in the inner disc, larger accretion rates (and thus younger discs) are favoured.
Detecting the proposed CH4–CO2 biosignature pair with the James Webb Space Telescope: TRAPPIST-1e and the effect of cloud/haze
Authors: Mikal-Evans Thomas 
Published: November 2021

ABSTRACT
It is widely anticipated that the James Webb Space Telescope (JWST) will be transformative for exoplanet studies. It has even been suggested that JWST could provide the first opportunity to search for biosignatures in an alien atmosphere using transmission spectroscopy. This claim is investigated, specifically for the proposed anoxic biosignature pair CH4–CO2. The most favourable known target is adopted (TRAPPIST-1e), with an assumed atmospheric composition similar to the Archean Earth. Compared to previous studies, a more systematic investigation of the effect that cloud/haze layers have on the detectability of CH4 and CO2 is performed. In addition to a clear atmosphere scenario, cloud/haze layers are considered at eight pressure levels between 600 and 1 mbar. These pressures cover a plausible range for H2O cloud and photochemical haze, based on observations of solar system atmospheres and physical models of tidally locked planets such as TRAPPIST-1e, although no assumptions regarding the cloud/haze-layer composition are made in this study. For the clear atmosphere and cloud/haze-layer pressures of 600–100 mbar, strong (5σ) detections of both CH4 and CO2 are found to be possible with approximately 5–10 co-added transits measured using the Near Infrared Spectrograph (NIRSpec) prism, assuming a dry stratosphere. However, approximately 30 co-added transits would be required to achieve the same result if a cloud/haze layer is present at 10 mbar. A cloud/haze layer at 1 mbar would prevent the detection of either molecule with the NIRSpec prism for observing programmes up to 50 transits (&gt;200 h of JWST time), the maximum considered.
Gravitational waves from tidal disruption events: an open and comprehensive catalog
Authors: Toscani Martina , Lodato Giuseppe , Price Daniel J , Liptai David 
Published: November 2021

ABSTRACT
We present an online, open, and comprehensive template library of gravitational waveforms produced during the tidal disruptions of stars by massive black holes, spanning a broad space of parameters. We build this library thanks to a new feature that we implement in the general relativistic version of phantom, a smoothed particle hydrodynamics code for three dimensional simulations in general relativity. We first perform a series of numerical tests to show that the gravitational wave (GW) signal obtained is in excellent agreement with the one expected from theory. This benchmark is done for well studied scenarios (such as binary stellar systems). We then apply our code to calculate the GW signals from tidal disruption events, finding that our results are consistent with the theoretical estimates obtained in previous studies for selected parameters. We illustrate interesting results from the catalog, where we stress how the gravitational signal is affected by variations of some parameters (like black hole spin, stellar orbital eccentricity, and inclination). The full catalog is available online. It is intended to be a living catalog.
Discrepancy between SAA and CRP levels linked to the difference of SAA/CRP ratio in the patients with early rheumatoid arthritis
Authors: Uda Hiroshi , Ebisu Rika , Maeda Keiji , Saiki Osamu 
Published: November 2021

ABSTRACT

Objectives
Indeed, serum amyloid A (SAA) and C-reactive protein (CRP) reportedly seem to have moderate correlation, but discrepancies between CRP and SAA levels have often been reported in patients with early rheumatoid arthritis (ERA). This study aimed to determine the reasons for this discrepancy.

Methods
ERA patients (n = 206) were enrolled and treated with anti-RA drugs. Clinical features and disease activities were estimated. CRP and SAA levels were monitored, and the SAA/CRP ratio was compared. Correlations between CRP and SAA levels in individuals and between individuals and disease activity scores were examined.

Results
In a follow-up study, the SAA/CRP ratio remained almost constant over time in the same patients. However, SAA/CRP ratios differed widely between patients (0.233–106.3). In patients with high SAA/CRP ratios (&gt;6.52), many (26.2%) had abnormal SAA values only. In patients with low SAA/CRP ratios (&lt;6.52), not a few (6.8%) exhibited abnormal CRP values only.

Conclusions
The SAA/CRP ratio remained virtually constant in the same patients but differed dramatically between patients, which clarifies the discrepancy between CRP and SAA levels. CRP is the better marker in low-ratio patients but not in high-ratio patients; the SAA/CRP ratio is critical for its interpretation.
Surgical treatment of wrist joint dysfunction in rheumatoid arthritis: A report of two cases
Authors: Kumagai Kosuke , Takemura Yoshinori , Okumura Noriaki , Amano Yasutaka , Yayama Takafumi , Mimura Tomohiro , Mori Kanji , Barrett-Jolley Richard , Imai Shinji 
Published: November 2021

ABSTRACT
In rheumatoid arthritis (RA), it is important to actively treat wrist dysfunction to improve patient outcomes. Herein, we report two cases of wrist dysfunction in RA patients who required partial wrist fusion soon after drug initiation. Case 1: A 38-year-old woman was referred to our hospital because of left wrist joint pain. At the time of examination, swelling and tenderness of the left wrist joint were observed. After 6 months of medication, no improvement in symptoms was noted; therefore, partial wrist fusion was performed. Case 2: A 38-year-old woman was referred to our hospital because of right wrist joint pain. A plain X-ray image showed fusion of the carpal bones. Due to previous failure of drug treatment, the patient opted for arthrodesis. The postoperative course was good in both cases, and the pain improved. In these cases of monoarthritic RA, synovitis and bone destruction were observed, but blood tests showed no features of active disease, and drug treatment was ineffective. In such cases, early surgical treatment should be considered, rather than continuing conservative treatment, to ensure the best outcomes.
Identification and characterization of histones inPhysarum polycephalumevidence a phylogenetic vicinity of Mycetozoans to the animal kingdom
Authors: Poulet Axel , Mishra Laxmi Narayan , Téletchéa Stéphane , Hayes Jeffrey J , Jacob Yannick , Thiriet Christophe , Duc Céline 
Published: November 2021

AbstractPhysarum polycephalum belongs to Mycetozoans, a phylogenetic clade apart from the animal, plant and fungus kingdoms. Histones are nuclear proteins involved in genome organization and regulation and are among the most evolutionary conserved proteins within eukaryotes. Therefore, this raises the question of their conservation in Physarum and the position of this organism within the eukaryotic phylogenic tree based on histone sequences. We carried out a comprehensive study of histones in Physarum polycephalum using genomic, transcriptomic and molecular data. Our results allowed to identify the different isoforms of the core histones H2A, H2B, H3 and H4 which exhibit strong conservation of amino acid residues previously identified as subject to post-translational modifications. Furthermore, we also identified the linker histone H1, the most divergent histone, and characterized a large number of its PTMs by mass spectrometry. We also performed an in-depth investigation of histone genes and transcript structures. Histone proteins are highly conserved in Physarum and their characterization will contribute to a better understanding of the polyphyletic Mycetozoan group. Our data reinforce that P. polycephalum is evolutionary closer to animals than plants and located at the crown of the eukaryotic tree. Our study provides new insights in the evolutionary history of Physarum and eukaryote lineages.
EPCO-07. HYBRID NEURO-GLIAL CELLULAR ARCHITECTURE IN HIGH-GRADE GLIOMA DRIVEN BY H3-G34R MUTATION
Authors: Laffy Julie , Nomura Masashi , He Chen , Bussema Lillian , Slyper Michal , Hover Laura , Gritsch Simon , Regev Aviv , Baker Suzanne , Tirosh Itay , Suva Mario 
Published: November 2021

Abstract
High-grade gliomas (HGG) with histone H3.3 G34R mutation are rare intractable tumours in the cerebral hemispheres that preferentially affect adolescents and young adults, but have unknown mechanisms of neuroanatomical specificity and tumourigenesis. Here, we performed single-nucleus RNA-sequencing of twenty patient samples, encompassing twelve tumours with G34R mutation and eight H3.3 wildtype HGGs, age- and location-matched. Both classes of HGG were heterogeneous, with malignant cells in multiple states, recapitulating neural and glial developmental trajectories. G34R HGG is distinguished by lack of malignant cells in the oligodendroglial lineage, and aberrant expression of neuronal programs superimposed over cellular states, resulting in hybrid glio-neuronal malignant programs. Singe-cell barcoding supports plasticity between cellular states in HGG with multiple possible transitions. CRISPR-correction of G34R in HGG models followed by scRNA-seq supports that the G34R mutation directly drives these aberrant programs. Our study provides a framework for studying the origin and tumourigenesis of paediatric gliomas.
EPCO-15. SPATIAL-TRANSCRIPTOMICS REVEALS UNIQUE MOLECULAR FEATURES OF FLUORESCENCE-SORTED 5-AMINOLEVULINIC ACID+ INFILTRATIVE TUMOR CELLS ASSOCIATED WITH RECURRENCE AND POOR SURVIVAL IN GLIOBLASTOMA
Authors: Andrieux Geoffroy , Das Tonmoy , Smith Stuart , Rahman Ruman , Chakraborty Sajib 
Published: November 2021

Abstract
Spatiotemporal heterogeneity of glioblastoma (GBM) originating from genomic and transcriptional variation in spatially distinct sites, may contribute to subtype switching in GBM prior to and upon recurrence. Fluorescence-guided neurosurgical resection utilizing 5-aminolevulinic acid (5ALA) has enabled the isolation of infiltrative margin tumor cells (5ALA+ cells) from a background of non-neoplastic cells. To falsify the hypothesis that the 5ALA+ subpopulation(s) is defined by a unique cellular state, we have explored the spatial-transcriptomic (ST) landscape to interrogate molecular signatures unique to infiltrating 5ALA+ cells in comparison to GBM core, rim, and invasive margin non-neoplastic cells. ST analysis reveals that GBM molecular subtype plasticity is not restricted to recurrence, but manifests regionally in a cell-type-specific manner. Whilst GBM core and rim are highly enriched with Classical and Proneural subtypes, 5ALA+ cells are uniquely enriched with the Mesenchymal subtype (MES). Upregulation of the wound response pathway in 5ALA+ cells implicate hijacking of the wound healing pathway of neural cells to promote tumor growth. Exon-intron split analysis revealed an upregulation of exonic counts for MES and wound-response genes in 5ALA+ cells, implying that these genes are under active post-transcriptional control. Network analysis suggests that wound response genes, including chemokine CCL2 that recruits regulatory T-cells and monocytic myeloid-derived suppressor cells, are controlled by an IRF8-mediated transcriptional program in 5ALA+ cells. A higher stemness signature both in 5ALA+ cells and non-neoplastic cells of the invasive margin emphasizes the role of this microenvironment in stemness acquisition and defines 5ALA+ cells as a rare sub-population of GBM stem cells. Finally, we establish a link between the unique molecular-signatures of 5ALA+ cells, and poor survival and GBM recurrence. Characterization of the 5ALA+ infiltrative sub-population offers an opportunity to develop more effective GBM treatments and urges focus away from the GBM proliferative core, upon which failed targeted therapies have been predicated.