bluuebunny/crossref_metadata_2025_split huggingface dataset:
P142 Lodderomyces elongisporus: A n emerging cause of fung emia
Authors: Kaur Harsimran , Gupta Parakriti , Shankarnarayan Shamanth , Pandey Abhishek , Ghosh Anup , Chakrabarti Arunaloke , Rudramurthy Shivaprakash 
Published: September 2022

Abstract

Poster session 2, September 22, 2022, 12:30 PM - 1:30 PM

Background
Lodderomyces elongisporus, earlier considered as a sexual state of Candida parapsilosis, was described as a distinct species based on ribosomal RNA gene sequencing. Few cases of human infections by this yeast have been described from Mexico, China, Malaysia, Kuwait, Australia, and the USA. We describe here eight cases of fungemia by L. elongisporus from a tertiary care hospital in North India.

Methods
Clinical characteristics and risk factors associated with L. elongisporus fungaemia were evaluated. Yeast isolated from blood culture (BD BACTEC™ 9240, New Jersey, USA) was identified by matrix-assisted laser desorption/ionization time-of-flight mass spectroscopy (MALDI-TOF MS, Bruker Daltonik GmbH, Bremen, Germany) and sequencing of D1/D2 region of a large subunit of ribosomal DNA. We performed antifungal susceptibility testing for amphotericin B, fluconazole, itraconazole, voriconazole, posaconazole, caspofungin, anidulafungin, and micafungin by the microbroth dilution method recommended by the Clinical and Laboratory Standards Institute (CLSI).

Results
We report eight cases of fungemia caused by L. elongisporus at our tertiary care center. Of these, three were infants (males) and five were adults (3 males and 2 females). The mean age of adults was 43.4 years. Among the pediatric cases, underlying diseases included congenital heart disease/atrophic kidney (neonate), tracheoesophageal fistula (4 months), and late-onset neonatal sepsis (LONS). Among the adults, underlying illnesses included acute kidney injury (n = 2), superior mesenteric artery thrombosis with bowel gangrene (n = 1), diabetes (n = 1), and central nervous system (CNS) lymphoma (n = 1). The iatrogenic factors included the history of surgery (n = 3), admission to ICU (n = 3), presence of urinary catheter (n = 4), and presence of central venous catheter (n = 1). Seven patients were on broad-spectrum antibiotics. The mean stay in the hospital was 20.38 days. Three of the patients were managed with fluconazole. Six patients improved while one left against medical advice (LAMA) and one expired. The range of minimum inhibitory concentration (MIC) of all the isolates against antifungals was as follows: amphotericin B (0.03-0.25 μg/ml), fluconazole (0.125 μg/ml), voriconazole (0.03 μg/ml), itraconazole (0.03-0.06 μg/ml), posaconazole (0.03-0.25 μg/ml), caspofungin (0.03-0.06 μg/ml), micafungin (0.03-0.06 μg/ml), and anidulafungin (0.03 μg/ml).

Conclusion
Lodderomyces elongisporus is an emerging pathogenic yeast causing fungemia in patients with comorbidities and undergoing surgery or invasive interventions. Though no antifungal breakpoints exist for this yeast, all the isolates exhibited low MICs to all the tested antifungals.
S2.5d Exploring multidrug resistance, fitness compensation, and collateral sensitivity in Candida auris : Fight fire with fire?
Authors: Carolus Hans , Sofras Dimitrios , Sephton-Clark Poppy , Goossens Louise , Chen Alicia , Pierson Siebe , Romero Celia Lobo , Subotić Ana , Meis Jacques F. , Cuomo Christina A. , Van Dijck Patrick 
Published: September 2022

Abstract

S2.5 Rare yeasts, September 21, 2022, 3:00 PM - 4:30 PM
Candida auris (C. auris) is a recently emerged human fungal pathogen of growing concern due to its ability to acquire extensive multidrug resistance (MDR) to all four antifungal drug classes. The unprecedented extent of MDR in C. auris, suggests accelerated resistance evolution, novel mechanisms of resistance, and/or potential fitness compensation. Despite being the first fungus to be officially considered an urgent antimicrobial resistance threat by the CDC (US), insights into the resistance mechanisms and evolutionary dynamics of C. auris are still scarce.

By using high-throughput in vitro experimental evolution with various antifungal drugs, we have obtained a library of resistant strains from four different clades. Through both genome and targeted sequencing, we have discovered novel mutations, especially for polyene resistance, which indicate new mechanisms of resistance and fitness compensation. For the validation of mutations, we have optimized a recyclable CRISPR/Cas9 tool for C. auris based on the C. albicans HIS-FLP system.

By mapping drug susceptibility responses of evolved strains across a library of several antifungals and repurposed drugs, we have discovered trends of cross-resistance and collateral sensitivity. Both phenomena have been extensively studied in tumors and bacteria but remain unexplored in fungi. In the light of these observations, we explore novel treatment schemes that prevent antifungal drug resistance development in C. auris and other pathogenic fungi.
Real-time detection of anomalies in large-scale transient surveys
Authors: Muthukrishna Daniel , Mandel Kaisey S , Lochner Michelle , Webb Sara , Narayan Gautham 
Published: September 2022

ABSTRACT
New time-domain surveys, such as the Vera C. Rubin Observatory Legacy Survey of Space and Time, will observe millions of transient alerts each night, making standard approaches of visually identifying new and interesting transients infeasible. We present two novel methods of automatically detecting anomalous transient light curves in real-time. Both methods are based on the simple idea that if the light curves from a known population of transients can be accurately modelled, any deviations from model predictions are likely anomalies. The first modelling approach is a probabilistic neural network built using Temporal Convolutional Networks (TCNs) and the second is an interpretable Bayesian parametric model of a transient. We demonstrate our methods’ ability to provide anomaly scores as a function of time on light curves from the Zwicky Transient Facility. We show that the flexibility of neural networks, the attribute that makes them such a powerful tool for many regression tasks, is what makes them less suitable for anomaly detection when compared with our parametric model. The parametric model is able to identify anomalies with respect to common supernova classes with high precision and recall scores, achieving area under the precision-recall curves above 0.79 for most rare classes such as kilonovae, tidal disruption events, intermediate luminosity transients, and pair-instability supernovae. Our ability to identify anomalies improves over the lifetime of the light curves. Our framework, used in conjunction with transient classifiers, will enable fast and prioritized followup of unusual transients from new large-scale surveys.
Polar alignment of a massive retrograde circumbinary disc around an eccentric binary
Authors: Abod Charles P , Chen Cheng , Smallwood Jeremy , Rabago Ian , Martin Rebecca G , Lubow Stephen H 
Published: September 2022

ABSTRACT
A test particle orbit around an eccentric binary has two stationary states in which there is no nodal precession: coplanar and polar. Nodal precession of a misaligned test particle orbit centres on one of these stationary states. A low-mass circumbinary disc undergoes the same precession and moves towards one of these states through dissipation within the disc. For a massive particle orbit, the stationary polar alignment occurs at an inclination less than 90°, which is the prograde-polar stationary inclination. A sufficiently high angular momentum particle has an additional higher inclination stationary state, the retrograde-polar stationary inclination. Misaligned particle orbits close to the retrograde-polar stationary inclination are not nested like the orbits close to the other stationary points. We investigate the evolution of a gas disc that begins close to the retrograde-polar stationary inclination. With hydrodynamical disc simulations, we find that the disc moves through the unnested crescent shape precession orbits and eventually moves towards the prograde-polar stationary inclination, thus increasing the parameter space over which circumbinary discs move towards polar alignment. If protoplanetary discs form with an isotropic orientation relative to the binary orbit, then polar discs may be more common than coplanar discs around eccentric binaries, even for massive discs. This has implications for the alignment of circumbinary planets.
Variability due to climate and chemistry in observations of oxygenated Earth-analogue exoplanets
Authors: Cooke G J , Marsh D R , Walsh C , Rugheimer S , Villanueva G L 
Published: September 2022

ABSTRACT
The Great Oxidation Event was a period during which Earth’s atmospheric oxygen (O2) concentrations increased from ∼10−5 times its present atmospheric level (PAL) to near modern levels, marking the start of the Proterozoic geological eon 2.4 billion years ago. Using WACCM6, an Earth System Model, we simulate the atmosphere of Earth-analogue exoplanets with O2 mixing ratios between 0.1 and 150 per cent PAL. Using these simulations, we calculate the reflection spectra over multiple orbits using the Planetary Spectrum Generator. We highlight how observer angle, albedo, chemistry, and clouds affect the simulated observations. We show that inter-annual climate variations, as well short-term variations due to clouds, can be observed in our simulated atmospheres with a telescope concept such as LUVOIR or HabEx. Annual variability and seasonal variability can change the planet’s reflected flux (including the reflected flux of key spectral features such as O2 and H2O) by up to factors of 5 and 20, respectively, for the same orbital phase. This variability is best observed with a high-throughput coronagraph. For example, HabEx (4 m) with a starshade performs up to a factor of two times better than a LUVOIR B (6 m) style telescope. The variability and signal-to-noise ratio of some spectral features depends non-linearly on atmospheric O2 concentration. This is caused by temperature and chemical column depth variations, as well as generally increased liquid and ice cloud content for atmospheres with O2 concentrations of &lt;1 per cent PAL.
An exploration of dust grain growth within WCd systems using an advected scalar dust model
Authors: Eatson J W , Pittard J M , Van Loo S 
Published: September 2022

ABSTRACT
Dust production is one of the more curious phenomena observed in massive binary systems with interacting winds. The high temperatures, UV photon flux, and violent shocks should destroy any dust grains that condense. However, in some extreme cases, dust production yields of approximately 30 per cent of the total mass-loss rate of the stellar winds have been observed. In order to better understand this phenomenon, a parameter space exploration was performed using a series of numerical models of dust producing carbon phase Wolf–Rayet (WCd) systems. These models incorporated a passive scalar dust model simulating dust growth, destruction, and radiative cooling. We find that reasonable dust yields were produced by these simulations. Significant changes in the dust yield were caused by changing the mass-loss rates of the stars, with a greater mass-loss rate contributing to increased dust yields. Similarly, a close orbit between the stars also resulted in higher dust yields. Finally, a high-velocity wind shear, which induces Kelvin–Helmholtz (KH) instabilities and wind mixing, drastically increases the dust yields.
Comprehensive bayesian modeling of tidal circularization in open cluster binaries part I: M 35, NGC 6819, NGC 188
Authors: Penev Kaloyan M , Schussler Joshua A 
Published: September 2022

Abstract
Tidal friction has long been recognized to circularize the orbits of binary stars over time. In this study, we use the observed distribution of orbital eccentricities in populations of binary stars to probe tidal dissipation. In contrast to previous studies, we incorporate a host of physical effects often neglected in other analyses, provide a much more general description of tides, model individual systems in detail (in lieu of population statistics), and account for all observational uncertainties. The goal is to provide a reliable measurement of the properties of tidal dissipation that is fully supported by the data, properly accounts for different dissipation affecting each tidal wave on each object separately, and evolves with the internal structure of the stars. We extract high precision measurements of tidal dissipation in short period binaries of Sun-like stars in three open clusters. We find that the tidal quality factor on the main sequence falls in the range $5.7 &lt; \log _{10}Q_\star ^{\prime } &lt; 6$ for tidal periods between 3 and 7.5 days. In contrast, the observed circularization in the 150 Myr old M 35 cluster requires that pre-main sequence stars are much more dissipative: $Q_\star ^{\prime } &lt; 4\times 10^4$. We test for frequency dependence of the tidal dissipation, finding that for tidal periods between 3 and 7.5 days, if a dependence exists, it is sub-linear for main-sequence stars. Furthermore, by using a more complete physical model for the evolution, and by accounting for the particular properties of each system, we alleviate previously observed tensions in the circularization in the open clusters analyzed.
Oscillation modes and gravitational waves from strangeon stars
Authors: Li Hong-Bo , Gao Yong , Shao Lijing , Xu Ren-Xin , Xu Rui 
Published: September 2022

Abstract
The strong interaction at low energy scales determines the equation of state (EOS) of supranuclear matters in neutron stars (NSs). It is conjectured that the bulk dense matter may be composed of strangeons, which are quark clusters with nearly equal numbers of u, d, and s quarks. To characterize the strong-repulsive interaction at short distance and the nonrelativistic nature of strangeons, a phenomenological Lennard-Jones model with two parameters is used to describe the EOS of strangeon stars (SSs). For the first time, we investigate the oscillation modes of non-rotating SSs and obtain their frequencies for various parameterizations of the EOS. We find that the properties of radial oscillations of SSs are different from those of NSs, especially for stars with relatively low central energy densities. Moreover, we calculate the f-mode frequency of nonradial oscillations of SSs within the relativistic Cowling approximation. The frequencies of the f-mode of SSs are found to be in the range from 6.7 kHz to $8.7\, \rm {kHz}$. Finally, we study the universal relations between the f-mode frequency and global properties of SSs, such as the compactness and the tidal deformability. The results we obtained are relevant to pulsar timing and gravitational waves, and will help to probe NSs’ EOSs and infer nonperturbative behaviours in quantum chromodynamics.
Forced eccentricity in circumbinary discs
Authors: Lubow Stephen H 
Published: September 2022

ABSTRACT
We analyse the eccentric response of a low-mass coplanar circumbinary disc to secular tidal forcing by a Keplerian eccentric orbit central binary. The disc acquires a forced eccentricity whose magnitude depends on the properties of the binary and disc. The largest eccentricities occur when there is a global apsidal resonance in the disc. The driving frequency by the binary is its apsidal frequency, which is equal to zero. A global resonance occurs when the disc properties permit the existence of a zero apsidal frequency free eccentric mode. Resonances occur for different free eccentric modes, which differ in the number of radial nodes. For a disc not at resonance, the eccentricity distribution has somewhat similar form to the eccentricity distributions in discs at resonance that have the closest matching disc aspect ratios. For higher disc aspect ratios, the forced eccentricity distribution in a 2D disc is similar to that of the fundamental free mode. The forced eccentricity distribution in a 3D disc is similar to that of higher order free modes, not the fundamental mode, unless the disc is very cool. For parameters close to resonance, large phase shifts occur between the disc and binary eccentricities that are locked in phase. Forced eccentricity may play an important role in the evolution of circumbinary discs and their central binaries.
Detection of a quasi-periodic oscillation at ∼40 mHz in Cen X-3 with Insight-HXMT
Authors: Liu Q , Wang W , Chen X , Yang W , Lu F J , Song L M , Qu J L , Zhang S , Zhang S N 
Published: September 2022

ABSTRACT
We investigated the quasi-periodic oscillation (QPO) features in the accretion-powered X-ray pulsar Cen X-3 observed by Insight-HXMT. For two observations in 2020 when Cen X-3 was in an extremely soft state, the power density spectrum revealed the presence of obvious QPO features at ∼40 mHz with an averaged fractional rms amplitude of ∼9 per cent. We study the mHz QPO frequency and rms amplitude over orbital phases, and find that the QPO frequency is ∼33–39 mHz at the orbital phase of 0.1–0.4, increasing to ∼37–43 mHz in the orbital phase of 0.4–0.8, but has no strong dependence on X-ray intensity. We also carried out an energy-dependent QPO analysis, the rms amplitude of the mHz QPOs have a decreasing trend as the energy increases from 2 to 20 keV. In addition, the QPO time-lag analysis shows that the time-delay is ∼20 ms (a hard lag) in the range of ∼5–10 keV, and becomes negative [time-lag of −(20–70) ms] above ∼10 keV. The different QPO theoretical models are summarized and discussed. In the end, we suggest that these energy-dependent timing features as well as the origin of mHz QPOs in Cen X-3 may be ascribed to an instability when the accretion disc is truncated near the corotation radius.
The early evolution of magnetar rotation – I. Slowly rotating ‘normal’ magnetars
Authors: Prasanna Tejas , Coleman Matthew S B , Raives Matthias J , Thompson Todd A 
Published: September 2022

ABSTRACT
In the seconds following their formation in core-collapse supernovae, ‘proto’-magnetars drive neutrino-heated magnetocentrifugal winds. Using a suite of two-dimensional axisymmetric magnetohydrodynamic simulations, we show that relatively slowly rotating magnetars with initial spin periods of P⋆0 = 50–500 ms spin down rapidly during the neutrino Kelvin–Helmholtz cooling epoch. These initial spin periods are representative of those inferred for normal Galactic pulsars, and much slower than those invoked for gamma-ray bursts and superluminous supernovae. Since the flow is non-relativistic at early times, and because the Alfvén radius is much larger than the proto-magnetar radius, spin-down is millions of times more efficient than the typically used dipole formula. Quasi-periodic plasmoid ejections from the closed zone enhance spin-down. For polar magnetic field strengths B0 ≳ 5 × 1014 G, the spin-down time-scale can be shorter than the Kelvin–Helmholtz time-scale. For B0 ≳ 1015 G, it is of the order of seconds in early phases. We compute the spin evolution for cooling proto-magnetars as a function of B0, P⋆0, and mass (M). Proto-magnetars born with B0 greater than $\simeq 1.3\times 10^{15}\, {\rm \, G}\, (P_{\star 0}/{400\, \rm \, ms})^{-1.4}(M/1.4\, {\rm M}_\odot)^{2.2}$ spin down to periods &gt;1 s in just the first few seconds of evolution, well before the end of the cooling epoch and the onset of classic dipole spin-down. Spin-down is more efficient for lower M and for larger P⋆0. We discuss the implications for observed magnetars, including the discrepancy between their characteristic ages and supernova remnant ages. Finally, we speculate on the origin of 1E 161348−5055 in the remnant RCW 103, and the potential for other ultra-slowly rotating magnetars.
Mapping time-dependent magnetic topologies of active stars
Authors: Finociety B , Donati J-F 
Published: September 2022

ABSTRACTThroughout the last decades, Zeeman–Doppler Imaging (ZDI) has been intensively used to reconstruct large-scale magnetic topologies of active stars from time-series of circularly polarized (Stokes V) profiles. ZDI being based on the assumption that the topology to be reconstructed is constant with time (apart from being sheared by differential rotation), it fails at describing stellar magnetic fields that evolve on time-scales similar to the observing period. We present a new approach, called TIMeS (for Time-dependent Imaging of Magnetic Stars), to derive the time-dependent large-scale magnetic topologies of active stars, from time-series of high-resolution Stokes V spectra. This new method uses the combined concepts of sparse approximation and Gaussian process regression to derive the simplest time-dependent magnetic topology consistent with the data. Assuming a linear relation between the Stokes V data and the reconstructed magnetic image, TIMeS is currently applicable to cases in which the magnetic field is not too strong (with an upper limit depending on v sin i). We applied TIMeS to several simulated data sets to investigate its ability to retrieve the poloidal and toroidal components of large-scale magnetic topologies. We find that the proposed method works best in conditions similar to those needed for ZDI, reconstructing reliable topologies with minor discrepancies at very low latitudes whose contribution to the data is small. We, however, note that TIMeS can fail at reconstructing the input topology when the field evolves on a time-scale much shorter than the stellar rotation cycle.
Genetic evidence for multiple mating and mixing of sperm from multiple males in the seminal receptacles of female Japanese flying squid (Todarodes pacificus)
Authors: Ohtani Ryusei , Yamamoto Jun , Yanagimoto Takashi , Adachi Kohsuke , Bower John R , Fujioka Hidefumi A , Hirose Miyuki , Nakaya Mitsuhiro , Suzuki Satoshi , Tokioka Shun 
Published: September 2022

ABSTRACT
The genetic diversity of sperm and spermatangia stored by mated Japanese flying squid (Todarodes pacificus) was examined to better understand how this ommastrephid squid mates and stores sperm. Analyses were conducted using spermatangia implanted in the lips of immature squid collected in Tsugaru Strait, northern Japan, in July–August 2019, spermatangia implanted in the lips of mature squid collected in the East China Sea in April 2019, and sperm stored in the seminal receptacles of squid collected off Tosashimizu, Kochi Prefecture, Japan, in February 2019. DNA was extracted, microsatellite loci were amplified using five PCR primers, and allele peaks were analysed. Analysis of the spermatangia confirmed that females in the field mate with multiple males, suggesting that males transfer from 1 to at least 14 spermatangia in each mating. Analysis of the seminal receptacles showed that sperm from multiple males are mixed within individual sperm chambers. Spermatangia were also found implanted in the lips of males, providing evidence of same-sex sexual behaviour. To date, studies of cephalopod mating systems have focused on coastal species, and the results of this study add to our growing knowledge of more oceanic species.