Miracle-dz/UniFAR-FTUs huggingface dataset:
Anomalous collisional absorption of laser light in plasma using particle-in-cell simulations

Collisional absorption of laser light in a homogeneous, under-dense plasma is studied by a new particle-in-cell (PIC) simulation code considering one-dimensional slab-plasma geometry. Coulomb collisions between charge particles in plasma are modeled by a Monte Carlo scheme. %[J. Comput. Phys. {\bf 25}, 205 (1977)]. %Both PIC and MC parts are individually benchmarked. For a given target thickness of a few times the wavelength of 800~nm laser of intensity $\I0$, fractional absorption ($\alpha$) of light due to Coulomb collisions (mainly between electrons and ions) is calculated at different electron temperature $\Te$ by introducing a total velocity $v = \sqrt{\vth^2 + \v0^2}$ dependent Coulomb logarithm $\ln\Lambda(v)$, where $\vth$, and $\v0$ are thermal and ponderomotive velocity of an electron. It is found that, in the low temperature regime ($\Te\lesssim15$~eV), fractional absorption of light anomalously increases with increasing $I_0$ up to a maximum corresponding to an intensity $I_c$, and then it drops when $I_0>I_c$. %(approximately) obeying the conventional scaling, i.e., %$\alpha \propto I_0^{-3/2}$ when $I_0>I_c$. Such an anomalous variation of $\alpha$ with $I_0$ in the low intensity regime was demonstrated earlier in experiments, and recently explained by classical and quantum models [Phys. Plasmas {\bf 21}, 013302 (2014); Phys. Rev. E {\bf 91}, 043102 (2015)]. % using the total velocity dependent cut-offs. %Here, we report anomalous nature of laser absorption by Here, for the first time, we report anomalous collisional laser absorption by %PIC simulations assisted by Monte Carlo collisions, PIC simulations, thus bridging the gap between models, simulations, and experimental findings.
Clinical Features, Phenotypic Markers and Outcomes of Diffuse Large B-Cell Lymphoma between HIV-Infected and HIV-Uninfected Chinese Patients

Simple Summary Diffuse large B-cell lymphoma (DLBCL) frequently occurs in HIV-infected patients. However, the effect of HIV infection on the outcome of the DLBCL population remains controversial. The aim of the present retrospective study was to compare clinical features, phenotypic markers and outcomes of BLBCL between HIV-infected and HIV-uninfected Chinese patients. Our study indicated HIV-infected DLBCL patients displayed high EBER expression but low CD20 and CD79a expression on histopathology. The overall response rate at end of chemotherapy and 1-year overall survival (OS) were low in HIV-infected patients, which may be associated with the higher incidence of leukopenia, neutropenia, thrombocytopenia and hypoalbuminemia, as well as high involvement of the central nervous system (CNS), gastrointestinal tract and bone marrow. Hypoalbuminemia and CNS involvement were independent risk factors for 1-year OS. HIV-infected DLBCL patients without CNS involvement had a favorable outcome if rituximab was included in the chemotherapy regimen. Abstract Background: The effect of HIV infection on the clinicopathological characteristics of diffuse large B-cell lymphoma (DLBCL) remains debatable. Methods: Fifty-three HIV-infected and ninety-three HIV-uninfected DLBCL patients were enrolled in the retrospective study by propensity score matching for sex, age, body mass index and international prognostic index (IPI) at a ratio of 1:2. The clinicopathological characteristics were compared between the two groups. Results: HIV-infected DLBCL patients had lower white blood cell counts [×109/L; 4.4 (3.4–5.6) vs. 6.1 (4.2–8.2), p < 0.001], platelet counts (×109/L; 184.7 ± 89.3 vs. 230.0 ± 113.9, p = 0.014) and serum albumin (g/L; 37.3 ± 6.9 vs. 41.3 ± 6.2, p < 0.001) but higher incidences of central nervous system (CNS) involvement (9.4% vs. 1.1%, p = 0.014), bone marrow involvement (24.5% vs. 11.5%, p = 0.044) and Epstein–Barr viremia (61.1% vs. 26.7%, p = 0.002) than HIV-uninfected patients. In terms of histopathology, HIV-infected patients had higher positivity of Epstein–Barr virus-encoded small RNA (EBER) (41.7% vs. 6.7%, p = 0.002), but lower CD20 (90.2% vs. 98.7%, p= 0.029) and CD79a (23.1% vs. 53.7%, p < 0.001) expression. The overall response rate (ORR) at the end of chemotherapy (70.2% vs. 87.8%, p= 0.012) and 1-year overall survival (OS) (61.7% vs. 84.2%, log-rank p = 0.006) in HIV-infected patients were significantly lower than those in HIV-uninfected patients. Multivariate analysis suggested IPI ≤2.0 [adjusted odds ratio (AOR) (95% confidence interval): 5.0 (1.2–21.2), p = 0.030] was associated with ORR, hypoalbuminemia [AOR: 3.3 (1.3–9.1), p = 0.018] and CNS involvement [AOR: 3.3 (1.0–10.5), p = 0.044] were associated with reduced 1-year OS in HIV-infected patients. Conclusion: HIV-infected DLBCL patients have unique blood profiles and phenotypic markers. Low ORR and 1-year OS were observed in HIV-infected DLBCL patients in our study, even in the HAART era.
INITIAL BEAM RESULTS FROM THE CORNELL HIGH-CURRENT ERL

Cornell University has built a high average current electron injector for use with an Energy Recovery Linac. The injector is designed for up to 100 mA average current at 5 MeV (33 mA at 15 MeV) and is expected to produce the ultra-low emittances needed for an ERL. An overview of the initial performance of this injector, the status of beam commissioning, and a summary of experiments being undertaken to demonstrate low emittance and high average current are presented.
Demographic comparison of the first, second and third waves of COVID-19 in a tertiary care hospital at Jaipur, India

Background: Coronavirus disease 2019 (COVID-19) infection in India demonstrated three peaks in India, with differences in presentation and outcome in all the three waves. The aim of the paper was to assess differences in the epidemiological, clinical features and outcomes of patients with COVID-19 presenting at a tertiary care hospital in the three waves at Jaipur, India. Methods: This was a retrospective study conducted at a tertiary care hospital at Jaipur, India. Demographic, clinical features and outcomes were compared of confirmed COVID-19 cases admitted during the first wave (16-7-2020 to 31-1-2021), second wave (16-3-2021 to 6-5-2021) and third wave (1-1-22 to 20-2-22) of the outbreak. Results: There were 1006 cases, 639 cases and 125 cases admitted during the three waves, respectively. The cases presenting in the second wave were significantly younger, with significantly higher prevalence of symptoms such as fever, cough, sore throat, nausea, vomiting, headache, muscle ache, loss of appetite and fatigue (P < 0.05). A significantly higher proportion of patients received Remdesivir in the second wave (P < 0.001). However, in the second wave, the use of low molecular weight heparin, plasma therapy, non-invasive and invasive ventilator were higher (P < 0.001). Co-morbid conditions were significantly higher in the admitted patients during the third wave (P < 0.05). Radiological scores were similar in second and third wave, significantly higher than the first wave. Lymphopenia and rise of inflammatory markers including C-reactive protein and interleukin-6 were more evident in the second wave (P < 0.001). The mean mortality, hospital stay and air-leak complications were also significantly higher in the second wave (P < 0.001). Conclusions: The second wave was more vicious in terms of symptoms, inflammatory markers, radiology, complications, requirement of ventilation and mortality. Mutation in the virus, lack of immunity and vaccination at the time point of second wave could have been the possible causes. The ferocity of the second wave has important implications for the government to formulate task forces for effective management of such pandemics.
An Evaluation of Cosmological Models from the Expansion and Growth of Structure Measurements

We compare a large suite of theoretical cosmological models to observational data from the cosmic microwave background, baryon acoustic oscillation measurements of expansion, Type Ia supernova measurements of expansion, redshift space distortion measurements of the growth of structure, and the local Hubble constant. Our theoretical models include parametrizations of dark energy as well as physical models of dark energy and modified gravity. We determine the constraints on the model parameters, incorporating the redshift space distortion data directly in the analysis. To determine whether models can be ruled out, we evaluate the p-value (the probability under the model of obtaining data as bad or worse than the observed data). In our comparison, we find the well-known tension of H0 with the other data; no model resolves this tension successfully. Among the models we consider, the large-scale growth of structure data does not affect the modified gravity models as a category particularly differently from dark energy models; it matters for some modified gravity models but not others, and the same is true for dark energy models. We compute predicted observables for each model under current observational constraints, and identify models for which future observational constraints will be particularly informative.
Is there a giant Kelvin–Helmholtz instability in the sloshing cold front of the Perseus cluster?

Deep observations of nearby galaxy clusters with Chandra have revealed concave 'bay' structures in a number of systems (Perseus, Centaurus and Abell 1795), which have similar X-ray and radio properties. These bays have all the properties of cold fronts, where the temperature rises and density falls sharply, but are concave rather than convex. By comparing to simulations of gas sloshing, we find that the bay in the Perseus cluster bears a striking resemblance in its size, location and thermal structure, to a giant ($\approx$50 kpc) roll resulting from Kelvin-Helmholtz instabilities. If true, the morphology of this structure can be compared to simulations to put constraints on the initial average ratio of the thermal and magnetic pressure, $\beta= p_{\rm th} / p_{\rm B}$, throughout the overall cluster before the sloshing occurs, for which we find $\beta=200$ to best match the observations. Simulations with a stronger magnetic field ($\beta=100$) are disfavoured, as in these the large Kelvin-Helmholtz rolls do not form, while in simulations with a lower magnetic field ($\beta=500$) the level of instabilities is much larger than is observed. We find that the bay structures in Centaurus and Abell 1795 may also be explained by such features of gas sloshing.
Triggering the formation of the supergiant H ii region NGC 604 in M 33

Formation mechanism of a supergiant H II region NGC 604 is discussed in terms of collision of H I clouds in M33. An analysis of the archival H I data obtained with the Very Large Array (VLA) reveals complex velocity distributions around NGC 604. The H I clouds are composed of two velocity components separated by ~ 20 km s^-1 for an extent of ~ 700 pc, beyond the size of the the H II region. Although the H I clouds are not easily separated in velocity with some mixed component represented by merged line profiles, the atomic gas mass amounts to 6 x 10^6 M_Sol and 9 x 10^6 M_Sol for each component. These characteristics of H I gas and the distributions of dense molecular gas in the overlapping regions of the two velocity components suggest that the formation of giant molecular clouds and the following massive cluster formation have been induced by the collision of H I clouds with different velocities. Referring to the existence of gas bridging feature connecting M33 with M31 reported by large-scale HI surveys, the disturbed atomic gas possibly represent the result of past tidal interaction between the two galaxies, which is analogous to the formation of the R136 cluster in the LMC.
The inner structure of ΛCDM haloes – II. Halo mass profiles and low surface brightness galaxy rotation curves

We use a set of high-resolution cosmological N-body simulations to investigate the inner mass profile of galaxy-sized cold dark matter (CDM) haloes. These simulations extend the numerical convergence study presented in Paper I of this series, and demonstrate that the mass profile of CDM galaxy haloes can be robustly estimated beyond a minimum converged radius of order r conv ∼ 1 h -1 kpc in our highest-resolution runs. The density profiles of simulated haloes become progressively shallower from the virial radius inwards, and show no sign of approaching a well-defined power law near the centre. At r conv , the density profile is steeper than expected from the formula proposed by Navarro, Frenk & White, which has a p α r -1 cusp, but significantly shallower than the steeply divergent p α r -1.5 cusp proposed by Moore et al. We perform a direct comparison of the spherically averaged dark matter circular velocity profiles with Ha rotation curves of a sample of low surface brightness (LSB) galaxies. We find that most galaxies in the sample (about 70 per cent) have rotation curves that are consistent with the structure of CDM haloes. Of the remainder, 20 per cent have rotation curves which cannot be fit by any smooth fitting function with few free parameters, and 10 per cent are inconsistent with CDM haloes. However, the latter consist mostly of rotation curves that do not extend to large enough radii to accurately determine their shapes and maximum velocities. We conclude that the inner structure of CDM haloes is not manifestly inconsistent with the rotation curves of LSB galaxies.
The Gaia DR2 view of the Gamma Velorum cluster: resolving the 6D structure

Gaia-ESO Survey observations of the young Gamma Velorum cluster led to the discovery of two kinematically distinct populations, Gamma Vel A and B, respectively, with population B extended over several square degrees in the Vela OB2 association. Using the Gaia DR2 data for a sample of high-probability cluster members, we find that the two populations differ not only kinematically, but are also located at different distances along the line of sight, with the main cluster Gamma Vel A being closer. A combined fit of the two populations yields ϖA = 2.895 ± 0.008 mas and ϖB = 2.608 ± 0.017 mas, with intrinsic dispersions of 0.038 ± 0.011 mas and 0.091 ± 0.016 mas, respectively. This translates into distances of 345.4+1.0+12.4−1.0−11.5 pc and 383.4+2.5+15.3−2.5−14.2 pc, respectively, showing that Gamma Vel A is closer than Gamma Vel B by ~38 pc. We find that the two clusters are nearly coeval, and that Gamma Vel B is expanding. We suggest that Gamma Vel A and B are two independent clusters located along the same line of sight.
Dynamical and Radiative Properties of X-Ray Pulsar Accretion Columns: Phase-averaged Spectra

The availability of the unprecedented spectral resolution provided by modern X-ray observatories is opening up new areas for study involving the coupled formation of the continuum emission and the cyclotron absorption features in accretion-powered X-ray pulsar spectra. Previous research focusing on the dynamics and the associated formation of the observed spectra has largely been confined to the single-fluid model, in which the super-Eddington luminosity inside the column decelerates the flow to rest at the stellar surface, while the dynamical effect of gas pressure is ignored. In a companion paper, we have presented a detailed analysis of the hydrodynamic and thermodynamic structure of the accretion column obtained using a new self-consistent model that includes the effects of both gas and radiation pressures. In this paper, we explore the formation of the associated X-ray spectra using a rigorous photon transport equation that is consistent with the hydrodynamic and thermodynamic structure of the column. We use the new model to obtain phase-averaged spectra and partially occulted spectra for Her X-1, Cen X-3, and LMC X-4. We also use the new model to constrain the emission geometry, and compare the resulting parameters with those obtained using previously published models. Our model sheds new light on the structure of the column, the relationship between the ionized gas and the photons, the competition between diffusive and advective transport, and the magnitude of the energy-averaged cyclotron scattering cross-section.
SPECTRAL COMPRESSIBILITY AT THE METAL-INSULATOR TRANSITION OF THE QUANTUM HALL EFFECT

The spectral properties of a disordered electronic system at the metal-insulator transition point are investigated numerically. A recently derived relation between the anomalous diffusion exponent $\eta$ and the spectral compressibility $\chi$ at the mobility edge, $\chi=\eta/2d$, is confirmed for the integer quantum Hall delocalization transition. Our calculations are performed within the framework of an unitary network-model and represent a new method to investigate spectral properties of disordered systems.
Scalar field dark matter in hybrid approach

We develop a hybrid formalism suitable for modeling scalar field dark matter, in which the phase-space distribution associated with the real scalar field is modeled by statistical equal-time two-point functions and gravity is treated by two stochastic gravitational fields in the longitudinal gauge (in this work we neglect vector and tensor gravitational perturbations). Inspired by the commonly used Newtonian Vlasov-Poisson system, we firstly identify a suitable combination of equal-time two-point functions that defines the phase-space distribution associated with the scalar field and then derive both a kinetic equation that contains relativistic scalar matter corrections as well as linear gravitational scalar field equations whose sources can be expressed in terms of a momentum integral over the phase-space distribution function. Our treatment generalizes the commonly used classical scalar field formalism, in that it allows for modeling of (dynamically generated) vorticity and perturbations in anisotropic stresses of the scalar field. It also allows for a systematic inclusion of relativistic and higher-order corrections that may be used to distinguish different dark matter scenarios. We also provide initial conditions for the statistical equal-time two-point functions of the matter scalar field in terms of gravitational potentials and the scale factor.
The impact of product name on consumer responses to meat alternatives

Purpose With the recent surge of plant-based menu items, it is critical to understand how to effectively communicate such products to consumers. This study aims to examine the impact of various descriptive names on consumers’ responses to novel meat alternatives in China, one of the emerging yet unexplored markets. Design/methodology/approach Two studies were conducted using a single factor ([descriptive name: “Renzao Rou [artificial meat]” vs “Sushi Rou [vegetarian/vegan meat]” vs “Zhiwu Rou” [plant-based meat]) between-subjects experimental design. Findings Study 1 shows that “Sushi Rou” and “Zhiwu Rou,” triggering more positive name associations, led to higher future consumption intention than “Renzao Rou. ” A qualitative analysis demonstrates the differences in the name associations. Study 2 replicates the naming effect and examines the role of specific product attributes. Perceived health, naturalness and novelty are the main drivers of favorable responses to “Zhiwu Rou” (vs “Renzao Rou”), whereas perceived health, taste and naturalness mediate the positive effect for “Sushi Rou” (vs “Renzao Rou”). Practical implications Food service operators interested in introducing meat alternatives in China should carefully choose the product name to attract specific segments. International chains should consider cultural norms when expanding to emerging markets. Originality/value To the best of the authors’ knowledge, this study is the first to reveal the product naming effect on meat alternative products from the perspective of marketing communications. It contributes to a deeper understanding of the underlying mechanism driving Chinese consumers’ responses.
Cosmological solutions in generalized hybrid metric-Palatini gravity

We construct exact solutions representing a Friedmann-Lema\^itre-Robsertson-Walker (FLRW) universe in a generalized hybrid metric-Palatini theory. By writing the gravitational action in a scalar-tensor representation, the new solutions are obtained by either making an ansatz on the scale factor or on the effective potential. Among other relevant results, we show that it is possible to obtain exponentially expanding solutions for flat universes even when the cosmology is not purely vacuum. We then derive the classes of actions for the original theory which generate these solutions.
The Fall of a Giant. Chemical evolution of Enceladus, alias the Gaia Sausage

In this Letter, we present the first chemical evolution model for Enceladus, alias the Gaia Sausage, to investigate the star formation history of one of the most massive satellites accreted by the Milky Way during a major merger event. Our best chemical evolution model for Enceladus nicely fits the observed stellar [$\alpha$/Fe]-[Fe/H] chemical abundance trends, and reproduces the observed stellar metallicity distribution function, by assuming low star formation efficiency, fast gas accretion time scale, and mild outflow intensity. We find that $80$ per cent of Enceladus stars have ages $>11.7$ Gyr. At the time of the merger with the Milky Way, we find for Enceladus a stellar mass $M_{\star} \approx 5 \times 10^{9} \text{M}_{\odot}$, with a gas fraction of $\sim 0.25$, if the assumed infall mass is $M_{\text{inf}}=10^{10}\,\text{M}_{\odot}$. The comparison between the age distribution of the stars in Enceladus from our best chemical evolution model and the predicted star formation history of the two-infall models of Noguchi (2018) and Spitoni et al. (2018) seems to suggest that a merger event between the Galaxy and systems like Enceladus could have been capable of inhibiting the gas accretion onto the Galaxy disc, heating up the gas in the halo at high redshifts. To firmly confirm or reject this hypothesis, however, we will need in the future more precise age measurements of Enceladus stars than those coming from isochrone-fitting analysis or chemical tagging like in this work, as achievable by means of asteroseismic techniques.
Orbital evolution in binary systems with giant stars

Using 3D radiation-hydrodynamic simulations and analytic theory, we analyze the orbital evolution of asymptotic-giant-branch (AGB) binary systems for various initial orbital separations and mass ratios, and thus different initial accretion modes. We present a convenient analytic framework to calculate the rate of orbital period change using input from simulations. We find that the angular momentum carried away by the L2 Lagrange point mass loss can effectively shrink the orbit when accretion occurs via wind-Roche-lobe overflow. This is in contrast to the large mass loss in Bondi-Hoyle accretion systems which acts to enlarge the orbit. We find that orbital period decay in AGB binary systems is faster when one accounts for the nonlinear evolution of the accretion mode as the binary starts to tighten. This can increase the fraction of binaries that result in common envelope, luminous red novae, Type Ia supernovae and planetary nebulae with tight central binaries. The results have implications for the probability and properties of planets orbiting closely around white dwarfs.