Miracle-dz/UniFAR-FTUs huggingface dataset:
A Real-Data Numerical Study of the Development of Precipitation along the Edge of an Elevated Mixed Layer

Abstract An 18-h numerical simulation of the weather associated with the severe-storm outbreak in the region of the Texas-Oklahoma panhandles, during the AVE-SESAME IV study period (9–10 May 1979), was performed using the Pennsylvania State University/National Center for Atmospheric Research (PSU/NCAR) mesoscale model. This simulation and the related sensitivity tests provided the four-dimensional data sets that were used to reach a better understanding of the processes that were involved in this case in the development of severe convection along the edge of the elevated mixed layer (EML). The sensitivity studies were performed to isolate the contributions of differential surface forcing, latent heating and the low-level moisture gradient to the development of the underrunning, its intensification, and the heavy rainfall. These studies showed that the differential surface heating at the edge of the EML is the most important single factor responsible for initiating the underrunning, and therefore the preci.
GENERALIZED GAUSSIAN SUMS CHERN-SIMONS-WITTEN-JONES INVARIANTS OF LEN-SPACES

Starting from evaluating all Gaussian sums, we calculate {τr, r≥2} (in the 4r-th cyclotomic fields) and {ξr, r odd≥3} (in the r-th cyclotomic fields) for all lens spaces L(p, q). We prove that they are all algebraic integers and show that ξr determines the Dedekind sum s(q, p), and hence determines the generalized Casson invariant of lens space. We conjecture these two properties hold for more general 3-manifold, and some evidences are discussed. Though the formulae are not simple, we are able to give necessary and sufficient conditions for lens spaces to have the same CSWJ invariants. Examples of lens spaces with the same invariants but different topological types are given. Some applications in number theory are also included.
Beyond Thimbles: Sign-Optimized Manifolds for Finite Density

The sign problem of relativistic field theories at finite fermion chemical potential has been approached by deforming the domain of integration into complex field space. We present a method for selecting a deformed manifold of integration which is a local maximum of the average phase, and demonstrate this method on the three-dimensional Thirring model. Finally, we compare the performance of this method, in the heavy-dense limit, to direct integration on the Lefschetz thimbles.
ALMA Multiple-transition Observations of High-density Molecular Tracers in Ultraluminous Infrared Galaxies

We present the results of our ALMA observations of 11 (ultra)luminous infrared galaxies ((U)LIRGs) at J = 4–3 of HCN, HCO+, and HNC and J = 3–2 of HNC. This is an extension of our previously published HCN and HCO+ J = 3–2 observations to multiple rotational J-transitions of multiple molecules, to investigate how molecular emission line flux ratios vary at different J-transitions. We confirm that ultraluminous infrared galaxies (ULIRGs) that contain or may contain luminous obscured active galactic nuclei (AGNs) tend to show higher HCN-to-HCO+ flux ratios than starburst galaxies, both at J = 4–3 and J = 3–2. For selected HCN-flux-enhanced AGN-important ULIRGs, our isotopologue H13CN, H13CO+, and HN13C J = 3–2 line observations suggest a higher abundance of HCN than HCO+ and HNC, which is interpreted to be primarily responsible for the elevated HCN flux in AGN-important galaxies. For such sources, the intrinsic HCN-to-HCO+ flux ratios after line opacity correction will be higher than the observed ratios, making the separation between AGNs and starbursts even larger. The signature of the vibrationally excited (v2 = 1f) HCN J = 4–3 emission line is seen in one ULIRG, IRAS 12112−0305 NE. P Cygni profiles are detected in the HCO+ J = 4–3 and J = 3–2 lines toward IRAS 15250+3609, with an estimated molecular outflow rate of ∼250–750 M⊙ yr−1. The SiO J = 6–5 line also exhibits a P Cygni profile in IRAS 12112+0305 NE, suggesting the presence of shocked outflow activity. Shock tracers are detected in many sources, suggesting ubiquitous shock activity in the nearby ULIRG population.
On the Shapes of Interstellar Grains: Modeling Extinction and Polarization by Speroids and Continuous Distributions of Ellipsoids

Although interstellar grains are known to be aspherical, their actual shapes remain poorly constrained. We assess whether three distributions of ellipsoidal shapes from the literature, employed principally for their convenient mathematical properties, are suitable for describing the shapes of interstellar grains. Randomly-selected shapes from each distribution are shown as illustrations. The often-used BHCDE distribution includes a very large fraction of extreme shapes: fully 10% of random draws have axial ratio a_3/a_1 > 19.7, and 5% have a_3/a_1 > 33. Of the three distributions considered, the CDE2 appears to be most realistic. For each of the three CDEs considered, we derive shape-averaged cross sections for extinction and polarization. Finally, we describe a method for "synthesizing" a dielectric function for an assumed shape or shape distribution if the actual absorption cross sections per grain volume are known from observations. This synthetic dielectric function predicts the wavelength dependence of polarization, which can then be compared to observations to constrain the grain shape.
Phase structure and critical processes of spectral curves in large N dualities

We examine the phase structure and the critical processes of the spectral curves that arise in the study of large N dualities between supersymmetric Yang-Mills theories and string models on local Calabi-Yau manifolds. These spectral curves are determined by a set of complex partial 't Hooft parameters and a system of cuts given by projections on the spectral curve of minimal supersymmetric cycles of the underlying Calabi-Yau manifold. Using a combination of analytical and numerical methods we give a complete description of the one-cut phase in the cubic model, determine the analytic condition satisfied by critical one-cut spectral curves, and give an algorithm to calculate the two-cut spectral curves of the cubic model for generic values of the partial 't Hooft parameters.
New inhomogeneous universes in scalar-tensor and f(R) gravity

A new family of spherically symmetric inhomogeneous solutions of Brans-Dicke gravity is generated using conformal transformation techniques and the Fonarev solution of general relativity as a seed. The latter is mapped from the Einstein to the Jordan conformal frame and this Jordan frame version constitutes a new solution of Brans-Dicke theory. The Brans-Dicke scalar field self-interacts with a power-law or inverse power-law potential in the Jordan frame. The new 4-parameter family of geometries thus generated, which is dynamical and asymptotically Friedmann-Lemaitre-Robertson-Walker, contains as special cases two previously known classes of solutions and solves also the field equations of f(R)=Rn gravity, which can also be seen as an ω=0 Brans-Dicke theory with a potential.
Formation and critical collapse of Skyrmions

We study first order phase transitions in the gravitational collapse of spherically symmetric skyrmions. Static sphaleron solutions are shown to play the role of critical solutions separating black-hole spacetimes from no-black-hole spacetimes. In particular, we find a new type of first order phase transition where subcritical data do not disperse but evolve towards a static regular stable solution. We also demonstrate explicitly that the near-critical solutions depart from the intermediate asymptotic regime along the unstable manifold of the critical solution.
Radio Emission from the Vela?Puppis Region

The Vela-Puppis region has been surveyed with Mills Cross radio telescopes, and radio isophotes plotted at two wavelengths. Many discrete sources have been observed. Several H II regions have been detected in emission at 3·5 m and in absorption at 15·2 m; the radiation from such objects is of thermal origin. The outstanding feature of this region is a group of strong non-thermal sources near the galactic equator. These are superimposed on an intense belt of radiation along the equator, and this, too, is certainly non-thermal in origin. Some correlation with galactic structure is suggested.
NSV 1440: first WZ Sge-type object in AM CVn stars and candidates

In 2015 and 2017, the AM CVn candidate NSV 1440 showed superoutbursts having the characteristic features of WZ Sge-type dwarf novae (DNe). By analogy with hydrogen-rich cataclysmic variables (CVs), we can interpret these outbursts as `double superoutbursts' which are composed of the first superoutburst with early superhumps and the second superoutburst with ordinary superhumps. The object also showed multiple rebrightenings after the main superoutbursts. Early superhumps had been never observed in AM CVn stars and candidates, thus NSV 1440 is the first confirmed WZ Sge-type AM CVn candidate. We obtained the early superhump period of 0.0252329(49) d and the growing (stage A) superhumps period of 0.025679(20) d from the 2015 superoutburst. We regarded the early superhump period as the orbital one. By using these periods we estimated the mass ratio $q = $0.045(2). This value suggests that NSV 1440 is indeed an AM CVn star and that the secondary is a semi-degenerate star.
Using the phase shift to asymptotically characterize the dipolar mixed modes in post-main-sequence stars

Mixed modes have been extensively observed in post-main-sequence stars by the Kepler and CoRoT space missions. The mixture of the p and g modes can be measured by the dimensionless coefficient $q$, the so-called coupling strength factor. In this paper we discuss the utility of the phase shifts $\theta$ from the eigenvalue condition for mixed modes as a tool to characterize dipolar mixed modes from the theoretical as well as the practical point of view. Unlike the coupling strength, whose variation in a given star is very small over the relevant frequency range, the phase shifts vary significantly for different modes. The analysis in terms of $\theta$ can also provide a better understanding of the pressure and gravity radial order for a given mixed mode. Observed frequencies of the Kepler red-giant star KIC 3744043 are used to test the method. The results are very promising.
How do different motives for R&D cooperation affect firm performance? – An analysis based on Swiss micro data

The starting point of our analysis is the empirical fact that firms pursue different goals when getting engaged in R&D collaborations, often more than one goal at the same time. Given that firms are driven by different motives for R&D cooperation, the aim of this article is to investigate the differences related to different motives with respect to the impact of R&D cooperation on firm innovativeness and firm productivity. Not only R&D cooperation in general but also cooperation driven by each of the seven motives considered in this paper correlate positively with the sales share of innovative products. With respect to innovativeness, the characterization of cooperation by the driving motive did not add much more than could be gained through the overall variable ‘R&D cooperation yes/no’. Technology-motivated collaborative activities show a weaker tendency to positive direct effects on productivity than cost-motivated cooperation. In this case, the distinction of several cooperation motives yields some additional insights as compared to the overall cooperation variable. On the whole, distinguishing various cooperation motives appears to be fruitful because it allows more differentiated insights that would remain hidden behind the overall variable “R&D cooperation yes/no”.
Initial conditions of the Universe: A sign of the sine mode

In the standard big bang model the universe starts in a radiation dominated era, where the gravitational perturbations are described by second order differential equations, which will generally have two orthogonal set of solutions. One is the so called {\it growing(cosine)} mode and the other is the {\it decaying(sine)} mode, where the nomenclature is derived from their behaviour on super-horizon(sub-horizon) scales. The decaying mode is qualitatively different to the growing mode of adiabatic perturbations as it evolves with time on \emph{super-horizon} scales. The time dependence of this mode on super-horizon scales is analysed in both the synchronous gauge and the Newtonian gauge to understand the true gauge invariant behaviour of these modes. We then explore constraints on the amplitude of this mode on scales between $k \sim 10^{-5}$ Mpc$^{-1}$ and $k \sim 10^{-1}$ Mpc$^{-1}$ using the temperature and polarization anisotropies from the cosmic microwave background, by computing the Fisher information. Binning the primordial power non-parametrically into 100 bins, we find that the decaying modes are constrained at comparable variance as the growing modes on scales smaller than the horizon today using temperature anisotropies. Adding polrisation data makes the decaying mode more constrained. The decaying mode amplitude is thus constrained by $\sim 1/l$ of the growing mode. On super-horizon scales, the growing mode is poorly constrained, while the decaying mode cannot substantially exceed the scale-invariant amplitude. This interpretation differs substantially from the past literature, where the constraints were quoted in gauge-dependent variables, and resulted in illusionary tight super-horizon decaying mode constraints. The results presented here can generally be used to non-parametrically constrain any model of the early universe.
The non-linear onset of neutrino-driven convection in two- and three-dimensional core-collapse supernovae

A toy model of the post-shock region of core-collapse supernovae is used to study the non-linear development of turbulent motions driven by convection in the presence of advection. Our numerical simulations indicate that buoyant perturbations of density are able to trigger self-sustained convection only when the instability is not linearly stabilized by advection. Large amplitude perturbations produced by strong shock oscillations or combustion inhomogeneities before the collapse of the progenitor are efficiently shredded through phase mixing and generate a turbulent cascade. Our model enables us to investigate several physical arguments that had been proposed to explain the impact of the dimensionality on the onset of explosions in global simulations of core-collapse supernovae. Three-dimensional (3D) simulations are found to lead to higher entropy values than two-dimensional (2D) ones. We attribute this to greater turbulent mixing and dissipation of the kinetic energy into heat in 3D. Our results show that the increase of entropy is enhanced with finer numerical resolution and larger perturbation amplitude.
Origin of MeV ion irradiation-induced stress changes in SiO2

The 4 MeV Xe ion irradiation of a thin thermally grown SiO2 film on a Si substrate leads to four different effects in which each manifests itself by a characteristic change in the mechanical stress state of the film: densification, ascribed to a beam-induced structural change in the silica network; stress relaxation by radiation-enhanced plastic flow; anisotropic expansion and stress generation; and transient stress relaxation ascribed to the annealing of point defects. Using sensitive wafer-curvature measurements, in situ measurements of the in-plane mechanical stress were made during and after ion irradiation at various temperatures in the range from 95 to 575 K, in order to study the magnitude of these effects, the mechanism behind them, as well as their interplay. It is found that the structural transformation leads to a state with an equilibrium density that is 1.7%–3.2% higher than the initial state, depending on the irradiation temperature. Due to the constraint imposed by the substrate, this trans.
The Assembly of galaxies in a hierarchically clustering universe

We study the formation of galaxies by using $N$-body/hydrodynamics simulations to investigate how baryons collect at the centre of dark matter halos. We treat the dark matter as a collisionless fluid and the baryons as an ideal gas. We include the effects of gravity, pressure gradients, hydrodynamical shocks, and radiative energy losses, but we neglect star formation. Our initial conditions assume a flat universe dominated by cold dark matter with a mean baryon abundance of 10\% by mass. Typical halos form through the merging of a few smaller systems which had themselves formed in a similar manner at higher redshift. The gas collects at the bottom of dark matter potential wells as soon as these are properly resolved by our simulations. There it settles into cold, tightly bound disks, and it remains cold during subsequent evolution. As their halos coalesce, these disks merge on a timescale that is consistent with dynamical friction estimates based on their {\it total} (gas + surrounding dark matter) mass. Both the merger rates of the disks and their mass spectrum are in remarkably good agreement with recent analytic models that describe the evolution of {\it dark halos} in a hierarchical universe. This very simple model of galaxy formation suffers from serious shortcomings. It predicts that most baryons should be locked up in galaxies, whereas in the real universe most baryons are thought to lie outside visible galaxies. In addition, it predicts the specific angular momentum of a disk to be only about 20\% that of its surrounding halo, corresponding to a radius smaller than that of observed spiral galaxy disks.
Some support properties for a class of ${\varLambda}$-Fleming–Viot processes

Using Donnelly and Kurtz's lookdown construction, we prove that the Lambda-Fleming-Viot process with underlying Brownian motion has a compact support at any fixed time provided that the associated Lambda-coalescent comes down from infinity not too slowly. We also find both upper and lower bounds on Hausdorff dimension for the support at any fixed time. When the associated Lambda-coalescent has a nontrivial Kingman component, the Hausdorff dimension for the support is exactly two at any fixed time. For such a Lambda-Fleming-Viot process, we further prove a one-sided modulus of continuity result for the ancestry process recovered from Donnelly and Kurtz's lookdown construction. As an application, we can prove that its support process also has the one-sided modulus of continuity (with modulus function C\sqrt{tlog(1/t)}) at any fixed time. In addition, we obtain that the support process is compact simultaneously at all positive times, and given the initial compactness, its range is uniformly compact over time interval [0,t) for all t>0. Under a mild condition on the Lambda-coalescence rates, we also find a uniform upper bound on Hausdorff dimension for the support and an upper bound on Hausdorff dimension for the range.
Study of hard and electromagnetic processes at CERN-SPS energies: an investigation of the high-$\mu_{\mathbf{B}}$ region of the QCD phase diagram with NA60+

The exploration of the phase diagram of Quantum ChromoDynamics (QCD) is carried out by studying ultrarelativistic heavy-ion collisions. The energy range covered by the CERN SPS ($\sqrt{s_{\rm \scriptscriptstyle{NN}}} \sim$ 6-17 GeV) is ideal for the investigation of the region of the phase diagram corresponding to finite baryochemical potential ($\mu_{\rm B}$), and has been little explored up to now. We propose in this document a new experiment, NA60+, that would address several observables which are fundamental for the understanding of the phase transition from hadronic matter towards a Quark-Gluon Plasma (QGP) at SPS energies. In particular, we propose to study, as a function of the collision energy, the production of thermal dimuons from the created system, from which one would obtain a caloric curve of the QCD phase diagram that is sensitive to the order of the phase transition. In addition, the measurement of a $\rho$-a$_1$ mixing contribution would provide conclusive insights into the restoration of the chiral symmetry of QCD. In parallel, studies of heavy quark and quarkonium production would also be carried out, addressing the measurement of transport properties of the QGP and the investigation of the onset of the deconfinement transition. The document also defines an experimental set-up which couples a vertex telescope based on monolithic active pixel sensors (MAPS) to a muon spectrometer with tracking (GEM) and triggering (RPC) detectors within a large acceptance toroidal magnet. Results of physics performance studies for most observables accessible to NA60+ are discussed, showing that the results of the experiment would lead to a significant advance of our understanding of strong interaction physics. The document has been submitted as an input to the European Particle Physics Strategy Update 2018-2020 (http://europeanstrategyupdate.web.cern.ch/).
Scanning tunneling spectroscopy of high-temperature superconductors

Tunneling spectroscopy has played a central role in the experimental verification of the microscopic theory of superconductivity in classical superconductors. Initial attempts to apply the same approach to high-temperature superconductors were hampered by various problems related to the complexity of these materials. The use of scanning tunneling microscopy and spectroscopy (STM and STS) on these compounds allowed the main difficulties to be overcome. This success motivated a rapidly growing scientific community to apply this technique to high-temperature superconductors. This paper reviews the experimental highlights obtained over the last decade. The crucial efforts to gain control over the technique and to obtain reproducible results are first recalled. Then a discussion on how the STM and STS techniques have contributed to the study of some of the most unusual and remarkable properties of high-temperature superconductors is presented: the unusually large gap values and the absence of scaling with the critical temperature, the pseudogap and its relation to superconductivity, the unprecedented small size of the vortex cores and its influence on vortex matter, the unexpected electronic properties of the vortex cores, and the combination of atomic resolution and spectroscopy leading to the observation of periodic local density of states modulations in the superconducting and pseudogap states and in the vortex cores.