Miracle-dz/UniFAR-FTUs huggingface dataset:
Interplay of Coulomb interactions and disorder in three-dimensional quadratic band crossings without time-reversal symmetry and with unequal masses for conduction and valence bands

Coulomb interactions famously drive three dimensional quadratic band crossing semimetals into a non-Fermi liquid phase of matter. In a previous work, Phys. Rev. B 95, 205106 (2017), the effect of disorder on this non-Fermi liquid phase was investigated, assuming that the bandstructure was isotropic, assuming that the conduction and valence bands had the same band mass, and assuming that the disorder preserved exact time-reversal symmetry and statistical isotropy. It was shown that the non-Fermi liquid fixed point is unstable to disorder, and that a runaway flow to strong disorder occurs. In this work, we extend that analysis by relaxing the assumption of time-reversal symmetry and allowing the electron and hole masses to differ (but continuing to assume isotropy of the low energy bandstructure). We first incorporate time-reversal symmetry breaking disorder, and demonstrate that there do not appear any new fixed points. Moreover, while the system continues to flow to strong disorder, time-reversal-symmetry-breaking disorder grows asymptotically more slowly than time-reversal-symmetry-preserving disorder, which we therefore expect should dominate the strong-coupling phase. We then allow for unequal electron and hole masses. We show that whereas asymmetry in the two masses is irrelevant in the clean system, it is relevant in the presence of disorder, such that the 'effective masses' of the conduction and valence bands should become sharply distinct in the low-energy limit. We calculate the RG flow equations for the disordered interacting system with unequal band masses, and demonstrate that the problem exhibits a runaway flow to strong disorder. Along the runaway flow, time-reversal-symmetry-preserving disorder grows asymptotically more rapidly than both time-reversal-symmetry-breaking disorder and the Coulomb interaction.
A Tight Upper Limit on Oscillations in the Ap Star ϵ Ursae Majoris from WIRE Photometry

Observations of ϵ UMa obtained with the star tracker on the Wide Field Infrared Explorer satellite during a month in mid-2000 are analyzed. This is some of the most precise photometry of an Ap star. The amplitude spectrum is used to set an upper limit of 75 parts per million for the amplitude of stellar pulsations in this star unless by coincidence it oscillates with a single mode at the satellite orbit, its harmonics, or their 1 day-1 aliases. This is the tightest limit put on the amplitude of oscillations in an Ap star. As the rotation period of ϵ UMa is relatively short (5.1 days), it cannot be argued that the observations were made at a wrong rotational phase. Our results thus support the idea that some Ap stars do not pulsate at all.
Assessment of turbulent boundary layers on a NACA4412 wing section at moderate Re

The results of a DNS of the flow around a wing section represented by a NACA4412 profile, with Rec = 400, 000 and 5 degree angle of attack, are presented in this study. The high-order spectral element code Nek5000 was used for the computations. The Clauser pressure-gradient parameter ? ranges from 0 and 85 on the suction side, and the maximum Re_theta and Re_tau values are around 2,800 and 373, respectively. Comparisons between the suction side with ZPG TBL data show a more prominent wake, a steeper logarithmic region and lower velocities in the buffer region. The APG also leads to a progressively increasing value of the inner peak in the tangential velocity fluctuations, as well as the development of an outer peak, which is also observed in the other components of the Reynolds stress tensor. Other effects of strong APGs are increased production and dissipation profiles across the boundary layer, together with enhanced viscous diffusion and velocity-pressure-gradient correlation values near the wall. All these effects are connected to the fact that the large-scale motions of the flow become energized due to the APG, as apparent from spanwise premultiplied power spectral density plots.
Roughening Transition in a Model for Dimer Adsorption and Desorption

A solid-on-solid growth model for dimer adsorption and desorption is introduced and studied numerically. The special property of the model is that dimers can desorb only at the edges of terraces. It is shown that the model exhibits a roughening transition from a smooth to a rough phase. In both phases the interface remains pinned to the bottom layer and does not propagate. Close to the transition certain critical properties are related to those of a unidirectionally coupled hierarchy of parity-conserving branching-annihilating random walks.
A Discrete Approximation to Gibbs Free Energy of Chemical Reactions is Needed for Accurately Calculating Entropy Production in Mesoscopic Simulations

In modeling the interior of cells by simulating a reaction-diffusion master equation over a grid of compartments, one employs the assumption that the copy numbers of various chemical species are small, discrete quantities. We show that in this case, textbook expressions for the change in Gibbs free energy accompanying a chemical reaction or diffusion between adjacent compartments become inaccurate. We derive exact expressions for these free energy changes under the assumption of discrete copy numbers and illustrate how these expressions reduce to the textbook expressions under a series of successive approximations leveraging the relative sizes of the stoichiometric coefficients and the copy numbers of the solutes and solvent. Numerical results are presented to corroborate the claim that if the copy numbers are treated as discrete quantities, then only these more exact expressions lead to correct equilibrium behavior. The newly derived expressions are critical for correctly tracking dissipation and entropy production in mesoscopic simulations based on the reaction-diffusion master equation formalism.
Hierarchical-environment-assisted non-Markovian speedup dynamics control

We investigate the qubit in the hierarchical environment where the first level is just one lossy cavity while the second level is the N-coupled lossy cavities. In the weak coupling regime between the qubit and the first level environment, the dynamics crossovers from the original Markovian to the new non-Markovian and from no-speedup to speedup can be realized by controlling the hierarchical environment, i.e., manipulating the number of cavities or the coupling strength between two nearest-neighbor cavities in the second level environment. And we find that the coupling strength between two nearest-neighbor cavities and the number of cavities in the second level environment have the opposite effect on the non-Markovian dynamics and speedup evolution of the qubit. In addition, in the case of strong coupling between the qubit and the first level environment, we can be surprised to find that, compared with the original non-Markovian dynamics, the added second level environment cannot play a beneficial role on the speedup of the dynamics of the system.
Complete devil's staircase in the one-dimensional lattice gas

2014 We calculate explicitly the exact form of the complete devil’s staircase for the lattice gas model. Thus, we show that the behaviour at the commensurate-incommensurate phase transition essentially depends on the long distance interactions. We question the assertion of Burkov about the universality properties of the devil’s staircase. J. Physique LETTRES 44 (1983) L-247 L-250 1~’ AVRIL 1983, Classification Physics Abstracts 05.20 68.20 64.90 The devil’s staircase, calculated by Burkov in his interesting paper [1], can also be explicitly calculated by the same method that we used in the first exact calculation of a complete devil’s staircase in 1978 [2]. In addition, our method has the advantage of having a rigorous mathematical foundation [3]. Our initial model was a variation on the discrete Frenkel-Kontorova model where the sine periodic potential was replaced by a piece-wise parabolic periodic potential. It was transformed into an integer model which had a similar form to the lattice gas model considered by Burkov. The details of these calculations in reference [2] were given in appendix A3 of reference [4b]. We also noted that the model studied by Bak and Bruinsma [5] could also be transformed into such a lattice gas model [6]. In addition by usihg a result given in reference [3c], which was essentially devoted to obtaining rigorous results applicable to quite a more general class of models, it was pointed out that our proofs and exact results could be extended unchanged to models with any kind of long range interactions given some necessary convexity conditions. The purpose of this comment is not to reproduce the substance of papers already published or about to appear but, 1) to show how our method, which is simpler, can be applied to the model studied by Burkov. Thus, we find again the equation of the devil’s staircase given by Burkov, 2) to question the universality properties of the devil’s staircase suggested by Burkov. Article published online by EDP Sciences and available at http://dx.doi. org/10.1051/jphyslet:01983004407024700 L-248 JOURNAL DE PHYSIQUE LETTRES The one-dimensional lattice gas model [1] with Hamiltonian is included in the class of models (34) of reference [6] where for each Um(x) there exists a positive constant Cm such that for all x, Um(x) > em > 0. (Many rigorous results were given for this class of models in reference [3].) (Note that if this condition is not satisfied, the devil’s staircase of (1) may not exist. ) When the atomic mean distance, I, which is the inverse of the atomic concentration, c, i.e. is fixed, the ground-state of model (1) is given by (see ref. [6] or [3a, 3b, 3c]) where a is an arbitrary phase. The energy per atom with condition (2) is
Molecular filament formation and filament–cloud interaction: Hints from Nobeyama 45 m telescope observations

We present Nobeyama 45m telescope C18O, 13CO, and 12CO(1-0) mapping observations towards an interstellar filament in the Taurus molecular cloud. We investigate the gas velocity structure along the filament and in its surrounding parent cloud. The filament is detected in the optically thin C18O emission as a single velocity component, ~1pc long, ~0.06pc wide structure. The C18O emission traces dust column densities larger than ~5x10^21 cm-2. The line-of-sight (LOS) velocity fluctuates along the filament crest with an average amplitude of ~0.2 km/s. The 13CO and 12CO integrated intensity maps show spatially extended emission around the elongated filament. We identify three extended structures with LOS velocities redshifted and blueshifted with respect to the average velocity of the filament identified in C18O. Based on combined analyses of velocity integrated channel maps and intensity variations of the optically thick 12CO spectra on and off the filament, we propose a 3-dimensional structure of the cloud surrounding the filament. We further suggest a multi-interaction scenario where sheet-like extended structures interact, in space and time, with the filament and are responsible for its compression and/or disruption, playing an important role in the star formation history of the filament. We also identify, towards the same field, a very faint filament showing a velocity field compatible with the filament formation process proposed by Inoue et al. (2017), where a filament is formed due to convergence of a flow of matter generated by the bending of the ambient magnetic field structure induced by an interstellar shock compression.
The topology determined by the symbolic powers of primary ideals

Let q be a p-primary ideal in a Noetherian ring R. The main theorem characterizes when the q-adic and q-symbolic topologies on R are linearly equivalent; that is, when there n kexists an integer k≥0 such that q(n) ⊆qn-k for all n≥k. Using this, it is shown that when this holds for q, then it holds for several other primary ideals related to q (both in R and in certain other rings related to R) and that the powers of q(n) are symbolic powers for all n≥k (so p has primary ideals all of whose powers are symbolic powers).
Large scale effective theory for cosmological bounces

An exactly solvable bounce model in loop quantum cosmology is identified which serves as a perturbative basis for realistic bounce scenarios. Its bouncing solutions are derived analytically, demonstrating why recent numerical simulations robustly led to smooth bounces under the assumption of semiclassicality. Several effects, easily included in a perturbative analysis, can however change this smoothness. The effective theory is not only applicable to such situations where numerical techniques become highly involved but also allows one to discuss conceptual issues. For instance, consequences of the notoriously difficult physical inner product can be implemented at the effective level. This indicates that even physical predictions from full quantum gravity can be obtained from perturbative effective equations.
A Characterization of the finite simple group L4(3)

In this paper we aim to give a characterization of the finite simple group L4(3) (i.e. PSL(4, 3)) by the structure of the centralizer of an involution contained in the centre of its Sylow 2-subgroup. More precisely, we shall prove the following result.
Effects of surface heat and moisture exchange on ARW-WRF warm-season precipitation forecasts over the central United States

Abstract The evolution of the daytime planetary boundary layer (PBL) and its association with warm-season precipitation is strongly impacted by land–atmosphere heat and moisture exchange (hereafter surface exchange). However, substantial uncertainty exists in the parameterization of the surface exchange in numerical weather prediction (NWP) models. In the current study, the authors examine 0–24-h convection-permitting forecasts with different surface exchange strengths for a 6-day period during the International H2O Project (IHOP_2002). Results indicate sensitivity in the timing of simulated afternoon convection initiation and subsequent precipitation amounts to variations in surface exchange strength. Convection initiation in simulations with weak surface exchange was delayed by 2–3 h compared to simulations with strong surface exchange, and area-averaged total precipitation amounts were less by up to a factor of 2. Over the western high plains (105°–100°W longitude), where deep convection is locally gen.
Unification and low-energy supersymmetry at one and two-loop orders

The status of coupling constant unification -- assuming the validity of the standard model or of its minimal supersymmetric extension at high energies -- and of relations between various Yukawa couplings (assuming the supersymmetri extension) which are implied in certain grand-unified theories, are studied in detail. Theoretical uncertainties in the calculations are emphasized, and low-energy constraints and predictions are derived. In particular, we find that bottom-tau unification favors a Higgs boson lighter than 110 GeV. The structure of the vacuum in the model studied is also discussed. Implications of embedding supersymmetric models in grand-unified theories are further explored and are shown to affect the soft supersymmetry breaking mass parameters of the models, and thus the spectrum at low-energy.
Limitation of blend type of resist platform on EUV lithography

Chemically amplified resist (CAR) system is being widely used not only for 248 nm and 193 nm lithography but for Extreme Ultra Violet Lithography (EUVL). [1] And CAR system is based on blend resist platform which is formulated with polymer and photo-acid generator (PAG) independently. In EUVL to aim at 22 nm node and beyond, EUV resists are required to achieve much higher acid generation efficiency and overcome RLS (Resolution, Line edge roughness, Sensitivity) trade-off using some ideas such as increase in PAG concentration and film absorption coefficient, suppression of acid diffusion length and so on. [2-6] Increase in PAG loading ratio is a promising strategy to improve EUV resist performance,[7-10] however there must be upper limitation of PAG loading ratio on blend resist platform due to lowering film Tg induced by a plasticization effect of blended PAG. This plasticization effect of blended PAG would have another impact to increase acid diffusion length, resulting in low resolution and significant thickness loss, especially on ultra thin film condition. On the other hand, utilizing the PAG having bulky cation structure was beneficial in order to maintain dark loss (in other word, top loss) of the patterned features, however, this type of cation would show low quantum yield driven by the substituent on a cation structure, so that total performance such as ultimate resolution deteriorated. From these results, the bound resist platform which has PAG unit on polymer backbone as branch would be promising platform because of its potential advantages such as suppression of dark loss, no plasticization effect and control of acid diffusion.
Spatial and Temporal Variations in Small-Scale Galactic H I Structure toward 3C 138

Several recent studies of Galactic H I absorption toward background quasars and pulsars have provided evidence that there are opacity changes in the neutral Galactic interstellar medium on size scales as small as a few AU. The nature of these opacity variations has remained a matter of debate but could reflect a variety of physical processes, including changes in the H I spin temperature or gas density. We present three epochs of Very Long Baseline Array (VLBA) observations of Galactic H I absorption toward the quasar 3C 138 with resolutions of 20 mas (∼10 AU). This analysis includes VLBA data from observations in 1999 and 2002 along with a reexamination of the 1995 VLBA data, reported by Faison and coworkers. Improved data reduction and imaging techniques have led to an order of magnitude improvement in sensitivity compared to previous work. With these new data we confirm the previously detected milliarcsecond-scale spatial variations in the H I opacity at the level of Δτmax = 0.50 ± 0.05. The typical size scale of the optical depth variations is ∼50 mas or 25 AU. In addition, for the first time we see clear evidence for temporal variations in the H I opacity over the 7 yr time span of our three epochs of data. We also attempt to detect the magnetic field strength in the H I gas using the Zeeman effect. From this analysis we have been able to place a 3 σ upper limit on the magnetic field strength per pixel of ∼45 μG. We have also been able to calculate for the first time the plane-of-sky covering fraction of the small-scale H I gas of ∼10%. This small covering fraction suggests that the filling factor of such gas is quite low, in agreement with recent optical observations. We also find that the line widths of the milliarcsecond-scale H I features are comparable to those determined from previous single-dish measurements toward 3C 138, suggesting that the opacity variations cannot be due to changes in the H I spin temperature. From these results we favor a density enhancement interpretation for the small-scale H I structures, although these enhancements appear to be of short duration and are unlikely to be in equilibrium.
Efficient Topology Optimization of Large Dynamic Finite Element Systems Using Fatigue

The present paper modifies and extends the recently developed equivalent static load method for the optimization of dynamically loaded linear elastic finite element systems with a huge number of degrees of freedom. In the equivalent static load method, dynamic loads have been transformed into equivalent static loads. This leads to an equivalent static response optimization with multiple loading conditions instead of a dynamic optimization problem. In the present paper, the equivalent static load algorithm is modified and extended by introducing a fatigue analysis in the iterative optimization procedure, where damage is used as suitable termination criterion of the iteration, as well as for the determination of a single and meaningful equivalent static load that leads to maximal damage in the structure. During the evolution process the structure is systematically stiffened by using the solid isotropic microstructure with penalization approach until a user-defined damage level is reached. Three standard examples from literature and an industrial application with a large number of degrees of freedom (600,000) demonstrate the computational efficiency of the proposed method.
Star Cluster Formation from Turbulent Clumps. I. The Fast Formation Limit

We investigate the formation and early evolution of star clusters, assuming that they form from a turbulent starless clump of a given mass bounded inside a parent self-gravitating molecular cloud characterized by a particular mass surface density. As a first step, we assume instantaneous star cluster formation and gas expulsion. We draw our initial conditions from observed properties of starless clumps. We follow the early evolution of the clusters up to 20 Myr, investigating the effects of different star formation efficiencies, primordial binary fractions and eccentricities, and primordial mass segregation levels. We investigate clumps with initial masses of embedded in ambient cloud environments with mass surface densities and . We show that these models of fast star cluster formation result, in the fiducial case, in clusters that expand rapidly, even considering only the bound members. Clusters formed from higher environments tend to expand more quickly and thus are soon larger than clusters born from lower conditions. To form a young cluster of a given age, stellar mass, and mass surface density, these models need to assume a parent molecular clump that is many times denser, which is unrealistic compared to observed systems. We also show that, in these models, the initial binary properties are only slightly modified by interactions, meaning that the binary properties, e.g., at 20 Myr, are very similar to those at birth. With this study, we set up the foundation for future work, where we will investigate more realistic models of star formation compared to this instantaneous, baseline case.
A New, Large-scale Map of Interstellar Reddening Derived from H i Emission

We present a new map of interstellar reddening, covering the 39% of the sky with low H i column densities ( N H I < 4 × 10 20 cm−2 or E ( B − V ) ≈ 45 mmag) at 16 . ′ 1 resolution, based on all-sky observations of Galactic H i emission by the HI4PI Survey. In this low-column-density regime, we derive a characteristic value of N H I / E ( B − V ) = 8.8 × 10 21 cm 2 mag − 1 for gas with ∣ v LSR ∣ < 90 km s−1 and find no significant reddening associated with gas at higher velocities. We compare our H i-based reddening map with the Schlegel et al. (SFD) reddening map and find them consistent to within a scatter of ≃ 5 mmag. Further, the differences between our map and the SFD map are in excellent agreement with the low-resolution ( 4 .° 5 ) corrections to the SFD map derived by Peek and Graves based on observed reddening toward passive galaxies. We therefore argue that our H i-based map provides the most accurate interstellar reddening estimates in the low-column-density regime to date. Our reddening map is made publicly available at doi.org/10.7910/DVN/AFJNWJ.
Waring's problem for sixteen biquadrates. Numerical results

Nous expliquons les algorithmes qui nous ont permis de verifier que tout entier congru a 4 modulo 80 dans l'intervalle [6 × 10 12 ; 2.17 × 10 14 ] est la somme de 5 bicarres, et que tout entier congru a 6, 21 ou 36 modulo 80 dans l'intervalle [6 × 10 12 ; 1.36 × 10 23 ] est la somme de 7 bicarres. Nous indiquons egalement des resultats deduits de calculs portant sur les petites sommes de bicarres. L'escalade de Dickson appliquee a ces resultats montre que tout entier de l'intervalle [13793; 10 245 est la somme de 16 bicarres.