Miracle-dz/UniFAR-FTUs huggingface dataset:
de Sitter symmetries and inflationary correlators in parity violating scalar-vector models

In this paper we use conformal field theory techniques to constrain the form of the correlations functions of an inflationary scalar-vector model described by the interaction term f1(ϕ)Fμ νFμ ν + f2(ϕ)̃Fμ νFμ ν. We use the fact that the conformal group is the relevant symmetry group acting on super horizon scales in an inflationary de Sitter background. As a result, we find that super horizon conformal symmetry, constraints the form of the coupling functions f1, f2 to be homogeneous functions of the same degree. We derive the general form of the correlators involving scalar and vector perturbations in this model and determine its squeezed limit scaling behaviour for super horizon scales. The approach followed here is useful to constraint the shape of scalar-vector correlators, and our results agree with recent literature on the subject, but don't allow us to determine amplitude factors of the correlators.
Ice dynamics in the Bothnian Bay inferred from ADCP measurements

A bottom mounted ADCP has monitored the ice motion and thickness in Bothnian Bay, Baltic Sea during the entire winter season 2004. The ADCP was deployed at 20 m depth at Falkensgrund well outside the land fast ice zone. The data shows that the ice motion is primarily driven by the wind but with a clear influence of internal ice stresses. The ice stresses become more dominant as the ice grow thicker with increasing number of observations with nearly stationary ice for relatively high wind speeds. A clear dependence of the ice/wind speed ratio to wind shifts is detected with higher ratio in the new wind direction. The effect of strain hardening is also seen in several events as decreasing ice speed, sometimes to zero, in spite of constant wind speed and wind direction. A rough force balance computation gives a compressive ice strength of about 9 × 104 Nm−2, which is much larger than normally used in numerical ice models. The ice thickness data show numerous ice ridges with ice draft well above 1 m passing the instrument. The ridges make up a large portion, 30–50%, of the total ice volume showing that dynamical processes are important for the total ice production in the Bothnian Bay.
Spinning-black-hole binaries: The orbital hang-up

We present the first fully-nonlinear numerical study of the dynamics of highly-spinning-black-hole binaries. We evolve binaries from quasicircular orbits (as inferred from post-Newtonian theory), and find that the last stages of the orbital motion of black-hole binaries are profoundly affected by their individual spins. In order to cleanly display its effects, we consider two equal-mass holes with individual spin parameters $S/{m}^{2}=0.757$, both aligned and antialigned with the orbital angular momentum (and compare with the spinless case), and with an initial orbital period of $125M$. We find that the aligned case completes three orbits and merges significantly after the antialigned case, which completes less than one orbit. The total energy radiated for the former case is $\ensuremath{\approx}7%$ while for the latter it is only $\ensuremath{\approx}2%$. The final Kerr hole remnants have rotation parameters $a/M=0.89$ and $a/M=0.44$ respectively, showing the unlikeliness of creating a maximally rotating black hole out of the merger two highly spinning holes.
On local estimates and the Stein method

The elegant adaptation of the Stein method by Chen (1975) to the case of integer-valued random variables is one of the most powerful techniques in the theory of approximations. The method employs properties of the solution of a special difference equation. Usually, the Stein-Chen method is used for estimates in total variation; see, for example, Barbour et al. (1992a; 1992b), Barbour and Chryssaphinou (2001), Brown and Xia (2001), Barbour and Cekanavidius (2002), and references therein. The slightly modified Stein-Chen method can be used for moderately large deviations; see Chen and Choi (1992). As shown by Barbour and Jensen (1989), the method is also suitable for uniform local estimates. Only a few papers are devoted to discrete non-uniform estimates; see Barbour (1987), Barbour et al. (1995), Chen and Roos (1995) and Chen (2000). Direct application of the Stein-Chen method requires solving the Stein equation for unbounded functions, which is a serious technical problem. So far, the most accurate estimates strongly depend on the properties of the approximating Poisson distribution and on the independence of random variables. Note that, for estimates in total variation, the Stein method is extended to cases more general than that of the Poisson approximation. In this paper, we show how recursive application of the Stein equation can reduce nonuniform local estimates to estimates of a difference operator in total variation. Our approach has the following advantages: there is no need to solve the Stein equation for unbounded functions; for the numerous cases with already established estimates in total variation, local non-uniform estimates can be obtained without much additional effort; and, in principle, the proposed approach can be extended to the sums of dependent random variables. On the other hand, the non-uniform functions in this paper are growing no faster than polynomials. For a Poisson approximation, a similar recursive approach was used by Barbour (1987). Note that Barbour (1987) and Barbour et al. (1995) used more general unbounded functions.
Lateralization of noise targets with interaural level differences presented within a noise interferer

The interaural level difference (ILD) of a lateralized target source is reduced when the target is presented together with background noise containing no ILD. It is unknown whether listeners simply use this reduced aggregate ILD or are still able to utilize the target ILD in a lateralization task. Behavioral experiments revealed that the temporal asynchrony between the onsets/offsets of the target and the background noise resulted in the population of listeners actually perceiving a larger ILD than the target ILD. For synchronous onsets/offsets, however, the perceived ILD depended on the coherence of the background noise. With coherent background noise, the population of subjects perceived a reduced ILD near the aggregate ILD. In contrast, the population of subjects made a reasonable estimate of the target ILD when the background noise was diffuse. Implementation of an Equalization Cancellation model and taking the compensatory level equalization that yields the lowest output as an estimate for the ILD re.
Light-induced magnetic precession in (Ga,Mn)As slabs : Hybrid standing-wave Damon-Eshbach modes

Coherent oscillations associated with spin precessions were observed in ultrafast optical experiments on ferromagnetic (Ga,Mn)As films. Using a complete theoretical description of the processes by which light couples to the magnetization, values for the anisotropy constants and the spin stiffness were unambiguously determined from the data. Estimates for the hole-Mn exchange coupling are significantly larger than those previously reported. Results also reveal an important negative contribution to the energy due to surface anisotropy leading to excitations that are a mixture of bulk waves and surface modes.
Dawkins vs. Gould: Survival of the Fittest

Arguments concerning Darwin’s account of evolution invariably generate a lot of heat, and have done so since the moment that Darwin began tentatively circulating his ideas in the mid-1840s, more than fifteen years before he was prepared to face the storm he knew would follow publication. Then as now, the heat arises not only from genuine disagreement over the science, but also disagreement over the broader significance of Darwin’s insights: do they give us reason to give up God, to adopt or resist particular moral norms or metaethical approaches, to marvel or despair at our place in the universe? Kim Sterelny aims to give a cool and impartial view of a series of hightemperature disputes between Richard Dawkins and Stephen Jay Gould. Both Dawkins and Gould write with zeal and are not averse to rhetoric or overstatement if they think it will promote a particular cause. Moreover, both have on occasion shown a wilful determination to caricature. Neither makes the kind of effort we might hope for when it comes to understanding what drives his opponent’s argument, nor does either take sufficient care to check whether particular concepts—gene, progress, saltation, constraint—are being used in the same way. But for all this, there are valuable ideas and arguments to be discovered and recovered in their work. Sterelny is right to insist as he does that they deserve to be taken seriously by both philosophers and evolutionary biologists. A book such as this needs to undertake a number of tasks, including clear exposition of the views in question, the marking-out of areas of both agreement and disagreement, the separation of substantive points from rhetorical excesses, an account of the immediate and the background reasons for the disagreement, and, finally, some attempt at arbitration. Sterelny scores well on clear exposition of Dawkins’s and Gould’s views and also on outlining areas of agreement, which he reminds us are considerable, and disagreement. Particularly welcome is a final chapter Brit. J. Phil. Sci. 54 (2003), 365–369, axg021
Recovery from High Values of Temporary Threshold Shift

Twelve normal observers were exposed to noise that produced at least 50 db of temporary threshold shift (TTS) measured 2 min after cessation of the noise. The TTS was measured at regular intervals until recovery was complete. Results indicate that while the recovery from these high values of TTS proceeds as a function of the logarithm of time during the first few hours, later recovery is instead linear in time.
Effective Induction Heating around Strongly Magnetized Stars

Planets that are embedded in the changing magnetic fields of their host stars can experience significant induction heating in their interiors caused by the planet’s orbital motion. For induction heating to be substantial, the planetary orbit has to be inclined with respect to the stellar rotation and dipole axes. Using WX UMa, for which the rotation and magnetic axes are aligned, as an example, we show that for close-in planets on inclined orbits, induction heating can be stronger than the tidal heating occurring inside Jupiter’s satellite Io; namely, it can generate a surface heat flux exceeding 2 W m−2. An internal heating source of such magnitude can lead to extreme volcanic activity on the planet’s surface, possibly also to internal local magma oceans, and to the formation of a plasma torus around the star aligned with the planetary orbit. A strongly volcanically active planet would eject into space mostly SO2, which would then dissociate into oxygen and sulphur atoms. Young planets would also eject CO2. Oxygen would therefore be the major component of the torus. If the O i column density of the torus exceeds ≈1012 cm−2, the torus could be revealed by detecting absorption signatures at the position of the strong far-ultraviolet O i triplet at about 1304 Å. We estimate that this condition is satisfied if the O i atoms in the torus escape the system at a velocity smaller than 1–10 km s−1. These estimates are valid also for a tidally heated planet.
7Li evolution in the thin and thick discs of the Milky Way

Recent detection of the isotope $^7$Be (that decays into $^7$Li) in the outburst of classical novae confirms the suggestion made in the 70s that novae could make $^7$Li. We reconsidered the role of novae as producers of Li by means of a detailed model of the chemical evolution of the Milky Way. We showed that novae could be the Galactic lithium source accounting for the observed increase of Li abundances in the thin disk with stellar metallicity. The best agreement with the upper envelope of the observed Li abundances is obtained for a delay time of ~ 1 Gyr for the nova production and for an effective Li yield of $1.8 (\pm 0.6) \times 10^{-5}$ $M_{\odot}$ over the whole nova life. Lithium in halo stars is depleted by ~ 0.35 dex, assuming the pristine abundance from standard big bang nucleosynthesis. We elaborate a model that matches the pristine stellar abundances, assuming that all stars are depleted by 0.35 dex. In this case, the delay remains the same, but the Li yields are doubled compared to the previous case. This model also has the merit to match the Li abundance in meteorites and young TTauri stars. The thick disk model, adopting the parameters derived for the thin disk, can also explain the absence of increase of Li abundances in its stars. The thick disk is old, but formed and evolved in a time shorter than that required by novae to contribute significantly to Li. Therefore, no Li enhancement is expected in thick disk stars. We show that the almost constant Li abundance in the thick disk results from the compensation of stellar astration by spallation processes.
An Extensive Census of Hubble Space Telescope Counterparts to Chandra X-Ray Sources in the Globular Cluster 47 Tucanae. I. Astrometry and Photometry

We report in this study of 47 Tucanae the largest number of optical identifications of X-ray sources yet obtained in a single globular cluster. Using deep Chandra ACIS-I imaging and extensive Hubble Space Telescope studies with Wide Field Planetary Camera 2 (WFPC2; including a 120 orbit program giving superb V and I images), we have detected optical counterparts to at least 22 cataclysmic variables (CVs) and 29 chromospherically active binaries (BY Dra and RS CVn systems) in 47 Tuc. These identifications are all based on tight astrometric matches between X-ray sources and objects with unusual (non-main-sequence [non-MS]) optical colors and/or optical variability. Several other CVs and active binaries have likely been found, but these have marginal significance because of larger offsets between the X-ray and optical positions, or colors and variability that are not statistically convincing. These less secure optical identifications are not subsequently discussed in detail. In the U versus U-V color-magnitude diagram (CMD), where the U band corresponds to either F336W or F300W, the CVs all show evidence for blue colors compared with the MS, but most of them fall close to the main sequence in the V versus V-I CMD, showing that the secondary stars dominate the optical light. The X-ray-detected active binaries have magnitude offsets above the MS (in both the U versus U-V or V versus V-I CMDs) that are indistinguishable from those of the much larger sample of optical variables (eclipsing and contact binaries and BY Dra variables) detected in the recent WFPC2 studies of Albrow et al. We also present the results of a new, deeper search for optical companions to millisecond pulsars (MSPs). One possible optical companion to an MSP (47 Tuc T) was found, adding to the two optical companions already known. Finally, we study several blue stars with periodic variability from Albrow et al. that show little or no evidence for X-ray emission. The optical colors of these objects differ from those of 47 Tuc (and field) CVs. An accompanying paper will present time series results for these optical identifications and will discuss X-ray-to-optical flux ratios, spatial distributions, and an overall interpretation of the results.
STABILITY OF MONOPOLE CONDENSATION IN SU(2) QCD

We propose to resolve the controversy regarding the stability of the monopole condensation in QCD by calculating the imaginary part of the one-loop effective action perturbatively. We calculate the imaginary part perturbatively to the order g2 with two different methods, with Feynman diagram and with Schwinger's method. Our result shows that with the magnetic background the effective action has no imaginary part, but with the electric background it acquires a negative imaginary part. This strongly indicates a stable monopole condensation in QCD.
Repeated Relativistic Ejections in GRS 1915+105

In 1994 February-August we observed with the VLA four ejection events of radio-emitting clouds from the high-energy source GRS 1915+105. These events are all consistent with antiparallel ejections of twin pairs of clouds moving away from the compact source at ~0.92 of the speed of light and angles of ~70° with respect to the line of sight. The flux ratios and time evolution of the expelled clouds are consistent with actual motions of the radiating matter rather than with the simple propagation of pulses in a medium moving at slower velocities. The large kinetic power of the sudden, short, and rather discontinuous ejections exceeds by more than an order of magnitude the maximum steady photon luminosity of the source, suggesting that in GRS 1915+105 a radiation acceleration mechanism of the ejecta is unlikely. As in other galactic and extragalactic radio sources, the decrease in flux density as a function of angular separation from the central source shows a steepening with distance. Additional ejection events have been observed in 1995 and 1997 and we compare them with the 1994 events.
Star formation quenching in green valley galaxies at 0.5 ≲ z ≲ 1.0 and constraints with galaxy morphologies

We calculate the star formation quenching timescales in green valley galaxies at intermediate redshifts ($z\sim0.5-1$) using stacked zCOSMOS spectra of different galaxy morphological types: spheroidal, disk-like, irregular and merger, dividing disk-like galaxies further into unbarred, weakly-barred and strongly-barred, assuming a simple exponentially-decaying star formation history model and based on the H$_{\delta}$ absorption feature and the $4000$ \AA ~break. We find that different morphological types present different star formation quenching timescales, reinforcing the idea that the galaxy morphology is strongly correlated with the physical processes responsible for quenching star formation. Our quantification of the star formation quenching timescale indicates that disks have typical timescales $60\%$ to 5 times longer than that of galaxies presenting spheroidal, irregular or merger morphologies. Barred galaxies in particular present the slowest transition timescales through the green valley. This suggests that although secular evolution may ultimately lead to gas exhaustion in the host galaxy via bar-induced gas inflows that trigger star formation activity, secular agents are not major contributors in the rapid quenching of galaxies at these redshifts. Galaxy interaction, associated with the elliptical, irregular and merger morphologies contribute, to a more significant degree, to the fast transition through the green valley at these redshifts. In the light of previous works suggesting that both secular and merger processes are responsible for the star formation quenching at low redshifts, our results provide an explanation to the recent findings that star formation quenching happened at a faster pace at $z\sim0.8$.
A pr 2 00 0 S-wave η ′-proton FSI ; phenomenological analysis of near-threshold production of π 0 , η , and η ′ mesons in proton-proton collisions

We describe a novel technique for comparing total cross sections for the reactions pp → ppπ0, pp → ppη, and pp → ppη close to threshold. The initial and final state proton-proton interactions are factored out of the total cross section, and the dependence of this reduced cross section on the volume of phase space is discussed. Different models of the proton-proton interaction are compared. We argue that the scattering length of the S-wave η-proton
Friction as a consistent quantum-mechanical concept

A quantum analog of friction (understood as a completely positive, Markovian, translation-invariant and phenomenological model of dissipation) is known to be in odds with the detailed balance in the thermodynamic limit. We show that this is not the case for quantum systems with internal (e.g. spin) states non-adiabatically coupled to translational dynamics. For such systems, a quantum master equation is derived which phenomenologically accounts for the frictional effect of a uniform zero temperature environment. A simple analytical example is provided. Conjectures regarding the finite temperature case are also formulated. The results are important for efficient simulations of complex molecular dynamics and quantum reservoir engineering applications.
GRAVITATIONAL FIELD OF MASSIVE POINT PARTICLE IN GENERAL RELATIVITY

Using various gauges of the radial coordinate we give a description of the static spherically symmetric space-times with point singularity at the center and vacuum outside the singularity. We show that in general relativity (GR) there exist innitely many such solutions to the Einstein equations which are physically dieren t and only some of them describe the gravitational eld of a single massive point particle. In particular, we show that the widespread Hilbert’s form of Schwarzschild solution does not solve the Einstein equations with a massive point particle’s stress-energy tensor. Novel normal coordinates for the eld and a new physical class of gauges are proposed, in this way achieving a correct description of a point mass source in GR. We also introduce a gravitational mass defect of a point particle and determine the dependence of the solutions on this mass defect. In addition we give invariant characteristics of the physically and geometrically dieren t classes of spherically symmetric static space-times created by one point mass.
When clusters collide - A numerical Hydro/N-body simulation of merging galaxy clusters

A 3D numerical simulation of two merging clusters of galaxies, using a hybrid Hydro/N-body code, is presented. The hydrodynamics of the code is solved by an Eulerian finite difference method. Initial results disclose that the X-ray emission of the dominant cluster becomes elongated and broadened; heating occurs at the core of the dominant cluster as a result of multiple shocks, and high velocity gas motions within the intracluster medium. It is predicted that clusters which have undergone recent mergers and do not have cooling flows will have high peculiar gas velocities and that the shocks and turbulence generated during the merger may power cluster-wide radio halos. Prolonged high-velocity gas motions through the dominant cluster core possibly play a major role in the formation and shaping of wide-angle tailed radio sources associated with central dominant galaxies. The N-body component of the simulation reveals the subcluster to be dispersed as it passes through the dominant cluster.
Optimal criteria based on the ecological function of an irreversible intercooled regenerative modified Brayton cycle

The optimal criterion of an irreversible regenerative intercooled modified Brayton cycle heat engine based on the ecological function is presented in this paper. The ecological function defined as the power output minus the dissipation due to irreversibility has been optimised with respect to the cycle temperatures and the optimum performance parameters are calculated for a typical set of operating conditions. It is found that there are optimal values of the intercooling and cycle pressure ratios as well as the turbine outlet temperature at which the cycle attains the maximum performance but the optimal values of these parameters are different for different cycle parameters such as the intercooling and cycle pressure ratios, turbine outlet temperature, etc. Moreover, the design problems of some important parameters are discussed in detail, and consequently, the optimum criteria for the intercooling and cycle pressure ratios and the turbine outlet temperature are obtained.