Miracle-dz/UniFAR-FTUs huggingface dataset:
Stability at Random Close Packing

The requirement that packings of hard particles, arguably the simplest structural glass, cannot be compressed by rearranging their network of contacts is shown to yield a new constraint on their microscopic structure. This constraint takes the form a bound between the distribution of contact forces P (f) and the pair distribution function g(r): if P (f) ∼ f and g(r) ∼ (r−σ0) −γ , where σ0 is the particle diameter, one finds that γ ≥ 1/(2+θ). This bound plays a role similar to those found in some glassy materials with long-range interactions, such as the Coulomb gap in Anderson insulators or the distribution of local fields in mean-field spin glasses. There is ground to believe that this bound is saturated, offering an explanation for the presence of avalanches of rearrangements with power-law statistics observed in packings.
A comprehensive examination of the Eridani system Verification of a 4 micron narrow-band high-contrast imaging approach for planet searches

Due to its proximity, youth, and solar-like characteristics with a spectral type of K2V, � Eri is one of the most extensively studied systems in an extrasolar planet context. Based on radial velocity, astrometry, and studies of the structure of its circumstellar debris disk, at least two planetary companion candidates toEri have been inferred in the literature (� Eri b, � Eri c). Some of these methods also hint at additional companions residing in the system. Here we present a new adaptive optics assisted high-contrast imaging approach that takes advantage of the favourable planet spectral energy distribution at 4 μm, using narrow-band angular differential imaging to provide an improved contrast at small and intermediate separations from the star. We use this method to search for planets at orbits intermediate betweenEri b (3.4 AU) andEri c (40 AU). The method is described in detail, and important issues related to the detectability of planets such as the age ofEri and constraints from indirect measurements are discussed. The non-detection of companion candidates provides stringent upper limits for the masses of additional planets. Using a combination of the existing dynamic and imaging data, we exclude the presence of any planetary companion more massive than 3 Mjup anywhere in theEri system. Specifically, with regards to the possible residual linear radial velocity trend, we find that it is unlikely to correspond to a real physical companion if the system is as young as 200 Myr, whereas if it is as old as 800 Myr, there is an allowed semi-major axis range between about 8.5 and 25 AU.
Water emission from the chemically rich outflow L1157

Context. In the framework of the Herschel-WISH key program, several ortho-H2O and para-H2O emission lines, in the frequency range from 500 to 1700 GHz, were observed with the HIFI instrument in two bow-shock regions (B2 and R) of the L1157 cloud, which hosts what is considered to be the prototypical chemically-rich outflow. Aims. Our primary aim is to analyse water emission lines as a diagnostic of the physical conditions in the blue (B2) and red-shifted (R) lobes to compare the excitation conditions. Methods. For this purpose, we ran the non-LTE RADEX model for a plane-parallel geometry to constrain the physical parameters (Tkin, NH2O and nH2) of the water emission lines detected. Results. A total of 5 ortho- and para-H2 16 O plus one o−H2 18 O transitions were observed in B2 and R with a wide range of excitation energies (27K ≤ Eu ≤ 215 K). The H2O spectra, observed in the two shocked regions, show that the H2 Op rof iles differ markedly in the two regions. In particular, at the bow-shock R, we observed broad (∼30 km s −1 with respect to the ambient velocity) redshifted wings where lines at different excitation peak at different red-shifted velocities. The B2 spectra are associated with a narrower velocity range (∼ 6k m s −1 ), peaking at the systemic velocity. The excitation analysis suggests, for B2, low values of column density NH2O ≤ 5 × 10 13 cm −2 , a density range of 10 5 ≤ nH2 ≤ 10 7 cm −3 , and warm temperatures (≥300 K). The presence of the broad red-shifted wings and multiple peaks in the spectra of the R region, prompted the modelling of two components. High velocities are associated with relatively low temperatures (∼100 K), NH2O � 5 × 10 12 ‐5 × 10 13 cm −2 and densities nH2 � 10 6 ‐10 8 cm −3 . L ower velocities are associated with higher excitation conditions with Tkin ≥ 300 K, very dense gas (nH2 ∼ 10 8 cm −3 ) and low column density (NH2O 3 �� ) region. In this context, H2O seems to be important in tracing different gas components with respect to other molecules, e.g. such as SiO, a classical jet tracer. We compare a grid of C- and J-type shocks spanning different velocities (10 to 40 km s −1 ) and two pre-shock densities (2 × 10 4 and 2 × 10 5 cm −3 ), with the observed intensities. Although none of these models seem to be able to reproduce the absolute intensities of the water emissions observed, it appears that the occurrence of J-shocks, which can compress the gas to very high densities, cannot be ruled out in these environments.
A Mexican hat with holes: calculating low-resolution power spectra from data with gaps

A simple method for calculating a low-resolution power spectrum from data with gaps is described. The method is a modification of the Δ-variance method previously described by Stutzki and Ossenkopf. A Mexican hat filter is used to single out fluctuations at a given spatial scale, and the variance of the convolved image is calculated. The gaps in the image, defined by the mask, are corrected for by representing the Mexican hat filter as a difference between two Gaussian filters with slightly different widths, convolving the image and mask with these filters and dividing the results before calculating the final filtered image. This method cleanly compensates for data gaps even if these have complicated shapes and cover a significant fraction of the data. The method was developed to deal with problematic 2D images, where irregular detector edges and masking of contaminating sources compromise the power spectrum estimates, but it can also be straightforwardly applied to 1D timing analysis or 3D data cubes from numerical simulations.
INTERPLAY OF NEUTRINO OPACITIES IN CORE-COLLAPSE SUPERNOVA SIMULATIONS

We have conducted a series of numerical experiments using spherically symmetric, general relativistic, neutrino radiation hydrodynamics with the code Agile-BOLTZTRAN to examine the effects of modern neutrino opacities on the development of supernova simulations. We test the effects of opacities by removing opacities or by undoing opacity improvements for individual opacities and groups of opacities. We find that improvements to electron capture (EC) on nuclei, namely EC on an ensemble of nuclei using modern nuclear structure models rather than the simpler independent-particle approximation (IPA) for EC on a mean nucleus, plays the most important role during core collapse of all tested neutrino opacities. Low-energy neutrinos emitted by modern nuclear EC preferentially escape during collapse without the energy downscattering on electrons required to enhance neutrino escape and deleptonization for the models with IPA nuclear EC. During shock breakout the primary influence on the emergent neutrinos arises from non-isoenergetic scattering (NIS) on electrons. For the accretion phase, NIS on free nucleons and pair emission by e+e− annihilation have the largest impact on the neutrino emission and shock evolution. Other opacities evaluated, including nucleon–nucleon bremsstrahlung and especially neutrino–positron scattering, have little measurable impact on neutrino emission or shock dynamics. Modern treatments of nuclear EC, e+e−-annihilation pair emission, and NIS on electrons and free nucleons are critical elements of core-collapse simulations of all dimensionality.
Pulsar state switching, timing noise and free precession

Recent radio pulsar observations have shown that a number of pulsars display interesting longterm periodicities in their spin-down rates. At least some of these pulsars also undergo sharp changes in pulse profile. This has been convincingly attributed to the stars abruptly switching between two different magnetospheric states. The sharpness of these transitions has been taken as evidence against free precession as the mechanism behind the long-term variations. We argue that such a conclusion is premature. By performing a simple best-fitting analysis to the data, we show that the relationship between the observed spin and modulation periods is of approximately the correct form to be accounted for by the free precession of a population of neutron stars with strained crusts, the level of strain being similar in all of the stars, and consistent with the star retaining a memory of a former faster rotation rate. We also provide an argument as to why abrupt magnetospheric changes can occur in precessing stars, and how such changes would serve to magnify the effect of precession in the timing data, making the observation of the precession more likely in those stars where such switching occurs. We describe how future observations could further test the precession hypothesis advanced here.
Momentum‐driven feedback and the M–σ relation in non‐isothermal galaxies

We solve for the velocity fields of momentum-conserving supershells driven from galaxy centres by steady winds from supermassive black holes or nuclear star clusters [central massive objects (CMOs)]. We look for the critical CMO mass that allows such a shell to escape from its host galaxy. In the case that the host galaxy dark matter halo is a singular isothermal sphere, we find that the critical CMO mass derived by King, which scales with the halo velocity dispersion as Mcrit∝σ4, is necessary, but not by itself sufficient, to drive shells to large radii in the halo. Furthermore, a CMO mass at least three times the King value is required to drive the shell to the escape speed of the halo. In the case of CMOs embedded in protogalaxies with non-isothermal dark matter haloes, which we treat here for the first time, we find a critical CMO mass that is sufficient to drive any shell (under a steady wind) to escape any galaxy with a peaked circular speed profile. In the limit of large halo mass, relevant to real galaxies, this critical CMO mass depends only on the value of the peak circular speed of the halo, scaling as . Our results therefore relate to observational scalings between black hole mass and asymptotic circular speed in galaxy spheroids. They also suggest a natural way of extending analyses of M–σ relations for black holes in massive bulges, to include similar relations for nuclear clusters in lower mass and disc galaxies.
Tensor eigenvalues and entanglement of symmetric states

Tensor eigenvalues and eigenvectors have been introduced in the recent mathematical literature as a generalization of the usual matrix eigenvalues and eigenvectors. We apply this formalism to a tensor that describes a multipartite symmetric state or a spin state, and we investigate to what extent the corresponding tensor eigenvalues contain information about the multipartite entanglement (or, equivalently, the classicality) of the state. This extends previous results connecting entanglement to spectral properties related to the state. While for spin-1 states the positivity of the smallest tensor eigenvalue is equivalent to separability, we show that for higher values of the angular momentum there is a correlation between entanglement and the value of the smallest tensor eigenvalue.
Bayesian reasoning in cosmology

We discuss epistemological and methodological aspects of the Bayesian approach in astrophysics and cosmology. The introduction to the Bayesian framework is given for a further discussion concerning the Bayesian inference in physics. The interplay between the modern cosmology, Bayesian statistics, and philosophy of science is presented. We consider paradoxes of confirmation, like Goodman's paradox, appearing in the Bayesian theory of confirmation. As in Goodman's paradox the Bayesian inference is susceptible to some epistemic limitations in the logic of induction. However Goodman's paradox applied to cosmological hypotheses seems to be resolved due to the evolutionary character of cosmology and accumulation new empirical evidences. We argue that the Bayesian framework is useful in the context of falsificability of quantum cosmological models, as well as contemporary dark energy and dark matter problem.
Combined asteroseismology, spectroscopy, and astrometry of the CoRoT B2V target HD 170580

Context. Space asteroseismology reveals that stellar structure and evolution models of intermediate- and high-mass stars are in need of improvement in terms of angular momentum and chemical element transport. Aims. We aim to probe the interior structure of a hot, massive star in the core-hydrogen-burning phase of its evolution. Methods. We analysed CoRoT space photometry, Gaia DR2 space astrometry, and high-resolution high signal-to-noise HERMES and HARPS time-series spectroscopy of the slowly rotating B2V star HD 170580. Results. From the time-series spectroscopy, we derive v sin i = 4 ± 2 km s−1, where the uncertainty results from the complex pulsational line-profile variability that has been so far ignored in the literature. We detect 42 frequencies with amplitudes above five times the local noise level. Amongst these we identify five rotationally split triplets and one quintuplet. Asteroseismic modelling based on CoRoT, Gaia DR2, and spectroscopic data leads to a star of M ∼ 8 M⊙ near core-hydrogen exhaustion and an extended overshoot zone. The detected low-order pressure-mode frequencies cannot be fit within the uncertainties of the CoRoT data by models without atomic diffusion. Irrespective of this limitation, the low-order gravity modes reveal HD 170580 to be a slow rotator with an average rotation period between 73 and 98 d and a hint of small differential rotation. Conclusions. Future Gaia DR3 data taking into account the multiplicity of the star, along with long-term TESS photometry would allow us to put better observational constraints on the asteroseismic models of this blue evolved massive star. Improved modelling with atomic diffusion, including radiative levitation, is needed to achieve compliance with the low helium surface abundance of the star. This poses immense computational challenges but is required to derive the interior rotation and mixing profiles of this star.
The similar stellar populations of quiescent spiral and elliptical galaxies

We compare the stellar population properties in the central regions of quiescent faceon spiral and elliptical logM∗/M⊙ > 10.4 galaxies, for a visually classified galaxy sample in SDSS DR7 at 0.04 < z < 0.1. In particular, we analyze [Z/H], r-band light-weighted ages and �(Mgb/hFei), a tracer of the overabundance of α-elements, for galaxies carefully selected to be composed by passive stellar populations. We constract samples of spiral and elliptical galaxies based on robust visual morphological classifications from Galaxy Zoo. At a given total stellar mass, quiescent spirals show slighlty younger (≃ 0.4 Gyrs), less α-enhanced (�(Mgb/hFei lower by 0.09) populations, while at a given central velocity dispersion they are more metal rich, but again at a very low level (0.03 dex). These trends can be attributed either to differences in dynamical structure or differences in stellar population properties. In any case, the small differences imply that, to first order, non-starforming spiral galaxies and ellipticals have very similar star-formation histories. Our passive spirals are carefully selected to not show any indications of ongoing star formation (obscured or unobscured) and thus are far from representative for all disk galaxies in the volume. Nonetheless, the main conclusion from our work is that those spiral galaxies which show no hints of ongoing star formation have stellar populations in their central regions equivalent to those of quiescent, bulge-dominated objects.
Dissonance from the Perspective of Agonistic Pluralism: A Study of Political Fragmentation on Facebook during the 2016 Austrian Presidential Election

ABSTRACT Contemporary public debates are often characterized by structural and substantial dissonances. This paper is concerned with normative and empirical evaluations of these dissonances and makes contributions on both levels. We argue that agonistic pluralism provides an insightful, yet often dismissed, theoretical perspective on the matter of political fragmentation. On the empirical level, we exemplify these considerations against the backdrop of the 2016 Austrian presidential elections and propose a corresponding measurement approach for political fragmentation. A combined network analysis and automated content analysis of comments on Facebook pages affiliated with political parties results in the following main findings: First, when looking at comments between different parties, fragmentation is at a low level at the beginning of the election campaign but increases over time. Second, degrees of fragmentation vary to a great extent between different parties. Third, offensive speech is one purpose for communication between political groups but not the main one.
Invisible Labor, Invisible Value: Unpacking Traditional Assessment of Academic Library Value

Academic libraries face mounting pressure to demonstrate their value to stakeholders, yet traditional assessments of their financial value ignore the work of librarians and library staff in producing usable collections and services for patrons. Through a survey of US academic library workers, we examine the range, scope, and financial value of labor performed in US academic libraries. Our findings reveal ways in which traditional assessment mechanisms render this labor invisible to stakeholders. We argue that making this labor more visible will help better communicate the value of academic libraries and ignite conversations about reducing workload and stress for library workers.
LHCb time-dependent results

This review reports preliminary results of time-dependent measurements of decays of B 0 mesons and B 0 mesons coming from the analysis of about 36 pb −1 of data collected by the LHCb experiment during the 2010 run of the Large Hadron Collider at √ s = 7 TeV.
Making History Matter: History-Advantage Sequence Training for Visual Dialog

We study the multi-round response generation in visual dialog, where a response is generated according to a visually grounded conversational history. Given a triplet: an image, Q&A history, and current question, all the prevailing methods follow a codec (i.e., encoder-decoder) fashion in a supervised learning paradigm: a multimodal encoder encodes the triplet into a feature vector, which is then fed into the decoder for the current answer generation, supervised by the ground-truth. However, this conventional supervised learning does NOT take into account the impact of imperfect history, violating the conversational nature of visual dialog and thus making the codec more inclined to learn history bias but not contextual reasoning. To this end, inspired by the actor-critic policy gradient in reinforcement learning, we propose a novel training paradigm called History Advantage Sequence Training (HAST). Specifically, we intentionally impose wrong answers in the history, obtaining an adverse critic, and see how the historic error impacts the codec’s future behavior by History Advantage — a quantity obtained by subtracting the adverse critic from the gold reward of ground-truth history. Moreover, to make the codec more sensitive to the history, we propose a novel attention network called History-Aware Co-Attention Network (HACAN) which can be effectively trained by using HAST. Experimental results on three benchmarks: VisDial v0.9&v1.0 and GuessWhat? , show that the proposed HAST strategy consistently outperforms the state-of-the-art supervised counterparts.
Reception of the values of the Aeschylus drama and mnemonic imprints by ancient tragedy spectators

Background: Ancient Greek tragedy remains today a special dramatic genre that expresses the concept of the classic through time, perhaps better than any other form of art and culture, representing, as a theatrical expression, the vision of the conception and expression of values of a particular era. In this context, the purpose of the present research is to study the humanitarian values of European culture, as they are expressed in ancient Greek drama, and to highlight the way in which these values are projected through modern drama and are impressed on the spectators. Methods: To achieve this goal, 105 spectators watched the tragedy of Aeschylus ‘Seven against Thebes’ directed by Cesaris Grauzinis and answered, both immediately after watching the performance and six months later, a questionnaire, in order to record their opinions about the theatre performance they had attended. Results: According to the findings of the comparative analyses, it emerged that the messages and values governing the work remain unchanged for its viewers over time. The memory is based on original audio-visual elements and directorial findings, confirming that it preserves the messages of the symbolism of the performance as well as the channels through which they were conveyed to the audience. Conclusions: The correspondences between the past and the present, as well as the contrasts on stage, contributed to the reproduction of the fundamental moral values that the dramatic work brought, highlighting the work and messages of Aeschylus.
Optimal Transport with a New Preprocessing for Deep-Learning Full Waveform Inversion

Full waveform inversion (FWI) has been implemented using deep learning techniques as an analogue recurrent neural network for geophysics. However, the cycle-skipping issue, from which the conventional FWI suffers, troubles the deeplearning aided FWI as well if the least-square loss function is used to measure the misfit between observed and synthetic data. We propose to use a Wasserstein distance loss function combined with a newly designed preprocessing transform, named integration affine scaling, for the inversion. This transform transfers the seismograms into probability densities, and significantly improves the inversion results. Numerical results show that the proposed method outperforms its counterparts in mitigating cycle-skipping, in comparison with other loss functions including the least-square, the absolute, and the quadratic Wasserstein distance losses.
THE TEMPERATURE-DEPENDENT NATURE OF CORONAL DIMMINGS

The opening-up of the magnetic field during solar eruptive events is often accompanied by a dimming of the local coronal emission. From observations of filament eruptions recorded with the Extreme-Ultraviolet Imager on STEREO during 2008–2009, it is evident that these dimmings are much more pronounced in 19.5 nm than in the lower-temperature line 17.1 nm, as viewed either on the disk or above the limb. We conclude that most of the cooler coronal plasma is not ejected but remains gravitationally bound when the loops open up. This result is consistent with Doppler measurements by Imada and coworkers, who found that the upflow speeds in a transient coronal hole increased dramatically above a temperature of 1 MK; it is also consistent with the quasistatic behavior of polar plumes, as compared with the hotter interplume regions that are the main source of the fast solar wind. When the open flux reconnects and closes down again, the trapped plasma is initially heated to such high temperatures that it is no longer visible at Fe ix 17.1 nm. Correspondingly, 17.1 nm images show a dark ribbon or “heat wave” propagating away from the polarity inversion line and coinciding with the brightened Fe xv 28.4 nm and Fe xii 19.5 nm post-eruptive loops and their footpoint areas. Such dark ribbons provide a clear example of dimmings that are not caused by a density depletion. The propagation of the “heat wave” is driven by the closing-down, not the opening-up, of the flux and can be observed both off-limb and on-disk.