Miracle-dz/UniFAR-FTUs huggingface dataset:
Towards real neutron star seismology: accounting for elasticity and superfluidity

We study the effects of an elastic crust on the oscillation spectrum of superfluid neutron stars. Within the two-fluid formalism, we consider Newtonian stellar models that include the relevant constituents of a mature neutron star. The core is formed by a mixture of superfluid neutrons and a conglomerate of charged particles, while the inner crust is described by a lattice of nuclei permeated by superfluid neutrons. We linearize the Poisson and the conservation equations of non-rotating superfluid stars and study the effects of elasticity, entrainment and composition stratification on the shear and acoustic modes. In both the core and the crust, the entrainment is derived from recent results for the nucleon effective mass. Solving the perturbation equations as an eigenvalue problem, we find that the presence of superfluid neutrons in the crust and their large effective mass may have significant impact on the star’s oscillation spectrum
Detecting Gender-based Violence aftereffects from Emotional Speech Paralinguistic Features

Speech is known to provide information regarding the person speaking, such as their gender, identity, emotions, and even disorders or trauma. In this paper we aim to answer the following question, can women who have suffered from gender-based violence (GBV) be distinguished from those who have not, just by using speech paralinguistic cues? In this work, we intend to demonstrate whether there exist measurable differences between the emotional expression in the voice of GBV victims (GBVV) and non-victims (Non-GBVV). The present study was carried out in the framework of the project EMPATIA-CM, whose aim is to understand the reaction of GBVV to dangerous situations and develop automatic mechanisms to protect them. For this purpose, we use data collected and partly published from the WEMAC Database, a multimodal database containing physiological and speech data from women who have and have not suffered from GBV while visualizing different emotion-eliciting video clips. With the performed analysis, it is proven that such differences exist indeed and, therefore, that suffering from GBV alters the way women react to the same emotion eliciting stimulus in terms of physical variables, specifically certain voice features.
Nonlocal games, synchronous correlations, and Bell inequalities.

A nonlocal game with a synchronous correlation is a natural generalization of a function between two finite sets, and has recently appeared in the context of quantum graph homomorphisms. In this work we examine analogues of Bell's inequalities for synchronous correlations. We show that, unlike general correlations and the CHSH inequality, there can be no quantum Bell violation among synchronous correlations with two measurement settings. However we exhibit explicit analogues of Bell's inequalities for synchronous correlations with three measurement settings and two outputs, provide an analogue of Tsirl'son's bound in this setting, and give explicit quantum correlations that saturate this bound.
On higher derivative corrections to Wess-Zumino and Tachyonic actions in type II super string theory

We evaluate in detail the string scattering amplitude to compute different interactions of two massless scalars, one tachyon and one closed string Ramond-Ramond field in type II super string theory. In particular we find two scalar field and two tachyon couplings to all orders of $\alpha'$ up to on-shell ambiguity. We then obtain the momentum expansion of this amplitude and apply this infinite number of couplings to actually check that the infinite number of tachyon poles of S-matrix element of this amplitude for the $p=n$ case (where $p$ is the spatial dimension of a D$_p$-brane and $n$ is the rank of a Ramond-Ramond field strength) to all orders of $\alpha'$ is precisely equal to the infinite number of tachyon poles of the field theory. In addition to confirming the couplings of closed string Ramond-Ramond field to the world-volume gauge field and scalar fields including commutators, we also propose an extension of the Wess-Zumino action which naturally reproduces these new couplings in field theory such that they could be confirmed with direct S-matrix computations. Finally we show that the infinite number of massless poles and contact terms of this amplitude for the $p=n+1$ case can be reproduced by Chern-Simons, higher derivative corrections of the Wess-Zumino and symmetrized trace tachyon DBI actions.
Multi-epoch parsec-scale observations of the blazar PKS 1510−089

We investigate the flux density variability and changes in the pc-scale radio structure of the flat spectrum radio quasar PKS 1510−089. This source was the target of multi-epoch very long baseline interferometry (VLBI) and space-VLBI observations at 4.8, 8.4 and 22 GHz carried out between 1999 and 2001. Comparison of the pc-scale structure observed at different epochs shows the presence of a non-stationary jet feature moving with a superluminal apparent velocity of 16.2c ± 0.7c. Over three epochs at 8.4 GHz, during this period, the core flux density varied by about 50 per cent, while the scatter in the jet flux density was within 10 per cent. The polarization percentage of both the core and the jet components significantly changed from 2 to 9 per cent, while the polarization angle of the core showed an abrupt change of about 90 ◦ , becoming roughly perpendicular to the jet direction, consistent with a change in the opacity. To complete the picture of the physical processes at work, we complemented our observations with multi-epoch Very Long Baseline Array data at 15 GHz from the MOJAVE programme spanning a time-baseline from 1995 to 2010. Since 1995 jet components were ejected roughly once per year with the same position angle and an apparent speed between 15c and 20c, indicating that no jet precession has taken place on a time-scale longer than a decade in our frame. The variability of the total intensity flux density together with variations in the polarization properties may be explained assuming either a change between the optically-thick and optically-thin regimes produced by a shock that varies the opacity, or a highly ordered magnetic field produced by the compression of the relativistic plasma by a shock propagating along the jet. Taking into account the high γ -ray emission from this source observed by the AGILE and Fermi satellites, we investigated the connection between the radio and γ -ray activity during 2007–10. Multiwavelength flux and polarization observations suggest that during some γ -ray-flaring episodes the emission at high (γ -ray) and low (radio) energies has origin in the same region.
Database dependence comparison in detection of physical access voice spoofing attacks

The antispoofing challenges are designed to work on a single database, on which we can test our model. The automatic speaker verification spoofing and countermeasures (ASVspoof) [1] challenge series is a community-led initiative that aims to promote the consideration of spoofing and the development of countermeasures. In general, the idea of analyzing the databases individually has been the dominant approach but this could be rather misleading. This paper provides a study of the generalization capability of antispoofing systems based on neural networks by combining different databases for training and testing. We will try to give a broader vision of the advantages of grouping different datasets. We will delve into the ”replay attacks” on physical data. This type of attack is one of the most difficult to detect since only a few minutes of audio samples are needed to impersonate the voice of a genuine speaker and gain access to the ASV system. To carry out this task, the ASV databases from ASVspoof-challenge [2], [3],[4] have been chosen and will be used to have a more concrete and accurate vision of them. We report results on these databases using different neural network architectures and set-ups.
THE EXTREMELY RED HOST GALAXY OF GRB 080207

We present optical, near-infrared, and Spitzer IRAC and MIPS observations of the host galaxy of the dark Swift gamma-ray burst GRB 080207. The host is faint, with extremely red optical–infrared colors (R − K = 6.3, 24 μm/R-band flux ∼1000) making it an extremely red object (ERO) and a dust-obscured galaxy (DOG). The spectral energy distribution (SED) shows the clear signature of the 1.6 μm photometric “bump,” typical of evolved stellar populations. We use this bump to establish the photometric redshift zphot as 2.2+0.2 − 0.3, using a vast library of SED templates, including M 82. The star formation rate (SFR) inferred from the SED fitting is ∼119 M☉ yr−1, the stellar mass 3 × 1011 M☉, and AV extinction from 1 to 2 mag. The ERO and DOG nature of the host galaxy of the dark GRB 080207 may be emblematic of a distinct class of dark GRB hosts, with high SFRs, evolved and metal-rich stellar populations, and significant dust extinction within the host galaxy.
Self-consistent two-phase AGN torus models - SED library for observers

We assume that dust near active galactic nuclei (AGNs) is distributed in a torus-like geometry, which can be described as a clumpy medium or a homogeneous disk, or as a combination of the two (i.e. a two-phase medium). The dust particles considered are fluffy and have higher submillimeter emissivities than grains in the diffuse interstellar medium. The dust-photon interaction is treated in a fully self-consistent three-dimensional radiative transfer code. We provide an AGN library of spectral energy distributions (SEDs). Its purpose is to quickly obtain estimates of the basic parameters of the AGNs, such as the intrinsic luminosity of the central source, the viewing angle, the inner radius, the volume filling factor and optical depth of the clouds, and the optical depth of the disk midplane, and to predict the flux at yet unobserved wavelengths. The procedure is simple and consists of finding an element in the library that matches the observations. We discuss the general properties of the models and in particular the 10 µm silicate band. The AGN library accounts well for the observed scatter of the feature strengths and wavelengths of the peak emission. AGN extinction curves are discussed and we find that there is no direct one-to-one link between the observed extinction and the wavelength dependence of the dust cross sections. We show that objects in the library cover the observed range of mid-infrared colors of known AGNs. The validity of the approach is demonstrated by matching the SEDs of a number of representative objects: Four Seyferts and two quasars for which hyperluminous infrared galaxy. Strikingly, for the five luminous GN models fit the SED without needing to postulate starburst activity.
On minor black holes in galactic nuclei

Small and intermediate mass black holes should be expected in galactic nuclei as a result of stellar evolution, minor mergers and gravitational dynamical friction. If these minor black holes accrete as X-ray binaries or ultra-luminous X-ray sources, and are associated with star formation, they could account for observations of many low luminosity AGN or LINERs. Accreting and inspiralling intermediate mass black holes could provide a crucial electromagnetic counterpart to strong gravitational wave signatures, allowing tests of strong gravity. Here we discuss observational signatures of minor black holes in galactic nuclei and we demonstrate that optical line ratios observed in LINERs or transition-type objects can be produced by an ionizing radiation field from ULXs. We conclude by discussing constraints from existing observations as well as candidates for future study.
Increasing STEM Grit among Underrepresented Groups: Lessons from Our Fathers

Research indicates that students with a high level of Grit and self-efficacy have higher levels of academic achievement. Grit is comprised of passion (con-sistency of interest) and perseverance of effort, for long-term goals. The pur-pose of this model is to increase Grit among underrepresented groups. It utilizes one aspect of self-efficacy, “vicarious experiences”, to increase STEM (Science, Technology, Engineering and Mathematics) Grit among underrepresented groups. Historical contributions from individuals from underrepresented groups in STEM fields are used vicariously to promote student Grit by showing examples of perseverance resulting in academic excellence. This model has implications for curriculum, instruction, assessment, professional development, and public policy articulation.
Ultra-High Sensitivity Surface-Micromachined Capacitive Differential Pressure Sensor for Low-Pressure Applications

An ultra-high sensitivity surface-micromachined capacitive differential pressure sensor and capacitance bridge readout circuit, with amplitude balancing for differential low-pressure gas measurement applications, was designed, fabricated, and characterized. The sensor membrane has a diameter of 800 <inline-formula> <tex-math notation="LaTeX">$\mu \text{m}$ </tex-math></inline-formula> with a thickness of 1 <inline-formula> <tex-math notation="LaTeX">$\mu \text{m}$ </tex-math></inline-formula> and the chip size is <inline-formula> <tex-math notation="LaTeX">$1.5\times 2\times 0.6$ </tex-math></inline-formula> mm3. The characterized sensor pressure range is 0–2000 Pa, with a full-scale capacitance difference span of 0.95 pF. Typical pressure error within the pressure range of 0–2000 Pa is ±0.5%, and the temperature coefficient is 0.044%/°C, both respectively from the pressure reading. [2022-0017]
ENHANCED OFF-CENTER STELLAR TIDAL DISRUPTIONS BY SUPERMASSIVE BLACK HOLES IN MERGING GALAXIES

Off-center stellar tidal disruption flares have been suggested to be a powerful probe of recoiling supermassive black holes (SMBHs) out of galactic centers due to anisotropic gravitational wave radiations. However, off-center tidal flares can also be produced by SMBHs in merging galaxies. In this paper, we computed the tidal flare rates by dual SMBHs in two merging galaxies before the SMBHs become self-gravitationally bounded. We employ an analytical model to calculate the tidal loss-cone feeding rates for both SMBHs, taking into account two-body relaxation of stars, tidal perturbations by the companion galaxy, and chaotic stellar orbits in triaxial gravitational potential. We show that for typical SMBHs with masses 107 M☉, the loss-cone feeding rates are enhanced by mergers up to Γ ∼ 10−2 yr−1, about two orders of magnitude higher than those by single SMBHs in isolated galaxies and about four orders of magnitude higher than those by recoiling SMBHs. The enhancements are mainly due to tidal perturbations by the companion galaxy. We suggest that off-center tidal flares are overwhelmed by those from merging galaxies, making the identification of recoiling SMBHs challenging. Based on the calculated rates, we estimate the relative contributions of tidal flare events by single, binary, and dual SMBH systems during cosmic time. Our calculations show that the off-center tidal disruption flares by un-bound SMBHs in merging galaxies contribute a fraction comparable to that by single SMBHs in isolated galaxies. We conclude that off-center tidal disruptions are powerful tracers of the merging history of galaxies and SMBHs.
Stochastic quantization of the spherical model and supersymmetry

We use the stochastic quantization method to construct a supersymmetric version of the quantum spherical model. This is based on the equivalence between the Brownian motion described by a Langevin equation and the supersymmetric quantum mechanics, which is connected with the existence of the Nicolai map. We investigate the critical behavior of the supersymmetric model at finite as well as at zero temperatures, showing that it exhibits both classical and quantum phase transitions, and determine the critical dimensions.
Medium Extracellular Vesicles—A Qualitative and Quantitative Biomarker of Prostate Cancer

For years, the diagnosis of prostate cancer has been understated. Despite the relatively low mortality rate, prostate cancer is still one of the most common neoplasms in men, which proves the need for continuous improvements in the diagnostics of this disease. New biomarkers may address these challenges in the form of extracellular vesicles (EV) secreted by prostate cancer cells. The available literature in the PubMed, SCOPUS, and ResearchGate databases from the last ten years was analyzed using search phrases such as extracellular vesicles, microparticles, microvesicles, cancer biomarkers, and prostate cancer. Then, the research was selected in terms of the size of the tested EVs (the EV medium of 100–1000 nm diameter, was taken into account), the latest versions of the literature were selected and compiled, and their results were compared. The group of extracellular vesicles contain a substantial amount of genetic information that can be used in research on the specificity of prostate cancer and other cancers. So far, it has been shown that EVs produced by PCa cells express proteins specific for these cells, which, thanks to their specificity, can make EV useful biomarkers of prostate cancer. Moreover, the importance of the quantitative release of EV from PCa cells has been demonstrated, which may be necessary to diagnose prostate cancer malignancy. Each method positively correlates with Gleason’s results and is even characterized by greater diagnostic sensitivity. Medium extracellular vesicles are a promising research material, and their specificity and sensitivity may allow them to be used in future prostate cancer diagnostics as biomarkers.
A Deep Radio Limit for the TRAPPIST-1 System

The first nearby very-low-mass star–planet-host discovered, TRAPPIST-1, presents not only a unique opportunity for studying a system of multiple terrestrial planets, but a means to probe magnetospheric interactions between a star at the end of the main sequence and its close-in satellites. This encompasses both the possibility of persistent coronal solar-like activity, despite cool atmospheric temperatures, and the presence of large-scale magnetospheric currents, similar to what is seen in the Jovian system. Significantly, the current systems include a crucial role for close-in planetary satellites analogous to the role played by the Galilean satellites around Jupiter. We present the first radio observations of the seven-planet TRAPPIST-1 system using the Karl G. Jansky Very Large Array, looking for both highly circularly polarized radio emission and/or persistent quiescent emissions. We measure a broadband upper flux density limit of <8.1 μJy across 4–8 GHz, and place these observations both in the context of expectations for stellar radio emission, and the possible electrodynamic engines driving strong radio emissions in very-low-mass stars and brown dwarfs, with implications for future radio surveys of TRAPPIST-1 like planet-hosts. We conclude that the magnetic activity of TRAPPIST-1 is predominantly coronal and does not behave like the strong radio emitters at the stellar/substellar boundary. We further discuss the potential importance of magnetic field topology and rotation rates, demonstrating that a TRAPPIST-1 like planetary system around a rapidly rotating very-low-mass star can generate emission consistent with the observed radio luminosities of very-low-mass stars and brown dwarfs.
News on the X-ray emission from hot subdwarf stars

Abstract In latest years, the high sensitivity of the instruments on-board the XMM-Newton and Chandra satellites allowed us to explore the properties of the X-ray emission from hot subdwarf stars. The small but growing sample of X-ray detected hot subdwarfs includes binary systems, in which the X-ray emission is due to wind accretion onto a compact companion (white dwarf or neutron star), as well as isolated sdO stars, in which X-rays are probably due to shock instabilities in the wind. X-ray observations of these low-mass stars provide information which can be useful for our understanding of the weak winds of this type of stars and can lead to the discovery of particularly interesting binary systems. Here we report the most recent results we have recently obtained in this research area.
Rapid convergence for simulations that project from particles onto a fixed mesh

The advantage of particle Lagrangian methods in computational fluid dynamics is that advection is accurately modeled. However, the calculation of space derivatives is complicated. On the other hand, Eulerian formulations benefit from a fixed mesh, but feature non-linear advection terms. It seems natural to combine these two, using particles to advect the information and a fixed mesh to calculate space derivatives. This idea goes back to Particle-in-Cell methods, and is here considered within the context of the finite element (FE) method for the fixed mesh, and the particle-FEM (pFEM) for the particles. A “projection” method is required to transfer field values from particles to mesh and vice versa — in this work simple interpolation is used. Our results confirm that projection errors, especially from particles to mesh, cause a slow convergence of the method if standard, linear, FEs, are employed — but also that the convergence rate is restored to values comparable to Lagrangian simulations if quadratically consistent shape functions for the particles are used. The same applies to computational resources, making projection a viable alternative to Lagrangian simulations. The procedure is validated on Zalesak’s disk problem, the Taylor-Green vortex sheet flow, and the Rayleigh-Taylor instability.
The magnitude of the non-adiabatic pressure in the cosmic fluid

Understanding the non-adiabatic pressure, or relative entropy, perturbation is crucial for studies of early-Universe vorticity and cosmic microwave background observations. We calculate the evolution of the linear non-adiabatic pressure perturbation from radiation domination to late times, numerically solving the linear governing equations for a wide range of wavenumbers. Using adiabatic initial conditions consistent with Wilkinson Microwave Anisotropy Probe seven-year data, we find nevertheless that the non-adiabatic pressure perturbation is non-zero and grows at early times, peaking around the epoch of matter/radiation equality and decaying in matter domination. At early times or large redshifts (z= 10 000) its power spectrum peaks at a comoving wavenumber k≈ 0.2 h Mpc−1, while at late times (z= 500) it peaks at k≈ 0.02 h Mpc−1.