Miracle-dz/UniFAR-FTUs huggingface dataset:
Using transient decreases of cosmic rays observed at Voyagers 1 and 2 to estimate the location of the heliospheric termination shock

We have examined the intensity-time profiles of outward moving transient decreases of anomalous and galactic cosmic rays observed by Voyager 1 (Vl) and Voyager 2 (V2) in 1998 and 1999 in the outer heliosphere. The goal of this study is to compare these intensity-time profiles with those obtained by le Roux and Fichtner [1999] using numerical simulations of the time-dependent cosmic ray modulation produced by the passage of large global merged interaction regions. Their calculations show that when these interaction regions reach the heliospheric termination shock, they weaken rapidly causing the intensity of both galactic and anomalous cosmic rays to increase rapidly. They suggest using this time of rapid increase and the propagation times of these events to determine the location of the termination shock. Three outward propagating transient decreases were observed during the 1998–1999 time period. Because of local temporal variations the first two events did not exhibit a le Roux-Fichtner type of rapid recovery. However, the third event starting on day 50 of 1999 at V1 exhibited a very sharply defined intensity-time profile with a very rapid recovery starting on day 88 ± 3 of 1999 that was observed in three energy channels on V1. From this time delay we are able to determine that the termination shock was 9.5–10.7 AU beyond V1 or at a distance of 82.6–83.8 AU at this time. The intensity-time profile at V2 was less sharp, but the rapid recovery that was observed occurred at the same time (±5 days) as that at V1, thus confirming the conclusions from the V1 data. At its present outward speed of 3.6 AU yr−1, V1 would be expected to encounter the termination shock at this location as early as the last quarter of 2001.
Option pricing and hedging with minimum local expected shortfall

We propose a versatile Monte-Carlo method for pricing and hedging options when the market is incomplete, for an arbitrary risk criterion (chosen here to be the expected shortfall), for a large class of stochastic processes, and in the presence of transaction costs. We illustrate the method on plain vanilla options when the price returns follow a Student-t distribution. We show that in the presence of fat-tails, our strategy allows us to significantly reduce extreme risks, and generically leads to low Gamma hedging. We also find that using an asymmetric risk function generates option skews, even when the underlying dynamics is unskewed. Finally, we show the proper accounting of transaction costs leads to an optimal strategy with reduced Gamma, which is found to outperform Leland's hedge.
Mesh Denoising Based on Spherical Wavelets in Reverse Engineering

This paper presents an approach for removing noises of 3D meshes using spherical wavelets. An input 3D mesh is firstly transformed into a spherical signal by a fast low distortion spherical parameterization. This spherical signal is then sampled regularly on the sphere and transformed into the wavelet domain where noises of 3D meshes can be removed easily. Experiments are taken with some typical 3D meshes, which reveals that our method can obtain good results.
UV surface habitability of the TRAPPIST-1 system

With the discovery of rocky planets in the temperate habitable zone (HZ) of the close-by cool star TRAPPIST-1 the question of whether such planets could harbour life arises. Habitable planets around red dwarf stars can orbit in radiation environments that can be life-sterilizing. UV flares from these stars are more frequent and intense than solar flares. Additionally, their temperate HZs are closer to the star. Here we present UV surface environment models for TRAPPIST-1's HZ planets and explore the implications for life. TRAPPIST-1 has high X-ray/EUV activity, placing planetary atmospheres at risk from erosion. If a dense Earth-like atmosphere with a protective ozone layer exists on planets in the HZ of TRAPPIST-1, UV surface environments would be similar to present-day Earth. However an eroded or an anoxic atmosphere, would allow more UV to reach the surface, making surface environments hostile even to highly UV-tolerant terrestrial extremophiles. If future observations detect ozone in the atmospheres of any of the planets in the HZ of TRAPPIST-1, these would be interesting targets for the search for surface life. We anticipate our assay to be a starting point for in-depth exploration of stellar and atmospheric observations of the TRAPPIST-1 planets to constrain their UV-surface-habitability.
Advanced analysis methods in high energy physics

During the coming decade, high energy physics experiments at the Fermilab Tevatron and around the globe will use very sophisticated equipment to record unprecedented amounts of data in the hope of making major discoveries that may unravel some of Nature’s deepest mysteries. The discovery of the Higgs boson and signals of new physics may be around the corner. The use of advanced analysis techniques will be crucial in achieving these goals. I will discuss some of the novel methods of analysis that could prove to be particularly valuable for finding evidence of any new physics, for improving precision measurements and for exploring parameter spaces of theoretical models.
CLASH-VLT: constraints on f(R) gravity models with galaxy clusters using lensing and kinematic analyses

We perform a maximum likelihood kinematic analysis of the two dynamically relaxed galaxy clusters MACS J1206.2-0847 at z=0.44 and RXC J2248.7-4431 at z=0.35 to determine the total mass profile in modified gravity models, using a modified version of the MAMPOSSt code of Mamon, Biviano and Bou'e. Our work is based on the kinematic and lensing mass profiles derived using the data from the Cluster Lensing And Supernova survey with Hubble (hereafter CLASH) and the spectroscopic follow-up with the Very Large Telescope (hereafter CLASH-VLT). We assume a spherical Navarro-Frenk-White (NFW hereafter) profile in order to obtain a constraint on the fifth force interaction range λ for models in which the dependence of this parameter on the environment is negligible at the scale considered (i.e. λ=const) and fixing the fifth force strength to the value predicted in f(R) gravity. We then use information from lensing analysis to put a prior on the other NFW free parameters. In the case of MACSJ 1206 the joint kinematic+lensing analysis leads to an upper limit on the effective interaction range λ≤1.61 mpc at Δχ2=2.71 on the marginalized distribution. For RXJ 2248 instead a possible tension with the ΛCDM model appears when adding lensing information, with a lower limit λ≥0.14 mpc at Δχ2=2.71. This is consequence of the slight difference between the lensing and kinematic data, appearing in GR for this cluster, that could in principle be explained in terms of modifications of gravity. We discuss the impact of systematics and the limits of our analysis as well as future improvements of the results obtained. This work has interesting implications in view of upcoming and future large imaging and spectroscopic surveys, that will deliver lensing and kinematic mass reconstruction for a large number of galaxy clusters.
Differential geometry of polymer models: worm-like chains, ribbons and Fourier knots

We analyse several continuum models of polymers: worm-like chains, ribbons and Fourier knots. We show that the torsion of worm-like chains diverges and conclude that such chains cannot be described by the Frenet–Serret (FS) equation of space curves. While the same holds for ribbons as well, their rate of twist is finite and, therefore, they can be described by the generalized FS equation of stripes. Finally, Fourier knots have finite curvature and torsion and, therefore, are sufficiently smooth to be described by the FS equation of space curves.
Control of post-disruption runaway electron beams in DIII-Da)

Recent experiments in the DIII-D tokamak have demonstrated real-time control and dissipation of post-disruption runaway electron (RE) beams. In the event that disruption avoidance, control, and mitigation schemes fail to avoid or suppress RE generation, active control of the RE beam may be an important line of defense to prevent the rapid, localized deposition of RE beam energy onto vulnerable vessel sections. During and immediately after the current quench, excessive radial compression of the runaway beams is avoided by a combination of techniques, improving the likelihood of the beams surviving this dynamic period without a fast termination. Once stabilized, the runaway beams are held in a steady state (out to the ohmic flux limit) with the application of active plasma current and position controls. Beam interaction with the vessel wall is minimized by avoiding distinct thresholds for enhanced wall interaction at small and large radii, corresponding to inner wall and outer limiter interaction, respectively. Staying within the “safe zone” between those radial thresholds allows for the sustainment of long-lived, quiescent runaway beams. The total beam energy and runaway electron population are then dissipated gradually by a controlled ramp-down of the runaway current.
Haldane model under nonuniform strain

We study the Haldane model under strain using a tight-binding approach, and compare the obtained results with the continuum-limit approximation. As in graphene, nonuniform strain leads to a time-reversal preserving pseudo-magnetic field that induces (pseudo) Landau levels. Unlike a real magnetic field, strain lifts the degeneracy of the zeroth pseudo Landau levels at different valleys. Moreover, for the zigzag edge under uniaxial strain, strain removes the degeneracy within the pseudo-Landau levels by inducing a tilt in their energy dispersion. The latter arises from next-to-leading order corrections to the continuum-limit Hamiltonian, which are absent for a real magnetic field. We show that, for the lowest pseudo-Landau levels in the Haldane model, the dominant contribution to the tilt is different from graphene. In addition, although strain does not strongly modify the dispersion of the edge states, their interplay with the pseudo-Landau levels is different for the armchair and zigzag ribbons. Finally, we study the effect of strain in the band structure of the Haldane model at the critical point of the topological transition, thus shedding light on the interplay between non-trivial topology and strain in quantum anomalous Hall systems.
Large Deformation and Instability of Soft Hollow Cylinder With Surface Effects

Surface stress, which is always neglected in classical elastic theories, has recently emerged as a key role in the mechanics of highly deformable soft solids. In this paper, the effect of surface stress on the deformation and instability of soft hollow cylinder is analyzed. By incorporating surface energy density function into the constitutive model of a hyper-elastic theory, explicit solutions are obtained for the large deformation of soft hollow cylinder under the uniform pressure loading and geometric everting. The surface tension and the residual surface stress have a significant effect on the large deformation and instability of the soft cylinder. When the pressure loading and geometric everting are applied on the soft hollow cylinder, significant changes in the critical condition of the creases are found by varying the surface parameters. Two models of instability, surface crease and global buckling behavior, will be generated on the soft hollow cylinder with the uniform pressure, and the formed instability model is dependent on the ratio of the thickness to the radius. The results in this work reveal that surface energy obviously influences both the deformation and the instability of soft hollow cylinder at finite deformation and will be helpful for understanding and predicting the mechanical behavior of soft structures accurately.
Religiosity / spirituality ( R / S ) in professional practice in pediatric oncology : resource or protocol ?

oncologia vivenciam R/E suas práticas. CINAHL, PsycINFO, SciELO Lilacs estudos produzidos nove qualitativos e três quantitativos. Os resultados foram apresentados em duas categorias temáticas: 1) A R/E como elemento que perpassa situações vividas no trabalho; 2) A R/E como uma dimensão presente na vida de pacientes e familiares. Evidenciou-se que, embora os profissionais da oncologia pediátrica considerem a R/E como uma dimensão importante no cuidado, a mesma ainda é compreendida como um recurso empregado sobretudo por pacientes e familiares, predominando, entre os profissionais, um sentido mais ligado a um protocolo do que a um efetivo recurso para o trabalho na área. Abstract The inclusion of religiosity/spirituality (R/S) as a dimension of health care still raises reflections, especially when we analyze professional practices. Thus, this integrative literature review aimed to analyze how pediatric oncology professionals experience R/S in their practices. Through the bases/libraries CINAHL, PsycINFO, Pubmed, SciELO and Lilacs, 12 studies produced between the years of 2009 and 2019 were retrieved, nine qualitative and three quantitative. The results were presented in two thematic categories: 1) R/S as an element that permeates situations experienced at work; 2) R/S as a dimension present in the lives of patients and family members. It became evident that, although pediatric oncology professionals consider R/S as an important dimension in care, it is still understood as a resource used mainly by patients and family members, with predominance, __________________________________________________________________________________________________ professionals, as something that is more linked to a protocol than an effective resource for working in the area.
A PDF-Based Formulation of Microphysical Variability in Cumulus Congestus Clouds*

AbstractCalculating unbiased microphysical process rates over mesoscale model grid volumes necessitates knowledge of the subgrid-scale (SGS) distribution of variables, typically represented as probability distribution functions (PDFs) of the prognostic variables. In the 2014 Journal of the Atmospheric Sciences paper by Kogan and Mechem, they employed large-eddy simulation of Rain in Cumulus over the Ocean (RICO) trade cumulus to develop PDFs and joint PDFs of cloud water, rainwater, and droplet concentration. In this paper, the approach of Kogan and Mechem is extended to deeper, precipitating cumulus congestus clouds as represented by a simulation based on conditions from the TOGA COARE field campaign. The fidelity of various PDF approximations was assessed by evaluating errors in estimating autoconversion and accretion rates. The dependence of the PDF shape on grid-mean variables is much stronger in congestus clouds than in shallow cumulus. The PDFs obtained from the TOGA COARE simulations for the calcul.
Spin-foam model for gravity coupled to massless scalar field

A spin-foam model is derived from the canonical model of loop quantum gravity coupled to a massless scalar field. We generalized to the full theory the scheme first proposed in the context of loop quantum cosmology by Ashtekar et al (2009 Phys. Lett. B 681 347–52), later developed by Henderson et al (2011 Class. Quantum Grav. 28 025003).
Radio-quiet Quasars in the Direction of the Northern Hubble Deep Field

We match quasars discovered in a multicolor survey centered on the northern Hubble Deep Field (HDF) with radio sources from an ultradeep radio survey. Although three out of 12 quasars are detected at a level below 0.2 mJy at 1.4 GHz, all of the quasars in the search area are radio quiet by the criterion Lr < 1025 h W Hz-1. We combine this information with other radio surveys of quasars so as to break the degeneracy between redshift and luminosity. In the redshift range 0.02 < z < 3.64, the radio-loud fraction increases with increasing optical luminosity, consistent with some degree of correlation between the nonthermal optical and radio emissions. More tentatively, for low-luminosity quasars in the range -22.5 < MB < -25, the radio-loud fraction decreases with increasing redshift. We can infer from this that the radio luminosity function evolves more slowly than the optical luminosity function. The mechanism that leads to strong radio emission in only a small fraction of quasars at any epoch is still unknown.
Superfluid phases of quark matter, II: Phenomenology and sum rules

We derive sum rules for a uniform, isotropic superfluid quark-gluon plasma with massless quarks, first laying out the phenomenological equations obeyed by a color superconductor in terms of macroscopic observables such as the superfluid mass and baryon densities, and the electric and magnetic gluon masses, and then expressing these quantities in terms of equilibrium correlation functions. From the transverse part of the long wavelength baryon current-momentum correlation function we derive an exact expression for the superfluid baryon density, and from the longitudinal part, an f-sum rule. From the transverse part of the long wavelength color current-current correlation function we derive the superfluid Meissner mass, and from the longitudinal part, the Debye mass. These masses constrain integrals of the transverse and longitudinal parts of the gluon propagator over frequencies, and provide self-consistent conditions for a solution to the gap equation beyond weak coupling.
The Configuration Structure of Entrepreneurial Team and InnovationModel for the Success of High Growth Unicorn Companies

: Emerging digital technologies brought a transformative impact on the development of unicorn companies. The entrepreneurial mechanism behind the high growth rate and high valuation of unicorn companies plays a significant role in understanding the growth of entrepreneurial companies. Grounded in the upper echelon theory, this paper constructs a joint effect model of entrepreneurial teams and innovation models jointly affecting the high growth of unicorn companies. Then, four configurations were obtained using the fuzzy-set qualitative comparative analysis method (fsQCA) to explain the success of unicorn companies. This research expands the applicable boundary of upper echelon theory in the research setting of unicorn companies. It provides entrepreneurial strategy maps for start-ups seeking continuous high growth in the era of the digital economy.
APOGEE Data Releases 13 and 14: Data and Analysis

The data and analysis methodology used for the SDSS/APOGEE Data Releases 13 and 14 are described, highlighting differences from the DR12 analysis presented in Holtzman et al. Some improvement in the handling of telluric absorption and persistence is demonstrated. The derivation and calibration of stellar parameters, chemical abundances, and respective uncertainties are described, along with the ranges over which calibration was performed. Some known issues with the public data related to the calibration of the effective temperatures (DR13), surface gravity (DR13 and DR14), and C and N abundances for dwarfs (DR13 and DR14) are highlighted. We discuss how results from a data-driven technique, The Cannon, are included in DR14 and compare those with results from the APOGEE Stellar Parameters and Chemical Abundances Pipeline. We describe how using The Cannon in a mode that restricts the abundance analysis of each element to regions of the spectrum with known features from that element leads to Cannon abundances can lead to significantly different results for some elements than when all regions of the spectrum are used to derive abundances.
Viewing Angle of Binary Neutron Star Mergers

The joint detection of the gravitational wave (GW) GW170817 and its electromagnetic (EM) counterparts GRB170817A and kilonova AT 2017gfo has triggered extensive study of the EM emission of binary neutron star mergers. A parameter which is common to and plays a key role in both the GW and the EM analyses is the viewing angle of the binary's orbit. If a binary is viewed from different angles, the amount of GW energy changes (implying that orientation and distance are correlated) and the EM signatures can vary, depending on the structure of the emission. Information about the viewing angle of the binary orbital plane is therefore crucial to the interpretation of both the GW and the EM data, and can potentially be extracted from either side. In the first part of this study, we present a systematic analysis of how well the viewing angle of binary neutron stars can be measured from the GW data. We show that if the sky position and the redshift of the binary can be identified via the EM counterpart and an associated host galaxy, then for 50$\%$ of the systems the viewing angle can be constrained to $\leq 7^{\circ}$ uncertainty from the GW data, independent of electromagnetic emission models. On the other hand, if no redshift measurement is available, the measurement of the viewing angle with GW alone is not informative, unless the true viewing angle is close to $90^{\circ}$. This holds true even if the sky position is measured independently. Then, we consider the case where some constraints on the viewing angle can be placed from the EM data itself. We show that the EM measurements can then be used in the analysis of GW data to improve the precision of the luminosity distance, and hence of the Hubble constant, by a factor of 2 to 3. That would allow for a $1\%$ measurement of the Hubble constant, independent of the cosmic distance ladder, in the next 5 years.
EVALUATION OF SEEING ON A 62-CM MIRROR

A 62-cm active optics telescope model with a Shack-Hartmann wavefront analyzer was used to measure the mirror seeing effect. The degradation of the imaging quality due to the generation of microthermal convection was quantitatively evaluated from diurnal monitoring measurements over 90 days and nights. The dependence of mirror seeing on the temperature difference between the mirror and the ambient air and the effect of flushing flow to blow away the microthermal turbulence were measured.