Miracle-dz/UniFAR-FTUs huggingface dataset:
Johannes and the seven dwarfs: Kepler detection of low-level day-timescale periodic photometric variations in white dwarfs

We make use of the high photometric precision of Kepler to search for periodic modulations among 14 normal (DA- and DB-type, likely non-magnetic) hot white dwarfs (WDs). In five, and possibly up to seven of the WDs, we detect periodic, ~2 hr to 10 d, variations, with semi-amplitudes of 60 - 2000 ppm, lower than ever seen in WDs. We consider various explanations: WD rotation combined with magnetic cool spots; rotation combined with magnetic dichroism; rotation combined with hot spots from an interstellar-medium accretion flow; transits by size ~50 - 200 km objects; relativistic beaming due to reflex motion caused by a cool companion WD; or reflection/re-radiation of the primary WD light by a brown-dwarf or giant-planet companion, undergoing illumination phases as it orbits the WD. Each mechanism could be behind some of the variable WDs, but could not be responsible for all five to seven variable cases. Alternatively, the periodicity may arise from UV metal-line opacity, associated with accretion of rocky material, a phenomenon seen in ~50% of hot WDs. Non-uniform UV opacity, combined with WD rotation and fluorescent optical re-emission of the absorbed UV energy, could perhaps explain our findings. Even if reflection by a planet is the cause in only a few of the seven cases, it would imply that hot Jupiters are very common around WDs. If some of the rotation-related mechanisms are at work, then normal WDs rotate as slowly as do peculiar WDs, the only kind for which precise rotation measurements have been possible to date. Followup observations for this sample, and the larger numbers of additional WDs now being monitored as part of the K2 Kepler mission extension, will soon discriminate among these possibilities.
Three‐dimensional artificial neural network model of the dayside magnetopause

Artificial neural networks (ANN) from the package NeuroShell 2 are applied to the modeling of the dayside magnetopause. The model data set is based on magnetopause crossings and on the corresponding hour-averaged measurements of the solar wind plasma and the interplanetary magnetic field. The ANN model represents the three-dimensional shape and size of the dayside magnetopause as a function of the solar wind dynamic pressure and the Bz and By components of the interplanetary magnetic field. The model describes the dynamics of the magnetic cusp and global asymmetry of the dayside magnetopause under a wide range of external conditions. Small variations in the size of the magnetopause as a function of the absolute value of By are presented quantitatively in the form of an analytic expression. The ANN model shows three regimes of magnetopause dynamics that are controlled by the Bz component: a pressure balance regime (Bz0 nT), a reconnection regime (0>Bz>−10 nT), and a regime of reconnection saturation (Bz<−10 nT). Also, three different regimes of magnetopause dynamics at the subsolar point are described by a modified pressure balance equation obtained from the ANN model.
Chiral Anomaly and Second Harmonic Generation in Weyl Semimetals

We study second harmonic generation in centrosymmetric Weyl semimetal with broken time reversal symmetry. We calculate electric current density at the double frequency of the propagating electromagnetic field in the presence of applied constant magnetic field, using the method of kinetic equation for electron distribution function. It is shown that the chiral anomaly contribution to second harmonic generation in the lowest order is linearly proportional to the applied magnetic field. The limit when the chiral anomaly dominates over the Lorentz-type contribution to second harmonic generation is discussed.
Particle swarm optimization with mutation

The particle swarm optimization algorithms converges rapidly during the initial stages of a search, but often slows considerably and can get trapped in local optima. This paper examines the use of mutation to both speed up convergence and escape local minima. It compares the effectiveness of the basic particle swarm optimization scheme (BPSO) with each of BPSO with mutation, constriction particle swarm optimization (CPSO) with mutation, and CPSO without mutation. The four test functions used were the Sphere, Ackley, Rastrigin and Rosenbrock functions of dimensions 10, 20 and 30. The results show that mutation hinders the motion of the swarm on the sphere but the combination of CPSO with mutation provides a significant improvement in performance for the Rastrigin and Rosenbrock functions for all dimensions and the Ackley function for dimensions 20 and 30, with no improvement for the 10 dimensional case.
Approximate Solution of Linear Differential Equations

Abstract : The approximate solution of linear differential equations, both homogeneous and nonhomogeneous, is investigated for systems with time varying coefficients. In particular, those systems which are asymptotically stable are investigated and quadratic error measures are defined as means of choosing the particular simple and soluble approximating systems which replace the original insoluble or difficult system. (Author)
A RADIAL VELOCITY TEST FOR SUPERMASSIVE BLACK HOLE BINARIES AS AN EXPLANATION FOR BROAD, DOUBLE-PEAKED EMISSION LINES IN ACTIVE GALACTIC NUCLEI

One of the proposed explanations for the broad, double-peaked Balmer emission lines observed in the spectra of some active galactic nuclei (AGNs) is that they are associated with sub-parsec supermassive black hole (SMBH) binaries. Here, we test the binary broad-line region hypothesis through several decades of monitoring of the velocity structure of double-peaked Hα emission lines in 13 low-redshift, mostly radio-loud AGNs. This is a much larger set of objects compared to an earlier test by Eracleous et al. and we use much longer time series for the three objects studied in that paper. Although systematic changes in radial velocity can be traced in many of their lines, they are demonstrably not like those of a spectroscopic binary in a circular orbit. Any spectroscopic binary period must therefore be much longer than the span of the monitoring (assuming a circular orbit), which in turn would require black hole masses that exceed by 1–2 orders of magnitude the values obtained for these objects using techniques such as reverberation mapping and stellar velocity dispersion. Moreover, the response of the double-peaked Balmer line profiles to fluctuations of the ionizing continuum and the shape of the Lyα profiles are incompatible with an SMBH binary. The binary broad-line region hypothesis is therefore disfavored. Other processes evidently shape these line profiles and cause the long-term velocity variations of the double peaks.
Voedingsadvies bij HFE-hemochromatose

Voor de erfelijke ziekte HFE-hemochromatose, waarbij ijzer zich in het lichaam stapelt, is aderlaten de standaard behandeling. Meestal worden wel enkele voedingsadviezen gegeven, maar deze zijn niet wetenschappelijk onderbouwd. Dit rapport beschrijft de huidige wetenschappelijke inzichten om tot een gefundeerd voedingsadvies te komen.
Effect of Cu deficiency on the optical properties and electronic structure of CuInSe2 and CuIn0.8Ga0.2Se2 determined by spectroscopic ellipsometry

Spectroscopic ellipsometry measurements of CuInSe2 (CIS) and CuIn0.8Ga0. 2Se2 (CIGS) reveal that there are important differences in electronic properties between stoichiometric CIS (CIGS) and Cu-poor CIS (CIGS). We find a reduction in the absorption strength in the spectral region of 1–3eV. This reduction can be explained in terms of the Cu 3d density of states. Cu-poor CIS (CIGS) materials show an increase in band gap due to the reduction in repulsion between Cu 3d and Se 4p states. The experimental results have important implications for the function of polycrystalline optoelectronic devices.
Detection of a QPO in five XMM–Newton observations of RE J1034+396

The X-ray quasi-periodic oscillation (QPO) at $\sim 2.6 \times 10^{-4}$ Hz in RE J1034+396 has been robustly observed in the 0.2-10 keV band of one $\sim 90$ ks XMM-Newton observation, but was not detected in subsequent observations. Here, we investigate the power spectral density (PSD) of 8 archival XMM-Newton observations of RE J1034+396, and search for the presence of QPOs in three energy bands: soft (0.3-0.8 keV); hard (1.0-4.0 keV) and total (0.2-10.0 keV). We find a significant detection of a QPO feature in the hard-band PSD of 5 low flux/spectrally-harder observations. The QPO frequency has remained persistent at $\sim 2.6 \times 10^{-4}$ Hz over $\sim 4$ years of observations, though it is no longer detected in the soft band, except in the original observation. This result increases the duration where the QPO is present by a factor of three (now $\sim 250$ ks), allowing for a better understanding of the QPO phenomenon observed in both Active Galactic Nuclei (AGN) and black hole X-ray binaries (BHBs).
IN ASPLUND SPACES, APPROXIMATELY CONVEX FUNCTIONS AND REGULAR FUNCTIONS ARE GENERICALLY DIFFERENTIABLE

We prove that an approximately convex function on an open subset of an Asplund space is generically Fr´echet differentiable, as are genuine convex functions. Thus, we give a positive answer to a question raised by S. Rolewicz. We also prove a more general result of that type for regular functions on an open subset of an Asplund space.
Preprint typeset in JHEP style-HYPER VERSION BPS dyons and Hesse flow

We revisit BPS solutions to classical N = 2 low energy effective gauge theories. It is shown that the BPS equations can be solved in full generality by the introduction of a Hesse potential, a symplectic analog of the holomorphic prepotential. We explain how for non-spherically symmetric, non-mutually local solutions, the notion of attractor flow generalizes to gradient flow with respect to the Hesse potential. Furthermore we show that in general there is a non-trivial magnetic complement to this flow equation that is sourced by the momentum current in the solution. ∗Email: dieter.vdbl@gmail.com ar X iv :1 11 1. 69 79 v2 [ he pth ] 3 F eb 2 01 2
Spherically symmetric solutions in covariant Horava-Lifshitz gravity

We study the most general case of spherically symmetric vacuum solutions in the framework of the covariant Horava-Lifshitz gravity, for an action that includes all possible higher order terms in curvature which are compatible with power-counting normalizability requirement. We find that solutions can be separated into two main classes: (i) solutions with nonzero radial shift function, and (ii) solutions with zero radial shift function. In the case (ii), spherically symmetric solutions are consistent with observations if we adopt the view of Horava and Melby-Tomson [P. Horava and C. M. Melby-Thompson, Phys. Rev. D 82, 064027 (2010). ], according to which the auxiliary field A can be considered as a part of an effective general relativistic metric, which is valid only in the IR limit. On the other hand, in the case (i), consistency with observations implies that the field A should be independent of the spacetime geometry, as the Newtonian potential arises from the nonzero radial shift function. Also, our aim in this paper is to discuss and compare these two alternative but different assumptions for the auxiliary field A.
The 1.4-GHz radio properties of hard X-ray-selected AGN

We thank the anonymous referee for the valuable comments that improved this work. FP thanks Davide Burlon and Piergiorgio Casella for the fruitful scientific discussions. AT and PC would like to thank Matteo Murgia for useful suggestions on the analysis of radio data. EM acknowledges Paola Parma for the technical support during part of the radio data analysis. FP acknowledges support by INTEGRAL ASI/INAF no. 2013-025.R. O.
Inverse Heat Conduction: Ill-Posed Problems

Description of the Inverse Heat Conduction Problem Exact Solutions of the Inverse Heat Conduction Problem Approximate Methods for Direct Heat Conduction Problems Inverse Heat Conduction Estimation Procedures Inverse Convolution Procedures Difference Methods for Solution of the One Dimensional Inverse Heat Conduction Problem Multiple Heat Flux Estimation Heat Transfer Coefficient Estimation Index.
Trichomoniasis refractory to 5-nitroimidazole therapy in Trinidad

Trichomoniasis is the most common non-viral sexually transmitted infection (STI) occurring worldwide and the majority of infected persons (70–85%) have mild or no genital symptoms. Symptoms in women may include a vaginal discharge which may be associated with vulval irritation and most infections can be effectively treated with metronidazole 500mg bd for seven days. Trichomoniasis unresponsive to 5-nitroimidazole therapy is uncommon but results in substantial therapeutic challenges, especially in resource limited countries. We present such a case which was eventually treated with a low-cost intravaginal combination of boric acid and clotrimazole cream.
Two type I topoisomerases maintain DNA topology in human mitochondria

Abstract Genetic processes require the activity of multiple topoisomerases, essential enzymes that remove topological tension and intermolecular linkages in DNA. We have investigated the subcellular localisation and activity of the six human topoisomerases with a view to understanding the topological maintenance of human mitochondrial DNA. Our results indicate that mitochondria contain two topoisomerases, TOP1MT and TOP3A. Using molecular, genomic and biochemical methods we find that both proteins contribute to mtDNA replication, in addition to the decatenation role of TOP3A, and that TOP1MT is stimulated by mtSSB. Loss of TOP3A or TOP1MT also dysregulates mitochondrial gene expression, and both proteins promote transcription elongation in vitro. We find no evidence for TOP2 localisation to mitochondria, and TOP2B knockout does not affect mtDNA maintenance or expression. Our results suggest a division of labour between TOP3A and TOP1MT in mtDNA topology control that is required for the proper maintenance and expression of human mtDNA.
Varying thin filament activation in the framework of the Huxley'57 model

Muscle contraction is triggered by the activation of the actin sites of the thin filament by calcium ions. It results that the thin filament activation level varies over time. Moreover, this activation process is also used as a regulation mechanism of the developed force. Our objective is to build a model of varying actin site activation level within the classical Huxley'57 two‐state framework. This new model is obtained as an enhancement of a previously proposed formulation of the varying thick filament activation within the same framework. We assume that the state of an actin site depends on whether it is activated and whether it forms a cross‐bridge with the associated myosin head, which results in four possible states. The transitions between the actin site states are controlled by the global actin sites activation level and the dynamics of these transitions is coupled with the attachment–detachment process. A preliminary calibration of the model with experimental twitch contraction data obtained at varying sarcomere lengths is performed.
Revisiting the variable star population in NGC 6229 and the structure of the horizontal branch

We report an analysis of new $V$ and $I$ CCD time-series photometry of the distant globular cluster NGC 6229. The principal aims were to explore the field of the cluster in search of new variables, and to Fourier decompose the RR Lyrae light curves in pursuit of physical parameters.We found 25 new variables: 10 RRab, 5 RRc, 6 SR, 1 CW, 1 SX Phe, and two that we were unable to classify. Secular period changes were detected and measured in some favourable cases. The classifications of some of the known variables were rectified. The Fourier decomposition of RRab and RRc light curves was used to independently estimate the mean cluster value of [Fe/H] and distance. From the RRab stars we found [Fe/H]$_{\rm UVES}$=$-1.31 \pm 0.01{\rm(statistical)} \pm 0.12{\rm(systematic)}$ ([Fe/H]$_{\rm ZW}=-1.42$),and a distance of $30.0\pm 1.5$ kpc, and from the RRc stars we found [Fe/H]$_{\rm UVES}$=$-1.29\pm 0.12$ and a distance of $30.7\pm 1.1$ kpc, respectively. Absolute magnitudes, radii and masses are also reported for individual RR Lyrae stars. Also discussed are the independent estimates of the cluster distance from the tip of the RGB, 34.9$\pm$2.4 kpc and from the P-L relation of SX Phe stars, 28.9$\pm$2.2 kpc. The distribution of RR Lyrae stars in the horizontal branch shows a clear empirical border between stable fundamental and first overtone pulsators which has been noted in several other clusters; we interpret it as the red edge of the first overtone instability strip.
Constructing a Galactic coordinate system based on near-infrared and radio catalogs

Context. The definition of the Galactic coordinate system was announced by the IAU Sub-Commission 33b on behalf of the IAU in 1958. An unrigorous transformation was adopted by the Hipparcos group to transform the Galactic coordinate system from the FK4-based B1950.0 system to the FK5-based J2000.0 system or to the International Celestial Reference System (ICRS). For more than 50 years, the definition of the Galactic coordinate system has remained unchanged from this IAU1958 version. On the basis of deep and all-sky catalogs, the position of the Galactic plane can be revised and updated definitions of the Galactic coordinate systems can be proposed. Aims. We re-determine the position of the Galactic plane based on modern large catalogs, such as the Two-Micron All-Sky Survey (2MASS) and the SPECFIND v2.0. This paper also aims to propose a possible definition of the optimal Galactic coordinate system by adopting the ICRS position of the Sgr A* at the Galactic center. Methods. The near-infrared 2MASS point source catalog and the SPECFIND v2.0 catalog of radio continuum spectra are used to determine the mean position of the Galactic plane on the celestial sphere. Byfittingthe data to an ideal Galactic equator, the parameters defining the Galactic coordinate system are obtained. Results. We find that the obliquity of the Galactic equator on the ICRS principal plane is about 0.4 ◦ (2MASS) and 0.6 ◦ (SPECFIND v2.0) larger than the J2000.0 value, which is widely used in coordinate transformations between the equatorial (α, δ) and the Galactic (�, b). Depending on the adopted parameters, data, and methods, the largest difference between the resulting Galactic coordinate systems is several arcminutes. We derive revised transformation matrices and parameters describing the orientation of the Galactic coordinate systems in the ICRS at the 1 milliarcsecond level to match the precision of modern observations. Conclusions. For practical applications, we propose that a revised definition of the Galactic coordinate system should be required in the near future.
The Use of Biological Markers in Risk Assessment

The use of biologic markers (such as DNA adducts) as more proximate measures of effective dose has many potential advantages for risk assessment. We can hope for: * Better modeling of dose-response relationships, by avoiding the at- tribution of high dose pharmacokinetic nonlinearities to the funda- mental multiple mutation process of carcinogenesis. * Better interspecies projection of doses and risks. * Improved evaluation of past doses in epidemiologic studies. * Insights into the magnitude and significance of human interindivid- ual variability. * Possibly some identification of previously unrecognized genetic hazards. * In the very long run, the quantification of rates of post-initiation stages in tumor development by comparative measurements of the prevalence of adducts, premalignant foci/clones and tumors as a function of age in different tissues. Realizing these advantages will require statistically oriented profession- als in risk assessment to gain familiarity with more complex, simulation- type modeling approaches with multiple points of comparison between theory and experiment-rather than the straightforward curve-fitting that has built the field to this point. It will also require some precautions to avoid mistakes and misuse of these new kinds of data and related theory.
Limited movement of an avian hybrid zone in relation to regional variation in magnitude of climate change

Studies of natural hybrid zones can provide documentation of range shifts in response to climate change and identify loci important to reproductive isolation. Using a temporal (36–38 years) comparison of the black‐capped (Poecile atricapillus) and Carolina (P. carolinensis) chickadee hybrid zone, we investigated movement of the western portion of the zone (western Missouri) and assessed whether loci and pathways underpinning reproductive isolation were similar to those in the eastern portion of the hybrid zone. Using 92 birds sampled along the hybrid zone transect in 2016 and 68 birds sampled between 1978 and 1980, we generated 11,669 SNPs via ddRADseq. These SNPs were used to assess movement of the hybrid zone through time and to evaluate variation in introgression among loci. We demonstrate that the interface has moved ~5 km to the northwest over the last 36–38 years, that is, at only one‐fifth the rate at which the eastern portion (e.g., Pennsylvania, Ohio) of the hybrid zone has moved. Temperature trends over the last 38 years reveal that eastern areas have warmed 50% more than western areas in terms of annual mean temperature, possibly providing an explanation for the slower movement of the hybrid zone in Missouri. Our results suggest hybrid zone movement in broadly distributed species, such as chickadees, will vary between areas in response to local differences in the impacts of climate change.
Improving entanglement of even entangled coherent states by a coherent superposition of photon subtraction and addition

A new entangled quantum state is introduced by applying local coherent superposition (CS) (ra†+ta) of photon subtraction and addition to each mode of an even entangled coherent state (EECS). The properties of entanglement are investigated in terms of the Einstein–Podolsky–Rosen (EPR) correlation, the degree of entanglement, and the average fidelity of quantum teleportation. It is found that single- and two-mode CS operations can improve the EPR correlation of the EECS in a big (>0.88) and small (<0.52) region of amplitude, respectively. The enhanced entanglement and fidelity depend on the even or odd order of CS. All optimal results are not achieved at two extreme cases of t=0, 1.