Miracle-dz/UniFAR-FTUs huggingface dataset:
Temperature and Humidity Dependence of Resistance in Nano-Diamond Powder

The electrical resistance of detonation nano-diamond powders was measured from liquid nitrogen temperature to room temperature and in relative humidity environments from around 10% to 100%. After sample exposures of several hours at 100% relative humidity at room temperature (around 295 K), when the temperature was reduced, the resistance increased to the upper measurement limit of our apparatus (120 M{\Omega}) at around 240 K. Upon warming, the resistance dropped back to the room temperature value, with some hysteresis. For sample exposures after several hours at 100% relative humidity at room temperature, as the relative humidity was reduced, the sample resistance increased to the upper range limit of the apparatus. As the relative humidity was then increased (all at room temperature), the resistance dropped. For samples exposed to low (~10%) relative humidity for several hours at room temperature, as the humidity was increased (at room temperature), the resistance decreased, and then increased when the humidity was reduced. The temperature behavior was markedly differ from that of powdered graphite and multi-walled carbon nano tubes.
A Galois connection between classical and intuitionistic logics. I: Syntax

In a 1985 commentary to his collected works, Kolmogorov remarked that his 1932 paper"was written in hope that with time, the logic of solution of problems [i.e., intuitionistic logic] will become a permanent part of a [standard] course of logic. A unified logical apparatus was intended to be created, which would deal with objects of two types - propositions and problems. "We construct such a formal system, as well as its predicate version QHC, which is a conservative extension of both the intuitionistic predicate calculus QH and the classical predicate calculus QC. The only new connectives ? and ! of QHC induce a Galois connection (i.e., a pair of adjoint functors) between the Lindenbaum posets (i.e. the underlying posets of the Lindenbaum algebras) of QH and QC. Kolmogorov's double negation translation of propositions into problems extends to a retraction of QHC onto QH; whereas Goedel's provability translation of problems into modal propositions extends to a retraction of QHC onto its QC+(? ) fragment, identified with the modal logic QS4. The QH+(! ) fragment is an intuitionistic modal logic, whose modality ! is a strict lax modality in the sense of Aczel - and thus resembles the squash/bracket operation in intuitionistic type theories. The axioms of QHC attempt to give a fuller formalization (with respect to the axioms of intuitionistic logic) to the two best known contentual interpretations of intiuitionistic logic: Kolmogorov's problem interpretation (incorporating standard refinements by Heyting and Kreisel) and the proof interpretation by Orlov and Heyting (as clarified by G\"odel). While these two interpretations are often conflated, from the viewpoint of the axioms of QHC neither of them reduces to the other one, although they do overlap.
RH 1.5D: a massively parallel code for multi-level radiative transfer with partial frequency redistribution and Zeeman polarisation

The emergence of three-dimensional magneto-hydrodynamic (MHD) simulations of stellar atmospheres has sparked a need for efficient radiative transfer codes to calculate detailed synthetic spectra. We present RH 1.5D, a massively parallel code based on the RH code and capable of performing Zeeman polarised multi-level non-local thermodynamical equilibrium (NLTE) calculations with partial frequency redistribution for an arbitrary amount of chemical species. The code calculates spectra from 3D, 2D or 1D atmospheric models on a column-by-column basis (or 1.5D). While the 1.5D approximation breaks down in the cores of very strong lines in an inhomogeneous environment, it is nevertheless suitable for a large range of scenarios and allows for faster convergence with finer control over the iteration of each simulation column. The code scales well to at least tens of thousands of CPU cores, and is publicly available. In the present work we briefly describe its inner workings, strategies for convergence optimisation, its parallelism, and some possible applications.
Assembly and speed control in ion exchange based modular phoretic micro-swimmers

We introduce and study ion exchange based modular micro-swimmers in low salt water which self-assemble into self-propelling complexes transporting cargo with speeds of several microns per second over extended distances and times. We systematically quantify the assembly shape and speed of the complexes for different combinations of ion exchange particles and cargo particles, salt types and concentrations, substrate types and cell geometries. Irrespective of experimental boundary conditions we observe a regular development of the assembly shape with increasing cargo number. Moreover, the swimming speed increases stepwise upon increasing the cargo number and then saturate at a maximum speed. The observed speeds depend systematically on the properties of the components and the cell geometry. We suggest a preliminary geometric model of self assembly and an active role of cargo for swimmer propulsion which is able to describe a large part of the observations in a qualitative way. Our study further shows how to control swimming performance and efficiency through suitable optimization of the components constituting our modular micro-swimmers.
DISCOVERY OF AN ULTRASOFT X-RAY TRANSIENT SOURCE IN THE 2XMM CATALOG: A TIDAL DISRUPTION EVENT CANDIDATE

We have discovered an ultrasoft X-ray transient source, 2XMMi J184725.1-631724, which was detected serendipitously in two XMM-Newton observations in the direction of the center of the galaxy IC 4765-f01-1504 at a redshift of 0.0353. These two observations were separated by 211 days, with the 0.2–10 keV absorbed flux increasing by a factor of about nine. Their spectra are best described by a model dominated by a thermal disk or a single-temperature blackbody component (contributing ≳80% of the flux) plus a weak power-law component. The thermal emission has a temperature of a few tens of eV, and the weak power-law component has a photon index of ∼3.5. Similar to the black hole X-ray binaries in the thermal state, our source exhibits an accretion disk whose luminosity appears to follow the L∝T4 relation. This would indicate that the black hole mass is about 105–106 M☉ using the best-fitting inner disk radius. Both XMM-Newton observations show variability of about 21% on timescales of hours, which can be explained as due to fast variations in the mass accretion rate. The source was not detected by ROSAT in an observation in 1992, indicating a variability factor of ≳64 over longer timescales. The source was not detected again in X-rays in a Swift observation in 2011 February, implying a flux decrease by a factor of ≳12 since the last XMM-Newton observation. The transient nature, in addition to the extreme softness of the X-ray spectra and the inactivity of the galaxy implied by the lack of strong optical emission lines, makes it a candidate tidal disruption event. If this is the case, the first XMM-Newton observation would have been in the rising phase and the second one in the decay phase.
Star formation efficiency as a function of metallicity: from star clusters to galaxies

We explore how the star formation efficiency (SFE) in a protocluster clump is regulated by metallicity-dependent stellar winds from the newly formed massive OB stars (M� ≥ 5M � ) on their main sequence. The model describes the coevolution of the mass function of gravitationally bound cores and of the initial mass function in a protocluster clump. Dense cores are generated uniformly in time at different locations in the clump, and contract over lifetimes that are a few times their free-fall times. The cores collapse to form stars that power strong stellar winds whose cumulative kinetic energy evacuates the gas from the clump and quenches further core and star formation. This sets the final SFE, SFEf. Models are run with various metallicities in the range Z/Z� = [0.1, 2]. We find that the SFEf decreases strongly with increasing metallicity. The SFEf–metallicity relation is well described by a decaying exponential whose exact parameters depend weakly on the value of the core formation efficiency. We find that there is almost no dependence of the SFEf–metallicity relation on the clump mass. This is due to the fact that an increase (decrease) in the clump mass leads to an increase (decrease) in the feedback from OB stars which is opposed by an increase (decrease) in the gravitational potential of the clump. The clump mass–cluster mass relations we find for all of the different metallicity cases imply a negligible difference between the exponent of the mass function of the protocluster clumps and that of the young clusters’ mass function. By normalizing the SFEs to their value for the solar metallicity case, we compare our results to SFE–metallicity relations derived on galactic scales and find a good agreement. As a by-product of this study, we also provide ready-to-use prescriptions for the power of stellar winds of main-sequence
Precision cosmology with a wide area XMM cluster survey

We explore the cosmological constraints expected from wide area XMM-type cluster surveys covering 50–200 deg2, under realistic observing conditions. We perform a Fisher matrix analysis, based on cluster number counts in combination with estimates of the two-point cluster correlation function. The effect of the survey design is implemented through an observationally well-tested cluster selection function. Special attention is given to the modelling of the shot noise and sample variance, which we estimate by applying our selection function to numerically simulated surveys. We then infer the constraints on the equation of state of the dark energy, considering various survey configurations. We quantitatively investigate the respective impact of the cluster mass measurements, of the correlation function and of the 1 < z < 2 cluster population. We show that, with some 20 Ms XMM observing time, it is possible to constrain the dark energy parameters at a level comparable to that expected from the next generation of cosmic probes. Such a survey also has the power to provide unique insights into the physics of high-redshift clusters and the properties of active galactic nuclei.
Biconformal symmetry and static Maxwell fields near higher-dimensional black holes

We study an electric field created by a static electric charge near the higher dimensional Reissner-Nordstrom black hole. The relation between the static Green functions on the D-dimensional Reissner-Nordstrom background and on the (D+2)-dimensional homogeneous Bertotti-Robinson spacetime is found. Using the biconformal symmetry we obtained a simple integral representation for the static Maxwell Green functions in arbitrary dimensions. We show that in a four-dimensional spacetime the static Green function obtained by the biconformal method correctly reproduces known results. We also found a closed form for the exact static Green functions and vector potentials in the five-dimensional Reissner-Nordstrom spacetime.
Dynamics of entropic uncertainty relation under quantum channels with memory

ABSTRACT Recently, Xu et al. [Phys. Rev. A 2012, 86, 012113] have explored the behaviour of the entropic uncertainty relation under the influence of local unital and nonunital noisy channels for a class of Bell-diagonal states. We here improve their results and investigate the entropic uncertainty relation under the influence of unital and nonunital noisy channels with memory. Different types of noisy channels with memory, such as amplitude damping channel (nonunital channel), phase-damping and depolarizing channels (unital channels) have been taken into account. Analytical or numerical results is presented. The effect of channels with memory on dynamics of the entropic uncertainty (or its lower bound) has been discussed in detail. Compare with previous results, our results show that, the entropic uncertainty (or its lower bound) subjecting to amplitude damping channel with memory will be reduced at first and then be lifted with the memory coefficient of channel μ increasing, however they will be only reduced under phase-damping and depolarizing channels in the presence of memory. Especially, in the limit of , the entropic uncertainty (or its lower bound) could be well protected and immune to decoherence of channels.
SHELS: TESTING WEAK-LENSING MAPS WITH REDSHIFT SURVEYS

Weak-lensing surveys are emerging as an important tool for the construction of “mass-selected” clusters of galaxies. We evaluate both the efficiency and completeness of a weak-lensing selection by combining a dense, complete redshift survey, the Smithsonian Hectospec Lensing Survey (SHELS), with a weak-lensing map from the Deep Lens Survey (DLS). SHELS includes 11,692 redshifts for galaxies with R ⩽ 20.6 in the 4 deg2 DLS field; the survey is a solid basis for identifying massive clusters of galaxies with redshift z ≲ 0.55. The range of sensitivity of the redshift survey is similar to the range for the DLS convergence map. Only four of the 12 convergence peaks with signal to noise ⩾3.5 correspond to clusters of galaxies with M ≳ 1.7 × 1014 M☉. Four of the eight massive clusters in SHELS are detected in the weak-lensing map yielding a completeness of ∼50%. We examine the seven known extended cluster X-ray sources in the DLS field: three can be detected in the weak-lensing map, three should not be detected without boosting from superposed large-scale structure, and one is mysteriously undetected even though its optical properties suggest that it should produce a detectable lensing signal. Taken together, these results underscore the need for more extensive comparisons among different methods of massive cluster identification.
Journal of Geophysical Research: Planets Mercury’s gravity, tides, and spin from MESSENGER radio science data

We analyze radio tracking data obtained during 1311 orbits of the MErcury Surface, Space ENvironment, GEochemistry, and Ranging (MESSENGER) spacecraft in the period March 2011 to April 2014. A least squares minimization of the residuals between observed and computed values of two-way range and Doppler allows us to solve for a model describing Mercury’s gravity, tidal response, and spin state. We use a spherical harmonic representation of the gravity ﬁeld to degree and order 40 and report error bars corresponding to 10 times the formal uncertainties of the ﬁt. Our estimate of the product of Mercury’s mass and the gravitational constant, GM =( 22031 . 87404 ± 9 × 10 − 4 ) km 3 s − 2 , is in excellent agreement with published results. Our solution for the geophysically important second-degree coeﬃcients ( ̄ C 2 , 0 = − 2 . 25100 × 10 − 5 ± 1 . 3 × 10 − 9 , ̄ C 2 , 2 = 1 . 24973 × 10 − 5 ± 1 . 2 × 10 − 9 ) conﬁrms previous estimates to better than 0.4% and, therefore, inferences about Mercury’s moment of inertia and interior structure. Our estimate of the tidal Love number k 2 = 0 . 464 ± 0 . 023 indicates that Mercury’s mantle may be hotter and weaker than previously thought. Our spin state solution suggests that gravity-based estimates of Mercury’s spin axis orientation are marginally consistent with previous measurements of the orientation of
Flux density measurements of gigahertz-peaked spectra candidate pulsars at 610 MHz using an interferometric imaging technique

We conducted radio interferometric observations of six pulsars at 610 MHz using the Giant Metrewave Radio Telescope. All these objects were claimed or suspected to be gigahertzpeaked spectra (GPS) pulsars. For half of the sources in our sample, interferometric imaging is the only way to estimate their flux at 610 MHz due to strong pulse scatter-broadening. In our case, these pulsars have very high dispersion measure values and we present their spectra with, for the first time, low-frequency measurements. The remaining three pulsars were observed at low frequencies using the conventional pulsar flux measurement method. The interferometric imaging technique allowed us to re-examine their fluxes at 610 MHz. We were able to confirm the GPS feature in the PSR B1823−13 spectrum and select a GPS candidate pulsar. These results clearly demonstrate that the interferometric imaging technique can be successfully applied to estimate the flux density of pulsars even in the presence of strong scattering.
Structure formation in a colliding flow: the Herschel view of the Draco Nebula

The Draco nebula is a high Galactic latitude interstellar cloud likely to have been formed by the collision of a Galactic halo cloud entering the disk of the Milky Way. Such conditions are ideal to study the formation of cold and dense gas in colliding flows of warm gas. We present Herschel-SPIRE observations that reveal the fragmented structure of the interface between the infalling cloud and the Galactic layer. This front is characterized by a Rayleigh-Taylor instability structure. From the determination of the typical length of the periodic structure (2.2 pc) we estimated the gas kinematic viscosity and the turbulence dissipation scale (0.1 pc) that is compatible with that expected if ambipolar diffusion is the main mechanism of energy dissipation in the WNM. The small-scale structures of the nebula are typical of that seen in some molecular clouds. The gas density has a log-normal distribution with an average value of $10^3$ cm$^{-3}$. The size of the structures is 0.1-0.2 pc but this estimate is limited by the resolution of the observations. The mass ranges from 0.2 to 20 M$_{\odot}$ and the distribution of the more massive clumps follows a power law $dN/d\log(M) \sim M^{-1.4}$. We identify a mass-size relation with the same exponent as that found in GMCs ($M\sim L^{2.3}$) but only 15% of the mass of the cloud is in gravitationally bound structures. We conclude that the increase of pressure in the collision is strong enough to trigger the WNM-CNM transition caused by the interplay between turbulence and thermal instability as self-gravity is not dominating the dynamics.
Top-quark pair production cross sections at NNLO+NNLL in pPb collisions at $\sqrt{s_{NN}}$ = 8.16 TeV

Total and fiducial top pair ($t\bar{t}$) production cross sections in proton-lead (pPb) collisions at $\sqrt{s_{NN}}$ = 8.16 TeV are computed at next-to-next-to-leading-order (NNLO) accuracy including next-to-next-to-leading-log (NNLL) gluon resummation, using the CT14 and CT10 proton parton distribution functions (PDF), and the EPPS16 and EPS09 nuclear PDF parametrizations for the lead ion. The total cross sections amount to $\sigma(pPb\to t\bar{t}+X) = 59.0 \pm 5.3$(CT14+EPPS16)$\,^{+1.6}_{-2.1}$(scale) nb, and $57.5 \pm \,^{+4.3}_{-3.3}$(CT10+EPS09)$\,^{+1.5}_{-2.0}$(scale) nb, with small modifications with respect to the result computed using the free proton PDF alone. The normalized ratio of pPb to pp cross sections (nuclear modification factor) is $R_{pPb} = 1.04 \,^{\pm 0.07(EPPS16)}_{\pm0.03(EPS09)}$. In the lepton+jets decay mode, $t\bar{t} \to b\bar{b} W(\ell\nu) W(q\bar{q}')$, one expects $\sim$600 $t\bar{t}$ events in the 180 nb$^{-1}$ integrated luminosity collected in pPb collisions at the LHC so far, after typical acceptance and efficiency losses. Differential cross sections at NLO accuracy are presented as a function of transverse momentum and rapidity of the top quarks, and of their decay b-jets and isolated leptons.
Observational tests of a two parameter power-law class modified gravity in Palatini formalism

CONTEXT: In this work we propose a modified gravity action $f(R)=({R}^{n}\ensuremath{-}{R}_{0}^{n}{)}^{1/n}$ with two free parameters of $n$ and ${R}_{0}$ and derive the dynamics of a universe for this action in the Palatini formalism. AIM: We do a cosmological comparison of this model with observed data to find the best parameters of a model in a flat universe. METHOD: To constrain the free parameters of model we use SNIa type Ia data in two sets of gold and union samples, CMB-shift parameter, baryon acoustic oscillation, gas mass fraction in cluster of galaxies, and large-scale structure data. RESULT: The best fit from the observational data results in the parameters of model in the range of $n={0.98}_{\ensuremath{-}0.08}^{+0.08}$ and ${\ensuremath{\Omega}}_{M}={0.25}_{+0.1}^{\ensuremath{-}0.1}$ with one sigma level of confidence where a standard $\ensuremath{\Lambda}\mathrm{CDM}$ universe resides in this range of solution.
QCD Analysis of Polarized Deep Inelastic Scattering Data

A QCD analysis of the world data on inclusive polarized deep inelastic scattering of leptons on nucleons is presented in leading and next–to–leading order. New parameterizations are derived for the quark and gluon distributions and the value of a s ( M Z ) is determined. Emphasis is put on the derivation of fully correlated error bands for these distributions which are directly applicable to determine experimental errors of other polarized observables. The impact of the variation of both the renormalization and factorization scales on the value of a s is studied. Finally a factorization– scheme invariant QCD analysis based on the observables g 1 ( x , Q 2 ) and dg 1 ( x , Q 2 ) / d log ( Q 2 ) is performed in next–to–leading order, which is compared to the standard analysis.
Gap formation and stability in non-isothermal protoplanetary discs

Several observations of transition discs show lopsided dust-distributions. A potential explanation is the formation of a large-scale vortex acting as a dust-trap at the edge of a gap opened by a giant planet. Numerical models of gap-edge vortices have thus far employed locally isothermal discs, but the theory of this vortex-forming or `Rossby wave' instability was originally developed for adiabatic discs. We generalise the study of planetary gap stability to non-isothermal discs using customised numerical simulations of disc-planet systems where the planet opens an unstable gap. We include in the energy equation a simple cooling function with cooling timescale $t_c=\beta\Omega_k^{-1}$, where $\Omega_k$ is the Keplerian frequency, and examine the effect of $\beta$ on the stability of gap edges and vortex lifetimes. We find increasing $\beta$ lowers the growth rate of non-axisymmetric perturbations, and the dominant azimuthal wavenumber $m$ decreases. We find a quasi-steady state consisting of one large-scale, over-dense vortex circulating the outer gap edge, typically lasting $O(10^3)$ orbits. Vortex lifetimes were found to generally increase with cooling times up to an optimal value, beyond which vortex lifetimes decrease. This non-monotonic dependence is qualitatively consistent with recent studies using strictly isothermal discs that vary the disc aspect ratio.
DUST AND POLYCYCLIC AROMATIC HYDROCARBON IN THE HD 34700 DEBRIS DISK

The debris disk around the Vega-type star HD 34700 is detected in dust thermal emission from the near-infrared (IR) to millimeter (mm) and submm wavelength range. Also detected is a distinct set of emission features at 3.3, 6.2, 7.7, 8.6, 11.3, and 12.7 &mgr; m ? > , which are commonly attributed to polycyclic aromatic hydrocarbon (PAH) molecules. We model the observed dust IR spectral energy distribution (SED) and PAH emission features of the HD 34700 disk in terms of porous dust and astronomical-PAHs. Porous dust together with a mixture of neutral and ionized PAHs closely explains the dust IR SED and PAH emission features observed in the HD 34700 disk. Due to the stellar radiation pressure and Poynting–Robertson drag together with the photodissociation of PAHs, substantial removal of dust and PAHs has occurred in the disk, and continuous replenishment of these materials is required to maintain their current abundances. This implies that these materials are not primitive but secondary products probably originating from mutual collisions among planetesimals, asteroids, and comets.