Miracle-dz/UniFAR-FTUs huggingface dataset:
Three-Dimensional Transient Electromagnetic Modeling Using Rational Krylov Methods

A computational method is given for solving the forward modeling problem for transient electromagnetic exploration. Its key features are discretization of the quasi-static Maxwell's equations in space using the first-kind family of curl-conforming Nedelec elements combined with time integration using rational Krylov subspace methods. We show how rational Krylov subspace methods may be used to solve the same problem in the frequency domain followed by a synthesis of the transient solution using the fast Hankel transform, arguing that the pure time-domain is more efficient. We also propose a simple method for selecting the pole parameters of the rational Krylov subspace method which leads to convergence within an a priori determined number of iterations independent of mesh size and conductivity structure. These poles are repeated in a cyclic fashion, which, in combination with direct solvers for the discrete problem, results in significantly faster solution times than previously proposed schemes.
Uniqueness of minimal surfaces whose boundary is a horizontal graph and some Bernstein problems in H 2 × R

We deduce that a connected compact immersed minimal surface in H 2 × R whose boundary has an injective horizontal projection on an admissible convex curve in ∂ ∞ H 2 × R , and satisﬁes an admissible bounded slope condition, is the Morrey’s solution of the Plateau problem and is a horizontal minimal graph. We prove that there is no entire horizontal minimal graph in H 2 × R .
C ∞ Smoothing for Weak Solutions of the Inhomogeneous Landau Equation

We consider the spatially inhomogeneous Landau equation with initial data that is bounded by a Gaussian in the velocity variable. In the case of moderately soft potentials, we show that weak solutions immediately become smooth, and remain smooth as long as the mass, energy, and entropy densities remain under control. For very soft potentials, we obtain the same conclusion with the additional assumption that a sufﬁciently high moment of the solution in the velocity variable remains bounded. Our proof relies on the iteration of local Schauder-type estimates.
Statistics of the cosmic Mach number from numerical simulations of a cold dark matter universe

Results are presented of an analysis of the cosmic Mach number, M, the ratio of the streaming velocity, v, to the random velocity dispersion, sigma, of galaxies in a given patch of the universe, which was performed on the basis of hydrodynamical simulations of the cold dark matter scenario. Galaxy formation is modeled by application of detailed physical processes rather than by the ad hoc assumption of 'bias' between dark matter and galaxy fluctuations. The correlation between M and sigma is found to be very weak for both components. No evidence is found for a physical 'velocity bias' in the quantities which appear in the definition of M. Standard cold-dark-matter-dominated universes are in conflict, at a statistically significant level, with the available observation, in that they predict a Mach number considerably lower than is observed.
Extremal properties associated with univalent subordination chains in C n

For a linear operator A ∈ L ( C n ) , let k + ( A ) be the upper exponential index of A and let m ( A ) = min {(cid:3)(cid:4) A ( z ), z (cid:5) : (cid:6) z (cid:6) = 1 } . Under the assumption k + ( A ) < 2 m ( A ) , we consider the family S 0 A ( B n ) of mappings which have A parametric representation on the Euclidean unit ball B n in C n , i.e. f ∈ S 0 A ( B n ) if and only if there exists an A -normalized univalent subordination chain f ( z , t ) such that f = f ( · , 0 ) and { e − tA f ( · , t ) } t ≥ 0 is a normal family on B n . We prove that if f = f ( · , 0 ) is an extreme point (respectively a support point) of S 0 A ( B n ) , then e − tA f ( · , t ) is an extreme point of S 0 A ( B n ) for t ≥ 0 (respectively a support point of S 0 A ( B n ) for t ≥ 0). These results generalize to higher dimensions related results due to I. Pell and Kirwan. We also deduce an n -dimensional version of an extremal principle due to Kirwan and Schober. In the second part of the paper, we consider extremal problems related to bounded mappings in S 0 A ( B n ) . To this end, we use ideas from control theory to investigate the (normalized) time-log M -reachable family ˜ R log M ( id B n , N A ) of (4.1) generated by the Carathéodory mappings, where M ≥ 1 and k + ( A ) < 2 m ( A ) . We prove that each mapping f in the above reachable family can be imbedded as the ﬁrst element of an A -normalized univalent subordination chain f ( z , t ) such that { e − tA f ( · , t ) } t ≥ 0 is a normal family and f ( · , log M ) = e A log M id B n . We also prove that the family ˜ R log M ( id B n , N A ) is compact and we deduce a density result related to the same family, which involves the subset ex N A of N A consisting of extreme points. These results are generalizations to C n of related results due to Roth. Finally, we are concerned with extreme points and support points associated with compact families generated by extension operators.
Linear-optics quantum Toffoli and Fredkin gates

We design linear optics multiqubit quantum logic gates. We assume the traditional encoding of a qubit onto state of a single photon in two modes (e.g. spatial or polarization). We suggest schemes allowing direct probabilistic realization of the fundamental Toffoli and Fredkin gates without resorting to a sequence of single- and two-qubit gates. This yields more compact schemes and potentially reduces the number of ancilla photons. The proposed setups involve passive linear optics, sources of auxiliary single photons or maximally entangled pairs of photons, and single-photon detectors. In particular, we propose an interferometric implementation of the Toffoli gate in the coincidence basis, which does not require any ancilla photons and is experimentally feasible with current technology.
Masses of Kepler-46b, c from Transit Timing Variations

We use 16 quarters of the Kepler mission data to analyze the transit timing variations (TTVs) of the extrasolar planet Kepler-46b (KOI-872). Our dynamical fits confirm that the TTVs of this planet (period days) are produced by a non-transiting planet Kepler-46c ( days). The Bayesian inference tool MultiNest is used to infer the dynamical parameters of Kepler-46b and Kepler-46c. We find that the two planets have nearly coplanar and circular orbits, with eccentricities somewhat higher than previously estimated. The masses of the two planets are found to be and Jupiter masses, with Mb being determined here from TTVs for the first time. Due to the precession of its orbital plane, Kepler-46c should start transiting its host star a few decades from now.
Electro-optic and electro-absorptive modulations of AlGaAs/GaAs quantum well using surface acoustic wave

The surface acoustic wave produced electron absorptive and electro-optic modulation in AlGaAs/ GaAs quantum well structures are theoretically analyzed. The quantum well structures are optimized by maximizing the optical confinement of the modal field in the active region and the piezoelectric effect of surface acoustic wave on the quantum wells. The effect of penetration depth of the surface acoustic wave on the number ~1‐25 periods! of quantum wells, serving as the active region, is being studied. For 1‐5 period structures, the quantum wells are designed on the top surface so that a strong piezoelectric effect can be obtained. For the 25-period structure, the quantum wells locate at a depth of two-thirds the acoustic-wave wavelength in order to obtain a uniform surface acoustic-wave-induced electric field. The results show that the single and five quantum well devices are suitable for absorptive modulation and optical modulation, respectively, while a general advantage of the 25-period quantum well modulator can shorten the modulation interaction length and increase the modulation bandwidth. The effective index change of these devices are at least ten times larger than the conventional surface acoustic wave devices. These results make the surface acoustic wave quantum well modulators more attractive for the development of acousto-optic device applications. © 1998 American Institute of Physics. @S0021-8979~98! 04202-9#
Superconducting Quantum Refrigerator: Breaking and Rejoining Cooper Pairs with Magnetic Field Cycles

We propose a solid state refrigeration technique based on repeated adiabatic magnetization/demagnetization cycles of a superconductor which acts as the working substance. The gradual cooling down of a substrate (normal metal) in contact with the working substance is demonstrated for different initial temperatures of the substrate. Excess heat is given to a hot large-gap superconductor. The on-chip refrigerator works in a cyclic manner because of an effective thermal switching mechanism: Heat transport between N/N versus N/S junctions is asymmetric because of the appearance of the energy gap. This switch permits selective cooling of the metal. We find that this refrigeration technique can cool down a 0.3cm$^{3}$ block of Cu by almost two orders of magnitude starting from 200mK, and down to about 1mK starting from the base temperature of a dilution fridge (10mK). The corresponding cooling power for a 1cm$\times$1cm interface are 25 nW and 0.06 nW respectively, which scales with the area of the interface.
Superfluid properties of the inner crust of neutron stars

Superfluid properties of the inner crust matter of neutron stars, formed by nuclear clusters immersed in a dilute neutron gas, are analyzed in a self-consistent Hartree-Fock-Bogoliubov approach. The calculations are performed with two pairing forces, fixed so as to obtain in infinite nuclear matter the pairing gaps provided by the Gogny force or by induced interactions. It is shown that the nuclear clusters can either suppress or enhance the pairing correlations inside the inner crust matter, depending on the density of the surrounding neutrons. The profile of the pairing field in the inner crust is rather similar for both pairing forces, but the values of the pairing gaps are drastically reduced for the force which simulates the polarization effects in infinite neutron matter.
PdIn contacts to n-type and p-type GaP

PdIn was used as a contact material to n‐type and p‐type GaP. On n‐type GaP it forms a low resistance ohmic contact upon rapid thermal annealing. PdIn/n‐GaP (S doped at 2–3 ×1018 cm−3) contacts annealed at 600 °C for 1 min had specific contact resistance’s lower than 1×10−4 Ω cm2. Unlike the contacts to n‐GaP, PdIn contacts to p‐GaP (Zn doped 1–2×1018 cm−3) show rectifying behavior at all annealing conditions. However, the effective Schottky barrier height seems to decrease significantly with thermal annealing. In addition to the electrical measurements, glancing angle x‐ray diffraction was used to characterize the contacts. The glancing angle x‐ray diffusion pattern of PdIn/n‐GaP, annealed at 600 °C for 1 min, is consistent with the formation of an (InyGa1−y)P phase due to the thermal annealing. The ohmic behavior of the PdIn contacts to n‐type GaP and the decrease in the contact’s Schottky barrier height on p‐type GaP is attributed to the formation of this (InyGa1−y)P phase at the contact’s interface.
Laboratory–Numerical Model Comparisons of Flow over a Coastal Canyon

Abstract Different modeling approaches are applied to the same geophysical flow in order to assess the ability of laboratory models to provide useful benchmarks in the development of oceanic numerical models. The test case considered here—that of the flow driven by an oscillatory forcing over a submarine canyon—involves background rotation, density stratification, and steep topography. Velocity fields measured by particle-tracking velocimetry and time series of density fluctuations are directly compared to the corresponding outputs from a high-order finite-element numerical ocean model. Quantitative comparison of the laboratory and numerical models shows good overall agreement in the structure and magnitude of the strongest residual currents, which occur at the level of the shelf break in the configuration presented here. The associated residual vorticity field is also structurally consistent between the two models, although the residual divergence is not. Residual currents higher up and lower down in the.
Effects of diametric load on fibre Bragg gratings fabricated in low birefringent fibre

The effect of diametric load on the wavelength of the reflected light from a low-birefringence fibre Bragg grating is studied. The effects of loads up to almost 90 N on a 2.5 cm length of fibre are examined. The experimental results show very good correspondance with the theoretical predictions.
HST F160W Imaging of Very Massive Galaxies at 1.5 < z < 3.0: Diversity of Structures and the Effect of Close Pairs on Number Density Estimates

We present a targeted follow-up Hubble Space Telescope WFC3 F160W imaging study of very massive galaxies ( ) selected from a combination of ground-based near-infrared galaxy surveys (UltraVISTA, NEWFIRM Medium Band Survey-II , UKIRT Infrared Deep Sky Survey (UKIDSS) Ultra-Deep Survey (UDS) at 1.5 < z < 3). We find that these galaxies are diverse in their structures, with ∼1/3 of the targets being composed of close pairs, and span a wide range in sizes. At 1.5 < z < 2.5, the sizes of both star-forming and quiescent galaxies are consistent with the extrapolation of the stellar mass–size relations determined at lower stellar masses. At 2.5 < z < 3.0, however, we find evidence that quiescent galaxies are systematically larger than expected based on the extrapolation of the relation derived using lower stellar mass galaxies. We used the observed light profiles of the blended systems to decompose their stellar masses and investigate the effect of the close pairs on the measured number densities of very massive galaxies in the early universe. We estimate correction factors to account for close-pair blends and apply them to the observed stellar mass functions (SMFs) measured using ground-based surveys. Given the large uncertainties associated with this extreme population of galaxies, there is currently little tension between the (blending-corrected) number density estimates and predictions from theoretical models. Although we currently lack the statistics to robustly correct for close-pair blends, we show that this is a systematic effect that can reduce the observed number density of very massive galaxies by up to a factor of ∼1.5, and should be accounted for in future studies of SMFs.
A four-field gyrofluid model with neoclassical effects for the study of the rotation velocity of magnetic islands in tokamaks

A four-field system of equations which includes the neoclassical flow damping effects and the lowest-order finite-Larmor-radius (FLR) corrections is deduced from a system of gyrofluid equations. The FLR corrections to the poloidal flow damping are calculated by solving a simplified version of the gyrokinetic equation. This system of equations is applied to the study of a chain of freely rotating magnetic islands in a tokamak, resulting from the nonlinear evolution of a resistive tearing mode, to determine the island rotation velocity consistently with the fields' radial profiles close to the resonant surface. The island rotation velocity is determined by imposing the torque balance condition. The equations thus deduced are applied to the study of two different collisionality regimes, namely the weak-damping regime and the intermediate-damping regime. The equations reduce, in the weak-damping regime, to a form already obtained in previous works, while an additional term, containing the lowest order FLR corrections to the poloidal flow damping, appears in the intermediate-damping regime. The numerical integration of the final system of equations allows the determination of the dependence of the island rotation velocity on the plasma collisionality and the island width compared to the ion Larmor radius. The results show that, in the intermediate-damping regime, the island rotation velocity is almost completely determined by the neoclassical effects, with the island width playing a minor role. The parameter η i = L n / L T, where Ln and LT are the density and temperature gradient length scales, plays an important role in determining the island rotation velocity.A four-field system of equations which includes the neoclassical flow damping effects and the lowest-order finite-Larmor-radius (FLR) corrections is deduced from a system of gyrofluid equations. The FLR corrections to the poloidal flow damping are calculated by solving a simplified version of the gyrokinetic equation. This system of equations is applied to the study of a chain of freely rotating magnetic islands in a tokamak, resulting from the nonlinear evolution of a resistive tearing mode, to determine the island rotation velocity consistently with the fields' radial profiles close to the resonant surface. The island rotation velocity is determined by imposing the torque balance condition. The equations thus deduced are applied to the study of two different collisionality regimes, namely the weak-damping regime and the intermediate-damping regime. The equations reduce, in the weak-damping regime, to a form already obtained in previous works, while an additional term, containing the lowest order FLR cor.
The Analysis of Gravitational Lens Surveys. II. Maximum Likelihood Models and Singular Potentials

We do a maximum likelihood analysis of three optical surveys for gravitational lenses. The results are consistent with lensing by normal galaxies modeled as singular isothermal spheres with standard values for observational parameters, aside from the need to add a small amount of ellipticity to produce the observed four image lenses. We tested the model for variations in the number of galaxies, the velocity dispersions of galaxies, the distribution of galaxies, the relation between luminosity and velocity dispersion, the quasar apparent magnitude number counts, and the mean magnification produced by the lenses
Hubble Space Telescope Advanced Camera for Surveys Weak-Lensing and Chandra X-Ray Studies of the High-Redshift Cluster MS 1054–0321

We present Hubble Space Telescope Advanced Camera for Surveys (ACS) weak-lensing and Chandra X-ray analyses of MS 1054-0321 at z = 0.83, the most distant and X-ray-luminous cluster in the Einstein Extended Medium-Sensitivity Survey (EMSS). The high-resolution mass reconstruction through ACS weak lensing reveals the complicated dark matter substructure in unprecedented detail, characterized by the three dominant mass clumps with the four or more minor satellite groups within the current ACS field. The direct comparison of the mass map with the Chandra X-ray image shows that the eastern weak-lensing substructure is not present in the X-ray image and, more interestingly, the two X-ray peaks are displaced away from the hypothesized merging direction with respect to the corresponding central and western mass clumps, possibly because of ram pressure. In addition, as observed in our previous weak-lensing study of another high-redshift cluster CL 0152-1357 at z = 0.84, the two dark matter clumps of MS 1054-0321 seem to be offset from the galaxy counterparts. We examine the significance of these offsets and discuss a possible scenario, wherein the dark matter clumps might be moving ahead of the cluster galaxies. The nonparametric weak-lensing mass modeling gives a projected mass of M(r < 1 Mpc) = (1.02 ± 0.15) × 1015 M☉, where the uncertainty reflects both the statistical error and the cosmic shear effects. Our temperature measurement of T = 8.9 keV utilizing the newest available low-energy quantum efficiency degradation prescription for the Chandra instrument, together with the isothermal β description of the cluster (rc = 16′′ ± 15′′ and β = 0.78 ± 0.08), yields a projected mass of M(r < 1 Mpc) = (1.2 ± 0.2) × 1015 M☉, consistent with the weak-lensing result.
Local bulk operators in AdS/CFT: A holographic description of the black hole interior

To gain insight into how bulk locality emerges from the holographic conformal ﬁeld theory, we reformulate the bulk to boundary map in as local a way as possible. In previous work, we carried out this program for Lorentzian AdS, and showed the support on the boundary could always be reduced to a compact region spacelike separated from the bulk point. In the present work the idea is extended to a complexiﬁed boundary, where spatial coordinates are continued to imaginary values. This continuation enables us to represent a local bulk operator as a CFT operator with support on a ﬁnite disc on the complexiﬁed boundary. We treat general AdS in Poincar´e coordinates and AdS 3 in Rindler coordinates. We represent bulk operators inside the horizon of a BTZ black hole and we verify that the correct bulk two point functions are reproduced, including the divergence when one point hits the BTZ singularity. We comment on the holographic description of black holes formed by collapse and discuss locality and holographic entropy counting at ﬁnite N . After some preliminaries we discuss AdS 3 in accelerating Rindler-like coordinates. We show that our Poincar´e results can be translated into accelerating coordinates
Implications of the Low Binary Black Hole Aligned Spins Observed by LIGO

We explore the implications of the low-spin components along the orbital axis observed in an Advanced LIGO O1 run on binary black hole (BBH) merger scenarios in which the merging BBHs have evolved from field binaries. The coalescence time determines the initial orbital separation of BBHs. This, in turn, determines whether the stars are synchronized before collapse, and hence determines their projected spins. Short coalescence times imply synchronization and large spins. Among known stellar objects, Wolf–Rayet (WR) stars seem to be the only progenitors consistent with the low aligned spins observed in LIGO’s O1, provided that the orbital axis maintains its direction during the collapse. We calculate the spin distribution of BBH mergers in the local universe, and its redshift evolution for WR progenitors. Assuming that the BBH formation rate peaks around a redshift of ∼2–3, we show that BBH mergers in the local universe are dominated by low-spin events. The high-spin population starts to dominate at a redshift of ∼0.5–1.5. WR stars are also progenitors of long gamma-ray bursts that take place at a comparable rate to BBH mergers. We discuss the possible connection between the two phenomena. Additionally, we show that hypothetical Population III star progenitors are also possible. Although WR and Population III progenitors are consistent with the current data, both models predict a non-vanishing fraction of high positive values of the BBHs’ aligned spin. If those are not detected within the coming LIGO/Virgo runs, it will be unlikely that the observed BBHs formed via field binaries.