Miracle-dz/UniFAR-FTUs huggingface dataset:
Comparison of Material Removal Rate of Aluminium Alloy AA6082 Using Novel AlTiN Coated Tool with Uncoated Carbide Tool while CNC Turning

Aim: This research study is about comparison of Material Removal Rate of aluminium alloy AA6082 while CNC turning using AlTiN (Aluminium Titanium Nitrate) novel tool coating and using Uncoated carbide tool. Materials and Methods: Workpiece materials used in this study for Turning operation is Aluminium alloy AA6082. Tools used are AlTiN coated tool and uncoated Carbide tool. There are two groups i.e, control group and experimental group, each group contains 20 workpieces and total workpieces are 40. The pre-test power for testing was 80%, Alpha=0.05% and CL was 95%, G power test was used to fix the number of samples for each group. Results: The level of cutting parameters and the resulting Material Removal Rate values are obtained for all machined workpieces with both Uncoated carbide tool and AlTiN coated tool and the results done by Turning operation. The mean Material Removal rate values using Uncoated Carbide tool is 0.16110g/s and AlTiN coated tool is 0.19745g/s and corresponding standard deviation values are 0.021472 and 0.039752 respectively. These values were obtained with a significance level of p=0.047 (p<0.05). Using AlTiN coated tool gives a higher Material Removal Rate than Uncoated carbide tool in CNC machining. Conclusion: Within the limitations of this study, by the observation of results obtained it could be concluded that the material removal rate of Aluminium Alloy AA6082 using AlTiN coated tool is more than Uncoated carbide tool.
Exploring School Principals’ Experiences During the First Four Months of the Pandemic as a Way to Reimagine Inclusive Education

This study involved interviewing Canadian principals (N = 37) to determine how they responded to students with special education needs during the COVID-19 pandemic. Yamamoto et al.’s (2014) concept of critical incidents and Heine et al.’s (2006) meaning maintenance model were used to evaluate the transformational power of principals’ pandemic experiences in order to reimagine inclusive education. Findings revealed that these critical incidents broadly fell into four categories: 1) family support and the complications associated with partnering with parents virtually, 2) meeting students’ needs in new and often innovative ways, 3) disparities in student experiences as a result of virtual schooling and 4) responses required in light of logistical and technical challenges.
Highly Ionized Gas as a Diagnostic of the Inner NLR

Abstract The spectra of AGN, from the ultraviolet to the near infrared, exhibit emission lines covering a wide range of ionization states, from neutral species such as [O i] λ 6300, up to [Fe iv] λ 5303. Here we report on some recent studies of the properties of highly ionized lines (HILs), plus two case studies of individual objects. Future IFU observations at high spatial and good spectral resolution will probe the excitation and kinematics of the gas in the zone between the extended NLR and unresolved BLR. Multi-component SED fitting can be used to link the source of photoionization with the strengths and ratios of the HILs.
Recurrent Cosmic Ray Modulations at Solar Minimum and Solar Maximum Over Three Solar Cycles

Cosmic ray modulations associated with coro- tating high-speed streams from coronal holes, though most prominent around and preceding solar minimum, are present throughout the solar cycle. We illustrate examples from the current solar maximum which arise in near-equatorial coro- nal holes and show that the relationship between streams and the associated cosmic ray modulations is similar to that pre- viously found for streams at solar minimum.
IGR J17354−3255 as a candidate intermediate supergiant fast X-ray transient possibly associated with the transient MeV AGL J1734−3310

We present spectral and temporal results from INTEGRAL long-term monitoring of the unidentified X-ray source IGR J17354−3255. We show that it is a weak persistent hard X-ray source spending a major fraction of the time in an out-of-outburst state with an average of 18–60 keV X-ray flux of ∼1.1 milliCrab, occasionally interspersed with fast X-ray flares (duration from a few hours to a few days) with a dynamic range as high as ∼200. From archival Swift/X-ray telescope observations, we also show that the dynamic range from non-detection to highest level of measured X-ray activity is >300. Our imager on board the lntegral satellite (IBIS) timing analysis strongly confirms the ∼8.4 d orbital period previously detected with Swift/burst alert telescope (BAT); in addition we show that the shape of the orbital profile is rather smooth and appears to be dominated by low-level X-ray emission rather than by bright outbursts; the measured degree of outburst recurrence is ∼25 per cent. The spectral and temporal characteristics of IGR J17354−3255 are highly indicative of a supergiant high-mass X-ray binary (SGXB) nature. However, our inferred dynamic ranges in both soft and hard X-rays are significantly greater than those of classical SGXB systems, but instead are typical of intermediate supergiant fast X-ray transients (SFXTs). Finally, we note for the first time that the observed fast flaring X-ray behaviour of IGR J17354−3255 is very similar to that detected with AGILE from the spatially associated MeV source AGL J1734−3310, suggesting a possible physical link between the two objects.
Loop Dynamics Analysis of PAM-4 Mueller–Muller Clock and Data Recovery System

This paper provides a framework for analyzing the loop dynamics of the clock and data recovery (CDR) system of ADC-based PAM-4 receivers, which will assist in extending the timing recovery loop bandwidth. This paper formulates an accurate linear model of linear and signed Mueller–Muller phase detector for baud-rate clock recovery. Different equalization configurations of continuous-time linear equalizer (CTLE) and feed-forward equalizer (FFE) are evaluated from a phase detector performance perspective to enable high CDR loop bandwidth. The impact of loop latency on the timing recovery of ADC-based PAM-4 receivers is also analyzed and demonstrated using accurate behavioral simulations. The analysis and behavioral results show that, to achieve high CDR loop bandwidth with a good jitter tolerance, the phase detector gain to noise ratio should be maximized, and CDR loop latency should be minimized.
Algorithmic quantum simulation of memory effects

We propose a method for the algorithmic quantum simulation of memory effects described by integro-differential evolution equations. It consists in the systematic use of perturbation theory techniques and a Markovian quantum simulator. Our method aims to efficiently simulate both completely positive and non-positive dynamics without the requirement of engineering non-Markovian environments. Finally, we find that small error bounds can be reached with polynomially scaling resources, evaluated as the number of performed measurements.
Permalloy-based carbon nanotube spin-valve

In this paper we demonstrate that permalloy (Py), a widely used Ni/Fe alloy, forms contacts to carbon nanotubes (CNTs) that meet the requirements for the injection and detection of spin-polarized currents in carbon-based spintronic devices. We establish the material quality and magnetization properties of Py strips in the shape of suitable electrical contacts and find a sharp magnetization switching tunable by geometry in the anisotropic magnetoresistance (AMR) of a single strip at cryogenic temperatures. In addition, we show that Py contacts couple strongly to CNTs, comparable to Pd contacts, thereby forming CNT quantum dots at low temperatures. These results form the basis for a Py-based CNT spin-valve exhibiting very sharp resistance switchings in the tunneling magnetoresistance, which directly correspond to the magnetization reversals in the individual contacts observed in AMR experiments.
Accretion discs with an inner spiral density wave

In a recent work by the first author, we show that accretion discs in binary systems could retrogradely precess by the same physics that causes the Earth to retrogradely precess [i.e. tidal torques by the Moon and the Sun (or a secondary star) on a tilted, spinning, non-spherical Earth (or e.g. a primary star surrounded by an accretion disc)]. In addition, we show that the state of matter and the geometrical shape of the celestial object could significantly affect the precessional value. For example, a cataclysmic variable (CV) dwarf novae (DN) non-magnetic system that shows negative superhumps in its light curve can be described by a retrogradely precessing, differentially rotating, tilted disc. Because the disc is a fluid and because the gas stream overflows the tilted disc and particles can migrate into inner disc annuli, coupled to the disc could be a retrogradely precessing inner ring that is located near the innermost annuli of the disc. However, numerical simulations by Bisikalo et al. and this work show that an inner spiral density wave can be generated instead of an inner ring. Therefore, we show that retrograde precession in non-magnetic, spinning, tilted CV DN systems can equally be described by a retrogradely precessing and differentially rotating disc with an attached retrogradely precessing inner spiral density wave so long as the wave appears at the same radius as the ring and within the plane of the tilted disc. We find that the theoretical results generated in this work agree well with the theoretical results presented in Montgomery and thus with the numerical simulations and select CV DN systems in Montgomery that may have a main-sequence secondary. Therefore, pressure effects do need to be considered in CV DN systems that exhibit negative superhumps if the accretion discs are tilted and have an inner spiral density wave that is in the plane of the disc.
Measurement of branching fractions, isospin asymmetries and angular observables in exclusive electroweak penguin decays

This thesis describes measurements of rare electroweak penguin decays performed with data collected by the Large Hadron Collider beauty experiment corresponding to 3 fb 1 of integrated luminosity. The purpose of these measurements is to search for physics beyond the theoretical framework known as the Standard Model (SM). Electroweak penguin decays are sensitive to virtual particles in extensions to the SM whose influence on the decay amplitude can be of similar strength to the SM contribution. The particular measurements that are described in this thesis are the di↵erential branching fractions and isospin asymmetries of B ! K(⇤)μ+μ decays as well as the angular observables in B! Kμμ decays. Although results are consistent with the SM, all the branching fractions of B! K(⇤)μ+μ decays tend to favour a lower value than theoretical predictions.
Far-infrared spectroscopy in ordered and disordered BaMg1/3Nb2/3O3 microwave ceramics

Ba(Mg1/3Nb2/3)O3 ceramics with suitable microwave dielectric properties for application in wireless communications and information access technologies were studied by far-infrared spectroscopy. Samples with different B-site ordering degrees, obtained by hydrothermal synthesis followed by sintering at various temperatures, were employed in this investigation. The sixteen infrared modes predicted by factor-group analysis were observed and adjusted according to a four-parameter semiquantum model. The dispersion parameters were determined in order to calculate the real part of the dielectric permittivity and the quality factors associated with the dielectric losses in the microwave region. The materials exhibited increasing e0 and Q values up to 1100 °C, increasing more substantially when the temperature attained 1300 °C. The B-site ordering played an important role on this behavior along with the microstructural evolution above 1100 °C (grain growth), which also increased the phonon lifetime and contributed to the Q improvement. Kramers–Kronig analyses were carried out in all experimental data and the contributions of the main optical polar modes to the dielectric and microwave properties were carefully analyzed in order to identify and attribute the Ba–BO3 external mode, the inner modes related to the O–Mg–O and O–Nb–O bending vibrations, and the stretching modes of each MgO6 and NbO6 octahedron.Ba(Mg1/3Nb2/3)O3 ceramics with suitable microwave dielectric properties for application in wireless communications and information access technologies were studied by far-infrared spectroscopy. Samples with different B-site ordering degrees, obtained by hydrothermal synthesis followed by sintering at various temperatures, were employed in this investigation. The sixteen infrared modes predicted by factor-group analysis were observed and adjusted according to a four-parameter semiquantum model. The dispersion parameters were determined in order to calculate the real part of the dielectric permittivity and the quality factors associated with the dielectric losses in the microwave region. The materials exhibited increasing e0 and Q values up to 1100 °C, increasing more substantially when the temperature attained 1300 °C. The B-site ordering played an important role on this behavior along with the microstructural evolution above 1100 °C (grain growth), which also increased the phonon lifetime and contributed .
An advanced design for the Gamma-RAy Polarimeter Experiment (GRAPE)

Understanding the underlying physics governing astrophysical jets associated with Gamma-Ray Bursts (GRBs) is necessary to advance the field of gamma-ray astronomy. Existing physics models can be constrained through GRB polarization studies. The Gamma-Ray Polarimeter Experiment (GRAPE) is a high-altitude balloon experiment designed to measure GRB polarization over the energy range of 50-500 keV at flight altitudes. A flight of the newest GRAPE design is scheduled to fly from Fort Sumner, NM in August 2023. The new design is based on an arrangement of small scintillation detector elements designed to measure photon interactions in three dimensions and provide modest imaging capabilities. The flight instrument consists of a 3-dimensional (7x7x5) array of high-Z (GAGG) and low-Z (P-terphenyl) scintillators each read out by individual Hamamtsu MultiPixel Photon Counters (MPPCs). Previous GRAPE missions have been sensitive to M-class solar flares and observations of the Crab Nebula with low signal to background ratios. The new design improves performance relative to the previous GRAPE design through the use of advanced scintillator materials, the ability to perform modest Compton imaging for source localization and background rejection, and by completely eliminating optical cross-talk. Background reduction is achieved using the imaging capabilities allowing for some level of event rejection for events inconsistent with the source direction. This paper will present the new module design and simulated response parameters to provide an estimate of the balloon payload sensitivity.
Orbiting phenomena in black hole scattering

Rainbow, glory and orbiting scattering are usually described by the properties of the classical deflection function related to the real part of the quantum mechanical scattering phase shift or by the diffractive pattern of the quantum mechanical cross sections. Here we show that the case of orbiting scattering of massless spin 0, 1 and 2 particles from Schwarzschild black holes can be characterized by a sudden rise in $|{R}_{l}{|}^{2}$ at a critical angular momentum ${l}_{C}$, which we show corresponds to the unstable circular orbits of these particles. For the cases $s=0$, 2, we attempt a new interpretation of the Regge-Wheeler potential by identifying the quantum mechanical corrections to the effective potential of massless particles. We probe into the black hole scattering by using numerical and semi-analytical methods which give very good agreements with the exact numerical results. The limitations of previously used approximations as compared to the exact and semi-analytical results are discussed.
STATISTICAL MECHANICS OF COLLISIONLESS ORBITS. IV. DISTRIBUTION OF ANGULAR MOMENTUM

It has been shown in previous work that DARKexp, which is a theoretically derived, maximum entropy, one shape parameter model for isotropic collisionless systems, provides very good fits to simulated and observed dark matter halos. Specifically, it fits the energy distribution, N(E), and the density profiles, including the central cusp. Here, we extend DARKexp N(E) to include the distribution in angular momentum, L2, for spherically symmetric systems. First, we argue, based on theoretical, semi-analytical, and simulation results, that while dark matter halos are relaxed in energy, they are not nearly as relaxed in angular momentum, which precludes using maximum entropy to uniquely derive N(E, L2). Instead, we require that when integrating N(E, L2) over squared angular momenta one retrieves the DARKexp N(E). Starting with a general expression for N(E, L2) we show how the distribution of particles in L2 is related to the shape of the velocity distribution function, VDF, and velocity anisotropy profile, β(r). We then demonstrate that astrophysically realistic halos, as judged by the VDF shape and β(r), must have linear or convex distributions in L2, for each separate energy bin. The distribution in energy of the most bound particles must be nearly flat, and become more tilted in favor of radial orbits for less bound particles. These results are consistent with numerical simulations and represent an important step toward deriving the full distribution function for spherically symmetric dark matter halos.
Generalized Least Squares for Trend Estimation of Summarized Dose–response Data

This paper presents a command, glst, for trend estimation across different exposure levels for either single or multiple summarized case–control, incidence-rate, and cumulative incidence data. This approach is based on constructing an approximate covariance estimate for the log relative risks and estimating a corrected linear trend using generalized least squares. For trend analysis of multiple studies, glst can estimate fixed- and random-effects metaregression models.
On the initial mass function and tilt of the fundamental plane of massive early-type galaxies

We investigate the most plausible stellar initial mass function (IMF) and the main origin of the tilt of the fundamental plane (FP) for old, massive early-type galaxies. We consider a sample of 13 bright galaxies of the Coma cluster and combine our results with those obtained from a sample of 57 lens galaxies in the same luminous mass range. We estimate the luminous mass and stellar mass-to-light ratio values of the sample galaxies by fitting their Sloan Digital Sky Survey multiband photometry with composite stellar population models computed with different dust-free, solar-metallicity templates and IMFs. We compare these measurements and those derived from two-component orbit-based dynamical modelling. The photometric and dynamical luminous mass estimates of the galaxies in our sample are consistent, within the errors, if a Salpeter IMF is adopted. On the contrary, with a Kroupa or Chabrier IMF the two luminous mass diagnostics differ at a more than 4σ level. For the massive Coma galaxies, their stellar mass-to-light ratio scales with luminous mass as the corresponding effective quantities are observed to scale on the FP. This indicates that the tilt of the FP is primarily caused by stellar population properties. We conclude that old, massive lens and non-lens early-type galaxies obey the same luminous and dynamical scaling relations, favour a Salpeter IMF, and suggest a stellar population origin for the tilt of the FP. The validity of these results for samples of early-type galaxies with different age and mass properties still remains to be tested.
THE OBSERVED PROPERTIES OF DWARF GALAXIES IN AND AROUND THE LOCAL GROUP

Positional, structural, and dynamical parameters for all dwarf galaxies in and around the Local Group are presented, and various aspects of our observational understanding of this volume-limited sample are discussed. Over 100 nearby galaxies that have distance estimates reliably placing them within 3 Mpc of the Sun are identified. This distance threshold samples dwarfs in a large range of environments, from the satellite systems of the MW and M31, to the quasi-isolated dwarfs in the outer regions of the Local Group, to the numerous isolated galaxies that are found in its surroundings. It extends to, but does not include, the galaxies associated with the next nearest groups, such as Maffei, Sculptor, and IC 342. Our basic knowledge of this important galactic subset and their resolved stellar populations will continue to improve dramatically over the coming years with existing and future observational capabilities, and they will continue to provide the most detailed information available on numerous aspects of dwarf galaxy formation and evolution. Basic observational parameters, such as distances, velocities, magnitudes, mean metallicities, as well as structural and dynamical characteristics, are collated, homogenized (as far as possible), and presented in tables that will be continually updated to provide a convenient and current online resource. As well as discussing the provenance of the tabulated values and possible uncertainties affecting their usage, the membership and spatial extent of the MW sub-group, M31 sub-group, and the Local Group are explored. The morphological diversity of the entire sample and notable sub-groups is discussed, and timescales are derived for the Local Group members in the context of their orbital/interaction histories. The scaling relations and mean stellar metallicity trends defined by the dwarfs are presented, and the origin of a possible “floor” in central surface brightness (and, more speculatively, stellar mean metallicity) at faint magnitudes is considered.
A NEW MULTI-DIMENSIONAL GENERAL RELATIVISTIC NEUTRINO HYDRODYNAMICS CODE FOR CORE-COLLAPSE SUPERNOVAE. II. RELATIVISTIC EXPLOSION MODELS OF CORE-COLLAPSE SUPERNOVAE

We present the first two-dimensional general relativistic (GR) simulations of stellar core collapse and explosion with the CoCoNuT hydrodynamics code in combination with the Vertex solver for energy-dependent, three-flavor neutrino transport, using the extended conformal flatness condition for approximating the space–time metric and a ray-by-ray-plus ansatz to tackle the multi-dimensionality of the transport. For both of the investigated 11.2 and 15 M☉ progenitors we obtain successful, though seemingly marginal, neutrino-driven supernova explosions. This outcome and the time evolution of the models basically agree with results previously obtained with the Prometheus hydro solver including an approximative treatment of relativistic effects by a modified Newtonian potential. However, GR models exhibit subtle differences in the neutrinospheric conditions compared with Newtonian and pseudo-Newtonian simulations. These differences lead to significantly higher luminosities and mean energies of the radiated electron neutrinos and antineutrinos and therefore to larger energy-deposition rates and heating efficiencies in the gain layer with favorable consequences for strong nonradial mass motions and ultimately for an explosion. Moreover, energy transfer to the stellar medium around the neutrinospheres through nucleon recoil in scattering reactions of heavy-lepton neutrinos also enhances the mentioned effects. Together with previous pseudo-Newtonian models, the presented relativistic calculations suggest that the treatment of gravity and energy-exchanging neutrino interactions can make differences of even 50%–100% in some quantities and is likely to contribute to a finally successful explosion mechanism on no minor level than hydrodynamical differences between different dimensions.