Miracle-dz/UniFAR-FTUs huggingface dataset:
Simultaneous Chandra, CSO, and VLA Observations of Sgr A*: The Nature of Flaring Activity

Sgr A*, the massive black hole at the center of the Galaxy, varies in radio through X-ray emission on hourly timescales. The flare activity is thought to arise from the innermost region of an accretion flow onto Sgr A*. We present simultaneous light curves of Sgr A* in radio, submillimeter and X-rays that show a possible time delay of 110 ± 17 minutes between X-ray and 850 μm suggesting that the submillimeter flare emission is optically thick. At radio wavelengths, we detect time lags of 20.4 ± 6.8, 30 ± 12, and 20 ± 6 minutes between the flare peaks observed at 13 and 7 mm (22 and 43 GHz) in three different epochs using the VLA. Linear polarization of 1% ± 0.2% and 0.7 ± 0.1% is detected at 7 and 13 mm, respectively, when averaged over the entire observation on 2006 July 17. A simple model of a bubble of synchrotron-emitting electrons cooling via adiabatic expansion can explain the time delay between various wavelengths, the asymmetric shape of the light curves, and the observed polarization of the flare emission at 43 and 22 GHz. The derived physical quantities that characterize the emission give an expansion speed of vexp ∼ 0.003–0.1 c, magnetic field of B ∼ 10–70 G, and particle spectral index p ∼ 1–2. These parameters suggest that the associated plasma cannot escape from Sgr A* unless it has a large bulk motion.
Considerations on the Mechanisms and Transition Temperatures of Superconductors

An overview of the momentum and frequency dependence of effective electron-electron interactions which favor electronic instability to a superconducting state in the angular-momentum channel $\ell$ and the properties of the interactions which determine $T_c$ is provided. Both interactions induced through exchange of phonons as well as purely electronic fluctuations of spin density, charge density or current density are considered. Special attention is paid to the role of quantum critical fluctuations including pairing due to their virtual exchange as well as de-pairing due to inelastic scattering. In light of the above, empirical data and theory specific to phonon induced superconductivity, in cold atoms, superfluidity in liquid $He^3$, superconductivity in some of the heavy fermion compounds, in Cuprates, in pncitides and the valence skipping compound, is reviewed. The physical basis for the following observation is provided: The universal ratio of s-wave $T_c$ to Fermi-energy for fermions at the unitarity limit with attractive interactions is about 0.15, the ratio of the maximum $T_c$ to the typical phonon frequency in phonon induced s-wave superconductivity is of the same order; the ratio of p-wave $T_c$ to the renormalized Fermi-energy in liquid $He^3$, a very strongly correlated Fermi-liquid near its melting pressure, is only $O(10^{-3})$; in the Cuprates and the heavy-fermions where d-wave superconductivity occurs in a region governed by a special class of quantum-critical fluctuations, this ratio rises to $O(10^{-2})$. These discussions also suggest factors important for obtaining higher $T_c$.
Origin and properties of strong inter-nucleon interactions

I start with a historical review of the attempts to construct theories for the origin of nuclear forces, for which I also summaries the most important properties. The review then shifts to its main focus, which is the chiral eective eld theory approach to nuclear forces. I summarize the current status of this approach and discuss the most important open issues: the proper renormalization of the chiral two-nucleon potential and sub-leading three-nucleon forces.
A comparison of gene organisations and phylogenetic relationships of all 22 squamate species listed in South Korea using complete mitochondrial DNA

﻿Abstract Studies using complete mitochondrial genome data have the potential to increase our understanding on gene organisations and evolutionary species relationships. In this study, we compared complete mitochondrial genomes between all 22 squamate species listed in South Korea. In addition, we constructed Maximum Parsimony (MP), Maximum Likelihood (ML) and Bayesian Inference (BI) phylogenetic trees using 13 mitochondrial protein-coding genes. The mitochondrial genes for all six species in the suborder Sauria followed the same organisation as the sequenced Testudines (turtle) outgroup. In contrast, 16 snake species in the suborder Serpentes contained some gene organisational variations. For example, all snake species contained a second control region (CR2), while three species in the family Viperidae had a translocated tRNA-Pro gene region. In addition, the snake species, Elapheschrenckii, carried a tRNA-Pro pseudogene. We were also able to identify a translocation of a tRNA-Asn gene within the five tRNA (WANCY gene region) gene clusters for two true sea snake species in the subfamily Hydrophiinae. Our BI phylogenetic tree was also well fitted against currently known Korean squamate phylogenetic trees, where each family and genus unit forms monophyletic clades and the suborder Sauria is paraphyletic to the suborder Serpentes. Our results may form the basis for future northeast Asian squamate phylogenetic studies.
Analysis of a coupled‐inductor double‐boost dc‐dc converter operating in discontinuous conduction mode

In this article, the steady‐state and dynamical behavior of a coupled‐inductor doble‐boost dc‐dc converter (CBC) operating in discontinuous conduction mode (DCM) is discussed. The CBC makes use of the magnetic coupling between the windings of two boost stages connected in cascade to achieve high voltage gains. Developments given here shown that the voltage stress on semiconductors can be reduced to values lower than the output voltage by selecting the relation between windings adequately. Moreover, the derivation of an averaged model predicts that the converter presents a first‐order dominant response at low frequencies. These properties add to other important CBC advantages such as low component count, high efficiency, and simple implementation and design. The operation in DCM is very attractive for applications where the primary source acts as a current generator, as in the case of photovoltaic panels or constant power loads. Based on the results, the CBC can be seen as an immediate substitute of the classical boost converter when high dc‐dc voltage gains are required. Different tests carried out on an experimental set‐up corroborate the analytical findings.
Updated galactic radio constraints on Dark Matter

We perform a detailed analysis of the synchrotron signals produced by dark matter annihilations and decays. We consider different set-ups for the propagation of electrons and positrons, the galactic magnetic field and dark matter properties. We then confront these signals with radio and microwave maps, including Planck measurements, from a frequency of 22 MHz up to 70 GHz. We derive two sets of constraints: conservative and progressive, the latter based on a modeling of the astrophysical emission. Radio and microwave constraints are complementary to those obtained with other indirect detection methods, especially for dark matter annihilating into leptonic channels.
Remark on the Novikov conjecture and the homotopy invariance of the Hirzebruch L-class

We use K-area homology to summarize some results about the Novikov conjecture and the Hirzebruch L-class. In fact, we provide necessary and sufficient conditions for closed manifolds to have a homotopy invariant L-class. In order to obtain additional properties we also introduce the cohomology of infinite K--area which preserves the cup product of singular cohomology.
Modeling electrostatic patch effects in Casimir force measurements

Electrostatic patch potentials give rise to forces between neutral conductors at distances in the micrometer range and must be accounted for in the analysis of Casimir force experiments. In this paper we develop a quasilocal model for describing random potentials on metallic surfaces. In contrast to some previously published results, we find that patches may provide a significant contribution to the measured signal and thus may be a more important systematic effect than was previously anticipated. Additionally, patches may render the experimental data at distances below 1 $\ensuremath{\mu}$m compatible with theoretical predictions based on the Drude model.
PROTOPLANETARY AND TRANSITIONAL DISKS IN THE OPEN STELLAR CLUSTER IC 2395

We present new deep UBVRI images and high-resolution multi-object optical spectroscopy of the young (∼6–10 Myr old), relatively nearby (800 pc) open cluster IC 2395. We identify nearly 300 cluster members and use the photometry to estimate their spectral types, which extend from early B to middle M. We also present an infrared imaging survey of the central region using the IRAC and MIPS instruments on board the Spitzer Space Telescope, covering the wavelength range from 3.6 to 24 μm. Our infrared observations allow us to detect dust in circumstellar disks originating over a typical range of radii from ∼0.1 to ∼10 au from the central star. We identify 18 Class II, 8 transitional disk, and 23 debris disk candidates, respectively, 6.5%, 2.9%, and 8.3% of the cluster members with appropriate data. We apply the same criteria for transitional disk identification to 19 other stellar clusters and associations spanning ages from ∼1 to ∼18 Myr. We find that the number of disks in the transitional phase as a fraction of the total with strong 24 μm excesses ([8] – [24] ≥ 1.5) increases from (8.4 ± 1.3)% at ∼3 Myr to (46 ± 5)% at ∼10 Myr. Alternative definitions of transitional disks will yield different percentages but should show the same trend.
A CATALOG OF 132,684 CLUSTERS OF GALAXIES IDENTIFIED FROM SLOAN DIGITAL SKY SURVEY III

Using the photometric redshifts of galaxies from the Sloan Digital Sky Survey III (SDSS-III), we identify 132,684 clusters in the redshift range of 0.05 ⩽ z < 0.8. Monte Carlo simulations show that the false detection rate is less than 6% for the whole sample. The completeness is more than 95% for clusters with a mass of M200 > 1.0 × 1014 M☉ in the redshift range of 0.05 ⩽ z < 0.42, while clusters of z > 0.42 are less complete and have a biased smaller richness than the real one due to incompleteness of member galaxies. We compare our sample with other cluster samples, and find that more than 90% of previously known rich clusters of 0.05 ⩽ z < 0.42 are matched with clusters in our sample. Richer clusters tend to have more luminous brightest cluster galaxies (BCGs). Correlating with X-ray and the Planck data, we show that the cluster richness is closely related to the X-ray luminosity, temperature, and Sunyaev–Zel'dovich measurements. Comparison of the BCGs with the SDSS luminous red galaxy (LRG) sample shows that 25% of LRGs are BCGs of our clusters and 36% of LRGs are cluster member galaxies. In our cluster sample, 63% of BCGs of rpetro < 19.5 satisfy the SDSS LRG selection criteria.
Application of theory to literary tourism: a comparison of parasocial interaction theory and co-creation theory

ABSTRACT During the COVID-19 quarantine, reading increased worldwide and with it the demand for literary tourism. While previous research has examined the motivations for literary tourists, no generalizable theory has emerged. After analyzing the previous work on literary tourism, this study compared the applicability of parasocial interaction theory and co-creation theory for literary tourists. This study conducted four surveys of both literary society members and the general public. Most of the antecedents of co-creation theory were significant for literary tourists while two of the antecedents of parasocial interaction theory were applicable for the public, although the overall model was supported. For researchers, this is one of the first papers to apply social science theories to literary tourism. For literary destinations, partnering with literary societies can attract guests who want to help create the experience for themselves and other society members.
The Enigmatic Spin Evolution of PSR J0537–6910: r-modes, Gravitational Waves, and the Case for Continued Timing

We discuss the unique spin evolution of the young X-ray pulsar PSR J0537–6910, a system in which the regular spin down is interrupted by glitches every few months. Drawing on the complete timing data from the Rossi X-ray Timing Explorer (from 1999 to 2011), we argue that a trend in the interglitch behavior points to an effective braking index close to n = 7, which is much larger than expected. This value is interesting because it would accord with the neutron star spinning down due to gravitational waves from an unstable r-mode. We discuss to what extent this, admittedly speculative, scenario may be consistent and if the associated gravitational-wave signal would be within reach of ground-based detectors. Our estimates suggest that one may, indeed, be able to use future observations to test the idea. Further precision timing would help to enhance the achievable sensitivity, and we advocate a joint observing campaign between the Neutron Star Interior Composition Explorer and the LIGO-Virgo network.
Green's functions and non-singlet glueballs on deformed conifolds

We study the Laplacian on Stenzel spaces (generalized deformed conifolds), which are tangent bundles of spheres endowed with Ricci flat metrics. The (2d − 2)-dimensional Stenzel space has SO(d) symmetry and can be embedded in through the equation ∑di = 1zi2 = ϵ2. We discuss Green's function with a source at a point on the Sd − 1 zero section of TSd − 1. Its calculation is complicated by mixing between different harmonics with the same SO(d) quantum numbers due to the explicit breaking by the ϵ-deformation of the U(1) symmetry that rotates zi by a phase. A similar mixing affects the spectrum of normal modes of warped deformed conifolds that appear in gauge/gravity duality. We solve the mixing problem numerically to determine certain bound state spectra in various representations of SO(d) for the d = 4 and d = 5 examples.
Luttinger-field approach to thermoelectric transport in nanoscale conductors

Thermoelectric transport in nanoscale conductors is analyzed in terms of the response of the system to a thermo-mechanical field, first introduced by Luttinger, which couples to the electronic energy density. While in this approach the temperature remains spatially uniform, we show that a spatially varying thermo-mechanical field effectively simulates a temperature gradient across the system and allows us to calculate the electric and thermal currents that flow due to the thermo-mechanical field. In particular, we show that, in the long-time limit, the currents thus calculated reduce to those that one obtains from the Landauer-B\"uttiker formula, suitably generalized to allow for different temperatures in the reservoirs, if the thermo-mechanical field is applied to prepare the system, and subsequently turned off at ${t=0}$. Alternatively, we can drive the system out of equilibrium by switching the thermo-mechanical field after the initial preparation. We compare these two scenarios, employing a model noninteracting Hamiltonian, in the linear regime, in which they coincide, and in the nonlinear regime in which they show marked differences. We also show how an operationally defined local effective temperature can be computed within this formalism.
Magnetically controlled mass-loss from extrasolar planets in close orbits

We consider the role magnetic fields play in guiding and controlling mass-loss via evaporative outflows from exoplanets that experience UV irradiation. First we present analytic results that account for planetary and stellar magnetic fields, along with mass-loss from both the star and planet. We then conduct series of numerical simulations for gas giant planets, and vary the planetary field strength, background stellar field strength, UV heating flux, and planet mass. These simulations show that the flow is magnetically controlled for moderate field strengths and even the highest UV fluxes, i.e., planetary surface fields $B_P\gtrsim 0.3$ gauss and fluxes $F_{UV}\sim10^{6}$ erg s$^{-1}$. We thus conclude that outflows from all hot Jupiters with moderate surface fields are magnetically controlled. The inclusion of magnetic fields highly suppresses outflow from the night-side of the planet. Only the magnetic field lines near the pole are open and allow outflow to occur. The fraction of open field lines depends sensitively on the strength (and geometry) of the background magnetic field from the star, along with the UV heating rate. The net effect of the magnetic field is to suppress the mass loss rate by (approximately) an order of magnitude. Finally, some open field lines do not allow the flow to pass smoothly through the sonic point; flow along these streamlines does not reach steady-state, resulting in time-variable mass-loss.
A COMPARATIVE ANALYSIS OF ECOLOGICAL FOOTPRINT OF RURAL-URBAN HOUSEHOLDS IN DISTRICT SWAT

Ecological footprint (EF) measure how much productive land area is required for producing the products and resources consumed and the waste generated by humans. The problem of ecological overshooting is being faced by many developing countries like Pakistan. According to the Global Footprint Network, Pakistan is one of the ecologically in deficit countries list i.e we are consuming more than the available biocapacity with us. The ecological footprint of Pakistan in 2012 was 0.8 Gha per capita and biocapacity 0.4 Gha per capita. This is high time to think that whether we are living within our ecological limits and how fast humans are depleting the earth’s biosphere. With this background, the present study aims to estimate the ecological footprints at households’ level taking into account the food, housing, transportation, consumer goods and services in district Swat. Besides, the drivers of the ecological footprint and their impact on the ecological footprint was also estimated. This study used primary data which was collected through questionnaire designed by the Stockholm Environment Institute (SEI). To support the analysis, additional information has also been collected through the self-designed questionnaire. The information obtained were converted into EF though calculator of SEI. The analysis was extended to rural and urban areas of district Swat. The study used a sample of 1063 households from 7 tehsils of district Swat. The sample size was proportionally allocated to rural and urban areas of the each tehsil. Accordingly, 744 and 319 households were selected from rural and urban areas respectively. The descriptive statistics alongwith regression model was used for the analysis. The findings revealed that carbon footprint is the major contributor to total EF. The rural households have higher EF than urban households. However, the ecological overshooting is observed in both rural and urban areas. The major influencing factors of the EF in district Swat are income, household size, education, location, (rural or urban), type of food used, fuel consumption, renewable sources of energy, solid waste, home type and size. Based on findings, it is recommended that the households should be encouraged to use renewable sources of energy in homes to reduce their EF. Particularly, the use of solar energy in the large houses should be ensured. The resources use needs to be monitored to reduce ecological overshooting. The waste generated needs to be properly recycled. The increasing carbon footprint should be controlled through sustainable practices in vehicles use and electric appliances at home. The households should be given environmental awareness and education through various means to reduce EF. Keywords:Ecological footprint
Collisionless magnetic reconnection in a plasmoid chain

Abstract. The kinetic features of plasmoid chain formation and evolution are investigated by two dimensional Particle-in-Cell simulations. Magnetic reconnection is initiated in multiple X points by the tearing instability. Plasmoids form and grow in size by continuously coalescing. Each chain plasmoid exhibits a strong out-of plane core magnetic field and an out-of-plane electron current that drives the coalescing process. The disappearance of the X points in the coalescence process are due to anti-reconnection, a magnetic reconnection where the plasma inflow and outflow are reversed with respect to the original reconnection flow pattern. Anti-reconnection is characterized by the Hall magnetic field quadrupole signature. Two new kinetic features, not reported by previous studies of plasmoid chain evolution, are here revealed. First, intense electric fields develop in-plane normally to the separatrices and drive the ion dynamics in the plasmoids. Second, several bipolar electric field structures are localized in proximity of the plasmoid chain. The analysis of the electron distribution function and phase space reveals the presence of counter-streaming electron beams, unstable to the two stream instability, and phase space electron holes along the reconnection separatrices.
NUMERICAL MODELING OF THE 2009 IMPACT EVENT ON JUPITER

We have investigated the 2009 July impact event on Jupiter using the ZEUS-MP 2 three-dimensional hydrodynamics code. We studied the impact itself and the following plume development. Eight impactors were considered: 0.5 km and 1 km porous (ρ = 1.760 g cm−3) and non-porous (ρ = 2.700 g cm−3) basalt impactors, and 0.5 km and 1 km porous (ρ = 0.600 g cm−3) and non-porous (ρ = 0.917 g cm−3) ice impactors. The simulations consisted of these bolides colliding with Jupiter at an incident angle of θ = 69° from the vertical and with an impact velocity of v = 61.4 km s−1. Our simulations show the development of relatively larger, faster plumes created after impacts involving 1 km diameter bodies. Comparing simulations of the 2009 event with simulations of the Shoemaker-Levy 9 (SL9) events reveals a difference in plume development, with the higher incident angle of the 2009 impact leading to a shallower terminal depth and a smaller and slower plume. We also studied the amount of dynamical chaos present in the simulations conducted at the 2009 incident angle. Compared to the chaos of the SL9 simulations, where θ ≈ 45°, we find no significant difference in chaos at the higher 2009 incident angle.
Arterial Stiffness following Endurance and Resistance Exercise Sessions in Older Patients with Coronary Artery Disease

Arterial stiffness (AS) is associated with coronary artery disease (CAD). Acute endurance training decreases AS, whereas acute resistance training increases it. However, these results are from studies in apparently healthy adults, and there is no information on the effects of such afterload AS in elderly patients with CAD. We aimed to investigate the effect of acute endurance or resistance training on the time course of changes in the indices of AS in elderly patients with CAD in order to understand how stiffness responds after training. We tested 18 trained men with CAD. AS was measured using central and peripheral pulse wave velocity (PWV) after 15 min of rest and after 5, 15, and 30 min of endurance and resistance training sessions. The endurance session consisted of high-intensity interval walking at 85–90% of maximum heart rate, and the resistance session consisted of 70% of the maximum of one repetition. An interaction effect was found for central and peripheral PWV (p ≤ 0.001; carotid, η2 = 0.72; aortic, η2 = 0.90; femoral, η2 = 0.74), which was due to an increase in PWV after resistance and a decrease in central and peripheral PWV after endurance. This study demonstrates that training mode influences the time course of AS responses to acute exercise in these patients. Acute endurance training decreased AS, whereas resistance training significantly increased it.