Miracle-dz/UniFAR-FTUs huggingface dataset:
The accretion regimes of a highly magnetized NS: the unique case of NuSTAR J095551+6940.8

We analyze archival Chandra HRC observations of the ultra luminous accreting pulsar M82-X2 (NuSTAR J095551+6940.8), and determine an upper limit of $ r_{co}, and the source luminosity is expected to drop by a large factor. We conclude that a magnetically threaded, radiation pressure-dominated disk, around a highly magnetized NS (B~10^{13} G) offers the best intepretation for all the currently observed properties of NuSTAR J095551+6940.8. This source offers an unprecedented opportunity to study the disk-magnetosphere interaction in a new regime of supercritical accretion, and across the transition between-radiation pressure and gas-pressure dominance inside the disk.
Spin ordering and electronic texture in the bilayer iridate Sr3Ir2O7

Through a neutron scattering, charge transport, and magnetization study, the correlated ground state in the bilayer iridium oxide Sr$_3$Ir$_2$O$_7$ is explored. Our combined results resolve scattering consistent with a high temperature magnetic phase that persists above 600 K, reorients at the previously defined $T_{AF}=280$ K, and coexists with an electronic ground state whose phase behavior suggests the formation of a fluctuating charge or orbital phase that freezes below $T^{*}\approx70$ K. Our study provides a window into the emergence of multiple electronic order parameters near the boundary of the metal to insulator phase transition of the 5d $J_{eff}=1/2$ Mott phase.
Muscle glycogen unavailability and fat oxidation rate during exercise: Insights from McArdle disease

Carbohydrate availability affects fat metabolism during exercise; however, the effects of complete muscle glycogen unavailability on maximal fat oxidation (MFO) rate remain unknown. Our purpose was to examine the MFO rate in patients with McArdle disease, comprising an inherited condition caused by complete blockade of muscle glycogen metabolism, compared to healthy controls. Nine patients (three women, aged 36 ± 12 years) and 12 healthy controls (four women, aged 40 ± 13 years) were studied. Several molecular markers of lipid transport/metabolism were also determined in skeletal muscle (gastrocnemius) and white adipose tissue of McArdle (Pygm p.50R*/p.50R*) and wild‐type male mice. Peak oxygen uptake ( V̇O2peak${\dot V_{{{\rm{O}}_{\rm{2}}}{\rm{peak}}}}$ ), MFO rate, the exercise intensity eliciting MFO rate (FATmax) and the MFO rate‐associated workload were determined by indirect calorimetry during an incremental cycle‐ergometer test. Despite having a much lower V̇O2peak${\dot V_{{{\rm{O}}_{\rm{2}}}{\rm{peak}}}}$ (24.7 ± 4 vs. 42.5 ± 11.4 mL kg−1 min−1, respectively; P < 0.0001), patients showed considerably higher values for the MFO rate (0.53 ± 0.12 vs. 0.33 ± 0.10 g min−1, P = 0.001), and for the FATmax (94.4 ± 7.2 vs. 41.3 ± 9.1 % of V̇O2peak${\dot V_{{{\rm{O}}_{\rm{2}}}{\rm{peak}}}}$ , P < 0.0001) and MFO rate‐associated workload (1.33 ± 0.35 vs. 0.81 ± 0.54 W kg−1, P = 0.020) than controls. No between‐group differences were found overall in molecular markers of lipid transport/metabolism in mice. In summary, patients with McArdle disease show an exceptionally high MFO rate, which they attained at near‐maximal exercise capacity. Pending more mechanistic explanations, these findings support the influence of glycogen availability on MFO rate and suggest that these patients develop a unique fat oxidation capacity, possibly as an adaptation to compensate for the inherited blockade in glycogen metabolism, and point to MFO rate as a potential limiting factor of exercise tolerance in this disease.
DISCOVERY OF A HIGHLY ENERGETIC PULSAR ASSOCIATED WITH IGR J14003−6326 IN THE YOUNG UNCATALOGED GALACTIC SUPERNOVA REMNANT G310.6−1.6

We report the discovery of 31.18 ms pulsations from the INTEGRAL source IGR J14003−6326 using the Rossi X-ray Timing Explorer (RXTE). This pulsar is most likely associated with the bright Chandra X-ray point source lying at the center of G310.6−1.6, a previously unrecognized Galactic composite supernova remnant (SNR) with a bright central non-thermal radio and X-ray nebula, taken to be the pulsar wind nebula (PWN). PSR J1400−6325 is amongst the most energetic rotation-powered pulsars in the Galaxy, with a spin-down luminosity of erg s−1. In the rotating dipole model, the surface dipole magnetic field strength is Bs = 1.1 × 1012 G and the characteristic age kyr. The high spin-down power is consistent with the hard spectral indices of the pulsar and the nebula of 1.22 ± 0.15 and 1.83 ± 0.08, respectively, and a 2–10 keV flux ratio FPWN/FPSR ∼ 8. Follow-up Parkes observations resulted in the detection of radio emission at 10 and 20 cm from PSR J1400−6325 at a dispersion measure of ∼560 cm−3 pc, which implies a relatively large distance of 10 ± 3 kpc. However, the resulting location off the Galactic plane of ∼280 pc would be much larger than the typical thickness of the molecular disk, and we argue that G310.6−1.6 lies at a distance of ∼7 kpc. There is no gamma-ray counterpart to the nebula or pulsar in the Fermi data published so far. A multi-wavelength study of this new composite SNR, from radio to very high-energy gamma rays, suggests a young (≲103 yr) system formed by a sub-energetic (≲1050 erg), low ejecta mass (Mej ∼ 3 M☉) supernova explosion that occurred in a low-density environment (n0∼ 0.01 cm−3).
Fabrication and analysis of chitosan oligosaccharide based mucoadhesive patch for oromucosal drug delivery

Abstract Objective Fabrication and analyses of mucoadhesive patches made from chitosan oligosaccharide for the purpose of oromucosal drug delivery. Significance The mucosal epithelium in the oral cavity, consisting of buccal and sublingual epithelium, has gained significant attention in the last decade as an alternative anatomical site for systemic drug delivery that could potentially minimize the challenges of solid oral dosage and parenteral delivery. In this study, we have fabricated and tested drug-loaded chitosan oligosaccharide-based patches for the oromucosal drug delivery. Methods The chitosan oligosaccharide (with and without alginate) based patches were fabricated using the conventional solvent casting method and were analyzed for their swelling capacity, hydrophilicity, anti-cancer activity, in vitro drug release, and in vivo drug release activity. The in-house developed artificial saliva was used for the swelling study. Results Alginate-containing patches showed lesser swelling ability compared to the bare chitosan oligosaccharide-based patches. The former was also found to be more hydrophobic compared to the latter one. Both the unloaded patches restricted the growth of epithelial cancer cells indicating their anti-cancer behavior. In vitro drug release indicated a super case II release pattern while in vivo study demonstrated the release of drug from the patch into the plasma indicating the purpose of the fabricated patch. Conclusions The chitosan oligosaccharide-based mucoadhesive hydrogel patch fabricated in this study can be highly suitable for possible translational purposes.
USING SYNTHETIC SPACECRAFT DATA TO INTERPRET COMPRESSIBLE FLUCTUATIONS IN SOLAR WIND TURBULENCE

Kinetic plasma theory is used to generate synthetic spacecraft data to analyze and interpret the compressible fluctuations in the inertial range of solar wind turbulence. The kinetic counterparts of the three familiar linear MHD wave modes—the fast, Alfvén, and slow waves—are identified, and the properties of the density–parallel magnetic field correlation for these kinetic wave modes are presented. The construction of synthetic spacecraft data, based on the quasi-linear premise—that some characteristics of magnetized plasma turbulence can be usefully modeled as a collection of randomly phased, linear wave modes—is described in detail. Theoretical predictions of the density–parallel magnetic field correlation based on MHD and Vlasov–Maxwell linear eigenfunctions are presented and compared to the observational determination of this correlation based on 10 years of Wind spacecraft data. It is demonstrated that MHD theory is inadequate to describe the compressible turbulent fluctuations and that the observed density–parallel magnetic field correlation is consistent with a statistically negligible kinetic fast wave energy contribution for the large sample used in this study. A model of the solar wind inertial range fluctuations is proposed composed of a mixture of a critically balanced distribution of incompressible Alfvénic fluctuations and a critically balanced or more anisotropic than critical balance distribution of compressible slow wave fluctuations. These results imply that there is little or no transfer of large-scale turbulent energy through the inertial range down to whistler waves at small scales.
STARSPOTS–TRANSIT DEPTH RELATION OF THE EVAPORATING PLANET CANDIDATE KIC 12557548b

Violent variation of transit depths and an ingress–egress asymmetry of the transit light curve discovered in KIC 12557548 have been interpreted as evidence of a catastrophic evaporation of atmosphere with dust ( Gyr−1) from a close-in small planet. To explore what drives the anomalous atmospheric escape, we perform time-series analysis of the transit depth variation of Kepler archival data for ∼3.5 yr. We find a ∼30% periodic variation of the transit depth with P1 = 22.83 ± 0.21 days, which is within the error of the rotation period of the host star estimated using the light curve modulation, Prot = 22.91 ± 0.24 days. We interpret the results as evidence that the atmospheric escape of KIC 12557548b correlates with stellar activity. We consider possible scenarios that account for both the mass loss rate and the correlation with stellar activity. X-ray and ultraviolet (XUV)-driven evaporation is possible if one accepts a relatively high XUV flux and a high efficiency for converting the input energy to the kinetic energy of the atmosphere. Star–planet magnetic interaction is another possible scenario, though huge uncertainty remains for the mass loss rate.
DISK FORMATION IN MAGNETIZED CLOUDS ENABLED BY THE HALL EFFECT

Stars form in dense cores of molecular clouds that are observed to be significantly magnetized. A dynamically important magnetic field presents a significant obstacle to the formation of protostellar disks. Recent studies have shown that magnetic braking is strong enough to suppress the formation of rotationally supported disks in the ideal MHD limit. Whether non-ideal MHD effects can enable disk formation remains unsettled. We carry out a first study on how disk formation in magnetic clouds is modified by the Hall effect, the least explored of the three non-ideal MHD effects in star formation (the other two being ambipolar diffusion and Ohmic dissipation). For illustrative purposes, we consider a simplified problem of a non-self-gravitating, magnetized envelope collapsing onto a central protostar of fixed mass. We find that the Hall effect can spin up the inner part of the collapsing flow to Keplerian speed, producing a rotationally supported disk. The disk is generated through a Hall-induced magnetic torque. Disk formation occurs even when the envelope is initially non-rotating, provided that the Hall coefficient is large enough. When the magnetic field orientation is flipped, the direction of disk rotation is reversed as well. The implication is that the Hall effect can in principle produce both regularly rotating and counter-rotating disks around protostars. The Hall coefficient expected in dense cores is about one order of magnitude smaller than that needed for efficient spin-up in these models. We conclude that the Hall effect is an important factor to consider in studying the angular momentum evolution of magnetized star formation in general and disk formation in particular.
AN EXTREME PULSAR TAIL PROTRUDING FROM THE FRYING PAN SUPERNOVA REMNANT

The Frying Pan (G315.9−0.0) is a radio supernova remnant with a peculiar linear feature (G315.78−0.23) extending 10′ radially outward from the rim of the shell. We present radio imaging and polarization observations obtained from the Molonglo Observatory Synthesis Telescope and the Australia Telescope Compact Array, confirming G315.78−0.23 as a bow-shock pulsar wind nebula (PWN) powered by the young pulsar J1437−5959. This is one of the longest pulsar tails observed in radio and it has a physical extent over 20 pc. We found a bow-shock standoff distance of 0.002 pc, smallest among similar systems, suggesting a large pulsar velocity over 1000 km s−1 and a high Mach number ∼200. The magnetic field geometry inferred from radio polarimetry shows a good alignment with the tail orientation, which could be a result of high flow speed. There are also hints that the postshock wind has a low magnetization and is dominated by electrons and positrons in energy. This study shows that PWNe can offer a powerful probe of their local environment, particularly for the case of a bow shock where the parent supernova shell is also detected.
Revisiting the pion leading-twist distribution amplitude within the QCD background field theory

We study the pion leading-twist distribution amplitude (DA) within the framework of Shifman-VainshteinZakharov sum rules under the background field theory. To improve the accuracy of the sum rules, we expand both the quark propagator and the vertex dz D. _ n of the correlator up to dimension-six operators in the background field theory. The sum rules for the pion DA moments are obtained, in which all condensates up to dimension-six have been taken into consideration. Using the sum rules, we obtain h.2 ij1 GeV 0.338 +/- 0.032, h.4 ij1 GeV 0.211 +/- 0.030 and h.6 ij1 GeV 0.163 +/- 0.030. It is shown that the dimension-six condensates shall provide sizable contributions to the pion DA moments. We show that the first Gegenbauer moment of the pion leading-twist DA is ap2 j1 GeV 0.403 +/- 0.093, which is consistent with those obtained in the literature within errors but prefers a larger central value as indicated by lattice QCD predictions.
On the stability of the thermal Comptonization index in neutron star low-mass X-ray binaries in their different spectral states

Context. Most of the spectra of neutron star low-mass X-ray binaries (NS LMXBs), whether they are persistent or transient, are characterized by the presence of a strong thermal Comptonization bump, which is thought to originate in the transition layer (TL) between the accretion disk and the NS surface. The observable quantities that characterize this component, which is dominating the emission below 30 keV, are the spectral index α and the rollover energy, both related to the electron temperature and optical depth of the plasma. Aims. Starting from observational results on a sample of NS LMXBs in different spectral states, we formulate the problem of X-ray spectral formation in the TL of these sources. We predict a stability of the thermal Comptonization spectral index in different spectral states if the energy release in the TL is much higher than the intercepted flux coming from the accretion disk. Methods. We use an equation for the energy balance and the radiative transfer diffusion equation for a slab geometry in the TL to derive a formula for the thermal Comptonization index α. We show that in this approximation the TL electron temperature kTe and optical depth τ0 can be written as a function of the energy flux from the disk intercepted by the corona (TL) and that in the corona itself, Qdisk/Qcor. Because the spectral index α depends on kTe and τ0, this in turn leads to a relation α = f (Qdisk/Qcor), with α ∼ 1 when Qdisk/Qcor � 1. Results. We show that the observed spectral index α for the sample of sources here considered lies in a belt around 1 ± 0.2 apart for the case of GX 354–0. Comparing our theoretical predictions with observations, we claim that this result, which is consistent with the condition Qdisk/Qcor � 1, can give us constraints on the accretion geometry of these systems, an issue that seems difficult to be solved with only the spectral analysis method.
Tracing star formation with non-thermal radio emission

Understanding the evolution of galaxies and in particular their star formation history is a central challenge of modern cosmology. Theoretical scenarios will be constrained by future ultra deep radio surveys. In this paper we present an analytical tool for analyzing radio data. Our physical model, based on an analytical description of the steady-state cosmic ray spectrum, explains the correlation between the non-thermal radio flux and the star formation rate (SFR). As cosmic rays are produced in supernova remnants, their injection rate is proportional to the supernova rate and thus also to the SFR. When these highly energetic charged particles travel in the magnetized interstellar medium they emit synchrotron radiation. As a result there is a relation between the SFR and the non-thermal radio emission. A crucial point is that synchrotron emission can be absorbed again by the free-free mechanism. This suppression becomes stronger with increasing number density of the gas, more precisely of the free electrons, and with decreasing frequency. We present an estimate of the critical frequency above which radio emission can be used as a tracer for the SFR. If the observed galaxy is redshifted, this critical frequency moves along with other spectral features to lower values in the observing frame. The method can therefore be successfully applied at high redshift. However, for high redshift, i.e. > 5 , and observations at high radio frequency bands, i.e. > 50 GHz, special caution should be paid, as the observed flux might be dominated by free-free emission or the thermal contribution.
The enrichment of the intergalactic medium with adiabatic feedback – I. Metal cooling and metal diffusion

A study of metal enrichment of the intergalactic medium (IGM) using a series of smooth particle hydrodynamics (SPH) simulations is presented, employing models for metal cooling and the turbulent diffusion of metals and thermal energy. An adiabatic feedback mechanism was adopted where gas cooling was prevented on the timescale of supernova bubble expansion to generate galactic winds without explicit wind particles. The simulations produced a cosmic star formation history (SFH) that is broadly consistent with observations until z � 0.5, and a steady evolution of the universal neutral hydrogen fraction (HI) that compares reasonably well with observations. The evolution of the mass and metallicities in stars and various gas phases was investigated. At z=0, about 40% of the baryons are in the warm-hot intergalactic medium (WHIM), but most metals (80%-90%) are locked in stars. At higher redshifts the proportion of metals in the IGM is higher due to more efficient loss from galaxies. The r also indicate that IGM metals primarily reside in the WHIM throughout cosmic history, which differs from simulations with hydrodynamically decoupled explicit winds. The metallicity of the WHIM lies between 0.01 and 0.1 solar with a slight decrease at lower redshifts. The metallicity evolution of the gas inside galaxies are broadly consistent with observations, but the diffuse IGM is under enriched at z � 2.5. Galactic winds most efficiently enrich the IGM for halos in the intermediate mass range 10 10 M � - 10 11 M � . At the low mass end gas is prevented from accreting onto halos and has very low metallicities. At the high mass end, the fraction of halo baryons escaped as winds declines along with the decline of stellar mass fraction of the galaxies. This is likely because of the decrease in star formation activity and decrease in wind escape efficiency. Metals enhance cooling which allows WHIM gas to cool onto galaxies and increases star formation. Metal diffusion allows winds to mix prior to escape, decreasing the IGM metal content in favour of gas within galactic halos and star forming gas. Diffusion significantly increases the amount of gas with low metallicities and changes the density-metallicity relation.
Fundamental Physics with Electroweak Probes of Nuclei

The past decade has witnessed tremendous progress in the theoretical and computational tools that produce our understanding of nuclei. A number of microscopic calculations of nuclear electroweak structure and reactions have successfully explained the available experimental data, yielding a complex picture of the way nuclei interact with electroweak probes. This achievement is of great interest from the pure nuclear-physics point of view. But it is of much broader interest too, because the level of accuracy and confidence reached by these calculations opens up the concrete possibility of using nuclei to address open questions in other sub-fields of physics, such as, understanding the fundamental properties of neutrinos, or the particle nature of dark matter. In this talk, I will review recent progress in microscopic calculations of electroweak properties of light nuclei, including electromagnetic moments, form factors and transitions in between lowlying nuclear states along with preliminary studies for single- and double-beta decay rates. I will illustrate the key dynamical features required to explain the available experimental data, and, if time permits, present a novel framework to calculate neutrino-nucleus cross sections for A > 12 nuclei.
Signatures of nonclassical effects in optical tomograms

Several nonclassical effects displayed by wave packets governed by nonlinear Hamiltonians can be identified and assessed directly from tomograms without attempting to reconstruct the Wigner function or the density matrix explicitly. We have demonstrated this for both single-mode and bipartite systems. We have shown that a wide spectrum of effects such as the revival phenomena, quadrature squeezing, and Hong–Mandel and Hillery type higher-order squeezing in a generic single-mode system and the double-well Bose–Einstein condensate (BEC) can be obtained from appropriate tomograms in a straightforward manner. We have examined the manner in which decoherence affects the nature of the state of a generic single-mode system at specific instants during temporal evolution. We have investigated entropic squeezing of the subsystem state of a bipartite system as it evolves in time, solely from tomograms. The procedures that we have demonstrated can be readily adapted to multimode systems. Further, for the double-well BEC we have identified an indicator of entanglement between subsystems that can be obtained directly from the tomogram. This mirrors the qualitative behavior of the subsystem von Neumann entropy and the subsystem linear entropy.
Automatised classification of WISE sources: first results, future prospects

We present the first results of our dedicated programme of automatised classification of galaxies, stars and quasars in the mid-infrared all-sky data from the WISE survey. We employ the Support Vector Machines (SVM) algorithm, which defines a hyperplane separating different classes of sources in a multidimensional space of arbitrarily chosen parameters. This approach consists of four general steps: 1) selection of the training sample, 2) selection of the optimal parameter space, 3) training of the classifier, 4) application to target data. Here, as the training set, we use sources from a cross-correlation of the WISE catalogue with the SDSS spectroscopic sample. The performance of the SVM classifier was tested as a function of size of the training set, dimension of the parameter space, WISE apparent magnitude and Galactic extinction. We find that our classifier provides promising results already for three classification parameters: magnitude, colour and differential aperture magnitude. Completeness and purity levels as high as 95% are obtained for quasars, while for galaxies and stars they vary between 80-95% depending on the magnitude, deteriorating for fainter sources.