Miracle-dz/UniFAR-FTUs huggingface dataset:
LITHIUM INVENTORY OF 2 M⊙ RED CLUMP STARS IN OPEN CLUSTERS: A TEST OF THE HELIUM FLASH MECHANISM

The temperature distribution of field Li-rich red giants suggests the presence of a population of Li-rich red clump (RC) stars. One proposed explanation for this population is that all stars with masses near 2 M⊙ experience a short-lived phase of Li-richness at the onset of core He-burning. Many of these stars have low 12C/13C, a signature of deep mixing that is presumably associated with the Li regeneration. To test this purported mechanism of Li enrichment, we measured abundances in 38 RC stars and 6 red giant branch (RGB) stars in four open clusters selected to have RC masses near 2 M⊙. We find six Li-rich stars (A(Li) ≥ 1.50 dex) of which only two may be RC stars. None of the RC stars have Li exceeding the levels observed in the RGB stars, but given the brevity of the suggested Li-rich phase and the modest sample size, it is probable that stars with larger Li-enrichments were missed simply by chance. However, we find very few stars in our sample with low 12C/13C. Such low 12C/13C, seen in many field Li-rich stars, should persist even after lithium has returned to normal low levels. Thus, if Li synthesis during the He flash occurs, it is a rare, but potentially long-lived occurrence rather than a short-lived phase for all stars. We estimate a conservative upper limit of the fraction of stars going through a Li-rich phase to be , based on stars that have low 12C/13C for their observed A(Li).
First Unambiguous Imaging of Large-scale Quasi-periodic Extreme-ultraviolet Wave or Shock

We report the first unambiguous quasi-periodic large-scale extreme-ultraviolet (EUV) wave or shock that was detected by the Atmospheric Imaging Assembly on board the Solar Dynamics Observatory. During the whip-like unwinding eruption of a small filament on 2012 April 24, multiple consecutive large-scale wavefronts emanating from AR11467 were observed simultaneously along the solar surface and a closed transequatorial loop system. In the meantime, an upward propagating dome-shaped wavefront was also observed, whose initial speed and deceleration are about 1392 km s−1 and 1.78 km s−2, respectively. Along the solar surface, the quasi-peridoic wavefronts had a period of about 163 ± 21 s and propagated at a nearly constant speed of 747 ± 26 km s−1; they interacted with active region AR11469 and launched a sympathetic upward propagating secondary EUV wave. The wavefronts along the loop system propagated at a speed of 897 km s−1, and they were reflected back at the southern end of the loop system at a similar speed. In addition to the propagating waves, a standing kink wave was also present in the loop system simultaneously. Periodicity analysis reveals that the period of the wavefronts was consistent with that of the unwinding helical structures of the erupting filament. Based on these observational facts, we propose that the observed quasi-periodic EUV wavefronts were most likely excited by the periodic unwinding motion of the filament helical structures. In addition, two different seismological methods are applied to derive the magnetic field strength of the loop system, and for the first time the reliability of these inversion techniques are tested with the same magnetic structure.
HIP 3678: a hierarchical triple stellar system in the centre of the planetary nebula NGC 246

We report the detection of a new low-mass stellar companion to the white dwarf HIP 3678 A, the central star of the planetary nebula NGC 246. The newly found companion is located about 1 arcsec (at projected separation of about 500 au) north-east of HIP 3678 A, and shares a common proper motion with the white dwarf and its known comoving companion HIP 3678 B. The hypothesis that the newly detected companion is a non-moving background object can be rejected on a significance level of more than 8 $\sigma$, by combining astrometric measurements from the literature with follow-up astrometry, obtained with Wild Field Planetary Camera 2/\textit{Hubble Space Telescope} and NACO/Very Large Telescope. From our deep NACO imaging data, we can rule out additional stellar companions of the white dwarf with projected separations between 130 up to 5500 au. In the deepest high-contrast NACO observation, we achieve a detection limit in the \textit{Ks} band of about 20 mag, which allows the detection of brown dwarf companions with masses down to 36$\,\rmn{M_{jup}}$ at an assumed age of the system of 260 Myr. To approximate the masses of the companions HIP 3678 B and C, we use the evolutionary Baraffe et al. models and obtain about 0.85\,M$_{\sun}$ for HIP 3678 B and about 0.1 M$_{\sun}$ for HIP 3678 C. According to the derived absolute photometry, HIP 3678 B should be a early to mid-K dwarf (K2--K5), while HIP 3678 C should be a mid-M dwarf with a spectral type in the range between M5 and M6.
The P1/HC-Pro of turnip mosaic virus has more inhibits RISC activity unlike the other potyviruses

Ectopically expressing viral suppressors of RNA silencing (VSR) in transgenic Arabidopsis overcome host range limitation and viral titer variation, and have similar VSR levels to investigate RNA silencing suppression. Therefore, identifying the insertion of the transgenic VSR gene and developing an endogenous AGO1-based in vitro RNA-inducing silencing complex (RISC) assay prompted further investigation into VSR-mediated suppression. Three P1/HC-Pro plants from turnip mosaic virus (TuMV) (P1/HC-Pro Tu ), zucchini yellow mosaic virus (P1/HC-Pro Zy ), and tobacco etch virus (P1/HC-Pro Te ) were investigated for in vitro RISC cleavage e�ciency. We identi�ed T-DNA insertion for these P1/HC-Pro plants and applied these plant materials to compare the endogenous AGO1 levels and RISC activity. Our results indicated that P1/HC-Pro Tu plants have lower AGO1 levels and lower RISC activity than the other P1/HC-Pro plants. In addition, the phenomena are consistent with those in TuMV-infected Arabidopsis, implying that HC-Pro Tu could directly interfere with AGO1 stability. In this study, we demonstrated the application of various plant materials with an in vitro RISC assay in VSR-mediated RNA silencing suppression. short-interfering TuMV strain (TuGK), ZYMV (HC-Pro Zy TuMV HC-Pro (HC-Pro Tu TEV HC-Pro (HC-Pro Te ), HUA ENHANCE 1 (HEN1), transgenic Arabidopsis expression of the P1/HC-Pro gene of TuMV (P1/HC-Pro Tu plant), transgenic Arabidopsis expression of the P1/HC-Pro gene of ZYMV (P1/HC-Pro Zy plant), transgenic Arabidopsis expression of the P1/HC-Pro gene of TEV (P1/HC-Pro Te plant), transgenic Arabidopsis expression of the P1/HC-Pro gene of TGK (P1/HC-Pro Tu-K plant), ATG8a knockout mutant in a P1/HC-Pro Tu background (P1/HC-Pro Tu /atg8a ge plant), N-terminus of AGO1 (his-AGO1 N240 ), viral suppressors of RNA silencing (VSR).
Local thermal equilibrium in quantum field theory on flat and curved spacetimes

The existence of local thermal equilibrium (LTE) states for quantum field theory in the sense of Buchholz, Ojima and Roos is discussed in a model-independent setting. It is shown that for spaces of finitely many independent thermal observables there always exist states which are in LTE in any compact region of Minkowski spacetime. Furthermore, LTE states in curved spacetime are discussed and it is observed that the original definition of LTE on curved backgrounds given by Buchholz and Schlemmer needs to be modified. Under an assumption related to certain unboundedness properties of the pointlike thermal observables, existence of states which are in LTE at a given point in curved spacetime is established. The assumption is discussed for the sets of thermal observables for the free scalar field considered by Schlemmer and Verch.
Coevolution of metallicity and star formation in galaxies to z ≃ 3.7 - II. A theoretical model

Recent work suggests that galaxy evolution, and the build-up of stellar mass (M-*) over cosmic time, is characterized by changes with redshift of star formation rate (SFR) and oxygen abundance (O/H). In a companion paper, we have compiled a large data set to study Metallicity Evolution and Galaxy Assembly (MEGA), consisting of similar to 1000 galaxies to z similar or equal to 3.7 with a common O/H calibration. Here we interpret the MEGA scaling relations of M*, SFR, and O/H with an updated version of the model presented by Dayal et al. This model successfully reproduces the observed O/H ratio of similar to 80 000 galaxies selected from the Sloan Digital Sky Survey to within 0.05-0.06 dex. By extending the model to the higher redshift MEGA sample, we find that although the specific mass loading of outflows does not change measurably during the evolution, the accretion rate and gas content of galaxies increase significantly with redshift. These two effects can explain, either separately or possibly in tandem, the observed lower metal abundance of high-z galaxies.
Invariant measures for some piecewise continuous maps

We study some special classes of piecewise continuous maps on a finite smooth partition of the compact phase space and look for invariant measures for such maps. We show that in the simplest one-dimensional case (so-called interval translation maps), this measure exists for any map. Moreover, they can always be selected non-atomic. We use this result to demonstrate that any piecewise translation map is metrically equivalent to an interval exchange map. In higher dimensions, we demonstrate that the invariant measure exists if the number of domains in the partition does not exceed the dimension of the space plus one. Finally, we provide a general conditions on approximation of invariant measures of a piecewise continuous map by invariant measures of piecewise translation maps.
Reverse Shock Emission Driven By Post-Merger Millisecond Magnetar Winds: Effects of the Magnetization Parameter

The study of short-duration gamma-ray bursts provides growing evidence that a good fraction of double neutron star mergers lead to the formation of stable millisecond magnetars. The launch of Poynting flux by the millisecond magnetars could leave distinct electromagnetic signatures that reveal the energy dissipation processes in the magnetar wind. In previous studies (Wang & Dai 2013b; Wang et al. 2015), we assume that the magnetar wind becomes completely lepton-dominated so that electrons/positrons in the magnetar wind are accelerated by a diffusive shock. However, theoretical modeling of pulsar wind nebulae shows that in many cases the magnetic field energy in the pulsar wind may be strong enough to suppress diffusive shock acceleration. In this paper, we investigate the reverse shock emission as well as the forward shock emission with an arbitrary magnetization parameter $\sigma$ of a magnetar wind. We find that the reverse shock emission strongly depends on $\sigma$, and in particular, $\sigma \sim 0.3$ leads to the strongest reverse shock emission. Future observations would be helpful to diagnose the composition of the magnetar wind.
Unfolding Smart Specialisation for Regional Economic Resilience: the role of Industrial Structure

The European Regional Development Funds for the programmatic cycle 2014-2020 aims to support regions that implement an innovation strategy based on Smart Specialisation. Within this framework, the European Commission emphasises the role of smart specialisation in favouring regional transformation, enhancing competitiveness and fostering resilience. However, the concepts of smart specialisation and resilience have been poorly combined. The article aims at investigating their relationship to understand if a smart specialisation strategy may promote the economic resilience of regions in response to major economic shocks. Drawing upon the concepts of adaptation/adaptability, the analysis investigates the relatedness of new industrial specialisations to the existing industrial structure before and after a shock occurrence. Evaluating the resilience of Italian provinces in relation to the economic crisis of 2008, the analysis aims to understand if provinces that resisted and recovered better followed a smart specialisation framework where new industrial specialisations are related to the existing industrial structure.
On the nature of the most obscured C-rich AGB stars in the Magellanic Clouds

The stars in the Magellanic Clouds with the largest degree of obscuration are used to probe the highly uncertain physics of stars in the asymptotic giant branch (AGB) phase of evolution. Carbon stars in particular, provide key information on the amount of third dredge-up (TDU) and mass loss. We use two independent stellar evolution codes to test how a dierent treatment of the physics aects the evolution on the AGB. The output from the two codes are used to determine the rates of dust formation in the circumstellar envelope, where the method used to determine the dust is the same for each case. The stars with the largest degree of obscuration in the LMC and SMC are identied
Refinement of Strichartz estimate for Airy equation in non-diagonal case and its application

In this paper, we give an improvement of the Strichartz estimate for Airy equation in the non-diagonal case. As an application, we prove the small data scattering and existence of a special non-scattering solutions, which are minimal in suitable sense, to the mass-subcritical generalized Korteweg-de Vries (gKdV) equation. Especially, we remove several technical restrictions on our previous work about the existence of a special non-scattering solution.
SOME POLYNOMIALS WITH UNIMODULAR ROOTS

In this paper we consider a sequence of polynomials deﬁned by some recurrence relation. They include, for instance, Poupard poly- nomials and Kreweras polynomials whose coeﬃcients have some combinatorial interpretation and have been investigated before. Extending a recent result of Chapoton and Han we show that each polynomial of this sequence is a self-reciprocal polynomial with positive coeﬃcients whose all roots are unimodular. Moreover, we prove that their arguments are uniformly distributed in the interval [0 , 2 π ).
Turbulent diffusion and galactic magnetism

Abstract Using the test-field method for nearly irrotational turbulence driven by spherical expansion waves it is shown that the turbulent magnetic diffusivity increases with magnetic Reynolds numbers. Its value levels off at several times the rms velocity of the turbulence multiplied by the typical radius of the expansion waves. This result is discussed in the context of the galactic mean-field dynamo.
[Fe ii] 1.64 μm FEATURES OF JETS AND OUTFLOWS FROM YOUNG STELLAR OBJECTS IN THE CARINA NEBULA

We present [Fe ii] 1.64 μm imaging observations for jets and outflows from young stellar objects (YSOs) over the northern part (∼24′ × 45′) of the Carina Nebula, a massive star-forming region. The observations were performed with IRIS2 of the Anglo-Australian Telescope and the seeing was ∼1. ″5 ± 0. ″5. Eleven jet and outflow features are detected at eight different regions and are termed ionized Fe objects (IFOs). One Herbig–Haro candidate that was missed in Hubble Space Telescope Hα observations is newly identified as HHc-16, referring to our [Fe ii] images. IFOs have knotty or longish shapes, and the detection rate of IFOs against previously identified YSOs is 1.4%, which should be treated as a lower limit. Four IFOs show anti-correlated peak intensities in [Fe ii] and Hα, where the ratio I([Fe ii])/I(Hα) is higher for longish IFOs than for knotty IFOs. We estimate the outflow mass loss rate from the [Fe ii] flux using two different methods. The jet-driving objects are identified for three IFOs (IFO-2, -4, and -7) for which we study the relations between the outflow mass loss rate and the YSO physical parameters from the radiative transfer model fitting. The ratios of the outflow mass loss rate over the disk accretion rate for IFO-4 and -7 are consistent with the previously reported values (10−2–10+1), while the ratio is higher for IFO-2. This excess may result from underestimating the disk accretion rate. The jet-driving objects are likely to be low- or intermediate-mass stars. Other YSO physical parameters, such as luminosity and age, show reasonable relations or trends.
Cosmological AMR MHD with Enzo

In this work, we present MHDEnzo, the extension of the cosmological code Enzo to include the effects magnetic fields through the ideal MHD approximation. We use a higher order Godunov Riemann solver for the computation of interface fluxes. We use two constrained transport methods to compute the electric field from those interface fluxes, which simultaneously advances the induction equation and maintains the divergence of the magnetic field. A third order divergence free reconstruction technique is used to interpolate the magnetic fields in the block structured AMR framework already extant in Enzo. This reconstruction also preserves the divergence of the magnetic field to machine precision. We use operator splitting to include gravity and cosmological expansion. We then present a series of cosmological and non cosmological tests problems to demonstrate the quality of solution resulting from this combination of solvers.
Organizational Support Factors for Minor League Baseball Player Development

This study examines organizational support in the context of minor league baseball to better understand how organizations can support athletes’ development. Exploratory results show that English and Spanish players identify salary/pay, off-season training opportunities, and nutritious food as their most important unmet development needs. English and Spanish respondents differently prioritized playing opportunities, communication with front office staff, health care, and equipment as unmet needs. Explanatory results show that organizational support factors (private problem support and second career support) explain 17% of the variation in minor league baseball players’ self-perceptions of development. The results provide guidance for Major League Baseball and its affiliates as they restructure the development system and for non-profits seeking to help players. Better pay and other financial support appear to be the most critical unmet needs where organizations can better support athletes.
New X-ray observations of IQ Aurigae and α2 Canum Venaticorum - Probing the magnetically channeled wind shock model in A0p stars

We present new X-ray observations of the A0p stars alpha^2 CVn (log Lx < 26.0 erg/s) and IQ Aur (log Lx = 29.6 erg/s) and find that their X-ray luminosities differ by at least three orders of magnitude. IQ Aur possesses a strong cool plasma component with X-ray emitting regions located well above the stellar surface, but also significant amounts of hot plasma. Further, a large X-ray flare is detected from IQ Aur, implying the presence of magnetic reconnection. Our comparison study of similar stars indicates that the occurrence of X-ray emission generated by magnetically channelled wind shocks (MCWS) strongly depends on stellar properties. X-ray emission is preferably generated by more luminous and massive objects such as IQ Aur. The MCWS scenario can consistently describe the X-ray emission of these A0p stars, assuming that the very strong magnetic confinement of the stellar wind has led to the build up of a rigidly rotating disk around the star, where magnetic reconnection and centrifugal breakout events occur.
Journal Pre-proof Structural performance of plastic block masonry unit

: The use of innovative materials with a sustainable application can have important benefits. Plastic bottles are increasingly becoming a menace to the environment due to their improper disposal. In this work, Polyethylene Terephthalate (PET) bottles of 500 ml volume were used and filled with different types of soil: Red Coffee Soil (RCS), Murram Soil (MS) and Black Cotton Soil (BCS). The objective of this work was to investigate the structural performance of plastic bottles filled with soil inserted into cement mortar as a walling material. The compressive strength of Inserted Bottle Block (IBB) and Inserted Bottle Wall (IBW) has been tested and results have been discussed. At 28 days, compressive strength test results show that, Inserted Bottle filled with Red Coffee Soil Block (IBB-RCS) and Inserted Bottle filled with Murram Soil Block (IBB-MS) had a compressive strength of 2.7 MPa and 2.8 MPa, respectively. These values were higher than the minimum requirement for masonry units specified by the Kenya standard, which is 2.5 MPa, while the compressive strength of the Inserted Bottle filled with Black Cotton Soil Block (IBB-BCS) was 1.8MPa. A compressive strength test on Inserted Bottle Walls (IBW) shows that Inserted Bottle filled with Murram Soil wall (IBW-MS) has a compressive strength of 1.2 MPa while Inserted Bottle filled with Red Coffee Soil wall (IBW-RCS) and Inserted Bottle filled with Black Cotton Soil wall (IBW-BCS) have a compressive strength of 1.4 MPa and 0.8 MPa respectively. This study revealed that Inserted bottle filled with soil blocks could be used as construction materials.
Chaos and turbulent nucleosynthesis prior to a supernova explosion

Three-dimensional (3D), time dependent numerical simulations of flow of matter in stars, now have sufficient resolution to be fully turbulent. The late stages of the evolution of massive stars, leading up to core collapse to a neutron star (or black hole), and often to supernova explosion and nucleosynthesis, are strongly convective because of vigorous neutrino cooling and nuclear heating. Unlike models based on current stellar evolutionary practice, these simulations show a chaotic dynamics characteristic of highly turbulent flow. Theoretical analysis of this flow, both in the Reynolds-averaged Navier-Stokes (RANS) framework and by simple dynamic models, show an encouraging consistency with the numerical results. It may now be possible to develop physically realistic and robust procedures for convection and mixing which (unlike 3D numerical simulation) may be applied throughout the long life times of stars. In addition, a new picture of the presupernova stages is emerging which is more dynamic and intere.
On Schmidt's Conjecture and Star Formation Scaling Laws

Abstract Ever since the pioneering work of Schmidt a half-century ago there has been great interest in finding an appropriate empirical relation that would directly link some property of interstellar gas with the process of star formation within it. Schmidt conjectured that this might take the form of a power-law relation between the rate of star formation (SFR) and the surface density of interstellar gas. However recent observations suggest that a linear scaling relation between the total SFR and the amount of dense gas within molecular clouds appears to be the underlying physical relation that most directly connects star formation with interstellar gas from scales of individual GMCs to those encompassing entire galaxies both near and far. Although Schmidt relations are found to exist within local GMCs, there is no Schmidt relation observed between GMCs. The implications of these results for interpreting and understanding the Kennicutt-Schmidt scaling law for galaxies are discussed.