Miracle-dz/UniFAR-FTUs huggingface dataset:
Rufinamide, a Triazole-Derived Antiepileptic Drug, Stimulates Ca2+-Activated K+ Currents While Inhibiting Voltage-Gated Na+ Currents

Rufinamide (RFM) is a clinically utilized antiepileptic drug that, as a triazole derivative, has a unique structure. The extent to which this drug affects membrane ionic currents remains incompletely understood. With the aid of patch clamp technology, we investigated the effects of RFM on the amplitude, gating, and hysteresis of ionic currents from pituitary GH3 lactotrophs. RFM increased the amplitude of Ca2+-activated K+ currents (IK(Ca)) in pituitary GH3 lactotrophs, and the increase was attenuated by the further addition of iberiotoxin or paxilline. The addition of RFM to the cytosolic surface of the detached patch of membrane resulted in the enhanced activity of large-conductance Ca2+-activated K+ channels (BKCa channels), and paxilline reversed this activity. RFM increased the strength of the hysteresis exhibited by the BKCa channels and induced by an inverted isosceles-triangular ramp pulse. The peak and late voltage-gated Na+ current (INa) evoked by rapid step depolarizations were differentially suppressed by RFM. The molecular docking approach suggested that RFM bound to the intracellular domain of KCa1.1 channels with amino acid residues, thereby functionally affecting BKCa channels’ activity. This study is the first to present evidence that, in addition to inhibiting the INa, RFM effectively modifies the IK(Ca), which suggests that it has an impact on neuronal function and excitability.
Dynamics of Hot Accretion Flow with Thermal Conduction

The purpose of this paper is to explore the dynamical behaviour of hot accretion flow with thermal conduction. The importance of thermal conduction on hot accretion flow is confirmed by observations of the hot gas that surrounds Sgr A$^*$ and a few other nearby galactic nuclei. In this research, the effect of thermal conduction is studied by a saturated form of it, as is appropriate for weakly collisional systems. The angular momentum transport is assumed to be a result of viscous turbulence and the $\alpha$-prescription is used for the kinematic coefficient of viscosity. The equations of accretion flow are solved in a simplified one-dimensional model that neglects the latitudinal dependence of the flow. To solve the integrated equations that govern the dynamical behaviour of the accretion flow, we have used an unsteady self-similar solution. The solution provides some insights into the dynamics of quasi-spherical accretion flow and avoids from limits of the steady self-similar solution. In comparison to accretion flows without thermal conduction, the disc generally becomes cooler and denser. These properties are qualitatively consistent with performed simulations in hot accretion flows. Moreover, the angular velocity increases with the magnitude of conduction, while the radial infall velocity decreases. The mass accretion rate onto the central object is reduced in the presence of thermal conduction. We found that the viscosity and thermal conduction have the opposite effects on the physical variables. Furthermore, the flow represents a transonic point that moves inward with the magnitude of conduction or viscosity.
Star formation around the mid-infrared bubble CN 148

We present a multi-wavelength study to analyse star formation associated with the mid-infrared bubble CN 148 (H ii region G10.3-0.1), which harbours an O5V-O6V star. The arc-shaped distribution of molecular CO(2-1) emission, the cold dust emission, and the polycyclic aromatic hydrocarbon features trace a photodissociation region (PDR) around the H ii region. We have identified 371 young stellar objects (YSOs) in the selected region and, interestingly, their spatial distribution correlates well with the PDR. Of these YSOs, 41 per cent are present in 13 clusters, each having visual extinction larger than 16 mag. The clusters at the edges of the bubble (both north-east and south-west) are found to be relatively younger than the clusters located further away from the bubble. We also find that four 6.7 GHz methanol masers, two extended green objects, an ultra-compact H ii region and a massive protostar candidate (as previously reported) are spatially positioned at the edges of the bubble. The existence of an apparent age gradient in YSO clusters and different early evolutionary stages of massive star formation around the bubble suggest their origin to be influenced by an H ii region expanding into the surrounding interstellar medium. The data sets are suggestive of triggered star formation.
Advances in Soilless Culture and Growing Media in Today’s Horticulture—An Editorial

The soilless culture system is a promising, intensive, and sustainable approach with various advantages for plant production. The Special Issue “Soilless Culture, Growing Media, and Horticultural Plants” includes 22 original papers and 1 review written by 84 authors from 15 countries. The purpose of this Special Issue was to publish high-quality research articles that address the recent developments in the cultivation of horticultural plants in soilless culture systems and solid growing media. The published articles investigated new developments in simplified and advanced systems; the interaction between soilless and environmental factors with their effects on plant growth and photosynthesis, and the accumulation of secondary metabolites; the analyses of nutrient solution and hydraulic properties of substrates and mixtures; and the microbe–plant growing media interactions. Climate change and environmental and ecological issues will determine and drive the development of soilless culture systems and the choice of growing media constituents in the near future. Bioresources and renewable raw materials have great potential for use as growing medium constituents.
An elusive radio halo in the merging cluster Abell 781

Deep radio observations of the galaxy cluster Abell 781 have been carried out using the Giant Metrewave Radio Telescope at 325 MHz and have been compared to previous 610-MHz observations and to archival Very Large Array (VLA) 1.4-GHz data. The radio emission from the cluster is dominated by a diffuse source located at the outskirts of the X-ray emission, which we tentatively classify as a radio relic. We detected residual diffuse emission at the cluster centre at the level of S325 MHz ∼ 15–20 mJy. Our analysis disagrees with Govoni et al., and on the basis of simple spectral considerations, we do not support their claim of a radio halo with the flux density of 20–30 mJy at 1.4 GHz. Abell 781, a massive and merging cluster, is an intriguing case. Assuming that the residual emission is indicative of the presence of a radio halo barely detectable at our sensitivity level, it could be a very steep spectrum source.
Oxidised low-density lipoprotein (oxLDL) as a biomarker for non-alcoholic fatty liver disease (NAFLD)

Background and Aim: NAFLD is a condition that is increasing dramatically in incidence and prevalence globally. There is known to be a direct relationship between conventional risk factors of metabolic syndrome and NAFLD. However, it is not a compulsion that these names risk factors will always be seen; it is, therefore, necessary to find investigations that could serve as predictive screening tests to catch the development of NAFLD in an individual at its earlier stages. OxLDL is a product of oxidative stress, and the circulating levels of the molecule seem to have possible risk predictor capability. With very little research previously conducted, the aim of the current study is to determine if there is a relationship between OxLDL and NAFLD. The study is limited to the Indian population. Method: A case-control study was conducted in a tertiary care teaching hospital; a total of 50 individuals were tested for circulating OxLDL levels. Of the tested subjects, 25 were patients with various stages of nonalcoholic liver disease, and 25 made up a control group of no liver pathology. Fasting blood samples were taken from all test subjects, and the serum underwent enzyme immunoassay to determine the OxLDL levels.
Complicity, trauma, love: an exploration of the experiences of LGBTQIA+ members from physical education spaces

ABSTRACT The dearth of research with lesbian, gay, bisexual, transgender, queer/questioning, intersex, and asexual plus (LGBTQIA+) members within the physical education (PE) community, is of great concern; to some degree members of this community are invisible in the profession. The unfortunate reality is that PE is largely recognised as a heteronormative space with deeply rooted gendered practices that often go unacknowledged. In PE, the high visibility of one’s body, and the value placed on ‘select’ bodies, uncovers and reinforces society’s ‘isms’ such as ‘genderism’ and ‘heterosexism’. The constantly recycled dualistic understanding of these social identities has made PE an ‘exclusive’ space. Drawing on feminism and poststructuralism as our theoretical lens, this scholarly collaboration utilised a collaborative autoethnography from intersectional voices who identify as members of the LGBTQIA + community (a lesbian teacher, bi-sexual teacher educator, transgender student, and an ally), to explore our experiences from the PE space. Data were generated by several qualitative methods, initially from our individual narratives, which then ‘birthed’ poetry and visual artefacts. Our findings highlighted how complicity helps to maintain the heteronormative space, the never-ending nature of trauma, and the love that we experienced in various forms. Moreover, we all expressed a love of PE, even if/when it conflicts with our ‘bodies’. We leave this as an unfinished collaboration filled with hope and love; one that invites you to join us in solidarity to create a safe, welcoming space for every member of our community.
The clustering and evolution of H-alpha emitters at z~1 from HiZELS

(Abridged) The clustering properties of a well-defined sample of 734 H-alpha emitters at z=0.84 obtained as part of the Hi-z Emission Line Survey (HiZELS) are investigated. The spatial correlation function is very well-described by (r/r_0)^-1.8, with r_0=2.7+-0.3Mpc/h. The correlation length r_0 increases strongly with H-alpha luminosity, L_H-alpha, from r_0~2Mpc/h for the most quiescent galaxies (star-formation rates of ~4M_sun/yr), up to r_0>5Mpc/h for the brightest galaxies in H-alpha. The correlation length also increases with increasing rest-frame K-band luminosity (M_K), but the r_0-L_H-alpha correlation maintains its full statistical significance at fixed M_K. At z=0.84, star-forming galaxies classified as irregulars or mergers are much more clustered than discs and non-mergers, but once the samples are matched in L_H-alpha and M_K, the differences vanish, implying that the clustering is independent of morphological type at z~1. The typical H-alpha emitters found at z=0.84 reside in dark-matter haloes of ~10^12M_sun, but those with the highest SFRs reside in more massive haloes of ~10^13M_sun. Comparing the results with those of H-alpha surveys at different redshifts, it is seen that although the break of the H-alpha luminosity function, L*, evolves by a factor of ~30 from z=0.24 to z=2.23, galaxies with the same L_H-alpha/L*(z) are found in dark matter haloes of similar masses, independently of cosmic time. This not only confirms that star-formation is more efficient at higher redshift, but also suggests a fundamental connection between the strong decrease of L* since z=2.23 and the quenching of star-formation in galaxies residing within dark-matter haloes significantly more massive than 10^12M_sun at any given epoch.
Operation and intrinsic error budget of a two-qubit cross-resonance gate

We analyze analytically, semi-analytically, and numerically the operation of Cross-Resonance (CR) gate for superconducting qubits (transmons). We find that a relatively simple semi-analytical method gives accurate results for the CNOT-equivalent gate duration and compensating single-qubit rotations. It also allows us to minimize the CNOT gate duration over the amplitude of the applied microwave drive and find dependence on the detuning between the qubits. However, full numerical simulations are needed to calculate intrinsic fidelity of the CR gate. We decompose numerical infidelity into contributions from various physical mechanisms, thus finding the intrinsic error budget. In particular, at small drive amplitudes the CR gate fidelity is limited by imperfections of the target-qubit rotations, while at large amplitudes it is limited by leakage. The gate duration and fidelity are analyzed numerically as functions of the detuning between qubits, their coupling, drive frequency, relative duration of pulse ramps, and microwave crosstalk. The effect of the echo sequence is also analyzed numerically. Our results show that the CR gate can provide intrinsic infidelity of less than $10^{-3}$ when a simple pulse shape is used.
Interplay between the small and the large scale structure of spacetime

Existence of frame invariant, maximum, time interval $T$, length $L$, and mass $M$ is postulated. In the de Sitter universe - (1) the life span of universe, (2) the circumference of universe at the point of maximum expansion, and (3) the mass of the universe - are candidates for $T$, $L$ and $M$ respectively. Impact of such invariant global parameters, on the definition of local physical quantities, such as velocity is discussed.
ournal of C osmology and A stroparticle hysics Constraints on modiﬁed gravity models from white dwarfs

Modiﬁed gravity theories can introduce modiﬁcations to the Poisson equation in the Newtonian limit. As a result, we expect to see interesting features of these modiﬁcations inside stellar objects. White dwarf stars are one of the most well studied stars in stellar astrophysics. We explore the eﬀect of modiﬁed gravity theories inside white dwarfs. We derive the modiﬁed stellar structure equations and solve them to study the mass-radius relationships for various modiﬁed gravity theories. We also constrain the parameter space of these theories from observations. singularities, serve as alternatives to dark / dark matter, solar and tests in compact The present paper is concerned with testing of four modiﬁed gravity theories against the physics of white dwarfs. These theories were initially proposed to address particular issue(s) and later on discussed in other astrophysical or cosmological scenarios. The scalar-vector-tensor gravity theory (STVG), also referred to as Modiﬁed Gravity (MOG) in the literature, was proposed by Moﬀat [2] as an extension to non-symmetric gravity theory (NGT) and the metric skew-tensor gravity theory (MTG), to explain ﬂattening of galaxy rotation curves without invoking dark matter [2, 3]. Later on Moﬀat and his collaborators studied the theory in the context of cluster dynamics [4], Bullet Cluster [5] and cosmology [2, 6] without considering the contributions from the dark matter component. Recently this theory has also been considered in the context of neutron stars [7] and recent observation of gravitational waves [8]. In all these settings the observations are claimed to be in good agreement with the theory.
Dense Molecular Clumps in the Envelope of the Yellow Hypergiant IRC+10420

The circumstellar envelope of the hypergiant star IRC+10420 has been traced as far out in as in 12CO J = 1–0 and 12CO J = 2–1, in dramatic contrast with the centrally condensed (thermal) SiO- but extended CO-emitting envelopes of giant and supergiant stars. We present an observation of the circumstellar envelope in that, when combined with the previous observation in , provides more stringent constraints on the density of the SiO-emitting gas than hitherto possible. The emission in peaks at a radius of ∼2″ whereas that in peaks at a smaller radius of ∼1″, giving rise to its ring-like appearance. The ratio of brightness temperature between and decreases from a value well above unity at the innermost measurable radius to about unity at a radius of ∼2″, beyond which this ratio remains approximately constant. Dividing the envelope into three zones as in models for the 12CO J = 1–0 and 12CO J = 2Dinh–1 emissions, we show that the density of the SiO-emitting gas is comparable with that of the CO-emitting gas in the inner zone but is at least an order of magnitude higher by comparison in both the middle and the outer zones. The SiO-emitting gas therefore originates from dense clumps, likely associated with the dust clumps seen in scattered optical light, surrounded by more diffuse CO-emitting interclump gas. We suggest that SiO molecules are released from dust grains due to shock interactions between the dense SiO-emitting clumps and the diffuse CO-emitting interclump gas.
Constraining spatial extent and temperature of dust around galaxies from far-infrared image stacking analysis

We propose a novel method to constrain the spatial extent of dust around galaxies through the measurement of dust temperature. Our method combines the dust emission of galaxies from far-infrared (FIR) image stacking analysis and the quasar reddening due to the dust absorption around galaxies. As a specific application of our method, we use the stacked FIR emission profiles of SDSS photometric galaxies over the IRAS 100$\mu$m map, and the recent measurement of the SDSS galaxy-quasar cross-correlation. If we adopt a single-temperature dust model, the resulting temperature is around 18K, which is consistent with a typical dust temperature for a central part of galaxies. If we assume an additional dust component with much lower temperature, the current data imply the temperature of the galactic dust needs to be higher, 20K to 30K. Since the model of the density and temperature distribution of dust adopted in the current paper is very simple, we cannot draw any strong conclusion at this point. Nevertheless our novel method with the elaborated theoretical model and multi-band measurement of dust will offer an interesting constraint on the statistical nature of galactic dust.
Geometric Microstates for the Three Dimensional Black Hole

We study microstates of the three dimensional black hole obtained by quantizing topologically non-trivial geometries behind the event horizon. In chiral gravity these states are found by quantizing the moduli space of bordered Riemann surfaces. In the semi-classical limit these microstates can be counted using intersection theory on the moduli space of punctured Riemann surfaces. We make a conjecture (supported by numerics) for the asymptotic behaviour of the relevant intersection numbers. The result is that the geometric microstates with fixed topology have an entropy which grows too slowly to account for the semiclassical Bekenstein-Hawking entropy. The sum over topologies, however, leads to a divergence. We conclude with some speculations about how this might be resolved to give an entropy proportional to horizon area.
Two-temperature, Magnetically Arrested Disc simulations of the jet from the supermassive black hole in M87

We present two-temperature, radiative general relativistic magnetohydrodynamic simulations of Magnetically Arrested Discs (MAD) that launch powerful relativistic jets. The mass accretion rates of our simulations are scaled to match the luminosity of the accretion flow around the supermassive black hole in M87. We consider two sub-grid prescriptions for electron heating: one based on a Landau-damped turbulent cascade, and one based on heating from trans-relativistic magnetic reconnection. The simulations produce jets with power on the order of the observed value for M87. Both simulations produce spectra that are consistent with observations of M87 in the radio, millimetre, and submillimetre. Furthermore, the predicted image core-shifts in both models at frequencies between 15 GHz and 86 GHz are consistent with observations. At 43 and 86 GHz, both simulations produce wide opening angle jets consistent with VLBI images. Both models produce 230 GHz images with distinct black hole shadows that are resolvable by the Event Horizon Telescope (EHT), though at a viewing angle of 17 degrees, the 230 GHz images are too large to match EHT observations from 2009 and 2012. The 230 GHz images from the simulations are dynamic on time-scales of months to years, suggesting that repeated EHT observations may be able to detect the motion of rotating magnetic fields at the event horizon.
Multi-lepton Signatures of a Hidden Sector in Rare B Decays

We explore the sensitivity of flavor-changing b{yields}s transitions to a (sub-) GeV hidden sector with generic couplings to the standard model through the Higgs, vector, and axion portals. The underlying two-body decays of B mesons, B{yields}X{sub s}S, and B{sup 0}{yields}SS, where S denotes a generic new GeV-scale particle, may significantly enhance the yield of monochromatic lepton pairs in the final state via prompt S{yields}ll decays. Existing measurements of the charged lepton spectrum in neutral-current semileptonic B decays provide bounds on the parameters of the light sector that are significantly more stringent than the requirements of naturalness. New search modes, such as B{yields}X{sub s}+n(ll) and B{sup 0}{yields}n(ll) with n{>=}2, can provide additional sensitivity to scenarios in which both the Higgs and vector portals are active, and are accessible to (super-) B factories and hadron colliders.
THE METALLICITY BIMODALITY OF GLOBULAR CLUSTER SYSTEMS: A TEST OF GALAXY ASSEMBLY AND OF THE EVOLUTION OF THE GALAXY MASS–METALLICITY RELATION

We build a theoretical model to study the origin of the globular cluster metallicity bimodality in the hierarchical galaxy assembly scenario. The model is based on empirical relations such as the galaxy mass–metallicity relation [O/H]–Mstar as a function of redshift, and on the observed galaxy stellar mass function up to redshift z ∼ 4. We make use of the theoretical merger rates as a function of mass and redshift from the Millennium simulation to build galaxy merger trees. We derive a new galaxy [Fe/H]–Mstar relation as a function of redshift, and by assuming that globular clusters share the metallicity of their original parent galaxy at the time of their formation, we populate the merger tree with globular clusters. We perform a series of Monte Carlo simulations of the galaxy hierarchical assembly, and study the properties of the final globular cluster population as a function of galaxy mass, assembly and star formation history, and under different assumptions for the evolution of the galaxy mass–metallicity relation. The main results and predictions of the model are the following. (1) The hierarchical clustering scenario naturally predicts a metallicity bimodality in the galaxy globular cluster population, where the metal-rich subpopulation is composed of globular clusters formed in the galaxy main progenitor around redshift z ∼ 2, and the metal-poor subpopulation is composed of clusters accreted from satellites, and formed at redshifts z ∼ 3–4. (2) The model reproduces the observed relations by Peng et al. for the metallicities of the metal-rich and metal-poor globular cluster subpopulations as a function of galaxy mass; the positions of the metal-poor and metal-rich peaks depend exclusively on the evolution of the galaxy mass–metallicity relation and the [O/Fe], both of which can be constrained by this method. In particular, we find that the galaxy [O/Fe] evolves linearly with redshift from a value of ∼0.5 at redshift z ∼ 4 to a value of ∼0.1 at z = 0. (3) For a given galaxy mass, the relative strength of the metal-rich and metal-poor peaks depends exclusively on the galaxy assembly and star formation history, where galaxies living in denser environments and/or early-type galaxies show a larger fraction of metal-poor clusters, while galaxies with a sparse merger history and/or late-type galaxies are dominated by metal-rich clusters. (4) The globular cluster metallicity bimodality disappears for galaxy masses around and below Mstar ∼ 109 M☉, and for redshifts z > 2.