Miracle-dz/UniFAR-FTUs huggingface dataset:
Biogeochemical Responses to Mixing of Glacial Meltwater and Hot Spring Discharge in the Mount St. Helens Crater

Environments where geothermal waters and glacier meltwater mix are common on Earth yet little is known about the biogeochemical processes that occur when hot, reduced geothermal water mixes with cold, oxidized glacial meltwater in natural systems. Mount St. Helens provides an ideal location to study the interaction between geothermal and glacier waters since the water sources, and their mixing environment in Step Creek, are exposed in the volcanic crater. We find that the two water sources contain distinct major ion, trace element, dissolved organic matter (DOM), and biological signatures. The hot spring contains high concentrations of biogeochemically reactive components (e.g., siderophile and chalcophile trace elements and DOM) compared to the glacier discharge but a large fraction of these solutes do not remain in solution after the waters mix. In contrast, glacier discharge contains fewer solutes but most of these solutes remain in solution after the waters mix. The mixing of glacier and hot spring water in Step Creek supports seston and benthic ecosystems that have higher phototrophic and microbial biomass than those in the source waters, suggesting that the mixing environment in this high‐gradient stream provide a more comprehensive suite of soluble and essential nutrients that promote primary production and DOM cycling.
Forthcoming Occultations of Astrometric Radio Sources by Planets

Astrometric observations of the radio source occultations by solar system bodies may be of large interest for testing gravity theories, dynamical astronomy, and planetary physics. In this paper, we present an updated list of the occultations of astrometric radio sources by planets expected in the nearest years. Such events, like the solar eclipses, generally speaking, can be only observed in a limited region. The map of the shadow path is provided for the events occurred in regions with several VLBI stations and hence the most interesting for radio astronomy experiments.
Acute Kidney Injury Following COVID-19 and Risk factors for Progression to Chronic Kidney Disease

Background: Acute kidney injury (AKI) is one of the frequent complications of COVID-19 infection. The predictors of progressive kidney disease for patients with COVID-19- associated AKI (COV-AKI) are unclear. In our study, we aimed to demonstrate the risk factors of non-recovery of COV-AKI. Method: COV-AKI developed in 901 of 3337 patients treated in our hospital for COVID-19 between April 1, 2020 and November 30, 2020. 331 of 901 patients with COV-AKI died at the hospital. Of these patients, 459 patients who met the inclusion criteria were included in the study, while 111 patients were excluded. At 3 months post-AKI, 399 of 459 cases (Group 1) recovered from AKI, and 60 (Group 2) did not. Results: The median age of the patients included in the study was 68 (59-76), and 44.9% (206) of them were women. Thirty-five of 60 patients in Group 2 developed de novo chronic kidney disease while 25 patients had a history of chronic kidney disease (CKD) and experienced a disease progression. We found that patients with low serum albumin levels (hypoalbuminemia) at admission (P<0.001) were associated with non-recovery of AKI or occurrence of CKD progression, in COV-AKI. Conclusions: Although the short-term outcomes of COV-AKI are relatively well-known, the long-term outcomes are needed to be clarified more. This study indicates hypoalbuminemia may be indicators of non-recovery in COV-AKI.
BeppoSAX Observation of NGC 3079

Using the BeppoSAX observatory, we have observed a nearby LINER/Seyfert 2 galaxy, NGC 3079, which is known as an outflow galaxy and a bright H2O maser source. Using the Phoswich Detection System, we have revealed that the NGC 3079 nucleus suffers from a Compton-thick absorption, with a hydrogen column density ~1025 cm-2. After corrected the absorption, the 2-10 keV luminosity becomes 1042-1043 ergs s-1 at a distance of 16 Mpc. It is 2-3 orders of magnitude higher than that observed in the Medium Energy Concentrator Spectrometer band (below 10 keV). We also detected a strong Fe K line at 6.4 keV with an equivalent width of 2.4 keV, which is consistent with the heavy absorption.
Mineralogy and Mineral Chemistry of Dioritic Dykes, Quartz Diorite Enclaves and Pyroxene of the Sungun Cu-Mo Porphyry Deposit, East Azerbaijan, Iran

The Sungun Cu-Mo porphyry deposit forms part of the Ahar–Arasbaran Magmatic Belt (AAMB). Its host Miocene porphyry stock is quartz monzonitic in composition and is cut by intermediate dykes that post-date mineralization. These dykes contain pyroxene and enclaves of ambiguous origin. Dykes of microdiorite are observed within quartz diorite dykes, whereas later diorite dykes contain three different kinds of enclaves (diorite, quartz diorite and hornfels) of sizes between 1 and 10 cm. Enclaves consist of plagioclase, hornblende and biotite, with accessory sphene, quartz and apatite. Chlorite compositions in microdiorite are within the chamosite range, whereas they are within the clinochlore range in diorite enclaves. Microprobe analyses of pyroxene indicate an augitic composition (Fs13.38-22.79Wo29.1-33.57En48.53-56.61), consistent with an igneous origin. Hornblende of the diorite enclaves formed at pressures ranging between 3 and 5.3 kilobars and temperatures between 714 and 731 °C. Average oxygen fugacity during rock formation is −14.75. Such high oxygen fugacities suggest that the diorite formed near the boundaries of a convergent margin. Amphibole compositions suggest that the diorite enclaves are sub-alkaline to mildly alkaline, consistent with reported whole-rock chemistry of the Sungun magmas. Pyroxenes were formed at pressures ranging between 11 and 15 kilobars (33–45 km) and temperatures between 1100 and 1400 °C. The amount of Fe3+ in clinopyroxene is also consistent with high oxygen fugacity within their environment of crystallization. Overall, these results have implications for our understanding of the origin of the Sungun Cu-Mo porphyry magmas and their mineral deposits in a lower-crustal setting.
Distribution of canonical determinants in QCD

The distribution of canonical determinants in QCD is determined by means of chiral perturbation theory. For a non-zero quark charge the canonical determinants take complex values. In the dilute pion gas approximation, we compute all moments of the magnitude of the canonical determinants, as well as the first nonvanishing moments of the real and imaginary parts. The non-trivial cancellation between the real and the imaginary parts of the canonical determinants is derived and the signal to noise ratio is discussed. The analytical distributions are compared to lattice data. The average density of the magnitude of the canonical determinants is determined as well and is shown to be given by a variant of the log-normal distribution.
THE CLUSTERING OF RADIO GALAXIES: BIASING AND EVOLUTION VERSUS STELLAR MASS

We study the angular clustering of ∼6 × 105 NVSS sources on scales ≳ 50 h - 1 Mpc ? > in the context of the ΛCDM scenario. The analysis partially relies on the redshift distribution of 131 radio galaxies, inferred from the Hercules and CENSORS survey, and an empirical fit to the stellar-to-halo mass relation. For redshifts z ≲ 0.7, the fraction of radio activity versus stellar mass evolves as f RL ∼ M * &agr; 0 + &agr; 1 z ? > , where α0 = 2.529 ± 0.184 and &agr; 1 = 1.854 − 0.761 + 0.708 . > The estimate on α0 is largely driven by the results of Best et al., while the constraint on α1 is new. We derive a biasing factor b ( z = 0.5 ) = 2.093 − 0.109 + 0.164 ? > between radio galaxies and the underlying mass. The function b ( z ) = 0.33 z 2 + 0.85 z + 1.6 ? > fits well the redshift dependence. We also provide convenient parametric forms for the redshift-dependent radio luminosity function, which are consistent with the redshift distribution and the NVSS source count versus flux.
Identification of Single and Combined Serum Metabolites Associated with Food Intake

Assessment of dietary intake is challenging. Traditional methods suffer from both random and systematic errors; thus objective measures are important complements in monitoring dietary exposure. The study presented here aims to identify serum metabolites associated with reported food intake and to explore whether combinations of metabolites may improve predictive models. Fasting blood samples and a 4-day weighed food diary were collected from healthy Swedish subjects (n = 119) self-defined as having habitual vegan, vegetarian, vegetarian + fish, or omnivore diets. Serum was analyzed for metabolites by 1H-nuclear magnetic resonance spectroscopy. Associations between single and combined metabolites and 39 foods and food groups were explored. Area under the curve (AUC) was calculated for prediction models. In total, 24 foods or food groups associated with serum metabolites using the criteria of rho > 0.2, p < 0.01 and AUC ≥ 0.7 were identified. For the consumption of soybeans, citrus fruits and marmalade, nuts and almonds, green tea, red meat, poultry, total fish and shellfish, dairy, fermented dairy, cheese, eggs, and beer the final models included two or more metabolites. Our results indicate that a combination of metabolites improve the possibilities to use metabolites to identify several foods included in the current diet. Combined metabolite models should be confirmed in dose–response intervention studies.
X-RAY DETERMINATION OF THE VARIABLE RATE OF MASS ACCRETION ONTO TW HYDRAE

Diagnostics of electron temperature (Te), electron density (ne), and hydrogen column density (NH) from the Chandra High Energy Transmission Grating spectrum of He-like Ne ix in TW Hydrae (TW Hya), in conjunction with a classical accretion model, allow us to infer the accretion rate onto the star directly from measurements of the accreting material. The new method introduces the use of the absorption of Ne ix lines as a measure of the column density of the intervening, accreting material. On average, the derived mass accretion rate for TW Hya is 1.5 × 10−9 M☉ yr−1, for a stellar magnetic field strength of 600 G and a filling factor of 3.5%. Three individual Chandra exposures show statistically significant differences in the Ne ix line ratios, indicating changes in NH, Te, and ne by factors of 0.28, 1.6, and 1.3, respectively. In exposures separated by 2.7 days, the observations reported here suggest a five-fold reduction in the accretion rate. This powerful new technique promises to substantially improve our understanding of the accretion process in young stars.
COMPACT PLANETARY SYSTEMS PERTURBED BY AN INCLINED COMPANION. I. VECTORIAL REPRESENTATION OF THE SECULAR MODEL

The non-resonant secular dynamics of compact planetary systems are modeled by a perturbing function that is usually expanded in eccentricity and absolute inclination with respect to the invariant plane. Here, the expressions are given in a vectorial form which naturally leads to an expansion in eccentricity and mutual inclination. The two approaches are equivalent in most cases, but the vectorial one is specially designed for those cases where an entire quasi-coplanar system tilts to a large degree. Moreover, the vectorial expressions of the Hamiltonian and of the equations of motion are slightly simpler than those given in terms of the usual elliptical elements. We also provide the secular perturbing function in vectorial form expanded in semi-major axis ratio allowing for arbitrary eccentricities and inclinations. The interaction between the equatorial bulge of a central star and its planets is also provided, as is the relativistic periapse precession of any planet induced by the central star. We illustrate the use of this representation to follow the secular oscillations of the terrestrial planets of the solar system and for Kozai cycles which may take place in exoplanetary systems.
Behavior of high-burnup BWR UO2 fuel with additives under reactivity-initiated accident conditions

ABSTRACT Fuels with additives are expected to provide enhanced fuel performance in fission gas retention owing to their large grain size, which elongates fission gas migration path. To investigate behavior of the fuels during a reactivity-initiated accident (RIA), RIA-simulated experiments OS-1 and LS-4 were performed on ADOPT (chromia- and alumina-doped UO2) fuel of 64 GWd/t and chromia-doped UO2 fuel of 48 GWd/t, respectively. The OS-1 rod failed at a fuel enthalpy increase of 160 J/g due to pellet–cladding mechanical interaction failure, which was the lowest failure limit among the test results ever obtained at the NSRR on high-burnup fuels from 40 to 65 GWd/tU. Comparison of the hydride morphologies in the cladding metallic layer between the rods subjected to the past NSRR tests suggests the contribution of radially oriented hydrides during base irradiation to the low failure limit. The LS-4 rod survived for a peak fuel enthalpy increase of 549 J/g, which resulted in cladding deformation of ~2.4% in the residual hoop strain and FGR of 1.4–6.1%. Whereas the low fission gas release exhibits the effect of additives, the cladding deformation is within the range explained by the deformation mechanism essentially identical to those recognized for high-burnup undoped fuels. Graphical Abtsract
Tissue-based diagnosis of systemic amyloidosis: Experience of the informal diagnostic center at Uppsala University Hospital

Diagnosis of systemic amyloidosis is a clinical challenge and usually relies on a tissue biopsy. We have developed diagnostic methods based on the presence of amyloid deposits in abdominal subcutaneous fat tissue. This tissue is also used to determine the biochemical type of amyloidosis, performed by western blot and immunohistochemical analyses with the aid of in-house developed rabbit antisera and mouse monoclonal antibodies. Mass spectrometric methods are under development for selected cases. The diagnostic outcome for 2018-2020 was studied. During this period, we obtained 1,562 biopsies, of which 1,397 were unfixed subcutaneous fat tissue with varying degrees of suspicion of systemic amyloidosis. Of these, 440 contained amyloid deposits. The biochemical nature of the amyloid was determined by western blot analysis in 319 specimens and by immunohistochemistry in further 51 cases.
In vitro Study of Moringa oleifera Lam. Leaf Extract Fractions against Multidrug-resistant Pseudomonas aeruginosa Strains from Surgical Wound Infections

Pseudomonas aeruginosa is an opportunistic pathogen that can cause serious surgical site infections and remains a major dilemma, especially in developing country like Nigeria. This issue has led to investigation of the antibacterial activity of Moringa oleifera leaf extract against multidrug-resistant (MDR) Pseudomonas aeruginosa strains. Pseudomonas aeruginosa strains were isolated from postoperative wounds at the two sites used in the study (Central Hospital, Benin and University of Benin Teaching Hospital) and antibiotic susceptibility testing was performed to identify MDR isolates. A qualitative phytochemical screening of leaves was performed using standard methods, followed by antibacterial testing of various M. oleifera leaf extracts against selected multidrug-resistant isolates. Results showed that 99 (35%) of the patients examined had wound infections, out of a total of 284 specimens collected. Thirty-four (54.8%) P. aeruginosa strains showed multidrug-resistance capacity from both learning sites. Qualitative analysis of phytochemicals revealed the presence of flavonoids, phenols, saponins, steroids, tannins and terpenoids. In vitro results of antibacterial tests showed that ethyl acetate extract from leaves of Moringa oleifera had the highest antibacterial activity against Pseudomonas aeruginosa strain Iraq.PA-9, followed by dichloromethane at a concentration of 100 mg/ml. The different effects may be attributed to secondary plant substances contained in different leaf extracts of Moringa oleifera. The results of this study demonstrated the potential of Moringa oleifera leaf extract as an antibacterial agent by inhibiting the growth of test organisms isolated from postoperative wound infections.
[S iv] IN THE NGC 5253 SUPERNEBULA: IONIZED GAS KINEMATICS AT HIGH RESOLUTION

The nearby dwarf starburst galaxy NGC 5253 hosts a deeply embedded radio-infrared supernebula excited by thousands of O stars. We have observed this source in the 10.5 μm line of S+3 at 3.8 km s−1 spectral and 1. ″4 spatial resolution, using the high-resolution spectrometer TEXES on the IRTF. The line profile cannot be fit well by a single Gaussian. The best simple fit describes the gas with two Gaussians, one near the galactic velocity with FWHM 33.6 km s−1 and another of similar strength and FWHM 94 km s−1 centered ∼20 km s−1 to the blue. This suggests a model for the supernebula in which gas flows toward us out of the molecular cloud, as in a “blister” or “champagne flow” or in the H ii regions modelled by Zhu.
EXAMINING THE RADIO-LOUD/RADIO-QUIET DICHOTOMY WITH NEW CHANDRA AND VLA OBSERVATIONS OF 13 UGC GALAXIES

We present the results from new ∼15 ks Chandra-ACIS and 4.9 GHz Very Large Array (VLA) observations of 13 galaxies hosting low-luminosity active galactic nuclei (AGNs). This completes the multiwavelength study of a sample of 51 nearby early-type galaxies described in Capetti & Balmaverde and Balmaverde & Capetti. The aim of the three previous papers was to explore the connection between the host galaxies and AGN activity in a radio-selected sample. We detect nuclear X-ray emission in eight sources and radio emission in all but one (viz., UGC 6985). The new VLA observations improve the spatial resolution by a factor of 10: the presence of nuclear radio sources in 12 of the 13 galaxies confirms their AGN nature. As previously indicated, the behavior of the X-ray and radio emission in these sources depends strongly on the form of their optical surface brightness profiles derived from Hubble Space Telescope imaging, i.e., on their classification as “core,” “power-law,” or “intermediate” galaxies. With more than twice the number of “power-law” and “intermediate” galaxies compared to previous work, we confirm with a much higher statistical significance that these galaxies lie well above the radio–X-ray correlation established in Fanaroff–Riley type I radio galaxies and the low-luminosity “core” galaxies. This result highlights the fact that the “radio-loud/radio-quiet” dichotomy is a function of the host galaxy's optical surface brightness profile. We present radio–optical–X-ray spectral indices for all 51 sample galaxies. Survival statistics point to significant differences in the radio-to-optical and radio-to-X-ray spectral indices between the “core” and “power-law” galaxies (Gehan's Generalized Wilcoxon test probability p for the two classes being statistically similar is <10−5), but not in the optical-to-X-ray spectral indices (p = 0.25). Therefore, the primary difference between the “core” and “power-law” galaxies is in their ability to launch powerful radio outflows. This result is consistent with the hypothesis of different formation processes and evolution histories in “core” and “power-law” galaxies: major mergers are likely to have created “core” galaxies, while minor mergers were instrumental in the creation of “power-law” galaxies.
Witten effect in a crystalline topological insulator

It has been noted a long time ago that a term of the form theta(e{sup 2}/2pih)Bcentre dotE may be added to the standard Maxwell Lagrangian without modifying the familiar laws of electricity and magnetism. theta is known to particle physicists as the 'axion' field and whether or not it has a nonzero expectation value in vacuum remains a fundamental open question of the standard model. A key manifestation of the axion term is the Witten effect: a unit magnetic monopole placed inside a medium with thetanot =0 is predicted to bind a (generally fractional) electric charge -e(theta/2pi+n) with n integer. Here we conduct a test of the Witten effect based on the recently established fact that the axion term with theta=pi emerges naturally in the description of the electromagnetic response of a class of crystalline solids called topological insulators--materials distinguished by strong spin-orbit coupling and nontrivial band structures. Using a simple physical model for a topological insulator we demonstrate the existence of a fractional charge bound to a monopole by an explicit numerical calculation. We also propose a scheme for generating an 'artificial' magnetic monopole in a topological insulator film that may be used to facilitate an experimental test ofmore » Witten's prediction. « less
Thermodynamics of Fermi gases in three dimensional fuzzy space

We use the recently derived density of states for a particle confined to a spherical well in three dimensional fuzzy space to compute the thermodynamics of a gas of non-interacting fermions confined to such a well. Special emphasis is placed on non-commutative effects and in particular non-commutative corrections to the thermodynamics at low densities and temperatures are computed where the non-relativistic approximation used here is valid. Non-commutative effects at high densities are also identified, the most prominent being the existence of a minimal volume at which the gas becomes incompressible. The latter is closely related to a low/high density duality exhibited by these systems, which in turn is a manifestation of an infra-red/ultra violet duality in the single particle spectrum. Both non-rotating and slowly rotating gasses are studied. Approximations are benchmarked against exact numerical computations for the non-rotating case and several other properties of the gas are demonstrated with numerical computations. Finally, a non-commutative gas confined by gravity is studied and several novel features regarding the mass-radius relation, density and entropy are highlighted.
ORBITAL MIGRATION OF PROTOPLANETS IN A MARGINALLY GRAVITATIONALLY UNSTABLE DISK

Core accretion and disk instability require giant protoplanets to form in the presence of disk gas. Protoplanet migration models generally assume disk masses low enough that the disk's self-gravity can be neglected. However, disk instability requires a disk massive enough to be marginally gravitationally unstable (MGU). Even for core accretion, an FU Orionis outburst may require a brief MGU disk phase. We present a new set of three-dimensional, gravitational radiation hydrodynamics models of MGU disks with multiple protoplanets, which interact gravitationally with the disk and with each other, including disk gas mass accretion. Initial protoplanet masses are 0.01 to 10 M⊕ for core accretion models, and 0.1 to 3 MJup for Nice scenario models, starting on circular orbits with radii of 6, 8, 10, or 12 AU, inside a 0.091 M☉ disk extending from 4 to 20 AU around a 1 M☉ protostar. Evolutions are followed for up to ∼4000 yr and involve phases of relative stability (e ∼ 0.1) interspersed with chaotic phases (e ∼ 0.4) of orbital interchanges. The 0.01 to 10 M⊕ cores can orbit stably for ∼1000 yr: monotonic inward or outward orbital migration of the type seen in low mass disks does not occur. A system with giant planet masses similar to our solar system (1.0, 0.33, 0.1, 0.1 MJup) was stable for over 1000 yr, and a Jupiter-Saturn-like system was stable for over 3800 yr, implying that our giant planets might well survive an MGU disk phase.