Initial Mass Research Articles

Eruptive novae in symbiotic systems

ABSTRACT We conduct numerical simulations of multiple nova eruptions in detached, widely separated symbiotic systems that include an asymptotic giant branch (AGB) companion to investigate the impact of white dwarf (WD) mass and binary separation on the evolution of the system. The accretion rate is determined using the Bondi–Hoyle–Lyttleton method, incorporating orbital momentum loss caused by factors such as gravitational radiation, magnetic braking, and drag. The WD in such a system accretes matter coming from the strong wind of an AGB companion until it finishes shedding its envelope. This occurs on an evolutionary time-scale of ≈3 × 105 yr. Throughout all simulations, we use a consistent AGB model with an initial mass of 1.0 M⊙ while varying the WD mass and binary separation, as they are the critical factors influencing nova eruption behaviour. We find that the accretion rate fluctuates between high and low rates during the evolutionary period, significantly impacted by the AGB’s mass loss rate. We show that unlike novae in cataclysmic variables, the orbital period may either increase or decrease during evolution, depending on the model, while the separation consistently decreases. Furthermore, we have identified cases in which the WDs produce weak, non-ejective novae and experience mass gain. This suggests that provided the accretion efficiency can be achieved by a more massive WD and maintained for long enough, they could potentially serve as progenitors for type Ia supernovae.

On the core-collapse supernova explanation for LAMOST J1010 + 2358

ABSTRACT Low-metallicity very massive stars with an initial mass of ∼140–$260\, \mathrm{M}_\odot$ are expected to end their lives as pair-instability supernovae (PISNe). The abundance pattern resulting from a PISN differs drastically from regular core-collapse supernova (CCSN) models and is expected to be seen in very metal-poor (VMP) stars of [Fe/H] ≲ −2. Despite the routine discovery of many VMP stars, the unique abundance pattern expected from PISNe has not been unambiguously detected. The recently discovered VMP star LAMOST J1010 + 2358, however, shows a peculiar abundance pattern that is remarkably well fit by a PISN, indicating the potential first discovery of a bonafide star born from gas polluted by a PISN. In this paper, we study the detailed nucleosynthesis in a large set of models of CCSN of Pop III and Pop II star of metallicity [Fe/H] = −3 with masses ranging from 12 to $30\, \mathrm{M}_\odot$. We find that the observed abundance pattern in LAMOST J1010 + 2358 can be fit at least equally well by CCSN models of ∼12–$14\, \mathrm{M}_\odot$ that undergo negligible fallback following the explosion. The best-fitting CCSN models provide a fit that is even marginally better than the best-fitting PISN model. We conclude the measured abundance pattern in LAMOST J1010 + 2358 could have originated from a CCSN and therefore cannot be unambiguously identified with a PISN given the set of elements measured in it to date. We identify key elements that need to be measured in future detections in stars like LAMOST J1010 + 2358 that can differentiate between CCSN and PISN origin.

Mechanistic Insights into Ferroptotic Cell Death in Pancreatic Islets.

Ferroptosis was recently identified as a non-apoptotic, iron-dependent cell death mechanism that is involved in various pathologic conditions. There is first evidence for its significance also in the context of islet isolation and transplantation. Transplantation of pancreatic human islets is a viable treatment strategy for patients with complicated diabetes mellitus type 1 (T1D) that suffer from severe hypoglycemia. A major determinant for functional outcome is the initial islet mass transplanted. Efficient islet isolation procedures and measures to minimize islet loss are therefore of high relevance. To this end, better understanding and subsequent targeted inhibition of cell death during islet isolation and transplantation is an effective approach. In this study, we aimed to elucidate the mechanism of ferroptosis in pancreatic islets. Using a rodent model, isolated islets were characterized relating to the effects of experimental induction (RSL3) and inhibition (Fer1) of ferroptotic pathways. Besides viability, survival, and function, the study focused on characteristic ferroptosis-associated intracellular changes such as MDA level, iron concentration and the expression of ACSL4. The study demonstrates that pharmaceutical induction of ferroptosis by RSL3 causes enhancement of oxidative stress and leads to an increase of intracellular iron, zinc and MDA concentration, as well as the expression of ACSL4 protein. Consequently, a massive reduction of islet function, viability, and survival was found. Fer1 has the potential to inhibit and attenuate these cellular changes and thereby protect the islets from cell death.

Are the ultra-high-redshift galaxies at z > 10 surprising in the context of standard galaxy formation models?

ABSTRACT A substantial number of ultra-high redshift (8 ≲ z ≲ 17) galaxy candidates have been detected with JWST, posing the question: Are these observational results surprising in the context of current galaxy formation models? We address this question using the well-established Santa Cruz semi-analytic models, implemented within merger trees from the new suite of cosmological N-body simulations gureft, which were carefully designed for ultra-high redshift studies. Using our fiducial models calibrated at z = 0, we present predictions for stellar mass functions, rest-frame UV luminosity functions, and various scaling relations. We find that our (dust-free) models predict galaxy number densities at z ∼ 11 (z ∼ 13) that are an order of magnitude (a factor of ∼30) lower than the observational estimates. We estimate the uncertainty in the observed number densities due to cosmic variance, and find that it leads to a fractional error of ∼20–30 per cent at z = 11 (∼30–80 per cent at z = 14) for a 100 arcmin2 field. We explore which processes in our models are most likely to be rate-limiting for the formation of luminous galaxies at these early epochs, considering the halo formation rate, gas cooling, star formation, and stellar feedback, and conclude that it is mainly efficient stellar-driven winds. We find that a modest boost of a factor of ∼4 to the UV luminosities, which could arise from a top-heavy stellar initial mass function, would bring our current models into agreement with the observations. Adding a stochastic component to the UV luminosity can also reconcile our results with the observations.

Использование метода дискретных элементов для имитационного моделирования выемки угля очистным комбайном

Timulation modeling as a method of studying complex technological processes is successfully used in mining. Due to the creation of digital models, it is possible to estimate and improve the efficiency of technical and organizational solutions used in difficult mining and geological conditions. The article describes the development of a simulation model of coal extraction by a shearer and its transportation to an armored conveyer. Fragmentation of a high coal seam was simulated under the action of the cutting planes of the shearer. The created model in the Rocky DEM simulation environment takes into account the physical and mechanical properties of materials and 3D structures of mining equipment. The method of discrete elements was used as a mathematical tool for computing fragmentation of the coalbed, which helped to perform the computing without loss of the initial mass and volume of the materials. During the validation of the simulation model, a series of tests were carried out to determine the angle of natural slope of non-spherical coal particles close in granulometric composition to the mass formed during the fragmentation of the coalbed. Based on the test results, an array of values of coal particle adhesion parameters was obtained, which allows conducting simulation studies in conditions of existing and projected coal mines.

Comprehensive study of optical, thermal, and gamma-ray shielding properties of Bi2O3–ZnO–PbO–B2O3 glasses

Abstract The Bi2O3–ZnO–PbO–B2O3 (BiZPB) glasses are prepared using the melt-quenching technique. As the concentration of lead oxide increases, the band gap energy (E g) decreases from 2.864 to 2.671 eV. The BiZPB glasses exhibit remarkable stability under thermal stress, as indicated by the thermogravimetric analysis graph, with only a marginal 0.5% loss in their initial mass. The decrease in the glass transition temperature (T g) of BiZPB glasses, with an increase in the PbO concentration, can be attributed to the specific influence of PbO on the glass structure and properties. The radiation shielding performance for the prepared glasses is evaluated using Phy-X software. The transmission factor (TF) for the 10B2O3–10ZnO–40PbO–40B2O3 glass sample is almost zero at 0.122 MeV, which means that this glass sample can attenuate almost all the photons with an energy of 0.122 MeV, whereas the TF values for this sample with thicknesses of 0.5 and 1 cm are 88 and 77%, respectively., it can be observed from the TF values that the prepared glasses have good attenuation performance against low energy (0.122, 0.245, and 0.344 MeV), while they have weak shielding performance against high energy radiation. The addition of PbO causes a reduction in TF, which means that the addition of an extra amount of PbO into the glasses results in an enhancement in the radiation shielding competence of the samples. The average half-value layer ( HVL ̅ \bar{{\rm{HVL}}} ) is also calculated. The results demonstrated that HVL ̅ \bar{{\rm{HVL}}} is at its lowest between 0.248 and 0.411 MeV, ranging between 0.396 and 0.513 cm.

Chronic anthropogenic disturbance alters litter decomposition and nutrient concentrations and stocks across a Caatinga dry forest chronosequence

Litter decomposition plays a key role in the cycling and storage of nutrients in terrestrial ecosystems. However, very little is known about decomposition processes and their underlying drivers in tropical dry forests, particularly in human-modified landscapes. Here, we evaluate decomposition rates and nutrient concentrations and stocks in the litter of a Caatinga dry forest chronosequence, in northeast Brazil. Litter decomposition was monitored for a year across forest stands of varying ages and old-growth forests. The litter decomposition rate was highly variable across forest stands, although on average decomposition occurred slowly, with approximately 50% of the initial litter mass still present after one year. The decomposition rate is responsive to forest type and negatively affected by chronic disturbance. Litter nutrient concentration decreased along the decomposition process, exhibiting a nutrient-specific mineralization rate. Response to drivers was also nutrient specific, with precipitation and chronic disturbances playing prominent roles. Nutrient stocks in the remaining litter were higher in old-growth forests, and final stocks of certain nutrients also responded to multiple drivers. Our results suggest that the Caatinga dry forest experiences a slow rate of litter decomposition and mineralization, although rates exhibit considerable variability across forest stands and environmental conditions. Thus, chronic disturbance plays a role by either facilitating or reducing litter decomposition, mineralization rate, and the stocks transferred to the soil. Consequently, these factors have implications for nutrient availability, including goat consumption and subsequent loss of nutrients.

Initial-final mass relation from white dwarfs within 40 pc

ABSTRACT We present an initial-final mass relation derived from the spectroscopically complete volume-limited 40 pc sample of white dwarfs. The relation is modelled using population synthesis methods to derive an initial stellar population which can be fit to the observed mass distribution of white dwarfs. The population synthesis accounts for binary evolution, where higher mass white dwarfs are more likely to be merger products than their lower mass counterparts. Uncertainties are accounted from the initial mass function, stellar metallicity, and age of the Galactic disc. We also consider biases induced by the spectral type of the white dwarf where pure-hydrogen atmosphere white dwarfs are likely to have more accurate masses, whilst the full white dwarf sample will have fewer biases arising from spectral evolution. We provide a four-piece segmented linear regression using Monte Carlo methods to sample the 1-σ range of uncertainty on the initial stellar population. The derived initial-final mass relation provides a self-consistent determination of the progenitor mass for white dwarfs in the Solar neighbourhood which will be useful to study the local stellar formation history.

The role of dietitian follow-ups on nutritional outcomes post–bariatric surgery

BackgroundCurrent evidence recommends dietary counselling with a registered dietitian (RD) for successful weight loss after metabolic bariatric surgery; however, there are limited data on the effect of RD follow-ups on micronutrient deficiencies. This study evaluated the effects of the number of postoperative RD visits on nutritional outcomes, including weight loss and micronutrient deficiencies. ObjectivesThe aim of this study was to evaluate the effects of the number of postoperative registered dietitian visits on nutritional outcomes, including weight loss and micronutrient deficiencies after metabolic and bariatric surgery. SettingCleveland Clinic Abu Dhabi, United Arab Emirates MethodsThis retrospective study included patients who underwent bariatric surgery between September 2015 and June 2020. Demographics, weight loss, micronutrients, and the number of postoperative RD visits were evaluated. Baseline and 12-month postsurgery outcomes were compared based on the number of RD follow-ups. ResultsA total of 174 primary and 46 revisions were included. Patients were 73.6% female, with a mean age of 40 years. The initial mean body mass index was 42.8 kg/m2. Number of RD visits were as follows: 0–1 (39 patients), 2 (59 patients), 3 (55 patients), and 4 or more (67 patients). Baseline (pre-operative) micronutrient values were within normal range. In comparison with the reference group (REF = 0–1 post-op RD visits), patients with 3 RD visits had 7% higher total body weight loss (P < .001) and maintained micronutrients within the normal range at 12 months postoperative. Mean differences in postoperative values were statistically significant (P < .05) for weight, vitamin B12, and vitamin D but not for hemoglobin, ferritin, calcium, folate, vitamin B1, copper, and zinc. ConclusionOur study suggests that three or more RD visits during the first 12 months after bariatric surgery are associated with improved outcomes, including significant percent total body weight loss and lower rates of micronutrient deficiencies.

Radiotherapy Consolidation Reduces Risk of Relapse in Diffuse Large B-Cell Lymphoma Patients with Bulky Disease in Complete Response after Frontline Immunochemotherapy: Results from a Retrospective Single Center Study

INTRODUCTION: The role of radiotherapy (RT) consolidation upfront in patients with diffuse large B-cell lymphoma (DLBCL) and bulky disease at diagnosis is controversial, especially in those in complete response (CR) after immunochemotherapy. METHODS: All patients with DLBCL diagnosed between January 2010 and June 2021 at AOU Città della Salute e della Scienza di Torino and treated frontline with RCHOP-like regimens were retrospectively selected. Patients with primary mediastinal lymphoma were excluded. Clinical and biological features as well as treatment and survival data for the whole population were collected. All patients with bulky disease (defined as ≥6 cm) at diagnosis who obtained CR (defined as PET/TC Deauville score ≤ 3) at the end of systemic treatment were further selected. Progression free survival (PFS) and overall survival (OS) were compared between patients receiving consolidative RT on initial bulky mass and those who did not. RESULTS: A total of 453 patients with DLBCL were identified. Median age was 68 years (IQR 58-77), 56% were males, 74% stage ≥3, 52% IPI ≥3. 140/451 (31%) had bulky disease at diagnosis. Median follow-up was 5 years. 5-year PFS and OS for the whole cohort were 59% and 66%, respectively. Bulky disease correlated with a significantly lower 5-year PFS (bulky 50% vs no bulky 64%, p = 0.0005) and OS (bulky 68% vs no bulky 60%, p = 0.01). 82 out of 140 patients with bulky disease (68/82 with a bulky ≥7 cm) were in CR after immunochemotherapy: 19/82 (23%) received RT (16/19 on bulky ≥7 cm), 63/82 (77%) did not (55/63 with a bulky ≥7 cm). There were no significant differences between the two groups regarding age, stage, ECOG PS, LDH levels, extranodal involvement and IPI. RT dose was 30 Gy in most patients (17/19); two patients received 36 Gy and 40 Gy. The 5-year PFS was 95% in the RT cohort and 58% in the no-RT cohort (p = 0.004); the 5-y OS was 95% in the RT cohort and 69% in the no-RT cohort (p = 0.038) (figure 1). A propensity score matching analysis confirmed the benefit of RT on PFS (HR 0.1, 95% CI 0.01-0.68, p = 0.019), and showed a non-statistically significant trend of better OS (p = 0.06). 14/24 relapses in the no-RT cohort occurred on the site of bulky disease. CONCLUSIONS: With the limit of a non-randomized retrospective study, our data showed a benefit of RT consolidation on bulky disease in patients with DLBCL in RC after frontline immunochemotherapy, significantly prolonging PFS and with a trend of improved OS in a propensity score matching analysis.

Taking the Milky Way for a spin: disc formation in the artemis simulations

ABSTRACT We investigate the formation (spin-up) of galactic discs in the artemis simulations of Milky Way (MW)-mass galaxies. In almost all galaxies, discs spin up at higher [Fe/H] than the MW. Those galaxies that contain an analogue of the Gaia Sausage-Enceladus (GSE) spin up at a lower average metallicity than those without. We identify six galaxies with spin-up metallicity similar to that of the MW, which formed their discs ∼8–11 Gyr ago. Five of these experience a merger similar to the GSE. The spin-up times correlate with the halo masses at early times: galaxies with early spin-up have larger virial masses at a lookback time tL = 12 Gyr. The fraction of stars accreted from outside the host galaxy is smaller in galaxies with earlier spin-ups. Accreted fractions small enough to be comparable to the MW are only found in galaxies with the earliest disc formation and large initial virial masses (M200c ≈ 2 × 1011 M⊙ at tL = 12 Gyr). We find that discs form when the halo’s virial mass reaches a threshold of M200c ≈ (6 ± 3) × 1011 M⊙, independent of the spin-up time. However, the failure to form a disc in other galaxies appears to be instead related to mergers at early times. We also find that discs form when the central potential is not particularly steep. Our results indicate that the MW assembled its mass and formed its disc earlier than the average galaxy of a similar mass.

Interphase of polyoctenamer‐single‐wall carbon nanotubes by thermogravimetric analysis in air

AbstractNon‐isothermal thermogravimetric analysis in air, of polyoctenamer‐single wall carbon nanotubes (PO‐SWNTs), loaded by various amounts of SWNTs up to 10% wt., at different heating rates (ranging from 5 to 40°C/min) is reported. The thermal degradation in the air of PO_SWNTs is dominated by a main single sigmoidal dependence, assigned to the polymer and eventually polymer‐nanofiller interphase, over which a weaker sigmoid assigned to the thermo‐oxidative degradation of the nanofiller is superimposed at higher temperatures. The temperature at which the nanocomposite's residual mass fraction reaches x% wt. of the initial mass, Tx%, is reported (for x = 5, 50, and 85). The dependence of Tx% on the heating rate and the loading by nanotubes is analyzed. The temperature derivative of the thermograms defines new parameters (inflection residual mass fraction and inflection temperature) and (degradation) width. Their dependence on the loading by SWNTs was reported. Estimation of the interphase in polymer‐based nanocomposites is based on the postulate that the dependence of the inflection temperature on the composition of the nanocomposite obeys a Fox‐like dependence, where the bulk polymer and the polymer trapped within the interphase are considered as a blend of two miscible polymers. Complementary Raman, x‐ray diffraction, and differential scanning calorimetry support these results.

Substantiation of technological resource-saving conditions for the use of equipment in the sand deposit mining

The mining and technological features of the Gusarovsky deposit of molding sands mining under the conditions of technological limitations of the existing enterprise have been studied. The granulometric composition of balance reserve sands, as well as overburden rocks, was analyzed. In order to obtain a high-quality commercial product with a minimum content of fine and clay particles from the initial rock mass of the surface and watered ledges, the parameters of the hydromechanized complex were substantiated by mining and processing. The calculation is based on the three most available options for filling the mining and processing complex (MPC). To substantiate the rational parameters of the MPC and ensure the purification of the commercial product from fine impurities, a graphical characteristic of the hydraulic vertical classifier GKCD2000 was constructed when supplying clean water and at a slurry concentration of 10%. The graphical characteristics of hydraulic transport systems were constructed in accordance with the design diagrams of the accepted variants of the complex. To substantiate the rational parameters of the pumping station, the characteristics of the mining and processing complex were constructed when pumping clean water and slurry at a concentration of 10%. For the first time, the rational parameters of the technological complex of mining and processing, consisting of a suction dredger – a transport slurry pipeline – and a vertical hydraulic classifier GKCD2000, have been substantiated. The development of a technological complex of mining and processing will allow the existing enterprise to continue developing the deposit and obtaining high-quality commercial products under the conditions of technological limitations.

How to make giant planets via pebble accretion

Planet formation is directly linked to the birthing environment that protoplanetary disks provide. The disk properties determine whether a giant planet will form and how it evolves. The number of exoplanet and disk observations is consistently rising, however, it is not yet possible to directly link these two populations. Therefore, a deep theoretical understanding of how planets form is crucial. Giant planets are not the most common exoplanets, but their presence in a disk can have significant consequences for the evolution of the disk itself and the planetary system undergoing formation. Their presence also offers more chances of spotting observational features in the disk structure. We performed numerical simulations of planet formation via pebble and gas accretion, while including migration, in a viscously evolving protoplanetary disk, with dust growing, drifting, and evaporating at the ice lines. In our investigation of the most favorable conditions for giant planet formation, we find that these are high disk masses, early formation, and a large enough disk to host a long-lasting pebble flux, so that efficient core growth can take place before the pebble flux decays over time. Specifically, core growth needs to start before 0.9 Myr to form a giant, with an initial disk mass of 0.04 M⊙ (or higher) and the disk radius needs to be larger than 50 AU. However, small disks with the same mass allow more efficient gas accretion onto already formed planetary cores, leading to more massive gas giants. Given the right conditions, high viscosity (α = 10−3) leads to more massive cores (compared to α = 10−4) and it also enhances gas accretion. At the same time, it causes faster type II migration rates, so the giants have a decreasing final position for increasing viscosity. Intermediate dust fragmentation velocities, between 4 and 7 m s−1, provide the necessary pebble sizes and radial drift velocities for maximized pebble accretion with optimal pebble flux. The starting location of a planetary embryo defines whether a giant planet will form, with the highest fraction of giants originating between 5 and 25 AU. Finally, a dust-to-gas ratio of 0.03 can compensate for lower disk masses with fDG ≤ 0.015, but early formation is still important in order to form giant planets. We conclude that there is no specific initial parameter that leads to giant planet formation; rather, it is the outcome of a combination of complementary factors. This also implies that the diversity of the exoplanet systems is the product of the intrinsic diversity of the protoplanetary disks and it is crucial to take advantage of the increasing number and quality of observations to constrain the disk population properties and ultimately devise planet formation theories.

Turbulent dynamo action and its effects on the mixing at the convective boundary of an idealized oxygen-burning shell

Convection is one of the most important mixing processes in stellar interiors. Hydrodynamic mass entrainment can bring fresh fuel from neighboring stable layers into a convection zone, modifying the structure and evolution of the star. Because flows in stellar convection zones are highly turbulent, multidimensional hydrodynamic simulations are fundamental to accurately capture the physics of mixing processes. Under some conditions, strong magnetic fields can be sustained by the action of a turbulent dynamo, adding another layer of complexity and possibly altering the dynamics in the convection zone and at its boundaries. In this study, we used our fully compressible SEVEN-LEAGUE HYDRO code to run detailed and highly resolved three-dimensional magnetohydrodynamic simulations of turbulent convection, dynamo amplification, and convective boundary mixing in a simplified setup whose stratification is similar to that of an oxygen-burning shell in a star with an initial mass of 25 M⊙. We find that the random stretching of magnetic field lines by fluid motions in the inertial range of the turbulent spectrum (i.e., a small-scale dynamo) naturally amplifies the seed field by several orders of magnitude in a few convective turnover timescales. During the subsequent saturated regime, the magnetic-to-kinetic energy ratio inside the convective shell reaches values as high as 0.33, and the average magnetic field strength is ∼1010 G. Such strong fields efficiently suppress shear instabilities, which feed the turbulent cascade of kinetic energy, on a wide range of spatial scales. The resulting convective flows are characterized by thread-like structures that extend over a large fraction of the convective shell. The reduced flow speeds and the presence of magnetic fields with strengths up to 60% of the equipartition value at the upper convective boundary diminish the rate of mass entrainment from the stable layer by ≈20% as compared to the purely hydrodynamic case.

Constraints on the multiplicity of the most massive stars known: R136 a1, a2, a3, and c

Context. The upper stellar mass limit is a fundamental parameter for simulations of star formation, galactic chemical evolution, and stellar feedback. An empirical bound on this parameter is therefore highly valuable. The most massive stars known to date are R 136 a1, a2, a3, and c, with reported masses in excess of 150–200 M⊙ and initial masses of up to ≈300 M⊙. They are located within the central cluster R 136a of the Tarantula nebula in the Large Magellanic Cloud (LMC), However, the mass estimation of these stars relies on the assumption that they are single. Aims. Via multi-epoch spectroscopy, we provide, for the first time, constraints on the presence of close stellar companions to the most massive stars known for orbital periods of up to ≈10 yr. Methods. We collected three epochs of spectroscopy for R 136 a1, a2, a3, and c with the Space Telescope Imaging Spectrograph (STIS) of the Hubble Space Telescope (HST) in the years 2020–2021 to probe potential radial-velocity (RV) variations. We combined these epochs with an additional HST/STIS observation taken in 2012. For R 136 c, we also used archival spectroscopy obtained with the Very Large Telescope (VLT). We used cross-correlation to quantify the RVs and establish constraints on possible companions to these stars up to periods of ≈10 yr. Objects are classified as binaries when the peak-to-peak RV shifts exceed 50 km s−1 and when the RV shift is significant with respect to errors. Results. R 136 a1, a2, and a3 do not satisfy the binary criteria and are thus classified as putatively single, although formal peak-to-peak RV variability on the level 40 km s−1 is noted for a3. Only R 136 c is classified as a binary, in agreement with the literature. We can generally rule out massive companions (M2 ≳ 50 M⊙) to R 136 a1, a2, and a3 out to orbital periods of ≲1 yr (separations ≲5 au) at 95% confidence, or out to tens of years (separations ≲100 au) at 50% confidence. Highly eccentric binaries (e ≳ 0.9) or twin companions with similar spectra could evade detection down to shorter periods (≳10 days), though their presence is not supported by the relative X-ray faintness of R 136 a1, a2, and a3. We derive a preliminary orbital solution with a 17.2 days period for the X-ray-bright binary R 136 c, though more data are needed to conclusively derive its orbit. Conclusions. Our study supports a lower bound of 150–200 M⊙ on the upper-mass limit at LMC metallicity.

Spectra of axions emitted from main sequence stars

We compute the detailed energy spectra of axions with two-photon coupling produced in stellar cores over a wide range of stellar masses. We focus on main sequence stars and base our calculations on the stellar interior profiles from MESA, for which we provide simple fits in an appendix. The obtained stellar axion spectra, combined with recent models of star formation history and stellar initial mass function, enable us to estimate the properties of the diffuse axion background sourced by all the stars in the universe. The fluxes of this stellar axion background and its decay photons are subdominant to but can in principle be disentangled from those expected from the Sun and the early universe based on their different spectral and spatial profiles.

Global strong solutions of three-dimensional compressible non-isentropic micropolar fluid equations with far field vacuum

We are concerned with the Cauchy problem of three-dimensional (3D) compressible non-isentropic micropolar fluid equations with far field vacuum. With the help of Serrin type blow-up criterion, we show the global existence and uniqueness of strong solutions provided that the initial mass is suitably small. Our work generalizes the result of Huang et al. (2021) [8] to the case that vacuum is allowed at infinity.

Preliminary Study to Assess the Impact of Dietary Rutin on Growth, Antioxidant Capacity, and Intestinal Health of Yellow Catfish, Pelteobagrus fulvidraco

This research aimed to examine the effects of dietary rutin supplementation on growth, body composition, serum biochemical indexes, liver enzyme activities and antioxidant-related genes expression, intestinal morphology, and microbiota composition of juvenile yellow catfish (Pelteobagrus fulvidraco). Rutin was added to the basal diets at doses of 0 (control), 100 mg/kg, and 500 mg/kg. Each diet was fed randomly into three tanks, each tank containing 30 fish with an initial body mass of (10.27 ± 0.62) g. The feeding trial was conducted in an indoor recirculating aquiculture system at 28 °C for 56 days. According to the findings, the inclusion of 100 mg/kg rutin significantly improved the growth performance of yellow catfish and reduced the feed conversion ratio; however, the growth promotion effect was diminished when the diet was supplemented with 500 mg/kg of rutin. The inclusion of 500 mg/kg rutin in the diet significantly reduced the level of crude lipid and protein of the whole fish. Serum activities of alkaline phosphatase, albumin, and total protein were all significantly increased when fish were fed the diet supplemented with 500 mg/kg rutin, while serum glucose was significantly lower compared to the control group. Meanwhile, dietary rutin at a concentration of 500 mg/kg significantly induced the hepatic mRNA expressions of antioxidant-related genes (including Cu/Zn-SOD, Mn-SOD, CAT, GPx) and inflammatory-associated genes (including TNFα, IL-10, LYZ). Incorporating rutin at doses of 100 mg/kg and 500 mg/kg into the diets resulted in a notable increase in superoxide dismutase (SOD) activity, while simultaneously reducing malondiadehyde (MDA) content in the liver and intestine. Intestinal villus height, villus width, muscular thickness, and lumen diameter were significantly increased with the administration of 500 mg/kg of dietary rutin. Gut microbial diversity analysis indicated that supplementing diets with 100 mg/kg and 500 mg/kg rutin significantly enhanced the abundance of Cetobacterium while decreasing Plesiomonas richness. In conclusion, dietary rutin levels at 100 mg/kg could enhance the growth, antioxidant capability, and intestinal health of yellow catfish under present experimental conditions.

The SN 2023ixf Progenitor in M101. I. Infrared Variability

Observational evidence points to a red supergiant (RSG) progenitor for SN 2023ixf. The progenitor candidate has been detected in archival images at wavelengths (≥0.6 μm) where RSGs typically emit profusely. This object is distinctly variable in the infrared (IR). We characterize the variability using pre-explosion mid-IR (3.6 and 4.5 μm) Spitzer and ground-based near-IR (JHK s ) archival data jointly covering 19 yr. The IR light curves exhibit significant variability with rms amplitudes in the range 0.2–0.4 mag, increasing with decreasing wavelength. From a robust period analysis of the more densely sampled Spitzer data, we measure a period of 1091 ± 71 days. We demonstrate using Gaussian process modeling that this periodicity is also present in the near-IR light curves, thus indicating a common physical origin, which is likely pulsational instability. We use a period–luminosity relation for RSGs to derive a value of M K = −11.58 ± 0.31 mag. Assuming a late M spectral type, this corresponds to at T eff = 3200 K and to at T eff = 3500 K. This gives an independent estimate of the progenitor’s luminosity, unaffected by uncertainties in extinction and distance. Assuming the progenitor candidate underwent enhanced dust-driven mass loss during the time of these archival observations, and using an empirical period–luminosity–based mass-loss prescription, we obtain a mass-loss rate of around (2–4) × 10−4 M ⊙ yr−1. Comparing the above luminosity with stellar evolution models, we infer an initial mass for the progenitor candidate of 20 ± 4 M ⊙, making this one of the most massive progenitors for a Type II SN detected to date.