Miracle-dz/UniFAR-FTUs huggingface dataset:
TIDAL STELLAR DISRUPTIONS BY MASSIVE BLACK HOLE PAIRS. II. DECAYING BINARIES

Tidal stellar disruptions have traditionally been discussed as a probe of the single, massive black holes (MBHs) that are dormant in the nuclei of galaxies. We have previously used numerical scattering experiments to show that three-body interactions between bound stars in a stellar cusp and a non-evolving “hard” MBH binary will also produce a burst of tidal disruptions, caused by a combination of the secular “Kozai effect” and by close resonant encounters with the secondary hole. Here, we derive basic analytical scalings of the stellar disruption rates with the system parameters, assess the relative importance of the Kozai and resonant encounter mechanisms as a function of time, discuss the impact of general relativistic (GR) and extended stellar cusp effects, and develop a hybrid model to self-consistently follow the shrinking of an MBH binary in a stellar background, including slingshot ejections and tidal disruptions. In the case of a fiducial binary with primary hole mass M1 = 107 M☉ and mass ratio q = M2/M1 = 1/81, embedded in an isothermal cusp, we derive a stellar disruption rate yr−1 lasting ∼3 × 105 yr. This rate is three orders of magnitude larger than the corresponding value for a single MBH fed by two-body relaxation, confirming our previous findings. For q ≪ 0.01, the Kozai/chaotic effect could be quenched due to GR/cusp effects by an order of magnitude, but even in this case the stellar-disruption rate is still two orders of magnitude larger than that given by standard relaxation processes around a single MBH. Our results suggest that ≳10% of the tidal-disruption events may originate in MBH binaries.
Local grand unification in the heterotic landscape

We consider the possibility that the unification of the electroweak interactions and the strong force arises from string theory, at energies significantly lower than the string scale. As a tool, an effective grand unified field theory in six dimensions is derived from an anisotropic orbifold compactification of the heterotic string. It is explicitly shown that all anomalies cancel in the model, though anomalous Abelian gauge symmetries are present locally at the boundary singularities. In the supersymmetric vacuum additional interactions arise from higher‐dimensional operators. We develop methods that relate the couplings of the effective theory to the location of the vacuum, and find that unbroken discrete symmetries play an important role for the phenomenology of orbifold models. An efficient algorithm for the calculation of the superpotential to arbitrary order is developed, based on symmetry arguments. We furthermore present a correspondence between bulk fields of the orbifold model in six dimensions, and the moduli fields that arise from compactifying four internal dimensions on a manifold with non‐trivial gauge background.
New runaway O-type stars in the first Gaia Data Release

Abstract We have detected 13 new runaway-star candidates of spectral type O combining the TGAS (Tycho-Gaia Astrometric Solution) proper motions from Gaia Data Release 1 (DR1) and the sample from GOSSS (Galactic O-Star Spectroscopic Survey). We have also combined TGAS and Hipparcos proper motions to check that our technique recovers many of the previously known O-type runaways in the sample.
ORIGINAL INTENSIVE CARE SAPS 3 as a 28-day mortality predictor in critically ill COVID-19 patients

Background : The case fatality rate (CFR) of COVID-19 was 8.7% in Indonesia on April 2020. Simplified Acute Physiology Score 3 (SAPS 3) has been used to predict the hospital mortality based on different variables including acute physiologic derangements, current conditions and interventions, and previous health status assess the severity of condition during the first hour of admission to the ICU. We assessed SAPS 3 to predict the outcome and mortality of critical COVID-19 patients in ICU over a period of 28 days. Methodology : This retrospective cohort study consisted of adult patients admitted to ICU with probable or confirmed COVID-19 in our hospital. We recorded the patients SAPS 3 score from the medical record as well as the 28-day mortality. Validity of the SAPS 3 score was done by the Area Under Curve (AUC) measurement and Hosmer-Lemeshow calibration test. Results : The mortality rate of critical COVID-19 patients was 43.8%. The age, intra-hospital location before ICU admission, use of vasoactive drugs (P < 0.0001), focal neurological deficits (P < 0.0001), respiratory failure (P = 0.004), creatinine ≥ 3.5 mg/dL (P = 0.005), and platelets < 50,000 /µL (P = 0.032) were significantly associated with 28-days mortality in the ICU. SAPS 3 showed good discrimination and predictability. The optimal cut-off point was 39 with 70.3% sensitivity and 74.4% specificity. Conclusion : SAPS3 score system was valid in predicting the 28-day mortality of COVID-19 patients in the ICU with good discrimination and calibration value; therefore, it is an important predictor tool for early prognosis screening that will help reduce the strain over the ICU resources.
A universal exponential factor in the dimensional crossover from graphene to graphite

A universal exponential factor, γc=π/2, is disclosed for the dimensional crossover of few-layer graphene (FLG) from two-dimensional graphene to three-dimensional graphite. γc is found by analyzing available experimental data on different properties of FLG with varying thickness. A theoretical study on the phonon spectrum of the vertical acoustic mode in FLG is carried out to further check this exponential factor γc. Interestingly, the same exponential factor appears in the dimensional crossover of the phonon mode. It turns out that the exponential factor γc is related to the homogeneous Helmholtz-like molal equation in the mass transfer with a first order chemical reaction. The finding should provide valuable information for experimentalists and theorists in the future investigation on thickness dependent properties of FLG.
THE AGE OF THE YOUNG BULGE-LIKE POPULATION IN THE STELLAR SYSTEM TERZAN 5: LINKING THE GALACTIC BULGE TO THE HIGH-Z UNIVERSE

The Galactic bulge is dominated by an old, metal-rich stellar population. The possible presence and the amount of a young (a few gigayears old) minor component is one of the major issues debated in the literature. Recently, the bulge stellar system Terzan 5 was found to harbor three sub-populations with iron content varying by more than one order of magnitude (from 0.2 up to two times the solar value), with chemical abundance patterns strikingly similar to those observed in bulge field stars. Here we report on the detection of two distinct main-sequence turnoff points in Terzan 5, providing the age of the two main stellar populations: 12 Gyr for the (dominant) sub-solar component and 4.5 Gyr for the component at super-solar metallicity. This discovery classifies Terzan 5 as a site in the Galactic bulge where multiple bursts of star formation occurred, thus suggesting a quite massive progenitor possibly resembling the giant clumps observed in star-forming galaxies at high redshifts. This connection opens a new route of investigation into the formation process and evolution of spheroids and their stellar content.
Evaluation of intraperitoneal [ 18 F]-FDOPA administration for micro-PET imaging in 1 mice and assessment of the effect of sub-chronic ketamine dosing on dopamine 2 synthesis capacity 3

Positron emission tomography (PET) using the radiotracer [ 18 F]-FDOPA provides a tool for studying brain 23 dopamine synthesis capacity in animals and humans. We have previously standardised a micro-PET 24 methodology in mice by intravenously administering [ 18 F]-FDOPA via jugular vein cannulation, and 25 assessment of striatal dopamine synthesis capacity, indexed as the influx rate constant Ki Mod of [ 18 F]-FDOPA, 26 using extended graphical Patlak analysis with the cerebellum as a reference region. This enables a direct 27 comparison between preclinical and clinical output values. However, chronic intravenous catheters are 28 technically difficult to maintain for longitudinal studies. Hence, in this study, intraperitoneal administration 29 of [ 18 F]-FDOPA was evaluated as a less invasive alternative that facilitates longitudinal imaging. Our 30 experiments comprised the following assessments: (i) comparison of [ 18 F]-FDOPA uptake between 31 intravenous and intraperitoneal radiotracer administration and optimisation of the time window used for 32 extended Patlak analysis, (ii) comparison of Ki Mod in a within-subject design of both administration routes, (iii) 33 test-retest evaluation of Ki Mod in a within-subject design of intraperitoneal radiotracer administration, and 34 (iv) validation of Ki Mod estimates by comparing the two administration routes in a mouse model of 35 hyperdopaminergia induced by sub-chronic ketamine. 36 Our results demonstrate that intraperitoneal [ 18 F]-FDOPA administration resulted in good brain uptake, with 37 no significant effect of administration route on Ki Mod estimates (intraperitoneal: 0.024+0.0047 min -1 , 38 intravenous: 0.022+0.0041 min -1 , p=0.42) and similar coefficient of variation (intraperitoneal: 19.6%; 39 intravenous: 18.4%). The technique had a moderate test-retest validity (intraclass correlation coefficient, 40 ICC=0.52, N=6), and thus supports longitudinal studies. Following sub-chronic ketamine administration, 41 elevated Ki Mod
Opleiding Informatica BlockStep, an A* algorithm toward Minecraft optimal world traversal for speedrunning

Minecraft is a popular game in which many players attempt speedruns. In this thesis, we discuss how we could use a reinforcement learning agent to break the world record. This agent will need to build on pre-defined optimal strategies to reduce the complexity of analysing the game world. This is possible, because Minecraft is partly deterministic. Parts of the strategies rely on an optimal path traversal algorithm. In this thesis, we describe the developement of a near-optimal version of the A* algorithm for path traversal in the Minecraft block world. The previous best algorithm for this task, named Baritone, also uses A*. An obvious disadvantage of Baritone, however, is the restricted movement. A player in Minecraft can turn in an infinite number of degrees. Baritone’s creators limited the turns to 45° intervals to make the algorithm less complex. Movement restrictions lead to less optimal paths. We would expect faster paths to be found by expanding the movement space. In 85% of the cases tested, we find that our hypothesis is correct and that our new BlockStep algorithm finds a faster path than Baritone.
The 1997 event in the Crab Pulsar in X-rays

In October 1997, radio pulses from the Crab Pulsar underwent abnormal delay. This was reported by two radio observatories, both of which explained this frequency dependent and time varying delay as being due to refractive effects of ionized shells in the Crab Nebula. Both groups also noted that, curiously and confusingly coincident with the frequency dependent delay, the Crab Pulsar also underwent an unusual slowing down, which they believed to be unrelated to the Crab Nebula and instead intrinsic to the Crab Pulsar, resulting in an additional delay that was frequency independent. However, it now appears that one of the groups attributes the frequency independent delay also to refractive effects. This work aims to verify whether at least a part of the frequency independent delay is indeed due to intrinsic slowing down of the Crab Pulsar. Timing analysis of the Crab Pulsar's October 1997 event has been done in X-rays, which are not delayed by the refractive and diffractive effects that affect radio waves; at X-rays only the intrinsic slowing down should contribute to any observed delay. Data mainly from the PCA instrument aboard the RXTE satellite have been used, along with a small amount of data from the PDS instrument aboard the BeppoSAX satellite. Analysis of the X-ray data, using the very accurate reference timing mode derived at radio frequencies, strongly supports the intrinsic slowing down hypothesis. Analysis using the reference timing model derived self-consistently from the limited X-ray data, which is less accurate, is not completely unambiguous regarding the above two hypotheses, but provides reasonable support for the intrinsic slowing down hypothesis. A significant fraction of the frequency independent delay during the October 1997 event is indeed due to intrinsic slowing down of the Crab Pulsar.
Seeing spin dynamics in atomic gases

The dynamics of internal spin, electronic orbital, and nuclear motion states of atoms and molecules have preoccupied the atomic and molecular physics community for decades. Increasingly, such dynamics are being examined within many-body systems composed of atomic and molecular gases. Our findings sometimes bear close relation to phenomena observed in condensed-matter systems, while on other occasions they represent truly new areas of investigation. I discuss several examples of spin dynamics that occur within spinor Bose-Einstein gases, highlighting the advantages of spin-sensitive imaging for understanding and utilizing such dynamics.
Signatures of Neutrino Cooling in the SN1987A Scenario

The neutrino signal from SN1987A confirmed the core-collapse scenario and the possible formation of a neutron star. Although this compact object has eluded all observations, theoretical and numerical developments have allowed a glimpse of the fate of it. In particular, a hypercritical accretion model has been proposed to forecast the accretion of $\sim 0.15 \:\mathrm{M_{\odot}}$ in two hours and the subsequent submergence of the magnetic field in the newborn neutron star. In this paper, we revisit the Chevalier's model in a numerical framework, focusing on the neutrino cooling effect on the supernova fall-back dynamics. For that, using a customized version of the FLASH code, we carry out numerical simulations of the accretion of matter onto the newborn neutron star in order to estimate the size of the neutrino-sphere, the emissivity and luminosity of neutrinos. As a signature of this phase, we estimate the neutrinos expected on SK neutrino experiment and their flavor ratios. This is academically important because, although currently it was very difficult to detect 1.46 thermal neutrinos and their oscillations, these fingerprints are the only viable and reliable way to confirm the hypercritical phase. Perhaps new techniques for detecting neutrino oscillations arise in the near future allowing us to confirm our estimates.
CLASSICAL BULGES, SUPERMASSIVE BLACK HOLES, AND AGN FEEDBACK: EXTENSION TO LOW-MASS GALAXIES

The empirical model of Lu et al. for the relation between star formation rate and halo mass growth is adopted to predict the classical bulge mass ( M cb ? > )–total stellar mass ( M ⋆ ? > ) relation for central galaxies. The assumption that the supermassive black hole (SMBH) mass ( M BH ? > ) is directly proportional to the classical bulge mass, with the proportionality given by that for massive galaxies, predicts a M BH ? > − M ⋆ ? > relation that matches well the observed relation for different types of galaxies. In particular, the model reproduces the strong transition at M ⋆ = 10 10.5 ? > − 10 11 M ⊙ ? > , below which M BH ? > drops rapidly with decreasing M ⋆ ? > . Our model predicts a new sequence at M ⋆ < 10 10.5 M ⊙ ? > , where M BH ∝ M ⋆ ? > but the amplitude is a factor of ∼50 lower than the amplitude of the sequence at M ⋆ > 10 11 M ⊙ ? > . If all SMBHs grow through similar quasar modes with a feedback efficiency of a few percent, then the energy produced in low-mass galaxies at redshift z ≳ 2 ? > can heat the circumgalactic medium up to a specific entropy level that is required to prevent excessive star formation in low-mass dark matter halos.
The spectrum of γ-ray burst: a clue

In this work, we numerically calculate the thermal radiation efficiency of the baryonic outflow. The possible outflow acceleration in the transparent stage, which lowers thermal radiation efficiency, has been taken into account. In the standard internal shock model for the prompt emission, the fast shells should move with a typical Lorentz factor similar to 5 Gamma(i) otherwise the gamma-ray burst (GRB) efficiency will be in disagreement with the observations, where Gamma(i) is the bulk Lorentz factor of the shocked/emitting region. The photosphere radius of these fast shells is small and the thermal radiation is too strong to be effectively outshone by the internal shock emission. This is particularly the case for some extremely bright events having Gamma(i) similar to 103, like GRBs 080319B and 080916C. The absence of a distinct thermal component in the spectrum of most GRBs challenges the standard internal shock model and may suggest a non-baryonic (magnetic) outflow component. Though the magnetic outflow model seems favoured by more and more data, it can hardly reproduce the typical GRB spectrum. In the photosphere-gradual magnetic dissipation scenario, the spectrum cuts off at similar to 1 GeV, too low to account for the observations of GRBs 080916C. In the sudden magnetic energy dissipation model, the low-energy spectrum is expected to be F(nu) proportional to nu-1/2, too soft to be consistent with the data F(nu) proportional to nu 0. We speculate that the low-energy spectrum puzzle could be unveiled by the mechanism that particles, in the magnetic dissipation process, are repeatedly accelerated.
Practice of street clinic teams and recording of actions in the e-SUS Primary Care

Objective: To describe the perceptions of Street Clinic teams about their practice and the use of the e-SUS Primary Health Care strategy to record their care. Method: Descriptive-exploratory study with a qualitative approach. Twenty professionals from three Street Clinics from the state of Goiás, Brazil. Self-administered questionnaires with a professional profile and focus groups were used, whose data were submitted to content analysis. Results: Two categories of analysis were identified: “Aspects that influence the work process of the Street Clinic teams” and “Records in the e-SUS Primary Health Care strategy by the Street Clinic”. Final considerations: The need for investment to overcome the challenges of qualified care for the homeless population was evidenced, for the effectiveness of records, considering their specificities and needs.
Fractal Pore and Its Impact on Gas Adsorption Capacity of Outburst Coal: Geological Significance to Coalbed Gas Occurrence and Outburst

Pore structure and methane adsorption of coal reservoir are closely correlated to the coalbed gas occurrence and outburst. Full-scale pore structure and its fractal heterogeneity of coal samples were quantitatively characterized using low-pressure N 2 gas adsorption (LP-N 2 GA) and high-pressure mercury intrusion porosimetry (HP-MIP). Fractal pore structure and adsorption capacities between outburst and nonoutburst coals were compared, and their geological signi ﬁ cance to gas occurrence and outburst was discussed. The results show that pore volume (PV) is mainly contributed by macropores ( > 1000nm) and mesopores (100 – 1000 nm), while speci ﬁ c surface area (SSA) is dominated by micropores ( < 10nm) and transition pores (10 – 100 nm). On average, the PV and SSA of outburst coal samples are 4.56 times and 5.77 times those of nonoutburst coal samples, respectively, which provide su ﬃ cient place for gas adsorption and storage. The pore shape is dominated by semiclosed pores in the nonoutburst coal, whereas open pores and inkbottle pores are prevailing in the outburst coal. The pore size is widely distributed in the outburst coal, in which not only micropores are dominant, but also, transition pores and mesopores are developed to a certain extent. Based on the data from HP-MIP and LP-N 2 GA, pore spatial structure and surface are of fractal characteristics with fractal dimensions D m 1 (2.81 – 2.97) and D n (2.50 – 2.73) calculated by Menger model and Frenkel – Halsey – Hill (FHH) model, respectively. The pore structure in the outburst coal is more heterogeneous as its D n and D m 1 are generally larger than those of the nonoutburst coal. The maximum methane adsorption capacities ( V L : 15.34 – 20.86 cm 3 /g) of the outburst coal are larger than those of the nonoutburst coal ( V L : 9.97 – 13.51cm 3 /g). The adsorptivity of coal samples is governed by the micropores, transition pores, and D n because they are positively correlated with the SSA. The outburst coal belongs to tectonically deformed coal (TDC) characterized by weak strength, rich microporosity, complex pore structure, strong adsorption capacity, but poor pore connectivity because of inkbottle pores. Therefore, the area of TDC is at high risk for gas outburst as there is a high-pressure gas sealing zone with abundant gas enrichment but limited gas migration and extraction.
Characterisations of ohmic and Schottky contacts of a single ZnO nanowire

Current voltage and Kelvin Probe Force Microscopy (KPFM) measurements were performed on single ZnO nanowires. Measurements are shown to be strongly correlated with the contact behavior, either ohmic or Schottky. The ZnO nanowires were obtained by metallo-organic chemical vapor deposition (MOCVD) and contacted using electronic-beam lithography. Depending on the contact geometry, good quality ohmic contacts (linear I V behavior) or non-linear (diode like) Schottky contacts were obtained. Current voltage and KPFM measurements on both types of contacted ZnO nanowires were performed in order to investigate their behavior. A clear correlation could be established between the I V curve, the electrical potential profile along the device and the nanowire geometry. Some arguments supporting this behavior are given based on a depleted region extension. This work will help to better understand the electrical behavior of ohmic contacts on single ZnO nanowires, for future applications in nanoscale field effect-transistors and nano-photodetectors.
Non‐thermal excitation and ionization in supernovae

We incorporate non-thermal excitation and ionization processes arising from non-thermal electrons that result from γ-ray energy deposition into our radiative transfer code cmfgen. The non-thermal electron distribution is obtained by solving the Spencer–Fano equation using the procedure of Kozma & Fransson. We applied the non-thermal calculations to the blue supergiant explosion model whose early evolution was studied in Dessart & Hillier. Non-thermal processes generally increase excitation and ionization and decrease the temperature of the ejecta. We confirm that non-thermal processes are crucial for modelling nebular spectra. Both optical H i and He i lines are significantly strengthened. While optical He i lines are not easily discerned in observational spectra due to severe blending with other lines, He i 2.058 μm provides an excellent opportunity to infer the influence of non-thermal processes. We also discuss the processes controlling the formation of He i lines during nebular epochs. Most lines of other species are only slightly affected. We also show that the inclusion of Fe i has substantial line-blanketing effects on optical spectra. Our model spectra and synthetic light curves are compared to the observations of SN 1987A. The spectral evolution shows broad agreement with the observations, especially Hα. The uncertainties of the non-thermal solver are studied, and are expected to be small. With this new addition of non-thermal effects in cmfgen, we now treat all known important processes controlling the radiative transfer of supernova ejecta, whatever the type and the epoch.