Miracle-dz/UniFAR-FTUs huggingface dataset:
Gap theorem on Kähler manifolds with nonnegative orthogonal bisectional curvature

Abstract In this paper we prove a gap theorem for Kähler manifolds with nonnegative orthogonal bisectional curvature and nonnegative Ricci curvature, which generalizes an earlier result of the first author [L. Ni, An optimal gap theorem, Invent. Math. 189 2012, 3, 737–761]. We also prove a Liouville theorem for plurisubharmonic functions on such a manifold, which generalizes a previous result of L. -F. Tam and the first author [L. Ni and L. -F. Tam, Plurisubharmonic functions and the structure of complete Kähler manifolds with nonnegative curvature, J. Differential Geom. 64 2003, 3, 457–524] and complements a recent result of Liu [G. Liu, Three-circle theorem and dimension estimate for holomorphic functions on Kähler manifolds, Duke Math. J. 165 2016, 15, 2899–2919].
Optimization of flocculation and clotting time of camel milk with camel and goat rennets, and chicken pepsin in comparison with cow milk using response surface method (RSM)

To solve the difficulty of coagulation of camel milk, three animal coagulating enzymes: Camel rennet, goat rennet, and chicken pepsin were used. The study was focused on the optimization of two milk coagulation key parameters: pH and temperature using the response surface methodology. The cow milk is used as reference. Characterization of the coagulating enzymes extract showed that the protein content is higher in chicken pepsin [20 ± 0.00 mg/ml] followed by camel and goat’s extracts [15.4 ± 0.00 mg/ml, 8.8 ± 0.00 mg/ml]. However, coagulating and specific activities were more important in camel rennet [111.12 ± 1.23 UP.ml-1, 7.21 ± 0.03 UP.mg-1] than in goat’s rennet and chicken pepsin. On the other hand, coagulant strength was for camel rennet 1/4166.67 SU, goat rennet 1/2531.64 SU, and chicken pepsin 1/6153.85 SU. Moreover, results of pH and temperature optimization of camel milk flocculation showed the following pairs: [X1 = 5.35, X2 = 42] for camel rennet, [X1 = 5.48, X2 = 30] for goat rennet and [X1 = 5.49, X2 = 39.45] for chicken pepsin. Also, the coagulation showed the following couples: [X1 = 5.37, X2 = 39.09] for camel rennet, [X1 = 5.36, X2 = 38.84] for goat rennet and [X1 = 5, X2 = 42] for chicken pepsin. The conclusion was flocculation and coagulation optimum points of camel and cow milk with coagulating enzymes studied are different based on surface plot analysis and the relationship between response and variables
THE DEPENDENCE OF STAR FORMATION ACTIVITY ON STELLAR MASS SURFACE DENSITY AND SERSIC INDEX IN zCOSMOS GALAXIES AT 0.5 < z < 0.9 COMPARED WITH SDSS GALAXIES AT 0.04 < z < 0.08

In order to try to understand the internal evolution of galaxies and relate this to the global evolution of the galaxy population, we present a comparative study of the dependence of star formation rates on the average surface mass densities (ΣM) of galaxies at 0.5 < z < 0.9 and 0.04 < z < 0.08, using the zCOSMOS and Sloan Digital Sky Survey (SDSS) surveys, respectively. We derive star formation rates, stellar masses, and structural parameters in a consistent way for both samples, and apply them to samples that are complete down to the same stellar mass at both redshifts. We first show that the characteristic step-function dependence of median specific star formation rate (SSFR) on ΣM in SDSS, seen by Brinchmann et al., is due to the change over from predominantly disk galaxies to predominantly spheroidal galaxies at the surface mass density logΣMchar∼8.5 at which the SSFR is seen to drop. Turning to zCOSMOS, we find a similar shape for the median SSFR–ΣM relation, but with median SSFR values that are about 5–6 times higher than for SDSS, across the whole range of ΣM, and in galaxies with both high and low Sersic indices. This emphasizes that galaxies of all types are contributing, proportionally, to the global increase in star formation rate density in the Universe back to these redshifts. The ΣMchar “step” shifts to slightly higher values of ΣM in zCOSMOS relative to SDSS, but this can be explained by a modest differential evolution in the size–mass relations of disk and spheroid galaxies. For low Sersic index galaxies, there is little change in the size–mass relation, as seen by Barden et al., although we suggest that this does not necessarily imply inside-out growth of disks, at least not in this redshift range. On the other hand, there is a modest evolution in the stellar mass–size relation for high Sersic index galaxies, with galaxies smaller by ∼25% at z ∼ 0.7. Taken together these produce a modest increase in ΣMchar. Low Sersic index galaxies have a SSFR that is almost independent of ΣM, and the same is probably also true of high Sersic index galaxies once obvious disk systems are excluded.
The Experience and Performance of Female Airline Pilots in Taiwan - A Tripartite Assessment

The pilot profession remains one of the most notable gender-imbalanced occupations in the aviation industry, with women making up a far lower percentage than men. Nevertheless, the experiences and challenges faced by female pilots in the workplace is worth exploring. Previous studies have mostly approached these issues from the perspective of male and/or female pilots, ignoring the opinions of managers responsible for flight operations. This study fills this research gap by adding flight operations managers' assessments of female pilots to explore the topic from a broader and comprehensive tripartite perspective. In addition, gender issues in the cockpit and the impact of female pilot participation are also discussed. The research is conducted through in-depth interviews covering flight operations managers, male pilots, and female pilots in three different Taiwanese airlines. The findings of this study reveal that the performance of female pilots is generally affirmed by flight operations managers and male pilots, and the participation of female pilots produces some chemical effects on the culture of the cockpit, which also contributes to crew resource management and flight safety. Contrary to previous research findings, the female pilots interviewed in this study do not feel that they are being challenged or abused in relation to their gender. Finally, several recommendations are given to the airlines to implement CRM training programs and recruit female pilots.
Exploring the Learning Experience of High-Performing Preclinical Undergraduate Dental Students: A Qualitative Study

The current study aimed to explore the perceptions of high-performing undergraduate dental students in learning dental materials science. One-on-one semi-structured interviews with high-performing students who scored 80 marks and above in dental materials were conducted using an online video-chat platform. A purposeful sampling method was employed, and six students fulfilled the criteria. The interviews were audio-recorded, transcribed verbatim, and analyzed qualitatively using a thematic approach. Three major themes were identified: (1) Learning strategies, (2) Learning enablers and barriers, and (3) Coping with learning challenges. Six sub-themes emerged from the “learning strategies” theme: memorizing and repeating, peer learning, seeking learning resources, study planning, paying attention during class, and mnemonics. The enabler sub-themes include motivation, lecture notes, teachers, and hands-on, whereas the barrier sub-theme is content understanding. Moreover, family support and de-stress appeared as the sub-themes in coping with learning challenges. In short, the present exploratory study identified several major themes and sub-themes that can help dental educators comprehend the complexity of learning dental materials science and how it affects students’ academic performances. The current findings also offer learning recommendations for low-performing students to improve their academic achievements in the dental materials science course.
Accumulative magnetic switching of ultra-high-density recording media by circularly polarized light

Manipulation of the magnetization by external energies other than magnetic field, such as spin-polarized current1-4, electric voltage5,6 and circularly polarized light7-11 gives a paradigm shift in magnetic nanodevices. Magnetization control of ferromagnetic materials only by circularly polarized light has received increasing attention both as a fundamental probe of the interactions of light and magnetism but also for future high-density magnetic recording technologies. Here we show that for granular FePt films, designed for ultrahigh-density recording, the optical magnetic switching by circularly polarized light is an accumulative effect from multiple optical pulses. We further show that deterministic switching of high anisotropy materials by the combination of circularly polarized light and modest external magnetic fields, thus revealing a pathway towards technological implementation.
Variable X-ray absorption in the mini-broad absorption line quasar PG 1126-041

We present the results of a multi-epoch observational campaign on the mini-broad absorption line quasar (mini-BAL QSO) PG 1126-041 performed with XMM-Newton from 2004 to 2009. Time-resolved X-ray spectroscopy and simultaneous UV and X-ray photometry were performed on the most complete set of observations and on the deepest X-ray exposure of a mini-BAL QSO to date. Complex X-ray spectral variability, found on time scales of both months and hours, is best reproduced by means of variable and massive ionized absorbers along the line of sight. In the highest signal-to-noise observation, highly-ionized X-ray absorbing material outflowing much faster than the UV absorbing one is detected. This highly-ionized absorber is found to be variable on very short time scales of a few hours.
Soccer: Is scoring goals a predictable Poissonian process?

The non-scientific event of a soccer match is analysed on a strictly scientific level. The analysis is based on the recently introduced concept of a team fitness (Eur. Phys. J. B, 67 (2009) 445) and requires the use of finite-size scaling. A uniquely defined function is derived which quantitatively predicts the expected average outcome of a soccer match in terms of the fitness of both teams. It is checked whether temporary fitness fluctuations of a team hamper the predictability of a soccer match. To a very good approximation scoring goals during a match can be characterized as independent Poissonian processes with pre-determined expectation values. Minor correlations give rise to an increase of the number of draws. The non-Poissonian overall goal distribution is just a consequence of the fitness distribution among different teams. The limits of predictability of soccer matches are quantified. Our model-free classification of the underlying ingredients determining the outcome of soccer matches can be generalized to different types of sports events.
WIMPs in a 3-3-1 model with heavy sterile neutrinos

In this work we show that from the spectrum of particles of a 3-3-1 gauge model with heavy sterile neutrinos we can have up to three Cold Dark Matter candidates as WIMPs. We obtain their relic abundance and analyze their compatibility with recent direct detection experiments, exploring the possibility of explaining the two events reported by CDMS-II. An interesting outcome of this 3-3-1 model, concerning direct detection of two WIMPs in the model, is a strong bound on the symmetry breaking scale, which imposes it to be above 3 TeV.
POLARIZATION SWINGS FROM CURVED TRAJECTORIES OF THE EMITTING REGIONS

We present a model of polarization swings in blazars from axially symmetric blobs propagating on curved trajectories. If the minimum inclination of the velocity vector to the line of sight is smaller than Γ-1, the polarization angle maximum rotation rate is simultaneous with the polarization degree minimum and a spike in the total flux. By measuring the maximum rotation rate and the moment of the polarization maximum, it is possible to estimate the distance covered by the blob and thus its approximate position. We apply this model to the recent polarization event in blazar 3C 279.
Driven-dissipative preparation of entangled states in cascaded quantum-optical networks

We study the dissipative dynamics and the formation of entangled states in driven cascaded quantum networks, where multiple systems are coupled to a common unidirectional bath. Specifically, we identify the conditions under which emission and coherent reabsorption of radiation drives the whole network into a pure stationary state with non-trivial quantum correlations between the individual nodes. We illustrate this effect in more detail for the example of cascaded two-level systems, where we present an explicit preparation scheme that allows one to tune the whole network through ‘bright’ and ‘dark’ states associated with different multi-partite entanglement patterns. In a complementary setting consisting of cascaded nonlinear cavities, we find that two cavity modes can be driven into a non-Gaussian entangled dark state. Potential realizations of such cascaded networks with optical and microwave photons are discussed.
A PHYSICAL APPROACH TO THE IDENTIFICATION OF HIGH-Z MERGERS: MORPHOLOGICAL CLASSIFICATION IN THE STELLAR MASS DOMAIN

At z ≳ 1, the distinction between merging and “normal” star-forming galaxies based on single band morphology is often hampered by the presence of large clumps which result in a disturbed, merger-like appearance even in rotationally supported disks. In this paper we discuss how a classification based on canonical, non-parametric structural indices measured on resolved stellar mass maps, rather than on single-band images, reduces the misclassification of clumpy but not merging galaxies. We calibrate the mass-based selection of mergers using the MIRAGE hydrodynamical numerical simulations of isolated and merging galaxies which span a stellar mass range of 109.8–1010.6 M⊙ and merger ratios between 1:1–1:6.3. These simulations are processed to reproduce the typical depth and spatial resolution of observed Hubble Ultra Deep Field (HUDF) data. We test our approach on a sample of real z ≃ 2 ? > galaxies with kinematic classification into disks or mergers and on ∼100 galaxies in the HUDF field with photometric/spectroscopic redshift between 1.5 ≤ z ≤ 3 and M > 109.4 M⊙. We find that a combination of the asymmetry AMASS and M20, MASS indices measured on the stellar mass maps can efficiently identify real (major) mergers with ≲20% contamination from clumpy disks in the merger sample. This mass-based classification cannot be reproduced in star-forming galaxies by H-band measurements alone, which instead result in a contamination from clumpy galaxies which can be as high as 50%. Moreover, we find that the mass-based classification always results in a lower contamination from clumpy galaxies than an H-band classification, regardless of the depth of the imaging used (e.g., CANDELS versus HUDF).
TWO LOCAL VOLUME DWARF GALAXIES DISCOVERED IN 21 cm EMISSION: PISCES A AND B

We report the discovery of two dwarf galaxies, Pisces A and B, from a blind 21 cm H i search. These were the only two galaxies found via optical imaging and spectroscopy of 22 H i clouds identified in the GALFA-H i survey as dwarf galaxy candidates. They have properties consistent with being in the Local Volume (<10 Mpc), and one has resolved stellar populations such that it may be on the outer edge of the Local Group (∼1 Mpc from M31). While the distance uncertainty makes interpretation ambiguous, these may be among the faintest star-forming galaxies known. Additionally, rough estimates comparing these galaxies to ΛCDM dark matter simulations suggest consistency in number density, implying that the dark matter halos likely to host these galaxies are primarily H i-rich. The galaxies may thus be indicative of a large population of dwarfs at the limit of detectability that are comparable to the faint satellites of the Local Group. Because they are outside the influence of a large dark matter halo to alter their evolution, these galaxies can provide critical anchors to dwarf galaxy formation models.
TYPE-I X-RAY BURSTS REVEAL A FAST CO-EVOLVING BEHAVIOR OF THE CORONA IN AN X-RAY BINARY

The coronae in X-ray binaries (XRBs) still remain poorly understood, although they have been believed for a long time to play a key role in modeling the characteristic outbursts of XRBs. Type-I X-ray bursts, the thermonuclear flashes happening on the surface of a neutron star (NS), can be used as a probe to the innermost region of an NS XRB, where the corona is believed to be located very close to the NS. We report the discovery of a tiny life cycle of the corona that is promptly co-evolved with the type-I bursts superimposed on the outburst of the NS XRB IGR J17473−2721. This finding may serve as the first evidence of directly seeing the rapid disappearance and formation of a corona in an XRB with a cooling/heating timescale of less than a second, which can strongly constrain the accretion models in XRBs at work.
A Keplerian disk around a Class 0 source: ALMA observations of VLA1623A

Context. Rotationally supported disks are critical in the star formation process. The questions of when they form and what factors influence or hinder their formation have been studied but are largely unanswered. Observations of early-stage YSOs are needed to probe disk formation. Aims: VLA1623 is a triple non-coeval protostellar system, with a weak magnetic field perpendicular to the outflow, whose Class 0 component, VLA1623A, shows a disk-like structure in continuum with signatures of rotation in line emission. We aim to determine whether this structure is in part or in whole a rotationally supported disk, i.e. a Keplerian disk, and what its characteristics are. Methods: ALMA Cycle 0 Early Science 1.3 mm continuum and C$^{18}$O (2-1) observations in the extended configuration are presented here and used to perform an analysis of the disk-like structure using position-velocity (PV) diagrams and thin disk modeling with the addition of foreground absorption. Results: The PV diagrams of the C$^{18}$O line emission suggest the presence of a rotationally supported component with a radius of at least 50 AU. Kinematical modeling of the line emission shows that the disk out to 180 AU is actually rotationally supported, with the rotation described well by Keplerian rotation out to at least 150 AU, and the central source mass is ~{}0.2 M$_{⊙}$ for an inclination of 55{deg}. Pure infall and conserved angular momentum rotation models are excluded. Conclusions: VLA1623A, a very young Class 0 source, presents a disk with an outer radius R$_{out}$ = 180 AU with a Keplerian velocity structure out to at least 150 AU. The weak magnetic fields and recent fragmentation in this region of {$ρ$} Ophiuchus may have played a leading role in the formation of the disk. Appendices are available in electronic form at http://www.aanda. org
M-theory, the signature theorem, and geometric invariants

The equations of motion and the Bianchi identity of the C-field in M-theory are encoded in terms of the signature operator. We then reformulate the topological part of the action in M-theory using the signature, which leads to connections to the geometry of the underlying manifold, including positive scalar curvature. This results in a variation on the miraculous cancellation formula of Alvarez-Gaum\'e and Witten in twelve dimensions and leads naturally to the Kreck-Stolz s-invariant in eleven dimensions. Hence M-theory detects diffeomorphism type of eleven-dimensional (and seven-dimensional) manifolds, and in the restriction to parallelizable manifolds classifies topological eleven-spheres. Furthermore, requiring the phase of the partition function to be anomaly-free imposes restrictions on allowed values of the s-invariant. Relating to string theory in ten dimensions amounts to viewing the bounding theory as a disk bundle, for which we study the corresponding phase in this formulation.
EXTENDED EMISSION FROM THE PSR B1259−63/SS 2883 BINARY DETECTED WITH CHANDRA

PSR B1259−63 is a middle-aged radio pulsar (P = 48 ms, τ = 330 kyr, and erg s−1) in an eccentric binary (Porb = 3.4 yr, e = 0.87) with a high-mass Be companion, SS 2883. We observed the binary near apastron with the Chandra ACIS detector on 2009 May 14 for 28 ks. In addition to the previously studied point-like source at the pulsar's position, we detected extended emission on the south–southwest side of this source. The point-like source spectrum can be described by the absorbed power-law model with the hydrogen column density NH = (2.5 ± 0.6) × 1021 cm−2, photon index Γ = 1.6 ± 0.1, and luminosity L0.5–8 keV ≈ 1.3 × 1033 d23 erg s−1, where d3 is the distance scaled to 3 kpc. This emission likely includes an unresolved part of the pulsar wind nebula (PWN) created by the colliding winds from the pulsar and the Be companion, and a contribution from the pulsar magnetosphere. The extended emission apparently consists of two components. The highly significant compact component looks like a southward extension of the point-like source image, seen up to ∼4″ from the pulsar position. Its spectrum has about the same slope as the point-like source spectrum, while its luminosity is a factor of 10 lower. We also detected an elongated feature extended ∼15″ southwest of the pulsar, but the significance of this detection is marginal. We tentatively interpret the resolved compact PWN component as a shocked pulsar wind blown out of the binary by the wind of the Be component, while the elongated component could be a pulsar jet.
RADIATION FEEDBACK IN ULIRGs: ARE PHOTONS MOVERS AND SHAKERS?

We perform multidimensional radiation hydrodynamics simulations to study the impact of radiation forces on atmospheres composed of dust and gas. Our setup closely follows that of Krumholz & Thompson, assuming that dust and gas are well-coupled and that the radiation field is characterized by blackbodies with temperatures ≳ 80 K, as might be found in ultraluminous infrared galaxies (ULIRGs). In agreement with previous work, we find that Rayleigh–Taylor instabilities develop in radiation supported atmospheres, leading to inhomogeneities that limit momentum exchange between radiation and dusty gas, and eventually providing a near balance of the radiation and gravitational forces. However, the evolution of the velocity and spatial distributions of the gas differs significantly from previous work, which utilized a less accurate flux-limited diffusion (FLD) method. Our variable Eddington tensor simulations show continuous net acceleration of the gas and never reach a steady state. In contrast, our FLD results show little net acceleration of the gas and settle into a quasi-steady, turbulent state with low velocity dispersion. The discrepancies result primarily from the inability of FLD to properly model the variation of the radiation field around structures that are less than a few optical depths across. We consider the effect of varying the optical depth and study the differences between two-dimensional and three-dimensional runs. We conclude that radiation feedback remains a plausible mechanism for driving high-Mach number turbulence in ULIRGs with sufficiently high optical depths. We discuss implications for observed systems and galactic-scale numerical simulations of feedback.