Miracle-dz/UniFAR-FTUs huggingface dataset:
Molecular epidemiology and biology of pancreatic cancer among Iranian patients: an updated preliminary review

Pancreatic cancer is one of the deadliest cancers, with a very poor prognosis and survival. The incidence and mortality of pancreatic cancer are increasing among the Iranian population. Pancreatic cancer is a multifactorial disease, and various genetic and environmental factors are involved in its pathogenesis. Genetic changes and epigenetic alterations feature prominently in the development of this disease; nevertheless, it is still not well defined for the Iranian population. According to these, the early detection of tumors is needed to reduce mortality in pancreatic cancer patients. This review aims to summarize the current knowledge about pancreatic cancer by focusing on cellular and molecular processes which have been observed among Iranian patients to elucidate the molecular pathobiology of pancreatic cancer. It is reported that immunity and inflammation, apoptosis, oxidative DNA damage and the development of diabetes mellitus are the most common cellular mechanisms, associated with pancreatic cancer. Moreover, this review introduces different factors including epigenetic (miRNAs, long non-coding RNAs and DNA methylation patterns) and genetic factors (DNA polymorphisms) as well as environmental and chemical factors that can serve as potential diagnostic, prognostic and/or therapeutic biomarkers to manage pancreatic cancer patients in the Iranian population.
Quantifying short-range correlations in nuclei

Background: Short-range correlations (SRC) are an important ingredient of the dynamics of nuclei. Purpose: An approximate method to quantify the magnitude of the two-nucleon (2N) and three-nucleon (3N) short-range correlations and their mass dependence is proposed. Method: The proposed method relies on the concept of the "universality" or "local nuclear character" of the SRC. We quantify the SRC by computing the number of independent-particle model (IPM) nucleon pairs and triples which reveal beyond-mean-field behavior. It is argued that those can be identified by counting the number of nucleon pairs and triples in a zero relative orbital momentum state. A method to determine the quantum numbers of pairs and triples in an arbitrary mean-field basis is outlined. Results: The mass dependence of the 2N and 3N SRC is studied. The predictions are compared to measurements. This includes the ratio of the inclusive inelastic electron scattering cross sections of nuclei to H-2 and He-3 at large values of the Bjorken variable. Corrections stemming from the center-of-mass motion of the pairs are estimated. Conclusions: We find that the relative probability per nucleon for 2N and 3N SRC has a soft dependence with mass number A and that the proton-neutron 2N SRC outnumber the proton-proton (neutron-neutron) 2N SRC. A linear relationship between the magnitude of the EMC effect and the predicted number of proton-neutron SRC pairs is observed. This provides support for the role of local nuclear dynamics on the EMC effect.
Improved brain community structure detection by two-step weighted modularity maximization

The human brain can be regarded as a complex network with interacting connections between brain regions. Complex brain network analyses have been widely applied to functional magnetic resonance imaging (fMRI) data and have revealed the existence of community structures in brain networks. The identification of communities may provide insight into understanding the topological functions of brain networks. Among various community detection methods, the modularity maximization (MM) method has the advantages of model conciseness, fast convergence and strong adaptability to large-scale networks and has been extended from single-layer networks to multilayer networks to investigate the community structure changes of brain networks. However, the problems of MM, suffering from instability and failing to detect hierarchical community structure in networks, largely limit the application of MM in the community detection of brain networks. In this study, we proposed the weighted modularity maximization (WMM) method by using the weight matrix to weight the adjacency matrix and improve the performance of MM. Moreover, we further proposed the two-step WMM method to detect the hierarchical community structures of networks by utilizing node attributes. The results of the synthetic networks without node attributes demonstrated that WMM showed better partition accuracy than both MM and robust MM and better stability than MM. The two-step WMM method showed better accuracy of community partitioning than WMM for synthetic networks with node attributes. Moreover, the results of resting state fMRI (rs-fMRI) data showed that two-step WMM had the advantage of detecting the hierarchical communities over WMM and was more insensitive to the density of the rs-fMRI networks than WMM.
Stellar feedback and bulge formation in clumpy discs

We use numerical simulations of isolated galaxies to study the effects of stellar feedback on the formation and evolution of giant star-forming gas ‘clumps’ in high-redshift, gas-rich galaxies. Such galactic discs are unstable to the formation of bound gas-rich clumps whose properties initially depend only on global disc properties, not the microphysics of feedback. In simulations without stellar feedback, clumps turn an order-unity fraction of their mass into stars and sink to the centre, forming a large bulge and kicking most of the stars out into a much more extended stellar envelope. By contrast, strong radiative stellar feedback disrupts even the most massive clumps after they turn ∼10–20 per cent of their mass into stars, in a time-scale of ∼10–100 Myr, ejecting some material into a superwind and recycling the rest of the gas into the diffuse interstellar medium (ISM). This suppresses the bulge formation rate by direct ‘clump coalescence’ by a factor of several. However, the galactic discs do undergo significant internal evolution in the absence of mergers: clumps form and disrupt continuously and torque gas to the galactic centre. The resulting evolution is qualitatively similar to bar/spiral evolution in simulations with a more homogeneous ISM.
Primary atomization of a liquid jet in crossflow

In this fluid dynamics video, we present a visualization of the primary atomization of a turbulent liquid jet injected into a turbulent gaseous crossflow. It is based on a detailed numerical simulation of the primary atomization region of the jet using a finite volume, balanced force, incompressible LES/DNS flow solver coupled to a Refined Level Set Grid (RLSG) solver to track the phase interface position. The visualization highlights the two distinct breakup modes of the jet: the column breakup mode of the main liquid column and the ligament breakup mode on the sides of the jet and highlights the complex evolution of the phase interface geometry.
Cervical cancer screening management practices and prevention in uMsunduzi Local Municipality primary care clinics

Background Although cervical cancer is preventable, it remains the most feared and second most common cancer in women worldwide, as well as the leading cause of cancer deaths in many low- and middle-income countries, including South Africa. Numerous studies conducted globally, in Africa and in South Africa revealed a knowledge gap about cervical cancer and its preventive strategies, including cervical cancer screening, among nurses and the general population. Aim The purpose was to investigate and describe nurses’ knowledge and management practices regarding cervical cancer screening in uMsunduzi Local Municipality, KwaZulu-Natal. Methods The study was directed by a positivism paradigm. A quantitative research approach and nonexperimental descriptive design was used in this study. Probability random sampling was used, and a self-administered questionnaire was used to collect data. Eighty-three professional nurses participated in the study. Results The study discovered that professional nurses working in selected clinics in uMsunduzi Local Municipality, KwaZulu-Natal, had a high level of knowledge about cervical cancer and its screening. Nonetheless, despite the high level of knowledge demonstrated, the level of practice remained low. Conclusion Cervical cancer morbidity and mortality have long been a major health concern in South Africa’s general population. The study found that PNs are knowledgeable about cervical cancer screening; conversely, practice was low. This paper includes recommendations for future research, nursing practice, nursing education and the Department of Health. Contribution This study contributed vastly to the body of knowledge in managing cervical cancer screening practices, particularly in health promotion and prevention of diseases at primary care level.
Participation: A Disciplinary Border for Architectural Research and Practice

This editorial note provides an extended summary and transversal analysis of ten articles gathered for the 2022 Special Issue on participation in contemporary architecture. The call for contribution circulated in June 2021 attracted papers from Central Europe (n=8) and North America (n=2), and presents an overview of ongoing practices and research in participatory architecture in these areas. The Special Issue aimed to study the connections between disciplines and gathered nine empirical cases and one literature review. In this editorial note, we first analyze these contributions to better understand the nature of architecture in participating in the profiles of end-users and project teams, and the scale of the projects. Secondly, we highlight four lessons taken from these practices and studies: we emphasize how participation in architecture (1) emerges and operates in interstitial spaces; (2) often deployed for and with “vulnerable” end-user groups, this “vulnerability” provides power and originality to processes and outcomes; (3) inspirational principles, guides, and frameworks are produced as outcomes; and finally, (4) social architectures are deployed beyond tangible concepts through a multilevel relationship to pedagogy. Finally, we observe that reflections on gender, politics, decoloniality, and disciplinary transfers remain underexplored and need to be explicitly studied and integrated.
Constraining black hole horizon effects by LIGO-Virgo detections of inspiralling binary black holes

General relativity predicts mass and spin growth of an inspiralling black hole due to an energy-momentum flux flowing through the black-hole horizon. The leading-order terms of this horizon flux introduce 2.5 and 3.5 post-Newtonian corrections to inspiral motions of binary black holes. The corrections may be measurable by gravitational waves detectors. Since the proper improvements to general relativity is still a mystery, it is possible that the true modified gravity theory introduces negligible direct corrections to the geodesics of test masses, while near horizon corrections are observable. We introduce a parameterization to describe arbitrary mass and spin growth of inspiralling black holes. Comparing signals of gravitational waves and a waveform model with parameterized horizon flux corrections, deviations from general relativity can be constrained. We simulate a set of gravitational waves signals following an astrophysical distribution with horizon flux modifications. Then, we perform a Bayesian analysis to obtain the expected constraints from the simulated response of the Advanced LIGO-Virgo detector network to the simulated signals. We show that the constraint can be improved by stacking multiple detections. The constraints of modified horizon flux can be used to test a specific class of modified gravity theories which predict dominant corrections near black-hole horizons over other types of corrections to general relativity. To support Hawking's area theorem at 90\% confidence level, over 10000 LIGO-Virgo detections are required. Within the lifetime of LIGO and Einstein Telescope, a future ground-based gravitational wave detector, near horizon corrections of modified gravity theories are potentially detectable if one of the modified gravity theory is true and the theory predicts a strong correction.
The First Billion Years project: proto-galaxies reionizing the universe

The contribution of stars in galaxies to cosmic reionization depends on the star formation history in the Universe, the abundance of galaxies during reionization, the escape fraction of ionizing photons and the clumping factor of the intergalactic medium. We compute the star formation rate and clumping factor during reionization in a cosmological volume using a high-resolution hydrodynamical simulation. We post-process the output with detailed radiative transfer simulations to compute the escape fraction of ionizing photons. Together, this gives us the opportunity to assess the contribution of galaxies to reionization self-consistently. The strong mass and redshift dependence of the escape fraction indicates that reionization occurred between z = 15 and 10 and was mainly driven by proto-galaxies forming in dark matter haloes with masses between 10 7 and 10 8 M� . More massive galaxies that are rare at these redshifts and have significantly lower escape fractions contribute less photons to the reionization process than the more-abundant low-mass galaxies. Star formation in the low-mass haloes is suppressed by radiative feedback from reionization, therefore these proto-galaxies only contribute when the part of the Universe they live in is still neutral. Afterz ∼ 10, massive galaxies become more abundant and provide most of the ionizing photons. In addition, we find that Population III stars are too short-lived and not frequent enough to have a major contribution to reionization. Although the stellar component of the proto-galaxies that produce the bulk of ionizing photons during reionization is too faint to be detected by theJamesWebbSpaceTelescope (JWST), these sources are brightest in the Hα and Lyα recombination lines, which will likely be detected by JWST in deep surveys.
Conching chocolate is a prototypical transition from frictionally jammed solid to flowable suspension with maximal solid content

Significance Chocolate conching is the process in which an inhomogeneous mixture of fat, sugar, and cocoa solids is transformed into a homogeneous flowing liquid. Despite the popularity of chocolate and the antiquity of the process, until now, there has been poor understanding of the physical mechanisms involved. Here, we show that two of the main roles of conching are the mechanical breakdown of aggregates and the reduction of interparticle friction through the addition of a dispersant. Intriguingly, the underlying physics we describe is related to the popular stunt of “running on cornstarch. ” The mixing of a powder of 10- to 50-μm primary particles into a liquid to form a dispersion with the highest possible solid content is a common industrial operation. Building on recent advances in the rheology of such “granular dispersions,” we study a paradigmatic example of such powder incorporation: the conching of chocolate, in which a homogeneous, flowing suspension is prepared from an inhomogeneous mixture of particulates, triglyceride oil, and dispersants. Studying the rheology of a simplified formulation, we find that the input of mechanical energy and staged addition of surfactants combine to effect a considerable shift in the jamming volume fraction of the system, thus increasing the maximum flowable solid content. We discuss the possible microscopic origins of this shift, and suggest that chocolate conching exemplifies a ubiquitous class of powder–liquid mixing.
The Effect of Cognitive Strategies and Facial Attractiveness on Empathic Neural Responses

Empathy is a phenomenon that brings together both emotions and an understanding of another person. Recent studies have disentangled the mechanisms of empathy into emotional and cognitive aspects. Event-related potential (ERP) studies suggest that emotional empathy is related to the modulation of the amplitude of early ERPs, and cognitive empathy is linked to later ERPs. In the current study, we examined the influences of facial attractiveness on empathic response and the effect of cognitive strategies with setting the participants’ attention to attractiveness or pain. Participants (N= 19) viewed photos of physically attractive and unattractive men and women receiving painful stimulation. The amplitude of the N2 component measured at the frontal regions was more negative in painful stimulation compared to the non-painful, but only for attractive faces. There were no differences between painful and non-painful stimulation for unattractive faces. The amplitude of the P3 measured at the central-parietal region component was more positive in the painful condition compared to the non-painful one, but only when participants performed a pain judgment task. There were no differences in the attractiveness judgment task. This study showed that the attractiveness of a model and drawing the participants’ attention to pain constitute an essential modulator of pain empathy.
The cooling time of white dwarfs produced from type Ia supernovae

Type Ia supernovae (SNe Ia) play a key role in measuring cosmological parameters, in which the Phillips relation is adopted. However, the origin of the relation is still unclear. Several parameters are suggested, e.g. the relative content of carbon to oxygen (C/O) and the central density of the white dwarf (WD) at ignition. These parameters are mainly determined by the WD's initial mass and its cooling time, respectively. Using the progenitor model developed by Meng & Yang, we present the distributions of the initial WD mass and the cooling time. We do not find any correlation between these parameters. However, we notice that as the range of the WD's mass decreases, its average value increases with the cooling time. These results could provide a constraint when simulating the SN Ia explosion, i.e. the WDs with a high C/O ratio usually have a lower central density at ignition, while those having the highest central density at ignition generally have a lower C/O ratio. The cooling time is mainly determined by the evolutionary age of secondaries, and the scatter of the cooling time decreases with the evolutionary age. Our results may indicate that WDs with a long cooling time have more uniform properties than those with a short cooling time, which may be helpful to explain why SNe Ia in elliptical galaxies have a more uniform maximum luminosity than those in spiral galaxies.
Service Function Chaining and Embedding With Heterogeneous Faults Tolerance in Edge Networks

In the 5G-and-beyond era, ultra-reliable low latency communication (URLLC) services are ubiquitous in edge networks. To enhance the performance metrics and the quality of service (QoS), URLLC services are delivered via a sequence of software-based network functions, also known as a service function chain (SFC). Towards reliable SFC delivery, it is imperative to incorporate fault-tolerance during SFC deployments. However, deploying an SFC with fault-tolerance is challenging because the protection mechanism needs to jointly consider multiple concurrent physical/virtual network failures and hardware/software failures. Considering these concurrent heterogeneous failures, this work investigates how to effectively deliver an SFC in edge networks with the objective of minimizing bandwidth resource consumption. First, we introduce the concept of <inline-formula> <tex-math notation="LaTeX">${k}$ </tex-math></inline-formula>-heterogeneous-faults-tolerance and propose an augmented protection graph, called <inline-formula> <tex-math notation="LaTeX">${k}$ </tex-math></inline-formula>-connected service function slices layered graph (KC-SLG). Based on the KC-SLG, we formulate a novel problem called <inline-formula> <tex-math notation="LaTeX">${k}$ </tex-math></inline-formula>-heterogeneous-faults-tolerant SFC embedding and propose an effective algorithm, called fault-tolerant service function graph embedding (FT-SFGE). FT-SFGE employs two proposed techniques: <inline-formula> <tex-math notation="LaTeX">${k}$ </tex-math></inline-formula>-connected network slicing (KC-NS) and <inline-formula> <tex-math notation="LaTeX">${k}$ </tex-math></inline-formula>-connected function slicing (KC-FS). Via thorough mathematical proofs, we show that KC-NS is 2-approximate. Extensive simulations show that KC-FS has the best average cost-efficiency when <inline-formula> <tex-math notation="LaTeX">${k}$ </tex-math></inline-formula> = 2, and FT-SFGE outperforms the schemes directly extended from the state-of-the-art.
MMTF DISCOVERY OF GIANT IONIZATION CONES IN MR 2251−178: IMPLICATIONS FOR QUASAR RADIATIVE FEEDBACK

We report the discovery of giant ionization cones in the 140 kpc nebula around quasar MR 2251−178 based on deep [O iii] λ5007/Hβ and [N ii] λ6583/Hα flux ratio maps obtained with the Maryland–Magellan Tunable Filter on the Baade–Magellan 6.5 m Telescope. These cones are aligned with the weak double-lobed radio source observed on smaller scale (<30 kpc). They have an opening angle ∼120° ± 10° and subtend ∼65%–90% of 4π sr, where the uncertainty takes into account possible projection effects. The material in the outer ionization cones is matter-bounded, indicating that all ionizing photons emitted through the cones escape from the system. The quasar ionizing flux is ∼2–3 times fainter outside of these cones, despite the largely symmetric geometry of the nebula in [O iii]. Overall, adding up the contributions from both inside and outside the cones, we find that ∼65%–95% of the quasar ionizing radiation makes its way out of the system. These results emphasize the need for line ratio maps to quantify the escape fraction of ionizing radiation from quasars and the importance of quasar radiative feedback on the intergalactic medium.
Non-Gaussianity from the bispectrum in general multiple field inflation

We study the non-Gaussianity from the bispectrum in multi-field inflation models with a general kinetic term. The models include multi-field K-inflation and multi-field Dirac–Born–Infeld (DBI) inflation as special cases. We find that, in general, the sound speeds for the adiabatic and entropy perturbations are different and they can be smaller than 1. Then the non-Gaussianity can be enhanced. Multi-field DBI inflation is shown to be a special case where both sound speeds are the same due to a special form of the kinetic term (Langlois et al 2008 Preprint 0804.3139 [hep-th]). We derive the exact second-and third-order actions including metric perturbations. In the small sound speed limit and at leading order in the slow-roll expansion, we derive the three-point function for the curvature perturbation which depends on both adiabatic and entropy perturbations. The contribution from the entropy perturbations has a different momentum dependence if the sound speeds for the entropy and adiabatic perturbations are different, which provides a possibility to distinguish multi-field models from single-field models. On the other hand, in the multi-field DBI case, the contribution from the entropy perturbations has the same momentum dependence as the pure adiabatic contributions and it only changes the amplitude of the three-point function (Langlois et al 2008 Preprint 0804.3139 [hep-th]). This could help to ease the constraints on the DBI-inflation models.