Miracle-dz/UniFAR-FTUs huggingface dataset:
Minimum glitch of the Crab pulsar and the crustquake as a trigger mechanism

We discuss the minimum glitch size of Crab observed by Espinoza et al. (2014). Modelling the crustquake as a trigger mechanism we estimate the size of the broken plate. The plate size obtained, D $\sim 100 m$ is comparable to plate size estimates for PSR J1119--6127. The plate size naturally leads to an estimate of the number of unpinned vortices involved in the glitch, $N \sim 10^{13} $. This number is of the same order in all Crab and Vela pulsar glitches. The mimimum glitch relates the constancy of all these numbers among different pulsars to the basic plate size involved in crust breaking. This in turn depends on the critical strain angle $\theta_{cr}$ of the Coulomb lattice in the neutron star crust. The minimum glitch size implies $\theta_{cr} \sim 10^{-1}$ in agreement with theoretical and computational estimates.
Coexistence of a non thermal jet and a complex ultra fast X-ray outflow in a moderately luminous AGN

Context: Recent XMM-Newton observations have revealed that IRAS 17020+4544 is a very unusual example of black hole wind-produced feedback by a moderately luminous AGN in a spiral galaxy. Aims: Since the source is known for being a radio emitter, we investigated about the presence and the properties of a non-thermal component. Methods: We observed IRAS 17020+4544 with the Very Long Baseline Array at 5, 8, 15, and 24 GHz within a month of the 2014 XMM-Newton observations. We further analysed archival data taken in 2000 and 2012. Results: We detect the source at 5 GHz and on short baselines at 8 GHz. At 15 and 24 GHz, the source is below our baseline sensitivity for fringe fitting, indicating the lack of prominent compact features. The morphology is that of an asymmetric double, with significant diffuse emission. The spectrum between 5 and 8 GHz is rather steep ($S(\nu)\sim\nu^{-(1.0\pm0.2)}$). Our re-analysis of the archival data at 5 and 8 GHz provides results consistent with the new observations, suggesting that flux density and structural variability are not important in this source. We put a limit on the separation speed between the main components of $<0.06c$. Conclusions: IRAS 17020+4544 shows interesting features of several classes of objects: its properties are typical of compact steep spectrum sources, low power compact sources, radio-emitting narrow line Seyfert 1 galaxies. However, it can not be classified in any of these categories, remaining so far a one-of-a-kind object.
Selective Exposure to Balanced Content and Evidence Type: The Case of Issue and Non-Issue Publics About Climate Change and Health Care

We examine three under-studied factors in selective exposure research. Linking issue publics and motivated reasoning literatures, we argue that selectivity patterns depend on (a) whether an individual is an issue public member; (b) the availability of balanced, pro-, and counter-attitudinal content; and (c) the evidence for a message claim (numerical vs. narrative). Using an online experiment (N = 560), we track information selection about climate change and health care. Most notably, on both issues, issue publics selected more balanced content with numerical evidence, compared with non-issue publics. We discuss the implications of our findings for the selective exposure literature.
New Low-mass Stars in the 25 Orionis Stellar Group and Orion OB1a Sub-association from SDSS-III/BOSS Spectroscopy

The Orion OB1a sub-association is a rich low-mass star (LMS) region. Previous spectroscopic studies have confirmed 160 LMSs in the 25 Orionis stellar group (25 Ori), which is the most prominent overdensity of Orion OB1a. Nonetheless, the current census of the 25 Ori members is estimated to be lower than 50% complete, leaving a large number of members to be still confirmed. We retrieved 172 low-resolution stellar spectra in Orion OB1a observed as ancillary science in the SDSS-III/BOSS survey, for which we classified their spectral types and determined physical parameters. To determine memberships, we analyzed the emission, Li iλ6708 absorption, and Na iλλ8183, 8195 absorption as youth indicators in stars classified as M type. We report 50 new LMSs spread across the 25 Orionis, ASCC 18, and ASCC 20 stellar groups with spectral types from M0 to M6, corresponding to a mass range of . This represents an increase of 50% in the number of known LMSs in the area and a net increase of 20% in the number of 25 Ori members in this mass range. Using parallax values from the Gaia DR1 catalog, we estimated the distances to these three stellar groups and found that they are all co-distant, at 338 ± 66 pc. We analyzed the spectral energy distributions of these LMSs and classified their disks into evolutionary classes. Using H-R diagrams, we found a suggestion that 25 Ori could be slightly older than the other two observed groups in Orion OB1a.
DISRUPTION OF STAR CLUSTERS IN THE INTERACTING ANTENNAE GALAXIES

We re-examine the age distribution of star clusters in the Antennae in the context of N-body+hydrodynamical simulations of these interacting galaxies. All of the simulations that account for the observed morphology and other properties of the Antennae have star formation rates that vary relatively slowly with time, by factors of only 1.3–2.5 in the past 108 yr. In contrast, the observed age distribution of the clusters declines approximately as a power law, dN/dτ∝τγ with γ = −1.0, for ages 106 yr ≲ τ ≲ 109 yr. These two facts can only be reconciled if the clusters are disrupted progressively for at least ∼108 yr and possibly ∼109 yr. When we combine the simulated formation rates with a power-law model, fsurv∝τδ, for the fraction of clusters that survive to each age τ, we match the observed age distribution with exponents in the range −0.9 ≲ δ ≲ −0.6 (with a slightly different δ for each simulation). The similarity between δ and γ indicates that dN/dτ is shaped mainly by the disruption of clusters rather than variations in their formation rate. Thus, the situation in the interacting Antennae resembles that in relatively quiescent galaxies such as the Milky Way and the Magellanic Clouds.
DISCOVERY OF γ-RAY PULSATION AND X-RAY EMISSION FROM THE BLACK WIDOW PULSAR PSR J2051−0827

We report the discovery of pulsed γ-ray emission and X-ray emission from the black widow millisecond pulsar PSR J2051−0827 by using the data from the Large Area Telescope (LAT) on board the Fermi Gamma-ray Space Telescope and the Advanced CCD Imaging Spectrometer array on the Chandra X-Ray Observatory. Using three years of LAT data, PSR J2051−0827 is clearly detected in γ-rays with a significance of ∼8σ in the 0.2–20 GeV band. The 200 MeV–20 GeV γ-ray spectrum of PSR J2051−0827 can be modeled by a simple power law with a photon index of 2.46 ± 0.15. Significant (∼5σ) γ-ray pulsations at the radio period were detected. PSR J2051−0827 was also detected in soft (0.3–7 keV) X-ray with Chandra. By comparing the observed γ-rays and X-rays with theoretical models, we suggest that the γ-ray emission is from the outer gap while the X-rays can be from intra-binary shock and pulsar magnetospheric synchrotron emissions.
OVR SEEN : Auditing Network Traffc and Privacy Policies in Oculus VR

Virtual reality (VR) is an emerging technology that enables new applications but also introduces privacy risks. In this paper, we focus on Oculus VR (OVR), the leading platform in the VR space and we provide the frst comprehensive analysis of personal data exposed by OVR apps and the platform itself, from a combined networking and privacy policy perspective. We experimented with the Quest 2 headset and tested the most popular VR apps available on the offcial Oculus and the SideQuest app stores. We developed OVR SEEN , a methodology and system for collecting, analyzing, and comparing network traffc and privacy policies on OVR. On the networking side, we captured and decrypted network traffc of VR apps, which was previously not possible on OVR, and we extracted data fows, defned as h app, data type, destination i . Compared to the mobile and other app ecosystems, we found OVR to be more centralized and driven by tracking and analytics, rather than by third-party advertising. We show that the data types exposed by VR apps include personally identi-fable information (PII), device information that can be used for fngerprinting, and VR-specifc data types. By comparing the data fows found in the network traffc with statements made in the apps’ privacy policies, we found that approximately 70% of OVR data fows were not properly disclosed. Furthermore, we extracted additional context from the privacy policies, and we observed that 69% of the data fows were used for purposes unrelated to the core functionality of apps.
The Influence of Sleep Quantity on Externalizing Behaviors in Adolescents: The Mediating Effect of Inhibition

Adolescents are particularly vulnerable to sleep disruptions due both to hormonal changes (causing a shift in circadian rhythms, Pieters et al., 2015) and to school and extra-curricular commitments leading to sleep restriction (Carskadon, 2011). Sleep quantity, in turn, has been independently linked to low response inhibition as well as externalizing behaviors (Lowe et al., 2017; Gregory & Sadeh, 2012). This study aims to build upon these findings by testing the hypothesis that decreased inhibition will mediate the relationship between low quantity of sleep and externalizing behaviors. A representative sample of adolescents in Chicago, Illinois was recruited to participate in a larger study of stress processes. Ninety-four of the participants were randomly selected from the larger study to also take part in a 4-day actigraph watch collection to track sleep quantity. Regression analyses identified associations between sleep quantity and inhibition and externalizing symptoms, whereas there were no associations identified between sleep quantity and inhibition. Results of mediational analyses wherein inhibition was tested as a mediator of the effects of sleep quantity on externalizing symptoms were not significant. Yet, the findings of this study can inform prevention and intervention strategies for at-risk youth as well as guide future research on risk and protective factors.
BIROn - Birkbeck Institutional Research Online Tilt adaptation aftereffects reveal fundamental perceptual characteristics of tactile orientation processing the hand.

Orientation information contributes substantially to our tactile perception such as feeling an object’s shape on the skin. For vision, a perceptual adaptation aftereffect (tilt aftereffect; TAE), which is well explained by neural orientation selectivity, has been used to reveal fundamental perceptual properties of orientation processing. Neural orientation selectivity has been reported in somatosensory cortices. However, little research has investigated the perceptual characteristics of the tactile TAE. The aim of the current study was to provide the first demonstration of a tactile TAE on the hand and investigate the perceptual nature of tactile TAE on the hand surface. We used a two-point stimulation with minimal input for orientation. We found clear TAEs on the hand surface: Adaptation induced shifts in subjective vertical sensation toward the orientation opposite to the adapted one. Further, adaptation aftereffects were purely based on orientation processing given that the effects transferred between different lengths across adaptor and test stimuli and type of stimuli. Finally, adaptation aftereffects were anchored to the hand: tactile TAE occurred independently of hand rotation and transferred from palm to dorsum sides of the hand, while the effects did not transfer between hands. Our findings demonstrate the existence of hand-centered perceptual processing for basic tactile orientation information.
[O II] nebular emission from Mg II absorbers: star formation associated with the absorbing gas

We present nebular emission associated with 198 strong Mg II absorbers at 0.35 $\le z \le$ 1.1 in the fibre spectra of quasars from the Sloan Digital Sky Survey. Measured [O II] luminosities (L$_{[O II]}$) are typical of sub-L$^{\star}$ galaxies with derived star formation rate (uncorrected for fibre losses and dust reddening) in the range of 0.5-20 ${\rm M_\odot\ yr^{-1}}$. Typically less than $\sim$ 3% of the Mg II systems with rest equivalent width, $W_{2796}$ $\ge$ 2 \AA, show L$_{[O II]} \ge 0.3$ L$^{\star}_{[O II]}$. The detection rate is found to increase with increasing $W_{2796}$ and $z$. No significant correlation is found between $W_{2796}$ and L$_{[O II]}$ even when we restrict the samples to narrow $z$-ranges. A strong correlation is seen between L$_{[O II]}$ and $z$. While this is expected from the luminosity evolution of galaxies, we show finite fibre size plays a very crucial role in this correlation. The measured nebular line ratios (like [O III]/[O II] and [O III]/H$\beta$) and their $z$ evolution are consistent with those of galaxies detected in deep surveys. Based on the median stacked spectra, we infer the average metallicity (log Z $\sim$8.3), ionization parameter (log $q$ $\sim$7.5) and stellar mass (log (M/M$_\odot$)$\sim$9.3). The Mg II systems with nebular emission typically have $W_{2796}$ $\ge 2$ \AA, Mg II doublet ratio close to 1 and W(Fe II$\lambda$2600)/$W_{2796}$ $\sim 0.5$ as often seen in damped Ly$\alpha$ and 21-cm absorbers at these redshifts. This is the biggest reported sample of [O II] emission from Mg II absorbers at low impact parameters ideally suited for probing various feedback processes at play in $z\le 1$ galaxies.
Dynamical friction of massive objects in galactic centres

Dynamical friction leads to an orbital decay of massive objects like young compact star clusters or massive black holes in central regions of galaxies. The dynamical friction force can be well approximated by Chandrasekhar's standard formula, but recent investigations show that corrections to the Coulomb logarithm are necessary. With a large set of N-body simulations we show that the improved formula for the Coulomb logarithm fits the orbital decay very well for circular and eccentric orbits. The local scalelength of the background density distribution serves as the maximum impact parameter for a wide range of power-law indices of -1 . -5. For each type of code the numerical resolution must be compared to the effective minimum impact parameter in order to determine the Coulomb logarithm. We also quantify the correction factors by using self-consistent velocity distribution functions instead of the standard Maxwellian often used. These factors enter directly the decay time-scale and cover a range of 0.5 . 3 for typical orbits. The new Coulomb logarithm combined with self-consistent velocity distribution functions in the Chandrasekhar formula provides a significant improvement of orbital decay times with correction up to one order of magnitude compared to the standard case. We suggest the general use of the improved formula in parameter studies as well as in special applications.
EFFECT OF STEAM BATH AND SAUNA BATH ON SERUM TRIGLYCERIDE LEVELS IN OBESE INDIVIDUALS- A COMPARATIVE STUDY

Background and Objectives Obesity is a medical condition in which excess or abnormal body fat gets accumulated in adipose tissue that causes adverse effects on health, which leads to reduced life expectancy. Its increasing prevalence worldwide makes obesity an important health issue. Steam bath is one of the most important forms of water treatments, which induces perspiration in a most natural way. Sauna bath, is a form of dry heat therapy practiced for purpose of relaxation and pleasure. Excessive intake of carbohydrate, fat or alcohol may each contribute to increased plasma triglyceride (TG) by different mechanism. Elevated triglyceride is common in obesity, diabetes and insulin resistance. Present study was aimed to evaluate and compare the effect of steam bath and sauna bath on serum triglycerides in obese individual. Materials and methods: A total of 100 Subjects were screened for inclusion and exclusion criteria and recruited. Randomly divided into 2 groups Group1 (Steam bath) and Group2 (Sauna Bath) Pre-assessments were recorded before the intervention. Intervention was given daily morning for 10days.Group 1(STB): Subjects received steam bath for 15 minutes. Group 2(SB): Subjects received sauna bath for 15 minutes. Post assessments were recorded after 10 days of intervention. RESULTS: Within group changes suggested significant changes in Triglyceride (p≤0.001), waist circumference (p≤0.001), hip circumference (p≤0.001), and BMI in both the groups on comparison with their respective baseline values. Waist hip ratio showed a greater change following sauna bath (p≤0.001) as compared to the steam bath (p=0.032). INTERPRETATION AND CONCLUSION: Sauna bath and steam bath are two different treatments in naturopathy application of these hydriatic therapies causes significant reduction in triglyceride levels also reduction in waist circumference and hip circumference were observed. Thus, application of sauna bath and steam bath treatments causes effective decrease in triglyceride levels among obese individuals.
Kazuistika Case report Pregnancy-Associated Cardiomyopathy (PACM) in a Preeclamptic Woman with Twin Pregnancy: A Case Report

Peripartum cardiomyopathy (PPCM) is an uncommon disease, a dilated cardiomyopathy type occurs in the ﬁ nal gestation month and within 5 months after giving birth. A related term, pregnancy-associated cardio- myopathy (PACM) occurs before it. The morbidity and mortality rates are high. Women with preeclampsia with twin pregnancies are at a markedly elevated risk of developing PACM/PPCM. A 40-year-old multiparous woman with twin pregnancy came to the emergency room at gestational week 20, exhibited cough, dyspnea, full bilateral rales, extremities edema, cardiomegaly, hypertension, proteinuria, and the left ventri- cular ejection fraction was 26%. She was diagnosed with acute lung edema, PACM, and preeclampsia. The pregnancy was terminated and treated with drug therapy of heart failure. Delay of diagnostic procedures may lead to severe maternal morbidity and infant mortality in this PACM case. It emphasized the need for attention of the risk factors, preeclamptic and twin pregnancy, and may be candidates for monitoring of left ventricular function. Early and appropriate management may prevent irreversible PACM. Klíčová slova: Peripartální kardiomyopatie
Steep Decay Phase Shaped by the Curvature Effect. II. Spectral Evolution

We derive a simple analytical formula to describe the evolution of spectral index β in the steep decay phase shaped by the curvature effect with the assumption that the spectral parameters and Lorentz factor of the jet shell are the same for different latitudes. Here, the value of β is estimated in the 0.3−10 keV energy band. For a spherical thin shell with a cutoff power-law (CPL) intrinsic radiation spectrum, the spectral evolution can be read as a linear function of observer time. For the situation with the Band function intrinsic radiation spectrum, the spectral evolution may be complex. If the observed break energy of the radiation spectrum is larger than 10 keV, the spectral evolution is the same as that shaped by jet shells with a CPL spectrum. If the observed break energy is less than 0.3 keV, the value of β would be a constant. For others, the spectral evolution can be approximated as a logarithmal function of the observer time in general.
ON ORIGIN AND DESTRUCTION OF RELATIVISTIC DUST AND ITS IMPLICATION FOR ULTRAHIGH ENERGY COSMIC RAYS

Dust grains may be accelerated to relativistic speeds by radiation pressure, diffusive shocks, and other acceleration mechanisms. Such relativistic grains have been suggested as primary particles of ultrahigh energy cosmic rays (UHECRs). In this paper, we first revisit the problem of acceleration by radiation pressure and calculate maximum grain velocities achieved. We find that grains can be accelerated to relativistic speeds with Lorentz factor γ < 2 ? > by powerful radiation sources, which is lower than earlier estimates showing that γ could reach ∼10. We then investigate different destruction mechanisms for relativistic grains traversing a variety of environments. In solar radiation, we find that the destruction by thermal sublimation and Coulomb explosions is important. We also quantify grain destruction due to electronic sputtering by ions and grain–grain collisions. Electronic sputtering is found to be rather inefficient, whereas the evaporation following grain–grain collisions is shown to be an important mechanism for which the a ∼ ? > 0.01–1 &mgr; m ? > grains would be destroyed after sweeping a gas column N coll ∼ 5 × 10 19 ? > – 5 × 10 20 cm − 2 ? > . Relativistic dust in the interstellar medium and intergalactic medium (IGM) would be disrupted by Coulomb explosions due to collisional charging after traversing a gas column N coll ∼ 10 17 cm − 2 ? > unless grain material is very strong. We show that photoelectric emission by optical and ultraviolet background radiation is also significant for the destruction of relativistic dust in the IGM. The obtained results indicate that relativistic dust from galaxies would be destroyed before reaching the Earth's atmosphere and unlikely to account for UHECRs.
Impact of Institutions and Policy on Economic Growth: Empirical Evidence

We reviewed the empirical evidence for the effect of institutions on per capita GDP growth. Although several of the literature suggested institutions are the primary cause of growth; empirical evidence is somewhat inconclusive. On one hand, it partly reflects that technical limitations - especially heterogeneity - have not been adequately addressed in these studies. On the other hand, there seems to be no consensus on which institutions specifically cause growth. We test the effect of four clusters of institutions (Using Rodrik-2005 Taxonomy) on growth using dynamic GMM panel estimation. The taxonomy provides a functional definition of institutions, allowing us to identify exactly the type of institutions that affect growth. Meantime, our methodology has been technically improved without the need to look for “external” tools to address the problem of homogeneity. More importantly, we can estimate the effects of institutional change (short-term effects of institutions) on growth, without assuming institutional stability. barrier (domestic regulatory environment). The fifth paper, entitled “Cross Countries Economic Performances - SPF Approach”, explores the differences in technical inefficiency (inefficient allocation of production inputs) and explains the diverse cross-country economic performances, using estimating a “global” stochastic production frontier (SPF) mod.
The structure and motion of incoherent {\Sigma}3 grain boundaries in FCC metals

Synthetic driving force molecular dynamics simulations were utilized to survey grain boundary mobility in three classes of incoherent {\Sigma}3 twin boundaries: , , and tilt boundaries. These boundaries are faceted on low energy planes, and step flow boundary motion occurs by glide of the triplets of partial dislocations that comprise the mobile facets. Systematic trends with inclination angle are identified and characterized. Observations of thermally activated, anti-thermal, and athermal motion are explained in terms of the orientation of the Shockley partial dislocations along close-packed and non-close-packed directions. Thermally activated boundaries follow a compensation effect associated with a facet roughening transition. As for all faceting boundaries, system size and driving force must be chosen with care to prevent simulation artifacts.
Lecture 6 : Simple Relaxation and Yield Problems

All of the microstructural elements discussed so far have been rigid. Most real nonNewtonian fluids are composed of deformable bodies, such as liquid drops or flexible polymers. Allowing deformable microstructure dramatically increases the complexity of the problem because the microstructure now has a large number of internal degrees of freedom. We will first consider the case of dilute suspensions where the interactions between the microscopic particles can be ignored.