Miracle-dz/UniFAR-FTUs huggingface dataset:
Efficacy of red low-level laser for postoperative pain management: A review of literature

Many patients who undergo surgical procedures experience acute postoperative pain, with less than half receiving adequate pain relief. Recent advancements in postoperative pain management include the market clearance by the US Food and Drug Administration for the utilisation of red low-level laser therapy in providing postoperative pain relief. The Food and Drug Administration market clearance was based on clinical data from randomised controlled trials that supported the safety and effectiveness of visible red laser therapy across various surgical procedures. This review of literature aims to evaluate the mechanisms of action, the dose–response curves and clinical outcomes of red low-level laser for postoperative pain management. A literature search was limited to randomised controlled trials that evaluated the use of red low-level laser therapy on postoperative pain. The results from the literature search found that seven studies met the search qualifications. The literature review findings demonstrated that red low-level laser therapy is a safe and effective treatment alternative for postoperative pain management. In addition to postoperative pain reduction, the findings of the literature revealed that red low-level laser therapy may promote healing and reduce the consumption of postoperative prescription analgesic drugs.
A RELATIONSHIP BETWEEN THE LENGTH AND ACTIVITY OF SUNSPOT CYCLES

In studying relationships between the length and the activity of sunspot cycles, three indices are considered for the activity of the 1 1 -year cycle in the number of sunspots : ( 1 ) the mean relative sunspot number for the whole cycle ; (2) the cycle totals of the relative spot numbers ; and (3) the maximum smoothed 12-month mean in the cycle. The data used are the Zurich relative sunspot numbers,1'2 1749-1951, and the cycle means, 1698-1755, derived by H. Fritz.3 The cycle totals are the sums of the monthly mean sunspot numbers in each cycle. The cycle means are the cycle totals divided by the number of months from one minimum to the next. These data are listed in Table I. The relationships between some parameters of sunspot number and cycle length are discussed.
Systematic Analysis of Spectral Energy Distributions and the Dust Opacity Indices for Class 0 Young Stellar Objects

We are motivated by the recent measurements of dust opacity indices (β) around young stellar objects (YSOs), which suggest that efficient grain growth may have occurred earlier than the Class I stage. The present work makes use of abundant archival interferometric observations at submillimeter, millimeter, and centimeter wavelength bands to examine grain growth signatures in the dense inner regions (<1000 au) of nine Class 0 YSOs. A systematic data analysis is performed to derive dust temperatures, optical depths, and dust opacity indices based on single-component modified blackbody fittings to the spectral energy distributions (SEDs). The fitted dust opacity indices (β) are in a wide range of 0.3–2.0 when single-component SED fitting is adopted. Four out of the nine observed sources show β lower than 1.7, the typical value of the interstellar dust. Low dust opacity index (or spectral index) values may be explained by the effect of dust grain growth, which makes . Alternatively, the very small observed values of β may be interpreted by the presence of deeply embedded and hot inner disks, which only significantly contribute to the observed fluxes at long wavelength bands. This possibility can be tested by the higher angular resolution imaging observations of ALMA or more detailed sampling of SEDs in the millimeter and centimeter bands. The β values of the remaining five sources are close to or consistent with 1.7, indicating that grain growth would start to significantly reduce the values of β no earlier than the late Class 0 stage for these YSOs.
The Spectral Energy Distribution of the Seyfert Galaxy Ton S180

We present spectral results from a multisatellite, broadband campaign on the narrow-line Seyfert 1 galaxy Ton S180 (PHL 912) performed at the end of 1999. We discuss the spectral energy distribution (SED) of the source, combining simultaneous Chandra, ASCA, and Extreme Ultraviolet Explorer data with contemporaneous Far Ultraviolet Spectroscopic Explorer (FUSE), Hubble Space Telescope, and ground-based optical and infrared data. The resulting SED shows that most of the energy is emitted in the 10-100 eV regime, which must be dominated by the primary energy source. No spectral turnover is evident in the UV regime. This, the strong soft X-ray emission, and the overall shape of the SED indicate that emission from the accretion disk peaks between 15 and 100 eV. High-resolution FUSE spectra showing UV absorption due to O VI and the lack of detectable X-ray absorption in the Chandra spectrum demonstrate the presence of a low column density of highly ionized gas along our line of sight. The highly ionized state of the circumnuclear gas is most likely linked to the high luminosity and steep spectrum of the active nucleus. Given the strong ionizing flux in Ton S180, it is possible that the clouds within a few tens of light days of the central source are too highly ionized to produce much line emission. Thus, the narrow width of the emission lines in Ton S180 is due to the emission arising from large radii.
Output feedback stabilizability and passivity in nonstationary and nonlinear systems

Passivity properties and passivity conditions have been shown to be very important for the stability of various methodologies of control with uncertainty in linear‐time‐invariant (LTI) systems. Many publications have defined the conditions that allow LTI systems to become strictly passive (and their transfer function strictly positive real) via constant or dynamic output feedback. As beyond the usual uncertainty, real‐world systems are not necessarily invariant, this paper expands the applicability of previous results to nonstationary and nonlinear systems. The paper first reviews a few pole–zero dynamics definitions in nonstationary systems and relates them to stability and passivity of the systems. The paper then finds the sufficient conditions that allow nonstationary systems to become stable and strictly passive via static or dynamic output feedback. Applications in robotics and adaptive control are also presented. Copyright © 2009 John Wiley & Sons, Ltd.
δ Ceti Is Not Monoperiodic: Seismic Modeling of a β Cephei Star from MOST Space-based Photometry

The β Cephei star δ Ceti was considered one of the few monoperiodic variables in its class. Despite (or perhaps because of) its apparently simple oscillation spectrum, it has been challenging and controversial to identify this star's pulsation mode and constrain its physical parameters seismically. Broadband time-resolved photometry of δ Ceti spanning 18.7 days with a duty cycle of about 65% obtained by the Microvariability and Oscillations of Stars (MOST) satellite—the first scientific observations ever obtained by MOST—reveals that the star is actually multiperiodic. Besides the well-known dominant frequency of f1 = 6.205886 day-1, we have discovered in the MOST data its first harmonic 2f1 and three other frequencies (f2 = 3.737, f3 = 3.673, and f4 = 0.318 day-1), all detected with a signal-to-noise ratio > 4. In retrospect, f2 was also present in archival spectral line-profile data but at lower S/N. We present seismic models whose modes match exactly the frequencies f1 and f2. Only one model falls within the common part of the error boxes of the star's observed surface gravity and effective temperature from photometry and spectroscopy. In this model, f1 is the radial (l = 0) first overtone, and f2 is the g2 (l = 2, m = 0) mode. This model has a mass of 10.2 ± 0.2 M☉ and an age of 17.9 ± 0.3 Myr, making δ Ceti an evolved β Cephei star. If f2 and f3 are rotationally split components of the same g2 mode, then the star's equatorial rotation velocity is either 27.6 km s-1 or half this value. Given its v sin i of about 1 km s-1, this implies that we are seeing δ Ceti nearly pole-on.
Osteohistological characterization of notosuchian osteoderms: Evidence for an overlying thick leathery layer of skin

Osteoderms are mineralized structures embedded in the dermis, known for nonavian archosaurs, squamates, xenarthrans, and amphibians. Herein, we compared the osteoderm histology of Brazilian Notosuchia of Cretaceous age using three neosuchians for comparative purposes. Microanatomical analyses showed that most of them present a diploe structure similar to those of other pseudosuchians, lizards, and turtles. This structure contains two cortices (the external cortex composed of an outer and an inner layers, and the basal cortex) and a core in‐between them. Notosuchian osteoderms show high bone compactness (>0.85) with varying degrees of cancellous bone in the core. The neosuchian Guarinisuchus shows the lowest bone compactness with a well‐developed cancellous layer. From an ontogenetic perspective, most tissues are formed through periosteal ossification, although the mineralized tissues observed in baurusuchid LPRP/USP 0634 suggest a late metaplastic development. Histology suggests that the ossification center of notosuchian osteoderm is located at the keel. Interestingly, we identified Sharpey's fibers running perpendicularly to the outer layer of the external cortex in Armadillosuchus arrudai, Itasuchus jesuinoi, and Baurusuchidae (LPRP/USP 0642). This feature indicates a tight attachment within the dermis, and it is evidence for the presence of an overlying thick leathery layer of skin over these osteoderms. These data allow a better understanding of the osteohistological structure of crocodylomorph dermal bones, and highlight their structural diversity. We suggest that the vascular canals present in some sampled osteoderms connecting the inner layer of the external cortex and the core with the external surface may increase osteoderm surface and the capacity of heat transfer in terrestrial notosuchians.
Radio variability properties for radio sources

In this paper, we used the database of the university of Michigan Radio Astronomy Observatory (UMRAO) at three (4.8 GHz, 8.0 GHZ, and 14.5 GHz) radio frequency to analyze the radio light curves by the power spectral analysis method in search of possible periodicity. The analysis results showed that the radio sources display astrophysically meaningful periodicity ranging from 2.2 to 20.8 years in their light curves at the three frequencies. We also calculated the variability parameters and investigated the correlations between the variability parameter and the flux density. For the variability parameters, we found that the parameters at higher frequency are higher than those in the lower frequency. In addition, the variability parameters of BL Lacertae objects are larger than those of flat-spectrum radio quasars. suggesting that they are more variable than flat spectrum radio quasars.
Magnetohydrodynamic density waves in a composite disc system of interstellar medium and cosmic ray gas

Multiwavelength observations from radio to soft X-ray bands of large-scale galactic spiral structures offer synthesized and comprehensive views of nearby disc galaxies. In the presence of a massive dark matter halo, the density-wave dynamics on galactic scales involves the stellar disc, the gas disc of the interstellar medium (ISM), the magnetic field and the cosmic ray gas (CRG). In this paper, we explore the dynamic and electromagnetic interplay between the magnetized ISM disc and the CRG disc so that structural and diagnostic features of optical, infrared and synchrotron radio-continuum emissions from a spiral galaxy can be understood physically. On time-scales of galactic density waves, cosmic rays collectively may be treated as a relativistically hot tenuous gas fluid that is tied to the large-scale mean magnetic field in transverse bulk motions but moves otherwise differently along the magnetic field relative to the ISM. For both fast and slow magnetohydrodynamic (MHD) density waves in a composite disc system of magnetized ISM and CRG, the minute CRG mass-density enhancement is phase shifted relative to the enhancement of the parallel magnetic field. Owing to the extremely small number of cosmic rays, the large-scale magnetic field enhancement dominates in synchrotron radio-continuum emissions (as if the CRG is almost unperturbed) for spiral structural manifestations. In addition to the fast and slow MHD density waves, there also exists a suprathermal MHD wave mode by which CRG adjusts itself with an effective suprathermal speed of sound close to the speed of light c.
Testing for personality consistency across naturally occurring behavioral contexts in sanctuary chimpanzees (Pan troglodytes)

Personality is both a reflection of the bio‐behavioral profile of individuals and a summary of how they typically interact with their physical and social world. Personality is usually defined as having distinct behavioral characteristics, which are assumed to be consistent over time and across contexts. Like other mammals, primates have individual differences in personality. Although temporal consistency is sometimes measured in primates, and contextual consistency is sometimes measured across experimental contexts, it is rare to measure both in the same individuals and outside of experimental settings. Here, we aim to measure both temporal and contextual consistency in chimpanzees, assessing their personality with behavioral observations from naturally occurring contexts (i.e., real‐life settings). We measured personality‐based behaviors in 22 sanctuary chimpanzees, in the contexts of feeding, affiliation, resting, and solitude, across two time periods, spanning 4 years. Of the 22 behaviors recorded, about 64% were consistent across two to four contexts and 50% were consistent over time. Ten behaviors loaded significantly onto three trait components: explorativeness, boldness‐sociability, and anxiety‐sociability, as revealed by factor analysis. Like others, we documented individual differences in the personality of chimpanzees based on reliably measured observations in real‐life contexts. Furthermore, we demonstrated relatively strong, but not absolute, temporal, and contextual consistency in personality‐based behaviors. We also found another aspect of individual differences in personality, specifically, the extent to which individual chimpanzees show consistency. Some individuals showed contextual and temporal consistency, whereas others show significant variation across behaviors, contexts, and/or time. We speculate that the relative degree of consistency in personality may vary within chimpanzees. It may be that different primate species vary in the extent to which individuals show consistency of personality traits. Our behavioral‐based assessment can be used with wild populations, increasing the validity of personality studies, facilitating comparative studies and potentially being applicable to conservation efforts.
Second-order QED corrections for few-electron heavy ions: reducible Breit-Coulomb correction and mixed self-energy-vacuum polarization correction

Some second order in alpha =e2/(h(cross)c) QED corrections are investigated for He-like heavy ions and for the 2p12/-2s shift for the Li-like ions. These corrections correspond to the reducible part of the two-photon exchange Breit-Coulomb graph and to the mixed self-energy-vacuum polarization graph. The calculations show that these corrections are important for the comparison of the recent theoretical and experimental results.
Massive particles in acoustic space-times: Emergent inertia and passive gravity

I show that massive-particle dynamics can be simulated by a weak, external perturbation on a potential flow in an ideal fluid. The perturbation defining a particle is dictated in a small (spherical) region that is otherwise free to roam in the fluid. Here I take it as an external potential that couples to the fluid density or as a rigid distribution of sources with vanishing total outflux. The effective Lagrangian for such particles is shown to be of the form mc{sup 2}l(U{sup 2}/c{sup 2}), where U{yields} is the velocity of the particle relative to the fluid and c the speed of sound. This can serve as a model for emergent relativistic inertia a la Mach's principle with m playing the role of inertial mass, and also of analog gravity where m is also the passive gravitational mass. The mass m depends on the particle type and intrinsic structure (and on position if the background density is not constant), while l is universal: For D-dimensional particles l{proportional_to}F(1,1/2;D/2;U{sup 2}/c{sup 2}) (F is the hypergeometric function). These particles have the following interesting dynamics: Particles fall in the same way in the analog gravitational field mimicked by the flow, independent of their internal structure,more » thus satisfying the weak equivalence principle. For D{<=}5 they all have a relativistic limit with the acquired energy and momentum diverging as U{yields}c. For D{<=}7 the null geodesics of the standard acoustic metric solve our equation of motion. Interestingly, for D=4 the dynamics is very nearly Lorentzian: l{proportional_to}-mc{sup 2}{gamma}{sup -1}{lambda}({gamma}) (up to a constant), with {lambda}=(1+{gamma}{sup -1}){sup -1} varying between 1/2 and 1 ({gamma} is the 'Lorentz factor' for the particle velocity relative to the fluid). The particles can be said to follow the geodesics of a generalized acoustic metric of a Finslerian type that shares the null geodesics with the standard acoustic metric. In vortex geometries, the ergosphere is automatically the static limit. As in the real world, in 'black hole' geometries circular orbits do not exist below a certain radius that occurs outside the horizon. There is a natural definition of antiparticles, and I describe a mock particle vacuum in whose context one can discuss, e.g., particle Hawking radiation near event horizons. « less
THE COMPLETE INFRARED VIEW OF ACTIVE GALACTIC NUCLEI FROM THE 70 MONTH SWIFT/BAT CATALOG

We systematically investigate the near- to far-infrared (FIR) photometric properties of a nearly complete sample of local active galactic nuclei (AGNs) detected in the Swift/Burst Alert Telescope (BAT) all-sky ultra-hard X-ray (14–195 keV) survey. Out of 606 non-blazar AGNs in the Swift/BAT 70 month catalog at high galactic latitudes of , we obtain IR photometric data of 604 objects by cross-matching the AGN positions with catalogs from the WISE, AKARI, IRAS, and Herschel infrared observatories. We find a good correlation between the ultra-hard X-ray and mid-IR luminosities over five orders of magnitude ( ). Informed by previous measurements of the intrinsic spectral energy distribution of AGNs, we find FIR pure-AGN candidates whose FIR emission is thought to be AGN-dominated with low star-formation activity. We demonstrate that the dust covering factor decreases with the bolometric AGN luminosity, confirming the luminosity-dependent unified scheme. We also show that the completeness of the WISE color–color cut in selecting Swift/BAT AGNs increases strongly with 14–195 keV luminosity.
Spontaneous Scaling Emergence In Generic Stochastic Systems

We extend a generic class of systems which have previously been shown to spontaneously develop scaling (power law) distributions of their elementary degrees of freedom. While the previous systems were linear and exploded exponentially for certain parameter ranges, the new systems fulfill nonlinear time evolution equations similar to the ones encountered in Spontaneous Symmetry Breaking (SSB) dynamics and evolve spontaneously towards "fixed trajectories" indexed by the average value of their degrees of freedom (which corresponds to the SSB order parameter). The "fixed trajectories" dynamics evolves on the edge between explosion and collapse/extinction. The systems present power laws with exponents which in a wide range (α −2 there is no "thermodynamic limit" and the fluctuations are dominated by a few, largest degrees of freedom which leads to macroscopic fluctuations, chaos, and bursts/intermittency.
GEMS: Which Galaxies Dominate the z ~ 0.7 Ultraviolet Luminosity Density?

We combine high-resolution images from GEMS with redshifts and spectral energy distributions from COMBO-17 to explore the morphological types of galaxies that dominate the z ~ 0.7 UV luminosity density. We analyzed rest-frame 280 nm and V-band luminosities of 1483 galaxies with 0.65 < z < 0.75, combining these with visual morphological classifications from F850LP images (approximately rest-frame V band) taken with HST ACS on the Extended Chandra Deep Field-South. We derive UV luminosity functions and j280 luminosity densities for spheroid-dominated galaxies, spiral galaxies, Magellanic irregular galaxies, and clearly interacting galaxies with morphologies suggestive of ongoing major mergers. We check the reliability of GEMS morphologies against the deeper GOODS images and quantify an incompleteness of the GEMS merger identification at the faint end. We derive the fractions of the global UV luminosity density j280 originating from the galaxy types and find that spiral and Magellanic irregular galaxies dominate with about 40% each. Interacting and merging galaxies account for roughly 20% of j280, while the contribution of early types is negligible. These results imply that the strong decline in the UV luminosity density of the universe observed from z ~ 1 until today is dominated by the decreasing UV luminosities of normal spiral galaxies, accompanied by the migration of UV-luminous star formation in irregular galaxies to systems of progressively lower mass and luminosity. These conclusions suggest that major-merger-driven star formation cannot dominate the declining cosmic star formation rate, unless major mergers are substantially more obscured than intensely star-forming spiral galaxies and the decline in observed cosmic star formation rate is substantially stronger than the already precipitous decline in uncorrected UV luminosity density.
Opposing seasonal temperature dependencies of CO2 and CH4 emissions from wetlands

Wetlands are critically important to global climate change because of their role in modulating the release of atmospheric greenhouse gases (GHGs) carbon dioxide (CO2) and methane (CH4). Temperature plays a crucial role in wetland GHG emissions, while the general pattern for seasonal temperature dependencies of wetland CO2 and CH4 emissions is poorly understood. Here we show opposite seasonal temperature dependencies of CO2 and CH4 emissions by using 36,663 daily observations of simultaneous measurements of ecosystem‐scale CO2 and CH4 emissions in 42 widely distributed wetlands from the FLUXNET‐CH4 database. Specifically, the temperature dependence of CO2 emissions decreased with increasing monthly mean temperature, but the opposite was true for that of CH4 emissions. Neglecting seasonal temperature dependencies may overestimate wetland CO2 and CH4 emissions compared to the use of a year‐based static and consistent temperature dependence parameter when only considering temperature effects. Our findings highlight the importance of incorporating the remarkable seasonality in temperature dependence into process‐based biogeochemical models to predict feedbacks of wetland GHG emissions to climate warming.