Miracle-dz/UniFAR-FTUs huggingface dataset:
On the Composition of GRBs' Collapsar Jets

The duration distribution of long gamma-ray bursts (GRBs) reveals a plateau at durations shorter than ∼20 s (in the observer frame) and a power-law decline at longer durations. Such a plateau arises naturally in the Collapsar model. In this model, the engine has to operate long enough to push the jet out of the stellar envelope and the observed duration of the burst is the difference between the engine’s operation time and the jet breakout time. The jet breakout time inferred from the duration distribution (∼10 s in the burst’s frame) is comparable to the breakout time of both analytic estimates and numerical simulations (both 2D and 3D) of a hydrodynamic jet (∼10 s for typical parameters). Recently, we have estimated analytically the breakout time of a Poynting-flux-dominated jet and have shown that it is consistent with 2D numerical simulations. We find that such a jet with the same overall energy breaks out much faster (1 s). If this result holds for 3D simulations it implies that only hydrodynamic jets are compatible with the duration of the plateau in the GRB duration distribution and hence the jet should be hydrodynamic during most of the time that its head is within the envelope of the progenitor star and around the time when it emerges from the star. This would naturally arise if the jet forms as a hydrodynamic jet in the first place or if it forms Poynting flux dominated but dissipates most of its magnetic energy early on within the progenitor star and emerges as a hydrodynamic jet.
Modeling and Computation of Batoid Swimming Inspired Pitching Impact on Wake Structure and Hydrodynamic Performance

Through direction numerical simulation (DNS) of a model manta ray body, pectoral fin scaled pitching effect on hydrodynamic performance and wake is investigated. The manta ray model is derived from high-speed video of manta ray swimming with motion of the model prescribed to match the actual manta ray. Rotation angles of the model skeletal joints is altered to scale the pitching. This results in four manta ray models with different pectoral fin pitching ratios. The models are simulated using an in-house developed immersed boundary method-based numerical solver. Notable discrepancies in thrust production during the downstroke are observed, with the θR = 1.0 case producing instantaneous thrust peak that is 19% higher than the θR = 0.72 model. Cycle averaged thrust is highest for the θR = 0.72 model case, however, which can be attributed to extended reverse thrust for the θR = 1.0 model. Through analysis of the near-body wake structures produced during the downstroke, late leading-edge vortex (LEV) formation is discovered to be primarily responsible for the detrimental reverse thrust seen for the θR = 1.0 model. Surface pressure contours confirm this finding. Meanwhile the upstroke possesses less pronounced force production.
The Effect of Rotation on the Spectrum of Vega

The discovery that Vega is a rapidly rotating pole-on star has raised a number of questions about this fundamental standard, including such issues as its composition, and in turn its mass and age. We report here a reanalysis of Vega’s composition. A full spectral synthesis based on the Roche model derived earlier from NPOI interferometry is used. We find the line shapes in Vega’s spectrum to be more complex than just flat-bottomed, which have been previously reported; profiles range from slightly self-reversed to simple “V” shapes. A high S/N spectrum, obtained by stacking spectra from the ELODIE archive, shows excellent agreement with the calculations, provided we add about 10 km s−1 of macroturbulence to the predicted spectra. From the abundance analysis, we find that Vega shows the peculiar abundance pattern of a λ Bootis star as previously suggested. We investigate the effects of rotation on the deduced abundances and show that the dominant ionization states are only slightly affected compared to analyses using nonrotating models. We argue that the rapid rotation requires that the star be fully mixed. The composition leads to masses and particularly ages that are quite different compared to what are usually assumed.
Complications and Functional Outcome Following Operative Treatment of Talus Neck and Body Fractures: A Systematic Review

Background: Central talar fractures are rare and often associated with impaired functional outcome. Despite recent advances in diagnosis and management of talus fractures, complications rates remain high and functional outcome is generally poor. This study aims to provide an overview of complication rates and functional outcome following operative treatment of talar neck and body fractures. This may help in clinical decision making by improving patients’ expectation management and tailored treatment strategies. Methods: A systematic review of the literature was conducted of studies published from January 2000 to July 2021 reporting functional outcome and/or complications following operative treatment of talar neck, body, or combined neck and body fractures. Keywords used were (Talar fracture) or (Talus fracture). Data on complication rates and functional outcome was extracted from selected articles. Results: A total of 28 articles were included in our analysis reporting 1086 operative treated talar fractures (755 neck [70%], 227 body fractures [21%], and 104 combined body and neck fractures [9%]). The mean follow-up was 48 (range 4-192) months. Complications occurred frequently with; 6% surgical site infection, 8% nonunion, 29% avascular necrosis, 64% osteoarthritis, and in 16% a secondary arthrodesis was necessary. A wide variety in functional outcome was reported; however, there seems to be a correlation between fracture classification and postoperative complications. Conclusion: Operative treatment of central talar fractures is associated with a high incidence of early and late complications and often leads to an impaired functional outcome. Standardization of talar fracture classification and scoring systems in combination with large sample-sized prospective studies are warranted to detect further predictive factors influencing tailormade treatment strategies and patient expectation management. Level of Evidence: Level III, Systematic review of case series and case-control studies.
Research and publication trends: Sports branding on the movie

Many films have raised the story of sports as the major story or as the background of a film. However, so far, no research has been obtained that analyzes the mapping of research results related to film and sports. Therefore, this study intends to examine various studies related to film and sports that global researchers have produced. This research uses the bibliometric method. The data source used is the Web of Science, while the tools used to process and display the data are ScientoPy and VosViewer. The results showed that the development of scientific publications starts 2000 to 2021 related to films and sports experienced fluctuating developments. Authors from America and England occupy the top positions for the number of publications. However, in the period 2020 and 2021, researchers from France and Canada are researchers who are more productive in publishing their scientific works. They included most published scientific works related to films and sports in the WoS version of the Social science category. However, Between 2020-2022, more are categorized into the subject of Communication and Film, Radio, & Television. Reference sources widely cited in scientific publications related to film and sports are books by Beeton with the title film-induced tourism (2005) and Crosson's work with the title sport and film (2013). The results of the keyword mapping show that six clusters represent some keywords used by the author in scientific works related to films and sports. In conclusion, sports and cinema research are fully developed in this research.
New molecules in IRC +10216: confirmation of C5S and tentative identification of MgCCH, NCCP, and SiH3CN

The carbon-star envelope IRC +10216 harbors a rich variety of molecules, with more than 80 detected to date. During the course of a λ 3m m survey of IRC+10216 carried out with the IRAM 30-m telescope we have detected various weak lines, with antenna temperatures of a few mK, which we assign to rotational transitions of four new molecules. The observation of three lines of C5S confirms a previous tentative identification of this molecule based on a line at 24.0 GHz. We also report the tentative identification of three molecules not yet observed in space: MgCCH, the first metal acetylide detected in space, and NCCP and SiH3CN, the phosphorus and silicon analogs of cyanogen (NCCN) and methyl cyanide (CH3CN). We derive the following column densities: N(C5S) = (2−14) × 10 12 cm −2 (depending on the rotational temperature adopted), N(MgCCH) = 2 × 10 12 cm −2 , N(NCCP) = 7 × 10 11 cm −2 ,a nd N(SiH3CN) = 10 12 cm −2 . The S-bearing carbon chain C5S is less abundant than C3S, while MgCCH has an abundance in between that of MgNC and those of MgCN and HMgNC. On the other hand, NCCP and SiH3CN are the least abundant P- and Si-bearing molecules observed to date in IRC +10216. Based on the behavior of similar molecules it is likely that these four species are formed in the outer circumstellar layers of IRC +10216. We discuss possible gas-phase formation routes.
FAST COALESCENCE OF MASSIVE BLACK HOLE BINARIES FROM MERGERS OF GALACTIC NUCLEI: IMPLICATIONS FOR LOW-FREQUENCY GRAVITATIONAL-WAVE ASTROPHYSICS

We investigate a purely stellar dynamical solution to the Final Parsec Problem. Galactic nuclei resulting from major mergers are not spherical, but show some degree of triaxiality. With N-body simulations, we show that equal-mass massive black hole binaries (MBHBs) hosted by them will continuously interact with stars on centrophilic orbits and will thus inspiral—in much less than a Hubble time—down to separations at which gravitational-wave (GW) emission is strong enough to drive them to coalescence. Such coalescences will be important sources of GWs for future space-borne detectors such as the Laser Interferometer Space Antenna (LISA). Based on our results for equal-mass mergers, and given that the hardening rate of unequal-mass binaries is similar, we expect that LISA will see between ∼10 and ∼ few × 102 such events every year, depending on the particular massive black hole (MBH) seed model as obtained in recent studies of merger trees of galaxy and MBH co-evolution. Orbital eccentricities in the LISA band will be clearly distinguishable from zero with e ≳ 0.001–0.01.
Silicate Scaling Formation: Impact of pH in High-Temperature Reservoir and Its Characterization Study

Silicate scaling tends to form and be aggravated during high pH Alkaline Surfactant Polymer (ASP) floods and this silicate scale deposition affects oil production. Hence, it is important to examine the conditions that lead to silicate scale forming. The severity of the silicate scaling reaction, the type and morphology of silica/silicate scale formed in an experimental ASP flood were studied for pH values 5, 8.5, and 11, whilst the temperature was kept constant at 90 ℃. In addition, the impact of calcium ion was studied and spectroscopic analyses were used to identify the extent of scaling reaction, morphology type and the functional group present in the precipitates. This was performed using imagery of the generated precipitates. It was observed that the silica/silicate scale is most severe at the highest pH and Ca:Mg molar ratios examined. Magnesium hydroxide and calcium hydroxide were observed to precipitate along with the silica and Mg-silicate/Ca-silicate scale at pH 11. The presence of calcium ions altered the morphology of the precipitates formed from amorphous to microcrystalline/crystalline. In conclusion, pH affects the type, morphology, and severity of the silica/silicate scale produced in the studied scaling system. The comprehensive and conclusive data showing how pH affects the silicate scaling reaction reported here are vital in providing the foundation to further investigate the management and prevention of this silicate scaling. Copyright © 2022 by Authors, Published by BCREC Group. This is an open access article under the CC BY-SA License (https://creativecommons.org/licenses/by-sa/4.0)
Gravitational radiation and isotropic change of the spatial geometry

To simplify a number of considerations in the weak field approximation, including the determination of the response of interferometric gravitational wave detectors, the "transverse traceless" (TT) gauge is often used. While the identification of the corresponding gauge invariant part of the metric perturbations in the pure vacuum case is obvious, it is not widely known that the determination and the use of the TT part is much more complicated and, in turn, much less rewarding when sources are involved. It is shown here that likewise the transverse part of the electric current in the Coulomb gauge within Maxwell's theory the sources of the TT gauge part of the metric perturbations become non-local. This, in practice, invokes the necessity of the use of more adequate projection operators then the ones applied, e.g, in the weak field limit, and in many post-Newtonian considerations. It is also pointed out that, whenever nonlinear effects are taken into account, some of the conclusions concerning the response of interferometric gravitational wave detectors may be influenced. In particular, attention is called on the possibility that gravitational radiation may produce an isotropic change of the spatial geometry.
PROPER MOTION AND TIMING OF TWO UNUSUAL PULSARS: CALVERA AND 1E 1207.4—5209

Using pairs of images from the Chandra High Resolution Camera we examine the proper motion of the central compact object (CCO) 1E 1207.4−5209 in the supernova remnant (SNR) PKS 1209−51/52, and the unusual pulsar Calvera that is possibly a CCO descendant. For 1E 1207.4−5209, an insignificant proper motion of &mgr; = 15 ± 7 ? > mas yr−1 is measured, corresponding to a corrected tangential velocity of v ⊥ , c < 180 ? > km s−1 at the distance of 2 kpc. This proves that the previously noted large offset of the pulsar from the apparent geometric center of the SNR is not due to high proper motion; evidently the symmetry of the remnant does not indicate its center of expansion. Calvera has a marginally significant proper motion of &mgr; = 69 ± 26 ? > mas yr−1, corresponding to v ⊥ , c = 86 ± 33 ? > km s−1 for a hypothetical distance of 0.3 kpc. Notably, its vector is away from the Galactic plane, although its high Galactic latitude of b = + 37 ° ? > may be more a consequence of its proximity than its velocity. We also provide updated timing solutions for each pulsar. Spanning 14.5 years, the ephemeris of 1E 1207.4−5209 has a small and steady frequency derivative that, because of the negligible proper motion, requires no kinematic correction. The derived surface dipole magnetic field strength of 1E 1207.4−5209 thus remains B s = 9.8 × 10 10 ? > G. Calvera has B s = 4.4 × 10 11 ? > G, intermediate between those of ordinary young pulsars and CCOs, suggesting that it may be on a trajectory of field growth that could account for the absence of descendants in the neighborhood of CCOs in the P – P ˙ ? > diagram.
Dietary polyphenols in the treatment of inflammatory bowel diseases

Ulcerative colitis and Crohn's disease, caused by chronic inflammation in the digestive tract, are inflammatory bowel diseases and have similar symptoms. Abnormal immune responses play a pretty important role in the pathogenesis of the disease. Proinflammatory mediators trigger inflammation, stimulate cell signaling molecules, and induce disease onset. Corticosteroids, anti-tumor necrosis factor-α antibodies, and immunosuppressants are some drugs used to treat the disease. However, these drugs have some side effects. In addition, surgical methods might be used in the treatment, but these methods may have some complications. Due to the negative impact on treatment options, alternative methods for reliable, inexpensive, and effective treatment are being sought. Secondary plant compounds with an aromatic or phenolic ring structure, so-called polyphenols or phenolic compounds, may modulate cellular signaling pathways and reduce intestinal inflammation due to their antioxidant and anti-inflammatory effects. Polyphenols may be evaluated as alternative methods for inflammatory bowel disease based on these properties. This review aims to investigate the effect of some polyphenols on inflammatory bowel disease.
First law and Smarr formula of black hole mechanics in nonlinear gauge theories

Motivated by the fact that Bardeen black holes do not satisfy the usual first law and Smarr formula, we derive a generalized first law from the Lagrangian of the nonlinear gauge field coupled to gravity. In our treatment, the Lagrangian is a function of the electromagnetic invariant as well as some additional parameters. Consequently, we obtain new terms in the first law. With our formula, we find the correct forms of the first law for Bardeen black holes and BI black holes. By scaling arguments, we also derive a general Smarr formula from the first law. Our results apply to a wide class of black holes with nonlinear gauge fields.
DISSECTING THE RED SEQUENCE. III. MASS-TO-LIGHT VARIATIONS IN THREE-DIMENSIONAL FUNDAMENTAL PLANE SPACE

The fundamental plane (FP) of early-type galaxies is observed to have finite thickness and to be tilted from the virial relation. Both of these represent departures from the simple assumption that dynamical mass-to-light ratios (Mdyn/L) are constant for all early-type galaxies. We use a sample of 16,000 quiescent galaxies from the Sloan Digital Sky Survey to map out the variations in Mdyn/L throughout the three-dimensional FP space defined by velocity dispersion (σ), effective radius (Re), and effective surface brightness (Ie). Dividing Mdyn/L into multiple components allows us to separately consider the contribution to the observed Mdyn/L variation due to stellar population effects, initial mass function (IMF) variations, and variations in the dark matter fraction within one Re. Along the FP, we find that the stellar population contribution given some constant IMF (M⋆,IMF/L) scales with σ such that M⋆,IMF/L ∝ f(σ). Meanwhile, the dark matter and/or IMF contribution (Mdyn/M⋆,IMF) scales with Mdyn such that Mdyn/M⋆,IMF ∝ g(Mdyn). This means that the two contributions to the tilt of the FP rotate the plane around different axes in the three-dimensional space. The observed tilt of the FP requires contributions from both, with dark matter/IMF variations likely comprising the dominant contribution. Looking at Mdyn/L variations through the thickness of the FP, we find that Mdyn/L variations must be dominated either by IMF variations or by real differences in the dark matter fraction with Re. This means that the finite thickness of the FP is due to variations in the stellar mass surface density within Re (Σ⋆,IMF), not the fading of passive stellar populations. It therefore represents genuine structural differences between early-type galaxies. These structural variations are correlated with galaxy star formation histories such that galaxies with higher Mdyn/M⋆,IMF have higher [Mg/Fe], lower metallicities, and older mean stellar ages. We discuss several physical mechanisms that might explain the observed co-variation between Mdyn/M⋆,IMF and galaxy star formation histories. It is difficult to explain the observed enhancement of α-elements in lower-surface-brightness galaxies by allowing the IMF to vary. Differences in dark matter fraction can be produced by variations in the “conversion efficiency” of baryons into stars or by the redistribution of stars and dark matter through dissipational merging. The former explanation, specifically a model in which some galaxies experience low conversion efficiencies due to premature truncation of star formation, provides a more natural explanation for the co-variation of Mdyn/M⋆,IMF and the observed stellar population properties.
Probing cosmic acceleration by using the SNLS3 SNIa dataset

We probe the cosmic acceleration by using the recently released SNLS3 sample of 472 type Ia supernovae. Combining this type Ia supernovae dataset with the cosmic microwave background anisotropy data from the Wilkinson Microwave Anisotropy Probe 7-yr observations, the baryon acoustic oscillation results from the Sloan Digital Sky Survey data release 7, and the Hubble constant measurement from the Wide Field Camera 3 on the Hubble Space Telescope, we measure the dark energy equation of state w and the deceleration parameter q as functions of redshift by using the Chevallier-Polarski-Linder parametrization. Our result is consistent with a cosmological constant at 1σ confidence level, without evidence for the recent slowing down of the cosmic acceleration. Furthermore, we consider three binned parametrizations (w is piecewise constant in redshift z) based on different binning methods. The similar results are obtained, i.e., the ΛCDM model is still nicely compatible with current observations.
Development Status and Suggestion of China Urban Bicycle Transport

: China has been once recognized as a bicycle kingdom in the world. However, China’s cycling trip has been pouring down in the last 20 years. Along with the “Internet Plus” and Sharing Economy’s arriving, APP-based sharing bicycles have become the pioneer of bicycle revival. In order to discuss the method to promote the revitalization movement from sectional management on the national level, this article analyzes the development status of bicycle transport and current problems firstly, and then madees a deep analysis of contributing fac-tors behind these problems. Policy suggestion is also proposed to promote bicycle return to cities from the per-spective of confirming bicycle function.
The nature of dark matter from the global high-redshift H i 21 cm signal

We study the imprint of dark matter (DM) annihilation on the global 21 cm signal from the Dark Ages to Cosmic Reionization. Motivated by recent observations, we focus on three DM candidates: (i) a 10 GeV Bino-like neutralino (ii) a 200 GeV Wino and (iii) a 1 TeV heavier particle annihilating into leptons. For each DM candidate we assume two values for the thermally averaged annihilation cross section hσvi, the standard thermal value hσvith = 3 × 10 26 cm 3 s 1 and the maximum value allowed by WMAP7 data, hσvimax. We include the enhancement of DM annihilations due to collapsed structures, detailed estimates of energy deposition into the intergalactic medium (IGM), as well realistic prescriptions for astrophysical sources of UV and X-ray radiation. In these models, the additional heat input from DM annihilation suppresses the mean 21cm brightness temperature offset by δTb ∼ few–100 mK. In particular, the very deep δTb ∼ −150 mK absorption feature at ∼ 20 < ∼ z < 25 predicted by popular models of the first galaxies is considerably reduced or totally erased by some of the considered DM candidates. Such an enhancement in IGM heating could come from either DM annihilations or a stronger-than-expected astrophysical component (i.e. abundant early X-ray sources). However, we find that the two signatures are not degenerate, since the DM heating is dominated by halos several orders of magnitude smaller than those hosting galaxies, whose fractional abundance evolves more slowly resulting in a smaller gradient: dδTb/dν < 4 mK/MHz in the range ν ∼ 60−80 MHz. The detection of such signals by future radio telescopes would be clear evidence of DM energy injection at high-redshifts.