Miracle-dz/UniFAR-FTUs huggingface dataset:
Expect and you shall perceive: People who expect better in turn perceive better behaviors from their romantic partners.

People who are happy with their romantic relationships report that their partners are particularly effective at meeting their everyday relational needs. However, the literature invites competing predictions about how people arrive at those evaluations. In pilot research, we validated a scale of concrete, specific relationship behaviors that can be performed by a romantic partner day-to-day. In Study 1, cross-lagged panel models examined how expectations of positive behaviors, perceptions of positive behaviors, and relationship quality predict changes in one another from week to week. People who expected more positive behaviors in turn perceived more positive behaviors from their partners 1 week later. Key effects extended to negative relationship behaviors (Study 2). In Study 3, the same pattern emerged in a dyadic sample, with expected behaviors predicting changes in perceived behaviors independent of the partner's own reports. Truth and bias analyses revealed that people with lower expectations had more negatively biased perceptions of their partners' behaviors, whereas high expectations were associated with better accuracy. We obtained these results in the context of specific, verifiable behaviors reported on over relatively short periods, underscoring how powerfully people's everyday relationship perceptions may be shaped by their more global perceptions. (PsycInfo Database Record (c) 2022 APA, all rights reserved).
Effect of Systemic Administration of Granulocyte-Colony Stimulating Factor on Rate of Fracture Healing of Bone Defect in Goats as Animal Model

Granulocyte-colony stimulating factor (G-CSF) serves as an important cytokine in haematopoiesis; released at both physiological and pathological conditions by a range of cells. We hypothesized that the systemic administration of G-CSF would produce an accelerated fracture-healing rate in non-union bone defects; thus, potentially leading to useful clinical applications. Ten male adult Katjang goats, weighing about 15-26 kilograms were randomly chosen and a tibial bone defect was induced in each animal. The defect was maintained by internal fixation with a titanium plate and reinforced by an external fiberglass cast. Post-operative radiographs were performed twice weekly and radiographic assessments were performed by evaluating the bridging and union measurements through a validated method. In the treatment group, the time for bridging and union exhibited statistically significant differences when compared with a control group. The outcomes of the present study establishing a notion that administration of G-CSF besides inducing haematopoiesis, promotes healing of fractures and non-union bone defects as well.
The Most Massive Active Galactic Nuclei at 1 ≲ z ≲ 2

We obtained near-infrared spectra of 26 Sloan Digital Sky Survey quasars at with reported rest-frame ultraviolet MBH ∼ 1010 M⊙ to critically examine the systematic effects involved with their mass estimations. We find that active galactic nuclei (AGNs) heavier than 1010 M⊙ often display double-peaked Hα emission, extremely broad Fe ii complex emission around Mg ii, and highly blueshifted and broadenedC iv emission. The weight of this evidence, combined with previous studies, cautions against the use of MBH values based on any emission line with a width over 8000 km s−1. Also, the MBH estimations are not positively biased by the presence of ionized narrow line outflows, anisotropic radiation, or the use of line FWHM instead of σ for our sample, and unbiased with variability, scatter in broad line equivalent width, or obscuration for general type-1 quasars. Removing the systematically uncertain MBH values, ∼1010 M⊙ black holes (BHs) in 1 ≲ z ≲ 2 AGNs can still be explained by anisotropic motion of the broad line region from ∼109.5 M⊙ BHs, although current observations support that they are intrinsically most massive, and overmassive to the host’s bulge mass.
Analysis of Fermi-LAT observations, UHECRs and neutrinos from the radio galaxy Centaurus B

Centaurus B (Cen B) is one of the closest and brightest radio-loud galaxy in the southern sky. This radio galaxy, proposed as a plausible candidate for accelerating ultra-high-energy cosmic rays (UHECRs), is near the highest-energy neutrino event reported (IC35) in the High-Energy Starting Events catalog. Pierre Auger observatory reported the highest energy comic rays during 10 years of collecting data with some of them around this source. In this paper, the analysis of the gamma-ray spectrum and the light curve above 200 MeV is presented with nine years of cumulative Fermi-LAT data around Cen B . Taking into consideration the multi-wavelength observations carried out about this radio galaxy, leptonic and hadronic scenarios are introduced in order to fit the spectral energy distribution, assuming that the gamma-ray flux is produced in a region close to the core and in the extended lobes. Using the best-fit values found, several physics properties of this radio galaxy are derived. Furthermore, a statistical analysis of the cosmic ray distribution around Cen B is performed, finding that this distribution is not different from the background at a level of significance of 5%. Considering the UHECR event associated to this source by Moskalenko et al. [1] and extrapolating its luminosity to low energies, we do not find enough evidence to associate the highest-energy neutrino event (IC35) with this radio galaxy.
Rehabilitating the Lagged Dependent Variable With Structural Equation Modeling

Abstract It has been argued that including the lagged dependent variable in panel models will open up unintended back-door paths and bias the estimates of the causal variable. We show that panel analysis in the structural equation modeling framework can get around this issue. Including the lagged dependent variable has the benefit of closing back-door paths due to some unobserved time-varying con-founders. We demonstrate this by looking at simulated data and provide examples in the lavaan package for R as well as Mplus.
Sign change of the Gruneisen parameter and magnetocaloric effect near quantum critical points

We consider the Gr\"uneisen parameter and the magnetocaloric effect near a pressure and magnetic field controlled quantum critical point, respectively. Generically, the Gr\"uneisen parameter (and the thermal expansion) displays a characteristic sign change close to the quantum-critical point signaling an accumulation of entropy. If the quantum critical point is the endpoint of a line of finite temperature phase transitions, ${T}_{c}\ensuremath{\propto}{({p}_{c}\ensuremath{-}p)}^{\ensuremath{\Psi}}$, then we obtain for $pl{p}_{c}$, (1) a characteristic increase $\ensuremath{\Gamma}\ensuremath{\sim}{T}^{\ensuremath{-}1∕(\ensuremath{\nu}z)}$ of the Gr\"uneisen parameter $\ensuremath{\Gamma}$ for $Tg{T}_{c}$, (2) a sign change in the Ginzburg regime of the classical transition, (3) possibly a peak at ${T}_{c}$, (4) a second increase $\ensuremath{\Gamma}\ensuremath{\sim}\ensuremath{-}{T}^{\ensuremath{-}1∕(\ensuremath{\nu}z)}$ below ${T}_{c}$ for systems above the upper critical dimension, and (5) a saturation of $\ensuremath{\Gamma}\ensuremath{\propto}1∕({p}_{c}\ensuremath{-}p)$. We argue that due to the characteristic divergencies and sign changes the thermal expansion, the Gr\"uneisen parameter and magnetocaloric effect are excellent tools to detect and identify putative quantum critical points.
Lipschitz stability for a stationary 2D inverse problem with unknown polygonal boundary

We consider the stability issue for the inverse problem of determining an unknown portion Σ of a two-dimensional simply connected domain from overdetermined boundary data for the Laplace equation. In this paper, we study the case in which Σ is a polygonal line. We prove a Lipschitz stability estimate under further a priori geometric assumptions on Σ.
Stringy negative-tension branes and the second law of thermodynamics

Negative energy objects generally lead to instabilities and a number of other disturbing behaviors. In particular, negative energy fluxes lead to a breakdown of the classical area theorem for black hole horizons, which can lead to violations of the second law of thermodynamics. The negative energy objects that arise in string theory involve special boundary conditions which remove the perturbative instabilities. We show that they have additional special features which allow them to evade contradiction with the second law. We identify one mechanism which applies for most orientifold planes in string theory, and distinct mechanisms for the O8-plane and the AdS soliton.
Inference of magnetic field strength and density from damped transverse coronal waves

A classic application of coronal seismology uses transverse oscillations of waveguides to obtain estimates of the magnetic field strength. The procedure requires information on the density of the structures. Often it ignores the damping of the oscillations. We computed marginal posteriors for parameters such as the waveguide density, the density contrast, the transverse inhomogeneity length scale, and the magnetic field strength under the assumption that the oscillations can be modelled as standing magnetohydrodynamic (MHD) kink modes damped by resonant absorption. Our results show that the magnetic field strength can be properly inferred, even if the densities inside and outside the structure are largely unknown. Incorporating observational estimates of plasma density further constrains the obtained posteriors. The amount of information that is included a priori for the density and the density contrast influences their corresponding posteriors, but very little the inferred magnetic field strength. The decision to include or leave out the information on the damping and the damping timescales has a minimal impact on the obtained magnetic field strength. In contrast to the classic method, which provides numerical estimates with error bars or possible ranges of variation for the magnetic field strength, Bayesian methods offer the full distribution of plausibility over the considered range of possible values. The methods applied to available datasets of observed transverse loop oscillations can be extended to prominence fine structures or chromospheric spicules, and implemented to propagating waves in addition to standing oscillations.
Arakelian 564: An Unusual Component in the X-Ray Spectra of Narrow-Line Seyfert 1 Galaxies

We present an ASCA observation of the narrow-line Seyfert 1 (NLSy1) galaxy Arakelian 564. The X-ray light curve shows rapid variability, but no evidence for energy dependence to these variations, within the 0.6-10 keV bandpass. A strong (EW ~ 70 eV) spectral feature is observed close to 1 keV. A similar feature has been observed in Ton S180, another member of the NLSy1 class of objects, but it has not been observed in broad-line Seyfert galaxies. The feature energy suggests a large contribution from Fe L-shell lines, but its intensity is difficult to explain in terms of emission and/or absorption from photoionized gas. The models that predict most emission at 1 keV are characterized by extreme values of column density, Fe abundance, and ionization parameter. Models based on gas in thermal equilibrium with kT ~ 1 keV provide an alternative parameterization of the soft spectrum. The latter may be interpreted as the hot intercloud medium, undergoing rapid cooling and producing strong Fe L-shell recombination lines. In all cases the physical conditions are rather different from those observed in broad-line Seyfert galaxies. The hard X-ray spectrum shows a broad and asymmetric Fe Kα line of large equivalent width (~550 eV), suggestive of significant emission from the inner accretion disk. The profile can be explained by a neutral disk viewed at ~60° to the line of sight, contrary to the hypothesis that NLSy1's are viewed pole-on. The large EW of this line, the strong 1 keV emission, and the strong optical Fe emission lines all suggest an extreme Fe abundance in this and perhaps other NLSy1's.
A possible higher-dimensional alternative to scalar-field inflationary theory

We examine the time evolution of the D=d+4 dimensional Einstein field equations subjected to a flat Robertson-Walker metric where the 3D and higher-dimensional scale factors are allowed to dynamically evolve at different rates. By adopting equations of state relating the 3D and higher-dimensional pressures to the density, we obtain an exact expression for the higher-dimensional scale factor as a function of the 3D scale factor. This relation allows us to write the higher-dimensional FRW field equations solely in terms of the 3D scale factor, thus yielding a set of effective 4D FRW field equations. Two limiting regimes are found that yield series solutions for the 3D scale factor in terms of the time. The fluid regime solution closely mimics that described by standard 4D FRW cosmology, offering a relatively late time behavior for the 3D scale factor after becoming valid in the early universe, and can give rise to a late-time accelerated expansion. This is shown to be preceded by an earlier volume regime solution, which offers a very early-time epoch of accelerated expansion when radiation is the dominant energy component, but only for the unique case of d=1. This volume regime solution is shown to turn on and then off, hence offering a natural entrance and exit from a possible inflationary epoch. The time scales describing these phenomena, including the transition from volume to fluid regime solution, are shown to fall within a small fraction of the first second when the fundamental constants of the theory are aligned with that of the Planck time. This model potentially offers a higher-dimensional alternative to scalar-field inflationary theory and a consistent cosmological theory, yielding a unified description of early- and late-time accelerated expansions via a 5D spacetime scenario.
Industry Size and Trade Protection in the Presence of Environmental Regulations: An Empirical Investigation of the Indian Manufacturing Sector

Abstract This paper tests the hypothesis pertaining to the interdependencies between trade and environmental policies in the presence of industry/firm lobbies, which is captured through industry/firm size. For an unbalanced panel of manufacturing firms in India at the five-digit National Industrial Classification (NIC), 2008 for the period 2008–2019, I find that firm size has a positive and significant impact on trade policy. The same holds true for a subset of firms that are polluting in nature (based on the Central Pollution Control Board classification). It is found that larger firms have a greater influence on those trade policies that are set unilaterally by the government. Also, there is no empirical support in favour of trade and environment linkages in the Indian context. This could be due to the fact that these two policies come under the domain of independent ministries of the government. Moreover, environmental safety assumes less significance and tends to adversely affect the competitiveness of the manufacturing sector. Notwithstanding the fact that environmental regulations are in place, the enforcement and monitoring mechanisms are remarkably weak on account of weak environmental institutions.
Can supernova kicks trigger EMRIs in the Galactic Centre?

One of the most promising gravitational wave (GW) sources detectable by the forthcoming LISA observatory are the so-called extreme-mass ratio inspirals (EMRIs), i.e. GW-driven inspirals of stellar-mass compact objects on to supermassive black holes (SMBHs). In this paper, we suggest that supernova (SN) kicks may trigger EMRIs in galactic nuclei by scattering newborn stellar black holes and neutron stars on extremely eccentric orbits; as a consequence, the time-scale over which these compact objects are expected to inspiral on to the central SMBH via GW emission may become shorter than the time-scale for other orbital perturbations to occur. By applying this argument to the Galactic Centre, we show that the S-cluster and the clockwise disc are optimal regions for the generation of such events: one SN out of ∼104 (∼105) occurring in the S-cluster (clockwise disc) is expected to induce an EMRI. If we assume that the natal kicks affecting stellar black holes are significantly slower than those experienced by neutron stars, we find that most SN-driven EMRIs involve neutron stars. We further estimate the time spanning from the SN to the final plunge on to the SMBH to be of the order of few Myr. Finally, we extrapolate the rate of SN-driven EMRIs per Milky Way to be up to 10−8 yr−1, thus we expect that LISA will detect up to a few tens of SN-driven EMRIs every year.
Eastern skunk cabbage (Symplocarpus foetidus), a common native wetland plant, shows reduced size and seedling abundance near invasive Japanese knotweed (Reynoutria japonica)

Abstract. Nonnative plants may shift community composition and reduce diversity through competition with native neighbors, or invasion patterns may reflect edaphic gradients that create suitable habitat for colonization. We tested the impacts of invasive Reynoutria japonica (Japanese knotweed) on performance of a co-occurring native plant, Symplocarpus foetidus (eastern skunk cabbage), to determine if invasion has potential to change community composition by altering population-level processes. We tested two hypotheses: (1) Reynoutria japonica invasion is correlated with reduced population performance in S. foetidus; (2) Reynoutria japonica invasion is correlated with environmental variation, and contrasting habitat preferences allow R. japonica and S. foetidus to coexist. Sampling took place in an urban riparian site in Pittsburgh, PA, USA. Data were collected from 26 1-m2 plots with R. japonica present (n = 13) or absent (n = 13). We recorded pH, texture, and moisture. Size and flowering of all S. foetidus individuals and R. japonica cover and abundance were recorded in each plot. Symplocarpus foetidus size was significantly reduced in invaded plots, and both size and seedling abundance were significantly negatively associated with R. japonica cover. Abundance was negatively associated with percent clay and positively associated with soil moisture; seedling abundance was also predicted by lower soil pH. In contrast, R. japonica was most abundant and had highest cover with high pH and lower percent sand. Flowering of S. foetidus did not differ significantly between invaded and uninvaded plots. We conclude that R. japonica invasion both suppresses S. foetidus and correlates with environmental heterogeneity. Reduced performance of S. foetidus in invaded plots suggests competitive suppression. While R. japonica negatively impacted S. foetidus, distinct microhabitat preferences may allow them to co-occur.
H2 and CO Emission from Disks around T Tauri and Herbig Ae Pre-Main-Sequence Stars and from Debris Disks around Young Stars: Warm and Cold Circumstellar Gas

We present ISO Short-Wavelength Spectrometer observations of H2 pure-rotational line emission from the disks around low- and intermediate-mass pre-main-sequence stars as well as from young stars thought to be surrounded by debris disks. The pre-main-sequence sources have been selected to be isolated from molecular clouds and to have circumstellar disks revealed by millimeter interferometry. We detect "warm" (T ≈ 100-200 K) H2 gas around many sources, including tentatively the debris-disk objects. The mass of this warm gas ranges from ~10-4 M☉ up to 8 × 10-3 M☉ and can constitute a nonnegligible fraction of the total disk mass. Complementary single-dish 12CO 3-2, 13CO 3-2, and 12CO 6-5 observations have been obtained as well. These transitions probe cooler gas at T ≈ 20-80 K. Most objects show a double-peaked CO emission profile characteristic of a disk in Keplerian rotation, consistent with interferometer data on the lower J lines. The ratios of the 12CO 3-2/13CO 3-2 integrated fluxes indicate that 12CO 3-2 is optically thick but that 13CO 3-2 is optically thin or at most moderately thick. The 13CO 3-2 lines have been used to estimate the cold gas mass. If a H2/CO conversion factor of 1 × 104 is adopted, the derived cold gas masses are factors of 10-200 lower than those deduced from 1.3 millimeter dust emission assuming a gas/dust ratio of 100, in accordance with previous studies. These findings confirm that CO is not a good tracer of the total gas content in disks since it can be photodissociated in the outer layers and frozen onto grains in the cold dense part of disks, but that it is a robust tracer of the disk velocity field. In contrast, H2 can shield itself from photodissociation even in low-mass "optically thin" debris disks and can therefore survive longer. The warm gas is typically 1%-10% of the total mass deduced from millimeter continuum emission, but it can increase up to 100% or more for the debris-disk objects. Thus, residual molecular gas may persist into the debris-disk phase. No significant evolution in the H2, CO, or dust masses is found for stars with ages in the range of 106-107 yr, although a decrease is found for the older debris-disk star β Pictoris. The large amount of warm gas derived from H2 raises the question of the heating mechanism(s). Radiation from the central star as well as the general interstellar radiation field heat an extended surface layer of the disk, but existing models fail to explain the amount of warm gas quantitatively. The existence of a gap in the disk can increase the area of material influenced by radiation. Prospects for future observations with ground- and space-borne observations are discussed.
The Jet-Disk Symbiosis in Blazar and Unified Model of FSRQs and BL Lac Objects

Using multi-wave band data for a large sample of 70 blazars, including 38 flat-spectrum radio quasars (FSRQs) and 32 BL Lac Objeces, we studied the correlations for both the flux and luminosity of the broad-line emission (FBLR) with the near-infrared flux (FK), X-ray flux (FX) and radio flux at 5GHz (FR), respectively. We could see that there is alwaysa strongcorrelationbetweenthe broad-lineandmulti-wavebandsfora sample of 70blazars; also, the slopes of the corresponding linear-regression equations are close to 1, which is consistent with the theoretical results. These results provide some new experimental evidence about coupling of the accretion disk and the jet of blazars. Simultaneously, we also indicated that the relative location of BL Lacs and FSRQs are quite separated, and that the luminosity of the the broad-line emission for BL Lacs is much less for FSRQs, which can prove that FSRQs and BL Lacs could be considered as a single population, or FSRQs and BL Lacs should be regarded as a class. But they are in different evolutionary stages of blazars, and have different types of accretion disks with different line-to-continuum ratios. Finally, the unified model of FSRQs and BL Lacs is also discussed.
A torque reversal of 4U 1907+09

Aims. We present an analysis of the accreting X-ray pulsar system 4U 1907+09 based on INTEGRAL data. The main focus of this analysis is a study of the timing behavior of this source. In addition we also show an analysis of the 5 - 90 keV spectrum. Methods. The data were extracted using the official INTEGRAL software OSA 5.1. Timing analysis was performed using epoch folding and pulsar pulse phasing. Results. We have measured 12 individual pulse periods for the years 2003 to 2005. We confirm earlier RXTE results that during 2003 the spin down became slower and show furthermore that after this phase 4U 1907+09 started to spin up with. P-pulse = -0.158 s yr(-1) in 2004. The similarity of the pulse period histories of 4U 1907+09 and 4U 1626-26 suggests that accretion onto an oblique rotator, as recently proposed by Perna et al., is a possible explanation for this change.