The Froissart-Martin bound states that two-particle diffraction cross section cannot rise with $s$ faster than ${\ln }^{2}s$, where $s$ is the Mandelstam variable. However, the diffraction production of many hadron showers separated by large rapidity gaps, when calculated within the standard Pomeron approach, leads to cross sections rising much faster than the Froissart-Martin bound. This is the point of Finkelstein-Kajantie problem. We consider the unitarization procedure based on Dyson-Schwinger equations with input froissaron propagators and a three-froissaron vertex depending on angular momenta of froissarons in it. The developed diffraction production model allows to resolve Finkelstein-Kajantie problem.

We present the first experimental search for the rare charm decay $D^0\to {\pi }^0\nu \overline{\nu }$. It is based on an $e^{+}{e}^{-}$ collision sample consisting of $10.6\times {10}^6$ pairs of $D^0{\overline{D}}^0$ mesons collected by the BESIII detector at $\sqrt{s}=3.773\mathrm{GeV}$, corresponding to an integrated luminosity of $2.93{\mathrm{fb}}^{-1}$. A data-driven method is used to ensure the reliability of the background modeling. No significant $D^0\to {\pi }^0\nu \overline{\nu }$ signal is observed in data and an upper limit of the branching fraction is set to be $2.1\times {10}^{-4}$ at the 90% confidence level. This is the first experimental constraint on charmed-hadron decays into dineutrino final states.

We study the interaction of the doubly bottom systems $BB$, $B^{*}B$, $B_{s}B$, $B_s^{*}B$, $B^{*}{B}^{*}$, $B^{*}{B}_s$, $B^{*}{B}_s^{*}$, $B_s{B}_s$, $B_s{B}_s^{*}$, $B_s^{*}{B}_s^{*}$ by means of vector meson exchange with Lagrangians from an extension of the local hidden gauge approach. The full s-wave scattering matrix is obtained implementing unitarity in coupled channels by means of the Bethe-Salpeter equation. We find poles below the channel thresholds for the attractively interacting channels $B^{*}B$ in $I=0$, $B_s^{*}B-B^{*}{B}_s$ in $I=\frac{1}{2}$, $B^{*}{B}^{*}$ in $I=0$, and $B_s^{*}{B}^{*}$ in $I=\frac{1}{2}$, all of them with $J^P=1^{+}$. For these cases the widths are evaluated identifying the dominant source of imaginary part. We find binding energies of the order of 10–20 MeV, and the widths vary much from one system to the other: of the order of 10–100 eV for the $B^{*}B$ system and $B_s^{*}B-B^{*}{B}_s$, about 6 MeV for the $B^{*}{B}^{*}$ system and of the order of 0.5 MeV for the $B_s^{*}{B}^{*}$ system.

We show the existence of strong (anti)correlations between the topological hot spots and the local values of the trace of the Polyakov loop in $2+1$ flavor QCD with physical quark mass, in the vicinity of the crossover transition corresponding to the simultaneous restoration of chiral symmetry and deconfinement. Using sophisticated lattice techniques, we have carefully identified the topological hot spots using quark zero modes and measured the short-distance fluctuations of the Polyakov loop about them, showing how the latter is repelled quite strongly around the peak of the zero modes. Though we could explain some aspects of these correlations within the instanton-dyon picture, our work sets the stage for a larger goal towards a systematic study of the role of different topological species that interact with the Polyakov loop, establishing the strong connection between topology and confinement.

In a two-dimensional conformal field theory with a moving mirror, known as a moving mirror model, the time evolution of the entanglement entropy shows a Page-like curve. This implies that the moving mirror model is useful to understand the island formula. In this paper, we study the time evolution of the subregion $\mathrm{complexity}=\mathrm{volume}$ (CV) complexity in the moving mirror model for a better understanding of the island formula of the complexity. In contrast to the entanglement entropy, the subregion CV complexity shows a peculiar behavior. We discuss this behavior in more detail.

We explore whether acceleration assists entanglement harvesting for a pair of uniformly accelerated detectors in three different acceleration scenarios, i.e., parallel, antiparallel and mutually perpendicular acceleration, both in the sense of the entanglement harvested and harvesting-achievable separation between the two detectors. Within the framework of entanglement harvesting protocols and the Unruh-DeWitt model of detectors locally interacting with massless scalar fields via a Gaussian switching function with an interaction duration parameter, we find that, in the sense of the entanglement harvested, acceleration is a mixed blessing insofar as it increases the harvested entanglement for a large detector energy gap relative to the interaction duration parameter, whilst inhibiting the entanglement harvested for a small energy gap. Regarding the harvesting-achievable separation range between the detectors, we further find that for very small acceleration and large energy gap, both relative to the duration parameter, acceleration-assisted enhancement can happen in all three acceleration scenarios. This is in sharp contrast to what was argued previously: that the harvesting-achievable range can be enhanced only for antiparallel acceleration. However, for a not too small acceleration relative to the duration parameter and an energy gap larger than the acceleration, we find that only detectors in parallel acceleration possess a harvesting-achievable range larger than those at rest.

We investigate retrolensing by two photon spheres in a novel black-bounce spacetime suggested by Lobo et al. which can correspond to a Schwarzschild black hole, a regular black hole, and a traversable wormhole including an Ellis-Bronnikov wormhole. In a case, the wormhole has a throat which acts as a photon sphere and it has another photon sphere outside of the throat. With the sun as a light source, an observer, and the wormhole are lined up in this order, sunlight reflected slightly outside of the throat and barely outside and inside of the outer photon sphere can reach the observer. We show that the light rays reflected by the outer photon sphere are dominant in retrolensing light curves in the case.

A problem which has now come to a head in general relativity, primarily as a result of the many recent detections of gravitational waves from the coalescence of compact binaries, is that there are very few viable theories against which to “test” it. To perform realistic tests of theories of gravity, we need to be able to look beyond general relativity and evaluate the consistency of a parametrized, physically acceptable, family of black hole metric alternatives with observational data from, especially, gravitational wave detections using, for example, an agnostic Bayesian approach. In this paper we further examine properties of one class of such metrics, which in fact arise as solutions of ungauged supergravity. In particular, we examine the massless, neutral, minimally coupled scalar wave equation in a general stationary, axisymmetric background metric such as that of a charged rotating black hole, when the scalar field is either time independent or in the low-frequency, near-zone limit, with a view to calculating the Love numbers of tidal perturbations, and of obtaining harmonic coordinates for the background metric. For a four-parameter family of charged asymptotically flat rotating black hole solutions of ungauged supergravity theory known as STU black holes, which includes Kaluza-Klein black holes and the Kerr-Sen black hole as special cases, we find that all time-independent solutions, and hence the harmonic coordinates of the metrics, are identical to those of the Kerr solution. In the low-frequency limit we find the scalar fields exhibit the same $SL(2,R)$ symmetry as holds in the case of the Kerr solution. We point out extensions of our results to a wider class of metrics, which includes solutions of Einstein-Maxwell-dilaton theory.

This work focuses on Conrady-Hnybida’s four-dimensional extended spinfoam model with timelike polyhedra, while we restrict all faces to be spacelike. First, we prove the absolute convergence of the vertex amplitude with timelike polyhedra, when $\mathrm{SU}(1,1)$ boundary states are coherent states or the canonical basis, or their finite linear combinations. Second, based on the finite vertex amplitude and a proper prescription of the $\mathrm{SU}(1,1)$ intertwiner space, we construct the extended spinfoam amplitude on an arbitrary cellular complex, taking into account the sum over $\mathrm{SU}(1,1)$ intertwiners of internal timelike polyhedra. We observe that the sum over $\mathrm{SU}(1,1)$ intertwiners is infinite for the internal timelike polyhedron that has at least two future-pointing and two past-pointing face normals. In order to regularize the possible divergence from summing over $\mathrm{SU}(1,1)$ intertwiners, we develop a quantum cutoff scheme based on the eigenvalue of the “shadow operator”. The spinfoam amplitude with timelike internal polyhedra (and spacelike faces) is finite, when two types of cutoffs are imposed. One is imposed on $j$ the eigenvalue of area operator, and the other is imposed on the eigenvalue of the shadow operator for every internal timelike polyhedron that has at least two future-pointing and two past-pointing face normals.

The detection of gravitational waves from extreme mass ratio inspirals (EMRIs) by the future space-based gravitational-wave detectors demands the generation of accurate enough waveform templates. Since the spin of the smaller secondary body cannot be neglected for the detection and parameter estimation of EMRIs, we study its influence on the phase of the gravitational waves from EMRIs with a spinning secondary. We focus on generic eccentric equatorial orbits around a Kerr black hole. To model the spinning secondary object, we use the Mathisson-Papapetrou-Dixon equations in the pole-dipole approximation. Furthermore, we linearize in spin the orbital variables and the gravitational-wave fluxes from the respective orbits. We obtain these fluxes by using the Teukolsky formalism in the frequency domain. We derive the evolution equations for the spin-induced corrections to the adiabatic evolution of an inspiral. Finally, through their numerical integration, we find the gravitational-wave phase shift between an inspiral of a spinning and a nonspinning body.

In this paper we provide new examples of anti–de Sitter black holes with a planar base manifold in four-dimensional critical gravity by considering nonlinear electrodynamics as a matter source. We find a general solution characterized by the presence of only one integration constant where, for a suitable choice of coupling constants, we can show the existence of one or more horizons. Additionally, we compute its nonzero thermodynamical quantities through a variety of techniques, testing the validity of the first law of thermodynamics as well as a Smarr formula. Finally, we analyze the local thermodynamical stability of the solutions. To our knowledge, these charged configurations are the first example with critical gravity where their thermodynamical quantities are not zero.

Early dark energy (EDE) is a proposed solution to the Hubble tension in which a new cosmological field accelerates cosmic expansion prior to recombination and reduces the physical size of the sound horizon. In previous work, a slight preference for a nonzero EDE contribution was found in the latest Atacama Cosmology Telescope data (ACT DR4), while the Planck satellite legacy data alone do not show evidence for it. In this work, we use the most recent public data from the South Pole Telescope (SPT-3G) to constrain the parameters of the EDE scenario. We find that at the current precision level of SPT-3G, an EDE contribution to the total energy density of the universe prior to recombination of $\sim 10\%$ cannot be ruled out, but that the data are also consistent with no EDE. The combination of ACT DR4 and SPT-3G with the Planck large-scale temperature anisotropy measurement shows a hint ($2.6\sigma$) for nonzero EDE; however, this preference disappears when the full Planck 2018 dataset is included.

We present a full forward-modeled $w\mathrm{CDM}$ analysis of the KiDS-1000 weak lensing maps using graph-convolutional neural networks (GCNN). Utilizing the cosmogrid, a novel massive simulation suite spanning six different cosmological parameters, we generate almost one million tomographic mock surveys on the sphere. Due to the large dataset size and survey area, we perform a spherical analysis while limiting our map resolution to HEALPix $n_{\mathrm{side}}=512$. We marginalize over systematics such as photometric redshift errors, multiplicative calibration and additive shear bias. Furthermore, we use a map-level implementation of the nonlinear intrinsic alignment model along with a novel treatment of baryonic feedback to incorporate additional astrophysical nuisance parameters. We also perform a spherical power spectrum analysis for comparison. The constraints of the cosmological parameters are generated using a likelihood-free inference method called Gaussian process approximate Bayesian computation (GPABC). Finally, we check that our pipeline is robust against choices of the simulation parameters. We find constraints on the degeneracy parameter of $S_8\equiv {\sigma }_8\sqrt{{\mathrm{\Omega }}_M/0.3}=0.78_{-0.06}^{+0.06}$ for our power spectrum analysis and $S_8=0.79_{-0.05}^{+0.05}$ for our GCNN analysis, improving the former by 16%. This is consistent with earlier analyses of the 2-point function, albeit slightly higher. Baryonic corrections generally broaden the constraints on the degeneracy parameter by about 10%. These results offer great prospects for full machine learning based analyses of ongoing and future weak lensing surveys.

We present the results obtained from the full-shape cosmology analysis of the redshift-space power spectra for four galaxy samples of the SDSS-III BOSS DR12 galaxy catalog over $0.2<z<0.75$. For the theoretical template, we use an emulator that was built from an ensemble set of $N$-body simulations, which enables fast and accurate computation of the redshift-space power spectrum of “halos.” Combining with the halo occupation distribution to model the galaxy-halo connection, we can compute the redshift-space power spectrum of BOSS-like galaxies in less than a CPU second, for an input model under flat $\mathrm{\Lambda }\mathrm{CDM}$ cosmology. In our cosmology inference, we use the monopole, quadrupole, and hexadecapole moments of the redshift-space power spectrum and include seven nuisance parameters, with broad priors, to model uncertainties in the galaxy-halo connection for each galaxy sample, but do not use any information on the abundance of galaxies. We demonstrate a validation of our analysis pipeline using the mock catalogs of BOSS-like galaxies, generated using different recipes of the galaxy-halo connection and including the assembly bias effect. Assuming weak priors on cosmological parameters, except for the BBN prior on ${\mathrm{\Omega }}_{\mathrm{b}}{h}^2$ and the CMB prior on $n_{\mathrm{s}}$, we show that our model well reproduces the BOSS power spectra. Including the power-spectrum information up to $k_{\max }=0.25h{\mathrm{Mpc}}^{-1}$, we find ${\mathrm{\Omega }}_{\mathrm{m}}=0.301_{-0.011}^{+0.012}$, $H_0=68.2\pm 1.4\mathrm{km}{\mathrm{s}}^{-1}{\mathrm{Mpc}}^{-1}$, and ${\sigma }_8=0.786_{-0.037}^{+0.036}$ for the mode and 68% credible interval, after marginalization over galaxy-halo connection parameters. We find little improvement in the cosmological parameters beyond a maximum wavelength $k_{\max }\simeq 0.2h{\mathrm{Mpc}}^{-1}$ due to the shot noise domination and marginalization of the galaxy-halo connection parameters. Our results are consistent with the Planck CMB results within $1\sigma$ statistical uncertainties.

Light-front wave functions play a fundamental role in the light-front quantization approach to QCD and hadron structure. However, a naive implementation of the light-front quantization suffers from various subtleties including the well-known zero-mode problem, the associated rapidity divergences which mixes ultraviolet divergences with infrared physics, as well as breaking of spatial rotational symmetry. We advocate that the light-front quantization should be viewed as an effective theory in which small $k^{+}$ modes have been effectively “integrated out,” with an infinite number of renormalization constants. Instead of solving light-front quantized field theories directly, we make the large momentum expansion of the equal-time Euclidean correlation functions in instant quantization as an effective way to systematically calculate light-front correlations, including the light-front wave function amplitudes. This large-momentum effective theory accomplishes an effective light-front quantization through lattice QCD calculations. We demonstrate our approach using an example of a pseudoscalar meson wave function.

We analyzed the invariant mass spectrum of near-threshold exotic states for one-channel candidates with a deep neural network. It can extract the scattering length and effective range, which would shed light on the nature of given states, from the experimental mass spectrum. As an application, the mass spectrum of the $X(3872)$ and the $T_{cc}^{+}$ are studied. The obtained scattering lengths, effective ranges, and most relevant thresholds are consistent with those from fitting to the experimental data. The advantage of the neural network is that it is more stable than the fitting, especially for low-statistic data. The network, which provides another way to analyze the experimental data, can also be applied to other one-channel near-threshold exotic candidates.

Yukawa couplings in the Lorentz- and $CPT$-violating Standard Model extension (SME) induce quantum contributions to the electromagnetic moments of quarks, which are calculated in the present paper and then used to define contributions to electromagnetic moments of nucleons. High-sensitivity measurements of the proton and neutron electromagnetic moments then yield constrains on SME coefficients, reaching bounds as restrictive as ${10}^{-12}$. This approach notably grants access to SME effects from the second and third quark families.

We study the weight or compositeness of the $\pi \pi -K\overline{K}$ and $\pi \eta -K\overline{K}$ in the composition of the $f_0(980)$ and $a_0(980)$ resonances, respectively. Either we use the saturation of the total width and compositeness, or we use a Flatté parametrization taking also into account the spectral function of a near-threshold resonance. We make connections and compare between these two methods. We take input values for the pole mass and width and, in addition, for the total compositeness or the decay-width branching ratio to the lighter channel for each resonance. It turns out that for the poles considered the meson-meson components are dominant for the $f_0(980)$, while for the $a_0(980)$ resonance they are subdominant. We also provide partial decay widths and partial compositeness coefficients, so that the $K\overline{K}$ component is the most important one for the $f_0(980)$. Additionally, this study stresses the need to distinguish between the bare and dressed couplings and widths in a Flatté parametrization. We elaborate on the connection between the partial-decay widths calculated in terms of the dressed couplings and the actual measured ones. Due to the coupled-channel dynamics when the pole lies near the heavier threshold in the second Riemann sheet some changes are needed with respect to standard relations.

We find that the inverse magnetic catalysis (IMC) for $U(1)$ axial symmetry can emerge around the chiral crossover regime in the thermomagnetic QCD with $2+1$ flavors at physical point. This phenomenon can be correlated with the IMC for the chiral $SU(2{)}_L\times SU(2{)}_R$ symmetry. We explicitly observe the axial inverse magnetic catalysis (AIMC) based on a Nambu-Jona-Lasinio model with $2+1$ quark flavors, where introduced anomalous magnetic moments of the quarks play the essential role to drive both the chiral IMC and AIMC. Our finding is shortly testable on lattices. Possible phenomenological and cosmological implications are also briefly addressed.