In this paper, we study the scattering amplitudes of $D^0{D}^0{\pi }^{+}\text{−}{D}^{*+}{D}^0$ coupled channels based on the $K$ matrix within the Chew-Mandelstam formalism. The $D^0{D}^0{\pi }^{+}$ invariant mass spectrum of LHCb is fitted, and the pole parameters of the $T_{cc}^{+}$ are extracted. The analysis of pole behavior suggests that the $T_{cc}^{+}$ may originate from a $D^{*+}{D}^0$ virtual state and is formed as a result of an interplay between an attractive interaction between $D^0$ and $D^{*+}$ and coupling to $D^0{D}^0{\pi }^{+}$ channel.

The photon polarization in $b\to s\gamma$ transitions is measured for the first time in radiative $b$ -baryon decays exploiting the unique spin structure of ${\mathrm{\Lambda }}_b^0\to \mathrm{\Lambda }\gamma$ decays. A data sample corresponding to an integrated luminosity of $6{\mathrm{fb}}^{-1}$ collected by the LHCb experiment in $pp$ collisions at a center-of-mass energy of 13 TeV is used. The photon polarization is measured to be ${\alpha }_{\gamma }=0.82_{-0.26-0.13}^{+0.17+0.04}$, where the first uncertainty is statistical and the second systematic. This result is in agreement with the Standard Model prediction and previous measurements in $b$ -meson decays. Charge-parity breaking effects are studied for the first time in this observable and found to be consistent with $CP$ symmetry.

Using $e^{+}{e}^{-}$ annihilation data corresponding to a total integrated luminosity of $6.32\mathrm{f}{\mathrm{b}}^{-1}$ collected at center-of-mass energies between 4.178 and 4.226 GeV with the BESIII detector, we perform an amplitude analysis of the decay $D_s^{+}\to K_S^0{K}_S^0{\pi }^{+}$ for the first time. An enhancement is observed in the $K_S^0{K}_S^0$ mass spectrum near $1.7\mathrm{GeV}/c^2$, which was not seen in $D_s^{+}\to K^{+}{K}^{-}{\pi }^{+}$ in an earlier work, implying the existence of an isospin one partner of the $f_0(1710)$. The branching fraction of the decay $D_s^{+}\to K_S^0{K}_S^0{\pi }^{+}$ is determined to be $\mathcal{B}(D_s^{+}\to K_S^0{K}_S^0{\pi }^{+})=(0.68\pm 0.04_{\mathrm{stat}}\pm 0.01_{\mathrm{syst}})\%$.

We find exact, analytic solutions of the holographic ac conductivity at arbitrary frequency $\omega$ and temperature $T$, in contrast to previous works where the ac conductivity was analytically obtained usually at small $\omega$ and $T$. These solutions enable us to study the analyticity properties of the current-current correlator $G(\omega )$ in detail. The first system we study is the ${\mathrm{AdS}}_5$ planar black hole with momentum dissipation, whose extremal limit has an ${\mathrm{AdS}}_2$ factor. Then we study ${\mathrm{AdS}}_4$ and ${\mathrm{AdS}}_5$ Einstein-dilaton systems whose special cases are maximal gauged supergravities. The solutions show how the poles move and how branch cuts emerge as the temperature varies. As a by-product, we obtain an R-current correlator in $\mathcal{N}=4$ super-Yang-Mills theory on a sphere at finite temperature in the large $N$ and strong coupling limit.

Our goal is to find a matrix model with ${\mathrm{BMS}}_3$ constraints built in. These constraints are imposed through loop equations. We solve them using a free field realization of the algebra and write down the partition function in eigenvalue form. We comment on the nature of this partition function and its relations with integrable systems.

We study the nonperturbative harvesting of classical and quantum correlations between two parties coupled to a quantum field. First, we consider a scenario with an arbitrary number of two-level systems that couple to a quantum field locally in time. Then, we study the impact of the presence of additional detectors (interlopers) on the ability for two target detectors (Alice and Bob) to acquire correlations through their interaction with the field. We analyze the harvesting of different correlation measures in this nonperturbative regime and we demonstrate that even a single interloper can completely sabotage all correlation harvesting between Alice and Bob by acting on the causal past of one of them. Specifically, we show that the interloper is able to interact with the field so that the field itself “floods” one of the parties with entropy. This prevents Alice and Bob from acquiring any correlations. Furthermore, we show that this kind of attack cannot be defended against.

Gravitational lensing of a light source by a black hole leads to the appearance of higher-order images produced by photons that loop around the black hole before reaching the observer. Higher-order images were widely investigated numerically and analytically, in particular using the so-called strong deflection limit of gravitational deflection. After recent observations of the black hole image, attention has been drawn to higher-order rings, which are lensed images of the accreting matter of the black hole environment and can appear near the boundary of the black hole shadow. In this article, we use the strong deflection limit technique to investigate higher-order ring images of the luminous accretion disk around a Schwarzschild black hole. We consider a thin disk given by the inner and outer radii and an observer located far from the black hole on the axis of symmetry. For this configuration, it becomes possible to find the angular radii, thicknesses, and solid angles of higher-order rings in the form of compact analytical expressions. We show that the size of the rings is mainly determined by the position of the inner boundary of the accretion disk, which makes it possible to use them to distinguish between different accretion models. Possible generalizations of our model to nonsymmetric images can help to make the estimation of black hole angular momentum. We also present the analytical estimation of fluxes from higher-order images. Our method makes it easy to investigate $n=2$ and $n=3$ higher-order rings, the possible observation of which in future projects is currently being discussed.

Emission of anisotropic gravitational radiation from a compact binary system leads to a flux of linear momentum. This results in recoil of the system. We investigate the rate of loss of linear momentum flux in the far zone of the source using various mass type and current type multipole moments for an inspiralling compact binary merger in quasielliptical orbits at 2.5 post-Newtonian order. We compute the linear momentum flux accurately up to $\mathcal{O}(e_t)$ in a harmonic coordinate. A 2.5 post-Newtonian quasi-Keplarian representation of the parametric solution to the post-Newtonian equation of motion for the compact binary system has been adopted here. We also provide a closed form expression for the accumulated linear momentum from the remote past through the binary evolution.

Three recent articles have claimed that it is possible to, at least in theory, either set up positive energy warp drives satisfying the weak energy condition (WEC), or at the very least, to minimize the WEC violations. These claims are, at best, incomplete since the arguments as presented only assert but do not prove the existence of one set of timelike observers, the comoving Eulerian observers, who see relatively “nice” physics. While these particular observers might arguably see a positive energy density, the WEC requires all timelike observers to see positive energy density. Therefore, one should carefully revisit this issue. A more careful analysis shows that the situation is actually much grimmer than advertised—within the framework adopted by those three papers all physically reasonable warp drives will certainly violate the WEC, and both the strong and dominant energy conditions. Under plausible subsidiary conditions the null energy condition is also violated. While warp drives are certainly interesting examples of speculative physics, the violation of the energy conditions, at least within the framework of standard general relativity, is unavoidable. Even in modified gravity, physically reasonable warp drives will still violate the purely geometrical null convergence condition and the timelike convergence condition which, in turn, will place very strong constraints on any modified-gravity warp drive.

We construct, for the first time, charged rotating black string solutions in four-dimensional Einsteinian cubic gravity, which are asymptotically anti–de Sitter. By assuming that the solutions are completely regular at the horizon and studying their near-horizon behavior, we find some thermodynamic properties, which can be accessed analytically. We compute independently the Hawking temperature, the Wald entropy, the mass, the angular momentum, the charge, and the electrostatic potential of the solutions, analytically. Using these, we show that the first law of thermodynamics for rotating black strings is exactly satisfied in both charged and uncharged cases. We also observe that, in the absence of Maxwell field, some of the solutions have positive specific heat, which makes them thermodynamically stable.

Nearby core-collapse supernovae (CCSNe) are powerful multimessenger sources for gravitational-wave, neutrino, and electromagnetic telescopes as they emit gravitational waves in the ideal frequency band for ground based detectors. Once a CCSN gravitational-wave signal is detected, we will need to determine the parameters of the signal and understand how those parameters relate to the source’s explosion, progenitor, and remnant properties. This is a challenge due to the stochastic nature of CCSN explosions, which is imprinted on their time series gravitational waveforms. In this paper, we perform Bayesian parameter estimation of CCSN signals using an asymmetric chirplet signal model to represent the dominant high-frequency mode observed in spectrograms of CCSN gravitational-wave signals. We use design sensitivity Advanced LIGO noise and CCSN waveforms from four different hydrodynamical supernova simulations with a range of different progenitor stars. We determine how well our model can reconstruct time-frequency images of the emission modes and show how well we can determine parameters of the signal such as the frequency, amplitude, and duration. We show how the parameters of our signal model may allow us to place constraints on the protoneutron star mass and radius, the turbulent kinetic energy onto the protoneutron star, and the time of shock revival.

The nature of the Fermi $\gamma$-ray Galactic Center excess (GCE) has remained a persistent mystery for over a decade. Although the excess is broadly compatible with emission expected due to dark matter annihilation, an explanation in terms of a population of unresolved astrophysical point sources, e.g., millisecond pulsars, remains viable. The effort to uncover the origin of the GCE is hampered in particular by an incomplete understanding of diffuse emission of Galactic origin. This can lead to spurious features that make it difficult to robustly differentiate smooth emission, as expected for a dark matter origin, from more “clumpy” emission expected from a population of relatively bright, unresolved point sources. We use recent advancements in the field of simulation-based inference, in particular density estimation techniques using normalizing flows, in order to characterize the contribution of modeled components, including unresolved point source populations, to the GCE. Compared to traditional techniques based on the statistical distribution of photon counts, our machine-learning-based method is able to utilize more of the information contained in a given model of the Galactic Center emission and in particular can perform posterior parameter estimation while accounting for pixel-to-pixel spatial correlations in the $\gamma$-ray map. This makes the method demonstrably more resilient to certain forms of model misspecification. On application to Fermi data, the method generically attributes a smaller fraction of the GCE flux to unresolved point sources when compared to traditional approaches. We nevertheless infer such a contribution to make up a non-negligible fraction of the GCE across all analysis variations considered, with at least ${38}_{-19}^{+9}\%$ of the excess attributed to unresolved point sources in our baseline analysis.

One has measured $f_{{\mathrm{\Omega }}_b}\mathcal{B}({\mathrm{\Omega }}_b^{-}\to {\mathrm{\Omega }}^{-}J/\mathrm{\Psi })$ at the level of ${10}^{-6}$, where the fragmentation faction $f_{{\mathrm{\Omega }}_b}$ is to evaluate the $b$ quark to ${\mathrm{\Omega }}_b^{-}$ production rate. Using the ${\mathrm{\Omega }}_b\to \mathrm{\Omega }$ transition form factors calculated in the light-front quark model, we predict $\mathcal{B}({\mathrm{\Omega }}_b^{-}\to {\mathrm{\Omega }}^{-}J/\mathrm{\Psi })=({5.3}_{-2.1-2.7}^{+3.3+3.8})\times {10}^{-4}$. In particular, we extract $f_{{\mathrm{\Omega }}_b}=({0.54}_{-0.22-0.28-0.15}^{+0.34+0.39+0.21})\times {10}^{-2}$, demonstrating that the $b$ to ${\mathrm{\Omega }}_b$ productions are much more difficult than the $b$ to ${\mathrm{\Lambda }}_b({\mathrm{\Xi }}_b)$ ones. Since $f_{{\mathrm{\Omega }}_b}$ has not been determined experimentally, $f_{{\mathrm{\Omega }}_b}$ added to theoretical branching fractions can be compared to future measurements of the ${\mathrm{\Omega }}_b$ decays.

Sterile neutrinos with keV-scale masses are popular candidates for warm dark matter. In the most straightforward case, they are produced via oscillations with active neutrinos. We introduce effective self-interactions of active neutrinos and investigate the effect on the parameter space of sterile neutrino mass and mixing. Our focus is on mixing with electron neutrinos, which is subject to constraints from several upcoming or running experiments like TRISTAN, ECHo, BeEST, and HUNTER. Depending on the size of the self-interaction, the parameter space moves closer to, or further away from, the one testable by those future experiments. In particular, we show that phase 3 of the HUNTER experiment would test a larger amount of parameter space in the presence of self-interactions than without them. We also investigate the effect of the self-interactions on the free-streaming length of the sterile neutrino dark matter, which is important for structure formation observables.

The exact eigenenergies of the $T_{4c}=[cc][\overline{c}\overline{c}]$, $T_{4b}=[bb][\overline{b}\overline{b}]$, and $T_{2[bc]}=[bc][\overline{b}\overline{c}]$ tetraquarks are calculated within the extended transitional Hamiltonian approach, in which the so-called Bethe ansatz within an infinite-dimensional Lie algebra is used. We fit the parameters appearing in the transitional region from phenomenology associated with potential candidates of tetraquarks. The rotation and vibration transitional theory seems to provide a better description of heavy tetraquarks than other attempts within the same formalism. Our results indicate that the pairing strengths are large enough to provide binding; an extended comparison with the current literature is also performed.

We use the sign-reweighting method to simulate the QCD chiral transition at real baryon densities on phenomenologically relevant lattices. This avoids the severe limitations of extrapolating from zero or imaginary chemical potential and the overlap problem of traditional reweighting approaches, opening up a new window to reliably study hot and dense strongly interacting matter from first principle lattice simulations. We demonstrate that sign reweighting can reach up to a baryochemical potential-temperature ratio of ${\mu }_B/T=2.7$, covering most of the Relativistic Heavy Ion Collider Beam Energy Scan range.

We construct a new type of Chandrasekhar transformation in Kerr spacetime using the different tortoise coordinate, which is useful for exact analysis to study the Teukolsky equation with arbitrary frequency. We also give the interpretation of our transformation using the formalism of the quantum Seiberg-Witten geometry.

In this paper, the polarization modes of gravitational waves in Horndeski gravity are studied under the Palatini formalism. After obtaining the linearized equation of perturbations in Minkowski background, we find that the polarization modes of gravitational waves depend on the selection of the theoretical parameters. The polarization modes can be divided into quite rich cases by parameters. In all cases of parameter selection, there are $+$ and $\times$ modes propagating at the speed of light but no vector modes. The only difference from general relativity is scalar modes, especially the scalar degrees of freedom can be 0, 1 or 2 in different cases. The appropriate parameter cases can be expected to be selected in the detection of gravitational wave polarization modes by Lisa, Taiji and TianQin in the future.

The neutrino-nucleus reactions are studied at energies from 0 to 3 GeV, using the crisp program. To simulate these reactions, crisp uses the Monte Carlo method through an intranuclear cascade model. Quasielastic, baryonic resonance formation, and deep inelastic scattering channels for the neutrino-nucleon interaction are considered. The total and differential particle emission cross sections were obtained, resulting in a good agreement with the values reported by the MiniBooNE experiment. The influence of nuclear effects on the studied reactions, such as fermionic motion and the Pauli blocking mechanism, was shown. By using only neutrino-nucleon interactions (1p1h), it was necessary to modify the axial mass of the quasielastic channels to $M_A=1.35\mathrm{GeV}$ (much higher than the value obtained in neutrino-deuterium reactions, $M_A=1.026\mathrm{GeV}$). The problem in adjusting $M_A$ is the need for known $M_A(A)$, where $A$ is the mass number, in case we want to study another target nucleus. The introduction of the 2p2h processes solves this and also reproduces the experimental data with $M_A=1.026\mathrm{GeV}$. To show this, we use the transverse enhancement model to implement the 2p2h dynamic in crisp, in such a way that it can be used with any target nucleus.

Photon rings near the edge of a black hole shadow are supposed to be a unique tool to validate general relativity and provide reliable measurements of principal black hole parameters: spin and mass. Such measurements are possible though only for nearby supermassive black holes (SMBH) with space-Earth very long baseline interferometry (S-VLBI) in the submillimeter wavelength range. For subrings to be distinguished S-EVLBI observations with long baselines at the Lagrangian Sun-Earth L2 libration point are needed. However, the average fluxes of nearby SMBH: Sagittarius ${\mathrm{A}}^{*}$ (Sgr ${\mathrm{A}}^{*}$) and $\mathrm{M}{87}^{*}-F_{\nu }\sim 1\mathrm{Jy}$, are still insufficient to detect the signal from the photon rings with even such long baselines. We argue that only manifestations of flares in the submillimeter waveband in their accretion disks can reveal observable signals from the photon rings with the S-EVLBI at L2. Such observations will become possible within the planned joint program of the Event Horizon Telescope (EHT) and Millimetron Space Observatory (MSO), and within the planned next generation EHT (ngEHT) project. Two different observational tests for photons rings are discussed. The first one involves observations of a time series of responds from subsequent subrings as can be seen in a 1D visibility function within the join EHT-MSO configuration, the second one—measurements of an increase of the angle between subsequent subrings in the 2D VLBI image which can be obtained within the ngEHT project.