On configurations with $2+1$-flavor dynamical domain-wall fermions, we calculate the RI/(S)MOM renormalization constants (RC) of overlap quark bilinears. Hypercubic (HYP) smearing is used to construct the overlap Dirac operator. We investigate the possible effects of the smearing on discretization errors in the RCs by varying the level of smearing from 0 to 1 and 2. The lattice is of size ${32}^3\times 64$ and with lattice spacing $1/a=2.383(9)\mathrm{GeV}$. The RCs in the $\overline{\mathrm{MS}}$ scheme at 2 GeV are given at the end, with the uncertainty of $Z_T$ reaching $\le 1\%$ for the tensor current. Results of the renormalized quark masses and hadron matrix elements show that the renormalization procedure suppresses the $\sim 30\%$ difference of the bare quantities with or without HYP smearing into the 3%–5% level.

In the presence of a momentum cutoff, effective theories seem unable to faithfully reproduce the so-called chiral anomaly in the Standard Model. A novel prospect to overcome this related issue is discussed herein via the calculation of the ${\gamma }^{*}{\pi }^0\gamma$ transition form factor $G^{{\gamma }^{*}{\pi }^0\gamma }(Q^2)$, whose normalization is intimately connected with the chiral anomaly and dynamical chiral symmetry breaking (DCSB). To compute such transition, we employ a contact interaction model of quantum chromodynamics (QCD) under a modified rainbow ladder truncation, which automatically generates a quark anomalous magnetic moment term, weighted by a strength parameter $\xi$. This term, whose origin is also connected with DCSB, is interpreted as an additional interaction that mimics the complex dynamics beyond the cutoff. By fixing $\xi$ to produce the value of $G^{{\gamma }^{*}{\pi }^0\gamma }(0)$ dictated by the chiral anomaly, the computed transition form factor, as well as the interaction radius and neutral pion decay width, turn out to be comparable with QCD-based studies and experimental data.

Using a data sample corresponding to an integrated luminosity of $2.93{\mathrm{fb}}^{-1}$ collected at a center-of-mass energy of 3.773 GeV with the BESIII detector at the BEPCII collider, we search for a scalar partner of the $X(3872)$, denoted as $X(3700)$, via $\psi (3770)\to \gamma \eta {\eta }^{\prime }$ and $\gamma {\pi }^{+}{\pi }^{-}J/\psi$ processes. No significant signals are observed and the upper limits of the product branching fractions $\mathcal{B}(\psi (3770)\to \gamma X(3700))·\mathcal{B}(X(3700)\to \eta {\eta }^{\prime })$ and $\mathcal{B}(\psi (3770)\to \gamma X(3700))·\mathcal{B}(X(3700)\to {\pi }^{+}{\pi }^{-}J/\psi )$ are determined at the 90% confidence level, for the narrow $X(3700)$ with a mass ranging from 3710 to $3740\mathrm{MeV}/c^2$, which are from 0.9 to $1.9(\times {10}^{-5})$ and 0.9 to $3.4(\times {10}^{-5})$, respectively.

We present analytic stationary and axially symmetric black hole solutions to the semiclassical Einstein equations that are sourced by the trace anomaly. We also find evidence that the same spacetime geometry satisfies the field equations of a subset of Horndeski theories featuring a conformally coupled scalar field. We explore various properties of these solutions and determine the domain of existence of black holes. These black holes display distinctive features, such as noncircularity, a non-spherically-symmetric event horizon, and violations of the Kerr bound.

TeV-range cosmic ray electrons and positrons (CREs) have been directly measured in the search for new physics or unknown astrophysical sources. CREs can inverse-Compton scatter solar photons and boost their energies into gamma ray bands. Any potential CRE excess would enhance the resultant inverse Compton emission spectrum in the relevant energy range, offering a new window to verify the measured CRE spectrum. In this paper, we show that an excess in the TeV range of the CRE spectrum, such as the one indicated by the DAMPE experiment, can induce a characteristic solar gamma ray signal. Accounting for contamination from extragalactic gamma ray backgrounds (EGB), we forecast the DAMPE feature is testable ($\gtrsim 4\sigma$) with a $\sim {10}^5{\mathrm{m}}^2\mathrm{yr}$ exposure in the off-disk direction. This can be achieved by long-exposure observations of water Cherenkov telescopes, such as LHAASO (7.2 years) and HAWC (25.9 years).

We study the topology of the thermodynamic space of four dimensional dyonic anti–de Sitter (AdS) black hole in three different ensembles: canonical, mixed, and grand canonical ensemble. While canonical ensemble refers to the ensemble with fixed electric and magnetic charges, mixed ensemble is an ensemble where we fix magnetic charge and electric potential. In the grand canonical ensemble, potentials corresponding to both electric and magnetic charges are kept fixed. In each of these ensembles, we first compute the topological charges associated with critical points. We find that while in both canonical and mixed ensembles, there exists one conventional critical point with topological charge $-1$, in the grand canonical ensemble, we find no critical point. Then, we consider the dyonic AdS black hole as topological defects in thermodynamic space and study its local and global topology by computing the winding numbers at the defects. We observe that while the topologies of the black hole in canonical and mixed ensembles are identical with total topological charge equaling 1, in the grand canonical ensemble, depending on the values of potentials, the total topological charge is either equal to 0 or 1. In canonical and mixed ensembles, either one generation and one annihilation points or no generation/annihilation points are found. In the grand canonical ensemble, depending on the values of potentials, we find either one generation point or no generation/annihilation point. Thus, we infer that the topological class of 4D dyonic AdS black hole is ensemble dependent.

We compute the leading order contribution to radiative losses in the case of spinning binaries with aligned spins due to their spin-orbit interaction. The orbital average along hyperboliclike orbits is taken through an appropriate spin-orbit modification to the quasi-Keplerian parametrization for nonspinning bodies, which maintains the same functional form, but with spin-dependent orbital elements. We perform consistency checks with existing post-Newtonian-based and post-Minkowskian (PM)-based results. In the former case, we compare our expressions for both radiated energy and angular momentum with those obtained in [G. Cho et al., From boundary data to bound states. Part III. Radiative effects, J. High Energy Phys. 04 (2022) 154] by applying the boundary-to-bound correspondence to known results for ellipticlike orbits, finding agreement. The linear momentum loss is instead newly computed here. In the latter case, we also find agreement with the low-velocity limit of recent calculations of the total radiated energy, angular momentum and linear momentum in the framework of an extension of the worldline quantum field theory approach to the classical scattering of spinning bodies at the leading PM order [G. U. Jakobsen et al., Gravitational Bremsstrahlung and Hidden Supersymmetry of Spinning Bodies, Phys. Rev. Lett. 128, 011101 (2022), M. M. Riva et al., Gravitational bremsstrahlung from spinning binaries in the post-Minkowskian expansion, Phys. Rev. D 106, 044013 (2022)]. We get exact expressions of the radiative losses in terms of the orbital elements, even if they are at the leading post-Newtonian order, so that their expansion for large values of the eccentricity parameter (or equivalently of the impact parameter) provides higher-order terms in the corresponding PM expansion, which can be useful for future crosschecks of other approaches.

During binary black hole (BBH) mergers, energy and momenta are carried away from the binary system as gravitational radiation. Access to the radiated energy and momenta allows us to predict the properties of the remnant black hole. We develop a Python package gw_remnant to extract the remnant mass, remnant spin, peak luminosity, and the final kick imparted on the remnant black hole from the gravitational waveforms. Using this package, we extract the remnant properties of the final black hole in case of nonspinning BBH mergers with mass ratios ranging from $q=2.5$ to $q=1000$ using waveform modes generated from BHPTNRSur1dq1e4, a recently developed numerical-relativity-informed surrogate model based on the black hole perturbation theory framework. We validate our results against the remnant properties estimated from numerical relativity (NR) surrogate models in the comparable mass-ratio regime and against recently available high-mass-ratio NR simulations at $q=[15,32,64]$. We find that our remnant property estimates computed from fluxes at future null infinity closely match the estimates obtained from the NR surrogate model of apparent horizon data. Using Gaussian process regression fitting methods, we train a surrogate model, BHPTNR_Remnant, for the properties of the remnant black hole arising from BBH mergers with mass ratios from $q=2.5$ to $q=1000$. Finally, we discuss potential improvements in the BHPTNRSur1dq1e4 waveform model when including remnant information. We make both the gw_remnant and BHPTNR_Remnant packages publicly available.

The gravitational and electromagnetic multipole moments of the charged rotating disc of dust, which is an axisymmetric, stationary solution of the Einstein-Maxwell equations in terms of a post-Newtonian expansion, are calculated and discussed. It turns out that the individual mass, angular momentum, electric and magnetic moments are ordered in the sense that higher moments have a lower absolute value. There is an interesting conjecture stating that the absolute values of all higher multipole moments of a uniformly rotating perfect fluid body are always greater than those of the corresponding Kerr spacetime, which we generalize to include charged bodies. We find that for the charged rotating disc of dust, the conjecture holds (within the limits of accuracy of the post-Newtonian expansion).

Massive black holes (MBHs) are crucial in shaping their host galaxies. How the MBH co-evolves with its host galaxy is a pressing problem in astrophysics and cosmology. The valuable information carried by the binary MBH is encoded in the gravitational waves (GWs), which will be detectable by the space-borne GW detector LISA. In the GW data analysis, usually only the dominant (2,2) mode of the GW signal is considered in the parameter estimation for LISA. However, including the higher harmonics in parameter estimation can break the degeneracy between the parameters, especially for the inclination angle and luminosity distance. This may enable the identification of GW signals without electromagnetic counterparts, known as “dark sirens.” Thus, incorporating higher harmonics will be beneficial to resolve the Hubble tension and constrain the cosmological model. In this paper, we investigate the role of higher harmonics in the parameter estimation for GWs emitted by binary MBHs. We demonstrate that including the (3,3) mode can lead to a ${10}^3$-times improvement in angular resolution and a ${10}^4$-times improvement in luminosity distance. Meanwhile, our results indicate that considering higher harmonics increases the probability of identifying over 70% host galaxies from ${10}^{-2}{\mathrm{Gpc}}^3$ cosmological volume threshold (corresponding ${10}^5$ host galaxies), while the probability is less than 8% for only the (2,2) mode. Thus, our results underscore the importance of including higher modes in the GW signal from binary MBHs, for LISA at least (3,3) mode.

We study the evolution of close triple black hole system with full numerical relativity techniques. We consider an equal mass non spinning hierarchical system with an inner binary ten orbits away from merger and study the effects of the third outer black hole on the binary’s merger time and its eccentricity evolution. We find a generic time delay and an increase in the number of orbits to merger of the binary, that can be modeled versus the distance $D$ to the third black hole as $\sim 1/D^{2.5}$. On the other hand, we find that the orientation of the third black hole orbit has little effect on the binary’s merger time when considering a fiducial initial distance of $D=30M$ to the binary (with initial orbital separation $d=8M$). In those scenarios the evolution of the inner binary eccentricity presents a steady decay, roughly as expected, but in addition shows a modulation with the timescale of the outer third black hole orbital semiperiod around the binary, resembling a beating frequency.

We examine the teleparallel formulation of nonminimally coupled scalar Einstein-Gauss-Bonnet gravity. In the teleparallel formulation, gravity is described by torsion instead of curvature, causing the usual Gauss-Bonnet invariant expressed through curvature to decay into two separate invariants built from torsion. Consequently, the teleparallel formulation permits broader possibilities for nonminimal couplings between spacetime geometry and the scalar field. In our teleparallel theory, there are two different branches of equations in spherical symmetry depending on how one solves the antisymmetric part of the field equations, leading to a real and a complex tetrad. We first show that the real tetrad seems to be incompatible with the regularity of the equations at the event horizon, which is a symptom that scalarized black hole solutions beyond the Riemannian Einstein-Gauss-Bonnet theory might not exist. Therefore, we concentrate our study on the complex tetrad. This leads to the emergence of scalarized black hole solutions, where the torsion acts as the scalar field source. Extending our previous work, we study monomial nonminimal couplings of degrees 1 and 2, which are intensively studied in conventional, curvature-based, scalar Einstein-Gauss-Bonnet gravity. We discover that the inclusion of torsion can potentially alter the stability of the resulting scalarized black holes. Specifically, our findings indicate that for a quadratic coupling, which is entirely unstable in the pure curvature formulation, the solutions induced by torsion may exhibit stability within certain regions of the parameter space. In a limiting case, we were also able to find black holes with a strong scalar field close to the horizon but with a vanishing scalar charge.

In the context of the discrepancies between the early and late universe, we emphasize the importance of independent measurements of the cosmic curvature in the late universe. We present an investigation of the model-independent measurement of the cosmic curvature parameter ${\mathrm{\Omega }}_k$ in the late universe with the latest Hubble parameter $H(z)$ measurements and type Ia supernovae (SNe Ia) data. For that, we use two reconstruction methods, the Gaussian process (GP) and artificial neural network (ANN) methods, to achieve the distance construction from $H(z)$ data. Our analysis reveals that the GP method provides the most precise constraint on ${\mathrm{\Omega }}_k$, with a constraint precision of $\xi ({\mathrm{\Omega }}_k)=0.13$, surpassing recent estimations using similar methods. The GP method consistently indicates a preference for a flat universe at the $2\sigma$ confidence level. Moreover, we find that the choice of reconstruction method influences the estimation of ${\mathrm{\Omega }}_k$. The ANN reconstruction method exhibits higher sensitivity to the addition of BAO $H(z)$ data, resulting in comparable constraint precision to the GP method. A discrepancy exists between the best-fit values obtained by these two reconstruction methods, indicating their dependence on the reconstruction approach. However, we anticipate that with the improvement of sample size and precision of observational $H(z)$ data, the estimation of ${\mathrm{\Omega }}_k$ using this approach will become more robust and reliable.

We study the production of a beyond the Standard Model (BSM) free-streaming relativistic particles which contribute to $N_{\mathrm{eff}}$ and investigate how much the predictions for the inflationary analysis change. We consider inflaton decay as the source of this dark radiation (DR) and use the cosmic microwave background (CMB) data from Planck-2018 to constrain the scenarios and identify the parameter space involving couplings and masses of the inflaton that will be within the reach of next-generation CMB experiments like spt-3g, CMB-S4, CMB-Bhārat, PICO, CMB-HD, etc. We find that if the BSM particle is produced only from the interaction with inflaton along with Standard Model (SM) relativistic particles, then its contribution to $N_{\mathrm{eff}}$ is a monotonically increasing function of the branching fraction, $B_X$ of the inflaton to the BSM particle $X$; Planck bound on $N_{\mathrm{eff}}$ rules out such $B_X\gtrsim 0.09$. Considering two different analyses of Planck+bicep data together with other cosmological observations, $N_{\mathrm{eff}}$ is treated as a free parameter, which relaxes the constraints on scalar spectral index ($n_s$) and tensor-to-scalar ratio ($r$). The first analysis leads to predictions on the inflationary models like hilltop inflation being consistent with the data. Second analysis rules out the possibility that BSM particle $X$ producing from the inflaton decay in Coleman-Weinberg inflation or Starobinsky inflation scenarios. To this end, we assume that SM Higgs is produced along with the BSM particle. We explore the possibilities that $X$ can be either a scalar or a fermion or a gauge boson and consider possible interactions with inflaton and find out the permissible range on the allowed parameter space Planck and those which will be within the reaches of future CMB observations.

We present the multipole component form of the gravitational-wave tidal phase for compact binary coalescences (MultipoleTidal), which consists of the mass quadrupole, the current quadrupole, and the mass octupole moments. We demonstrate the phase evolution and the phase difference between the tidal multipole moments (MultipoleTidal) and the mass quadrupole (PNTidal) as well as the numerical-relativity calibrated model (NRTidalv2). We find the MultipoleTidal gives a larger phase shift than the PNTidal, and is closer to the NRTidalv2. We compute the matches between waveform models to see the impact of the tidal multipole moments on the gravitational wave phases. We find the MultipoleTidal gives larger matches to the NRTidalv2 than the PNTidal, in particular, for high masses and large tidal deformabilities. We also apply the MultipoleTidal model to binary neutron star coalescence events GW170817 and GW190425. We find that the current quadrupole and the mass octupole moments give no significant impact on the inferred tidal deformability.

Core-collapse supernovae are a useful laboratory to probe the nature of exotic particles. If axionlike particles (ALPs) are produced in supernovae, they can affect the transfer of energy and leave traces in observational signatures. In this work, we present results from two-dimensional supernova models including the effects of the production and the absorption of ALPs that couple with photons. It is found that the additional heating induced by ALPs can enhance the diagnostic energy of explosion, $E_{\mathrm{diag}}$. For example, for moderate ALP-photon coupling, we find explosion energies $\sim 0.6\times {10}^{51}\mathrm{erg}$ compared to our reference model without ALPs of $\sim 0.4\times {10}^{51}\mathrm{erg}$ in the first $\sim 0.5\mathrm{s}$ postbounce explored in this work. Our findings indicate that when the coupling constant is sufficiently high, the neutrino luminosities and mean energies are decreased because of the additional cooling of the proto-neutron star via ALPs. The gravitational wave amplitude is also reduced because the mass accretion on the proto-neutron star is suppressed. Although the ALP-photon coupling can foster explodability, including enhancing the explosion energy closer to recent observations, more long-term simulations in three spatial dimensions are needed to draw robust conclusions.

It is known that the leading-order tidal effects in gravitational waveforms can be quantified by tidal deformability, while higher order terms, e.g., harmonic overtones of Love number and dynamical tides, have not been well investigated yet. The concept of a “form factor,” which is different from but resembles the effective tidal deformability, for the tidal interactions between neutron stars in coalescing binaries is illustrated here. The form factor effectively incorporates the contribution of dynamical tides. The dependence of tidal form factor on tidal deformability, spins, and inclination angles is modeled and expressed in a closed form.

Jets provide one of the primary probes of the quark-gluon plasma produced in ultrarelativistic heavy ion collisions and the cold nuclear matter explored in deep inelastic scattering experiments. However, despite important developments in the last years, a description of the real-time evolution of QCD jets inside a medium is still far from being complete. In our previous work, we have explored quantum technologies as a promising alternative theoretical laboratory to simulate jet evolution in QCD matter, to overcome inherent technical difficulties in present calculations. Here, we extend our previous investigation from the single particle $|q⟩$ to the $|q⟩+|qg⟩$ Fock space, taking into account gluon production. Based on the light-front Hamiltonian formalism, we construct a digital quantum circuit that tracks the evolution of a multiparticle jet probe in the presence of a medium described as a stochastic color field. Studying the momentum broadening of the jet state, we observe sizable sub-eikonal effects by comparing to eikonal estimates. We also study the medium-induced modifications to the gluon emission probability, which exhibit small corrections compared to the vacuum splitting function. In addition, we study the time evolution of the von-Neumann entropy associated with the quark component; we find that the exponential of the entropy grows linearly in time for the bare quark but superlinearly when taking into account gluon emission.

The deeply inelastic scattering is one of the most important processes in studying the nucleon structure. Theoretical calculations for both the inclusive one and the semi-inclusive one are generally carried out in the virtual photon-nucleon collinear frame in which the virtual photon does not have the transverse components. Expressions in this frame are written in relatively simple forms. Nevertheless, it is also meaningful to calculate the scattering process in the electron-nucleon collinear frame where new measurement schemes are obtained. In the present paper, we reconsider the semi-inclusive deeply inelastic scattering process in the electron-nucleon collinear frame and present the results of azimuthal asymmetries and quark intrinsic asymmetries. We find that the differential cross sections in these two frames are the same at a leading twist level but different at a higher twist level. Azimuthal asymmetries and intrinsic asymmetries in these two frames have the same forms but different kinematic factors. For the sake of completeness, both the electromagnetic and the weak interactions are considered in our calculations. The neutral current measurements in the scattering process could be used as electroweak precision tests that can provide new accurate determinations of the electroweak couplings.