We consider the redshift drift and position drift associated with astrophysical sources in a formalism that is suitable for describing emitters and observers of light in an arbitrary spacetime geometry, while identifying emitters of a given null-geodesic bundle that arrives at the observer worldline. We then restrict the situation to the special case of a Lemaître-Tolman-Bondi (LTB) geometrical structure and solve for light rays propagating through the structure with arbitrary impact parameters, i.e., with arbitrary angles of entry into the LTB structure. The redshift drift signal emitted by comoving sources and viewed by a comoving observer turns out to be dominated by Ricci curvature and electric Weyl curvature contributions as integrated along the connecting light ray. This property simplifies the computations of the redshift drift signal tremendously, and we expect that the property extends to more complicated models including Swiss-cheese models. When considering several null rays with random impact parameters, the mean redshift drift signal is well approximated by a single Ricci focusing term. This suggests that the measurement of cosmological redshift drift can be used as a direct probe of the strong energy condition in a realistic universe where photons pass through many successive structures.

We study the impact of a binary companion on black hole superradiance at orbital frequencies away from the resonance bands of the superradiant cloud. A superradiant state can couple to a strongly absorptive state via the tidal perturbation of the companion, thereby acquiring a suppressed superradiance rate. Below a critical binary separation, this superradiance rate becomes negative, and the boson cloud gets absorbed by the black hole. This critical binary separation leads to tight constraints on the resonant transitions of the cloud. Especially, a companion with mass ratio $q>{10}^{-3}$ invalidates all fine structure transitions, as well as almost all Bohr transitions except those starting from the $|{\psi }_{211}⟩$ state. Meanwhile, the backreaction on the companion manifests itself as a torque acting on the binary, producing floating/sinking orbits that can be verified via pulsar timing. In addition, the possible termination of cloud growth may help to alleviate the current bounds on the ultralight boson mass from various null detections.

Many alternative theories of gravity screen a Yukawa-type potential. This article shows Keplerian-type parametrization for the solution of Yukawa type potential accurate equations of motion for two nonspinning compact objects moving in an eccentric orbit, using the mean anomaly. From the analytical solution some of the post-Keplerian parameters are derived. Consequently, a bound from the Solar System is presented.

We present for the first time Next-to-Leading (NLO) QCD renormalization group (RG) evolution matrices for nonleptonic $\mathrm{\Delta }F=2$ transitions in the Standard Model effective field theory (SMEFT). To this end we transform first the known two-loop QCD anomalous dimension matrices (ADMs) of the BSM (Beyond the SM) operators in the so-called Buras Misiak Urban basis into the ones in the common weak effective theory (WET) basis (the so-called Jenkins Manohar Stoffer basis) for which tree-level and one-loop matching to the SMEFT are already known. This subsequently allows us to find the two-loop QCD ADMs for the SMEFT nonleptonic $\mathrm{\Delta }F=2$ operators in the Warsaw basis. Having all these ingredients we investigate the impact of these NLO QCD effects on the QCD RG evolution of SMEFT Wilson coefficients for nonleptonic $\mathrm{\Delta }F=2$ transitions from the new physics scale $\mathrm{\Lambda }$ down to the electroweak scale ${\mu }_{\mathrm{ew}}$. The main benefit of these new contributions is that they allow one to remove renormalization scheme dependences present in the one-loop matchings both between the WET and SMEFT and also between SMEFT and a chosen UV completion. But the Next-to-Leading (NLO) QCD effects, calculated here in the Naive dimensional regularisation minimal subtraction scheme, turn out to be small, in the ballpark of a few percent but larger than one-loop Yukawa top effects when only the $\mathrm{\Delta }F=2$ operators are considered. The more complicated class of nonleptonic $\mathrm{\Delta }F=1$ decays will be presented soon in another publication.

The recent measurement of the $W$ boson mass by the CDF collaboration adds an anomaly to the longstanding discrepancy in the muon anomalous magnetic moment, $\mathrm{\Delta }{a}_{\mu }$. Although type-X in the two-Higgs-doublet model provides an attractive solution to $\mathrm{\Delta }{a}_{\mu }$ through a light pseudoscalar $A$, the model confronts the exotic Higgs decays of $h\to AA$ and the lepton flavor universality data in the $\tau$ and $Z$ decays. To save the model, we propose that the light pseudoscalar be Higgs-phobic. Through the random scanning over the entire parameter space, we perform a comparative study of the Higgs-phobic type-X with and without the CDF $m_W$ measurement, called the CDF and PDG cases, respectively. Both cases can explain the two anomalies as well as all the other constraints, but have significant differences in the finally allowed parameter space. For example, a small region with almost degenerate masses of new Higgs bosons around 100 GeV is allowed only in the PDG case. The cutoff scale of the model is also studied via the analysis of renormalization group equations, which reaches up to ${10}^5\mathrm{GeV}$ (${10}^7\mathrm{GeV}$) in the CDF (PDG) case. Since the dominant decay modes are $A\to \tau \tau$, $H\to ZA$, and $H^{\pm }\to W^{\pm }A$ in most of the viable parameter space, we propose the $4\tau +V{V}^{\prime }$ states as the golden discovery channel at the LHC.

We study a scenario to derive four-dimensional modular flavor symmetric models from a higher-dimensional theory by assuming the compactification consistent with the modular symmetry. In our scenario, wave functions in extra-dimensional compact space are modular forms. That leads to constraints on combinations between modular weights and ${\mathrm{\Gamma }}_N$ (${\mathrm{\Gamma }}_N^{\prime }$) representations of matter fields. We also present illustrating examples.

Smearing the bare quantum fields in lattice calculations before applying composite hadron creation operators has a long record of substantially improving overlaps onto low-lying energy eigenstates. A technique called distillation which defines smearing for quark fields as a low-rank linear projection operator into a small vector space of smooth gauge-covariant fields has proven to be both effective and versatile in hadron spectroscopy calculations albeit with significant computational cost. In this paper, more general operators in this space of smooth fields are introduced and optimized, which enhances the performance of the method when tested on systems of heavy quark-antiquark pairs close to the charmonium energy scale.

In this paper, we carry out the next-to-leading-order QCD corrections to $Z\to {\eta }_Q+g+g(Q=c,b)$ (labeled as $gg$) through the color-singlet (CS) state of $Q\overline{Q}[{{}^{1}S}_0^{[1]}]$, with the aim of assessing the impact of this process on $Z$ bosons decaying into inclusive ${\eta }_Q$. We find that the QCD corrections to the $gg$ process can notably enhance its leading-order results, especially for the ${\eta }_c$ case, which would then greatly increase the existing predictions of ${\mathrm{\Gamma }}_{Z\to {\eta }_Q+X}$ given by the CS-dominant process $Z\to {\eta }_Q[{{}^{1}S}_0^{[1]}]+Q+\overline{Q}$. Moreover, with these significant QCD corrections, the $gg$ process would exert crucial influence on the CS-predicted ${\eta }_Q$ energy distributions. In conclusion, in the CS studies of $Z\to {\eta }_Q+X$, besides $Z\to {\eta }_Q[{{}^{1}S}_0^{[1]}]+Q+\overline{Q}$, $Z\to {\eta }_Q[{{}^{1}S}_0^{[1]}]+g+g$ can provide phenomenologically indispensable contributions as well.

The forward-backward charge asymmetry ($A_{\mathrm{FB}}$) at hadron colliders is sensitive to both the electroweak (EW) symmetry breaking represented by the effective weak mixing angle ${\sin }^2{\theta }_{\mathrm{eff}}^{\ell }$, and the proton structure information in the initial state modeled by the parton distribution functions (PDFs). Due to their strong correlation, the precisions of determination on ${\sin }^2{\theta }_{\mathrm{eff}}^{\ell }$ and PDFs using the measured $A_{\mathrm{FB}}$ spectrum are limited. In this paper, we define a set of structure parameters which factorize the unique proton information of the relative difference between quarks and antiquarks in the $A_{\mathrm{FB}}$ observation. Other than the conventional way of extracting ${\sin }^2{\theta }_{\mathrm{eff}}^{\ell }$ from the convolution of PDF and EW calculations, we propose a new method to simultaneously determine the value of ${\sin }^2{\theta }_{\mathrm{eff}}^{\ell }$ and the proton structure terms by fitting to the observed $A_{\mathrm{FB}}$ distribution, and point out the necessity of specifying additional observations to further reduce the uncertainties on the proton structure terms, respectively, so that model-independent high precision ${\sin }^2{\theta }_{\mathrm{eff}}^{\ell }$ and proton structure measurements can be achieved at the future LHC experiments.

By analyzing an electron-positron collision data sample corresponding to an integrated luminosity of $2.93{\mathrm{fb}}^{-1}$ taken at the center-of-mass energy of 3.773 GeV with the BESIII detector, we obtain for the first time the absolute branching fractions for seven $D^0$ and $D^{+}$ hadronic decay modes and search for the hadronic decay $D^0\to K_S^0{K}_S^0{\pi }^0$ with much improved sensitivity. The results are $\mathcal{B}(D^0\to K_S^0{\pi }^0{\pi }^0{\pi }^0)=(7.64\pm 0.30\pm 0.29)\times {10}^{-3}$, $\mathcal{B}(D^0\to K^{-}{\pi }^{+}{\pi }^0{\pi }^0{\pi }^0)=(9.54\pm 0.30\pm 0.31)\times {10}^{-3}$, $\mathcal{B}(D^0\to K_S^0{\pi }^{+}{\pi }^{-}{\pi }^0{\pi }^0)=(12.66\pm 0.45\pm 0.43)\times {10}^{-3}$, $\mathcal{B}(D^{+}\to K_S^0{\pi }^{+}{\pi }^0{\pi }^0)=(29.04\pm 0.62\pm 0.87)\times {10}^{-3}$, $\mathcal{B}(D^{+}\to K_S^0{\pi }^{+}{\pi }^{+}{\pi }^{-}{\pi }^0)=(15.28\pm 0.57\pm 0.60)\times {10}^{-3}$, $\mathcal{B}(D^{+}\to K_S^0{\pi }^{+}{\pi }^0{\pi }^0{\pi }^0)=(5.54\pm 0.44\pm 0.32)\times {10}^{-3}$, $\mathcal{B}(D^{+}\to K^{-}{\pi }^{+}{\pi }^{+}{\pi }^0{\pi }^0)=(4.95\pm 0.26\pm 0.19)\times {10}^{-3}$, and $\mathcal{B}(D^0\to K_S^0{K}_S^0{\pi }^0)<1.45\times {10}^{-4}$ at the 90% confidence level. Here, the first uncertainties are statistical, and the second ones are systematic. The newly studied decays greatly enrich the knowledge of the $D\to \overline{K}\pi \pi \pi$ and $D\to \overline{K}\pi \pi \pi \pi$ hadronic decays and open a bridge to access more two-body hadronic $D$ decays containing scalar, vector, axial, and tensor mesons in the charm sector.

The $\mathrm{MINER}\nu \mathrm{A}$ experiment reports double-differential cross-section measurements for ${\nu }_{\mu }$-carbon interactions with three-momentum transfer $|\overrightarrow{q}|<1.2\mathrm{GeV}$ obtained with medium energy exposures in the NuMI beam. These measurements are performed as a function of the three-momentum transfer and an energy transfer estimator called the available energy defined as the energy that would be visible in the detector. The double-differential cross sections are compared to the genie and nuwro predictions along with the modified version of genie which incorporates new models for better agreement with earlier measurements from $\mathrm{MINER}\nu \mathrm{A}$. In these measurements, the quasielastic, resonance, and multinucleon knockout processes appear at different kinematics in this two-dimensional space. The results can be used to improve models for neutrino interactions needed by neutrino oscillation experiments.

We consider the $\varrho$-Minkowski spacetime, a model with linear noncommutativity involving the time and azimuthal angle. We study its quantum symmetries, the $\varrho$-Poincaré quantum group, and analyze the concepts of localizability and quantum observers.

The gravitational chiral quantum anomaly is calculated in the framework of the extended Rarita-Schwinger-Adler (RSA) field theory, which includes the interaction with an additional spin $1/2$ field. It is shown that the factor in the gravitational chiral anomaly normalized to the Dirac field anomaly is equal to $-19$. The resulting value distinguishes the RSA theory from the other theories of spin $3/2$. A direct verification of the conformality of the RSA theory in the strong interaction limit at the level of one-loop three-point graphs is made.

We construct exact solutions of magnetically charged black holes in the vector-tensor Horndeski gravity and discuss their main features. Unlike the analogous electric case, the field equations are linear in a simple (quite standard) parametrization of the metric tensor, and they can be solved analytically even when a cosmological constant is added. The solutions are presented in terms of hypergeometric functions, which makes the analysis of the black hole properties relatively straightforward. Some of the aspects of these black holes are quite ordinary, like the existence of extremal configurations with maximal magnetic charge for a given mass or the existence of a mass with maximal temperature for a given charge, but others are somewhat unexpected, like the existence of black holes with a repulsive gravitational field. We perform our analysis for both signs of the nonminimal coupling constant and find black hole solutions in both cases but with significant differences between them. The most prominent difference is the fact that the black holes for the negative coupling constant have a spherical surface of curvature singularity rather than a single point. On the other hand, the gravitational field produced around this kind of black holes is always attractive. Also, for small enough magnetic charge and negative coupling constant, extremal black holes do not exist, and all magnetic black holes have a single horizon. In addition, we study the trajectories around these magnetic black holes for light as well as massive particles either neutral or electrically charged. Finally, we compare the main features of these black holes with their electric counterparts, adding some aspects that have not been discussed before, like temperature, particle trajectories, and light deflection by electrically charged Horndesky black holes.

In this paper the motion of charged and uncharged test particles in the rotating nonlinearly charged black hole (BH) is examined. Its asymptotics can be de Sitter or anti–de Sitter, depending on the value of the nonlinear parameter; consequently this BH can present one, two or three horizons, the third one being the cosmological horizon in the de Sitter case. Angular and radial test particle motions are analyzed and compared with its linear electromagnetic counterpart, the Kerr-Newman black hole (KN-BH). Several differences arise with the KN-BH, namely, the equatorial asymmetry is enhanced by the nonlinear electrodynamics field and for charged particles the access to one of the poles is forbidden; besides, a second circular orbit in the neighborhood of the external horizon appears, and the presence of the nonlinear electromagnetic field increases the curvature producing bounded orbits closer to the horizon.

We present a unified description of the matter and dark energy epochs using a class of scalar-torsion theories. We provide a Hamiltonian description, and by applying Noether’s theorem and requiring the field equations to admit linear-in-momentum conservation laws, we obtain two specific classes of scalar-field potentials. First, we extract analytic solutions and perform a detailed dynamical analysis. We show that the system possesses critical points that correspond to scaling solutions in which the effective, total equation-of-state parameter is close to zero and points in which it is equal to the value $-1$; the equation of state of the cosmological constant. Therefore, during evolution, the Universe remains for sufficiently long at the epoch corresponding to dust-matter domination, while at later times it enters the accelerated epoch and eventually results in the de Sitter phase. Finally, in contrast to other unified scenarios, such as Chaplygin gas-based models and Horndeski-based constructions, the present scenario is free from instabilities and pathologies at the perturbative level.

Derrick-type virial identities, obtained via dilatation (scaling) arguments, have a variety of applications in field theories. We deconstruct such virial identities in relativistic gravity showing how they can be recast as self-evident integrals of appropriate combinations of the equations of motion. In spherical symmetry, the appropriate combination and gauge choice guarantee the geometric part can be integrated out to yield a master form of the virial identity as a nontrivial energy-momentum balance condition, valid for both asymptotically flat black holes and self-gravitating solitons, for any matter model. Specifying the matter model we recover previous results obtained via the scaling procedure. We then discuss the more general case of stationary, axisymmetric, asymptotically flat black hole or solitonic solutions in general relativity, for which a master form for their virial identity is proposed, in a specific gauge but regardless of the matter content. In the flat spacetime limit, the master virial identity for both the spherical and axial cases reduces to a balance condition for the principal pressures, discussed by Deser.

We study the evolution of a test scalar field on the background geometry of a regular loop quantum black hole characterized by two loop quantum gravity correction parameters, namely, the polymeric function and the minimum area gap. The calculations of quasinormal frequencies in asymptotically flat spacetime are performed with the help of higher-order Wentzel-Kramers-Brillouin expansion and related Padé approximants, the improved asymptotic iteration method, and time-domain integration. The effects of free parameters of the theory on the quasinormal modes are studied and deviations from those of the Schwarzschild black holes are investigated. We show that the loop quantum gravity correction parameters have opposite effects on the quasinormal frequencies and the loop quantum black holes are dynamically stable.

We investigate the viability of a recently proposed generalization of the Ashtekar-Olmedo-Singh spacetime for the effective description of the interior region of a Schwarzschild black hole within the framework of loop quantum cosmology. The approach is based on a choice of polymerization parameters that is more general than the ones previously considered in the literature and that results in the natural appearance of two times to describe the solutions. If one is interested in examining the physics derived from this model, it is fundamental to ensure that one can attain a well-defined effective geometry in the whole region under consideration, in particular as regards the redundancy of the two times, which one needs to express in terms of a single time coordinate. In order to determine whether this requirement is met, we analyze the definition of these times and their relation. We show that one can reach an acceptable interior spacetime geometry by exploiting the freedom to define the origins of the two times independently.

Fast, highly accurate, and reliable inference of the sky origin of gravitational waves would enable real-time multimessenger astronomy. Current Bayesian inference methodologies, although highly accurate and reliable, are slow. Deep learning models have shown themselves to be accurate and extremely fast for inference tasks on gravitational waves, but their output is inherently questionable due to the blackbox nature of neural networks. In this work, we merge Bayesian inference and deep learning by applying importance sampling on an approximate posterior generated by a multiheaded convolutional neural network. The neural network parametrizes Von Mises-Fisher and Gaussian distributions for the sky coordinates and two masses for given simulated gravitational wave injections in the LIGO and Virgo detectors. We generate skymaps for unseen gravitational-wave events that highly resemble predictions generated using Bayesian inference in a few minutes. Furthermore, we can detect poor predictions from the neural network, and quickly flag them.