Solutions with anti-D3 branes in a Klebanov-Strassler geometry with positive charge dissolved in fluxes have a certain singularity corresponding to a diverging energy density of the Ramond-Ramond and Neveu-Schwarz–Neveu-Schwarz three-form fluxes. There are many hopes and arguments for and against this singularity, and we attempt to settle the issue by examining whether this singularity can be cloaked by a regular event horizon. This is equivalent to the existence of asymptotically Klebanov-Tseytlin or Klebanov-Strassler black holes whose charge measured at the horizon has the opposite sign to the asymptotic charge. We find that no such Klebanov-Tseytlin solution exists. Furthermore, for a large class of Klebanov-Strassler black holes we considered, the charge at the horizon must also have the same sign as the asymptotic charge and is completely determined by the temperature, the number of fractional branes and the gaugino masses of the dual gauge theory. Our result suggests that antibrane singularities in backgrounds with charge in the fluxes are unphysical, which in turn raises the question as to whether antibranes can be used to uplift anti–de Sitter vacua to deSitter ones. Our results also point to a possible instability mechanism for the antibranes.

The observation of gravitational waves with a global network of interferometric detectors such as advanced LIGO, advanced Virgo, and KAGRA will make it possible to probe into the nature of space-time structure. Besides Einstein’s general theory of relativity, there are several theories of gravitation that passed experimental tests so far. The gravitational-wave observation provides a new experimental test of alternative theories of gravity because a gravitational wave may have at most six independent modes of polarization whose properties and number of modes are dependent on theories of gravity. This paper develops a method to reconstruct an arbitrary number of modes of polarization in time-series data of an advanced detector network. The method does not rely on any specific model, which gives a model-independent test of alternative theories of gravity.

We calculate the axial current decay constants of taste non-Goldstone pions and kaons in staggered chiral perturbation theory through next-to-leading order. The results are a simple generalization of the results for the taste Goldstone case. New low-energy couplings are limited to analytic corrections that vanish in the continuum limit; certain coefficients of the chiral logarithms are modified, but they contain no new couplings. We report results for quenched, fully dynamical, and partially quenched cases of interest in the chiral SU(3) and SU(2) theories.

We study a chiral Lagrangian that describes the two- and three-body decays of a pseudoscalar glueball into scalar and pseudoscalar mesons. The various branching ratios are a parameter-free prediction of our approach. We compute the decay channels for a pseudoscalar glueball with a mass of 2.6 GeV, as predicted by lattice QCD in the quenched approximation, which is in the reach of the PANDA experiment at the upcoming Facility for Antiproton and Ion Research. For completeness, we also repeat the calculation for a glueball mass of 2.37 GeV that corresponds to the mass of the resonance $X(2370)$ measured in the BESIII experiment.

Ultraluminous infrared galaxies (ULIRGs) are the most luminous and intense starburst galaxies in the Universe. Both their star formation rates and their gas surface mass densities are very high, implying a high supernova rate and an efficient energy conversion of energetic protons. A small fraction of these supernovae are the so-called hypernovae, with a typical kinetic energy $\sim {10}^{52}\mathrm{erg}$ and a shock velocity $\ge {10}^9\mathrm{cm}{\mathrm{s}}^{-1}$. The strong shocks driven by hypernovae are able to accelerate cosmic ray protons up to ${10}^{17}\mathrm{eV}$. These energetic protons lose a good fraction of their energy through proton-proton collision when ejected into very dense interstellar media, and as a result, produce high-energy neutrinos ($\le 5\mathrm{PeV}$). Recent deep infrared surveys provide solid constraints on the number density of ULIRGs across a wide redshift range $0\le z\le 2.3$, allowing us to derive the flux of diffuse neutrinos from hypernovae. We find that at PeV energies, the diffuse neutrinos contributed by ULIRGs are comparable to atmosphere neutrinos with the flux of $2\times {10}^{-9}\mathrm{GeV}{\mathrm{cm}}^{-2}{\mathrm{s}}^{-1}{\mathrm{sr}}^{-1}$ by assuming the injected cosmic ray spectrum to be $d{N}_{\mathrm{p}}^{\prime }/d{\epsilon }_{\mathrm{p}}^{\prime }\propto {\epsilon }_{\mathrm{p}}^{\prime -2}$.

The charged Higgs boson is quite common in many new physics models. In this study we examine the potential of observing a heavy charged Higgs boson in its decay mode of top quark and bottom quark in the type-II two-Higgs-doublet model. In this model, the chirality structure of the coupling of a charged Higgs boson to the top and bottom quark is very sensitive to the value of $\tan \beta$. As the polarization of the top quark can be measured experimentally from the top-quark decay products, one could make use of the top-quark polarization to determine the value of $\tan \beta$. We perform a detailed analysis of measuring top-quark polarization in the production channels $gb\to t{H}^{-}$ and $g\overline{b}\to \overline{t}{H}^{+}$. We calculate the helicity amplitudes of the charged Higgs boson production and decay. Our calculation shows that the top quark from the charged Higgs boson decay provides a good probe for measuring $\tan \beta$, especially for the intermediate $\tan \beta$ region. On the contrary, the top quark produced in association with the charged Higgs boson cannot be used to measure $\tan \beta$ because its polarization is highly contaminated by the $t$-channel kinematics.

The diffractive photon production at large momentum transfer and large energies is a probe of the parton dynamics of the diffractive exchange. In this paper we revisit the leading order Balitsky-Fadin-Kuraev-Lipatov equation approach for this process and estimate, for the first time, the differential and total cross sections considering the next-to-leading order corrections for the Balitsky-Fadin-Kuraev-Lipatov characteristic function. We obtain a reasonable agreement with the DESY-HERA data.

In the present work, we apply the one-boson-exchange potential model to investigate the possibility of $Y(2175)$ and $\eta (2225)$ as bound states of $\Lambda \overline{\Lambda }({}^{3}S_1)$ and $\Lambda \overline{\Lambda }({}^{1}S_0)$, respectively. We consider the effective potential from the pseudoscalar $\eta$ exchange and ${\eta }^{\prime }$ exchange, the scalar $\sigma$ exchange, and the vector $\omega$ exchange and $\varphi$ exchange. The $\eta$- and ${\eta }^{\prime }$-meson-exchange potential is a repulsive force for the state ${}^{1}S_0$ and attractive for ${}^{3}S_1$. The results depend very sensitively on the cutoff parameter of the $\omega$ exchange (${\Lambda }_{\omega }$) and least sensitively on that of the $\varphi$ exchange (${\Lambda }_{\varphi }$). Our result suggests the possible interpretation of $Y(2175)$ and $\eta (2225)$ as the bound states of $\Lambda \overline{\Lambda }({}^{3}S_1)$ and $\Lambda \overline{\Lambda }({}^{1}S_0)$, respectively.

As is well known, both Weyl and Weitzenböck spacetimes were initially used as attempts to geometrize the electromagnetic field. In this paper, we prove that this field can also be regarded as a geometrical quantity in an extended version of the Weitzenböck spacetime. The new geometry encompasses features of both Weyl and Weitzenböck spacetimes. In addition, we obtain Einstein’s field equations coupled to the Maxwell energy-momentum tensor from a purely geometrical action and, to exemplify the advantage of using this new geometry when dealing with conformal invariance, we construct a model that is equivalent to a known conformal-invariant teleparallel model.

We construct traversable thin-shell wormholes in the Dvali-Gabadadze-Porrati theory with cylindrical symmetry applying the cut and paste procedure to a flat black string solution of the five-dimensional vacuum Einstein field equations. In contrast to general relativity case, where thin-shell wormholes violate both weak and null energy conditions, we show that static wormholes are supported by normal matter while vacuum wormholes do not exist.

Large-$N_c$ QCD matter at intermediate baryon density and low temperatures has been conjectured to be in the so-called quarkyonic phase, i.e., to have a quark Fermi surface and on top of it a confined spectrum of excitations. It has been suggested that the presence of the quark Fermi surface leads to a homogeneous phase with restored chiral symmetry, which is unstable towards creating condensates that break both the chiral and translational symmetry. Motivated by these exotic features, we investigate properties of cold baryonic matter in the single-flavor Sakai-Sugimoto model, searching for a holographic realization of the quarkyonic phase. We use a simplified mean-field description and focus on the regime of parametrically large baryon densities, of the order of the square of the ’t Hooft coupling, as they turn out to lead to new physical effects similar to the ones occurring in the quarkyonic phase. One effect—the appearance of a particular marginally stable mode breaking translational invariance and linked with the presence of the Chern-Simons term in the flavor-brane Lagrangian—is known to occur in the deconfined phase of the Sakai-Sugimoto model, but turns out to be absent here. The other, completely new phenomenon that we, preliminarily, study using strong simplifying assumptions are density-enhanced interactions of the flavor-brane gauge field with holographically represented baryons. These seem to significantly affect the spectrum of vector and axial mesons and might lead to approximate chiral symmetry restoration in the lowest part of the spectrum, where the mesons start to qualitatively behave like collective excitations of the dense baryonic medium. We discuss the relevance of these effects for holographic searches of the quarkyonic phase and conclude with a discussion of various subtleties involved in constructing a mean-field holographic description of a dense baryonic medium.

The description of the Casimir effect via the conventional light front frame gives the result that no finite Casimir energy density exists when the boundary conditions are related to the unphysical situation where the boundaries move at the speed of light. In the present paper, we investigate if the consideration of the oblique light front coordinates, more convenient for studies in thermal light front quantum field theories, can also be used to describe in a physically consistent manner the Casimir effect in the light front dynamics. Using these coordinates, we show that the correct prescription in the light front formalism to recover the standard Casimir effect involves two aspects: the presence of boundaries that are not at the speed of light and that impose conditions to the field taken at the same Minkowski time.

We develop a relativistic lattice Boltzmann (LB) model, providing a more accurate description of dissipative phenomena in relativistic hydrodynamics than previously available with existing LB schemes. The procedure applies to the ultrarelativistic regime, in which the kinetic energy (temperature) far exceeds the rest mass energy, although the extension to massive particles and/or low temperatures is conceptually straightforward. In order to improve the description of dissipative effects, the Maxwell-Jüttner distribution is expanded in a basis of orthonormal polynomials, so as to correctly recover the third-order moment of the distribution function. In addition, a time dilatation is also applied, in order to preserve the compatibility of the scheme with a Cartesian cubic lattice. To the purpose of comparing the present LB model with previous ones, the time transformation is also applied to a lattice model which recovers terms up to second order, namely up to the energy-momentum tensor. The approach is validated through quantitative comparison between the second- and third-order schemes with Boltzmann approach multiparton scattering (the solution of the full relativistic Boltzmann equation) for moderately high viscosity and velocities, and also with previous LB models in the literature. Excellent agreement with BAMPS and more accurate results than previous relativistic lattice Boltzmann models are reported.

The Wigner function, which provides a phase-space description of quantum systems, has various applications in quantum mechanics, quantum kinetic theory, quantum optics, radiation transport and others. The concept of the Wigner function has been extended to quantum fields, scalar and electromagnetic. Then, one deals with the Wigner functional which gives a distribution of field and its conjugate momentum. We introduce here the Wigner functional of fermionic fields of the values in a Grassmann algebra. Properties of the functional are discussed and its equation of motion, which is of the Liouville form, is derived.

The addition of certain nonrenormalizable terms to the usual action density of a free scalar field leads to nonrenormalizable theories whose exact Euclidian and Minkowskian Green’s functions are less singular than those of the free theory. In some cases, they are finite. One may use lattice methods to extract physical information from these less singular, nonrenormalizable theories.

We present the theory of a supersymmetric ghost condensate coupled to $N=1$ supergravity. This is accomplished using a general formalism for constructing locally supersymmetric higher-derivative chiral superfield actions. The theory admits a ghost condensate vacuum in de Sitter spacetime. Expanded around this vacuum, the scalar sector of the theory is shown to be ghost-free with no spatial gradient instabilities. By direct calculation, the fermion sector is found to consist of a massless chiral fermion and a massless gravitino. By analyzing the supersymmetry transformations, we find that the chiral fermion transforms inhomogeneously, indicating that the ghost condensate vacuum spontaneously breaks local supersymmetry with this field as the Goldstone fermion. Although potentially able to get a mass through the super-Higgs effect, the vanishing superpotential in the ghost condensate theory renders the gravitino massless. Thus local supersymmetry is broken without the super-Higgs effect taking place. This is in agreement with, and gives an explanation for, the direct calculation.

We present analytical solutions of Maxwell’s equations around a rotating non-Kerr black hole immersed in an external uniform magnetic field. The influence of a magnetic field on the effective potential of the radial motion of a charged test particle around a rotating non-Kerr black hole immersed in an external magnetic field are investigated by using the Hamilton-Jacobi equation of motion. The dependence of the minimal radius of the circular orbits $r_{\mathrm{mc}}$ and the radius of the innermost stable circular orbits (ISCOs) from the deformation and the magnetic parameters for the motion of charged particles around a rotating non-Kerr black hole are also presented. An increase of the magnetic field decreases the ISCO radius, while the negative deformation parameter may lead to a larger ISCO radius. A comparison of the numerical results of ISCOs around a non-Kerr black hole with the observational data for the ISCO radius of rapidly rotating black holes [R. Shafee et al., Astrophys. J. 636, L113 (2006)] provides the upper limit for the deformation parameter as $ϵ\le 22$.

We study circular shells in a ($2+1$)-dimensional background within the framework of Einstein-Born-Infeld theory. For shells around black holes we analyze the mechanical stability under perturbations preserving the symmetry. Shells around vacuum are also discussed. We find a large range in the values of the parameters compatible with stable configurations.

Massive spectroscopic surveys will measure the redshift space distortion (RSD) induced by galaxy peculiar velocity to unprecedented accuracy and open a new era of precision RSD cosmology. We develop a new method to improve the RSD modeling and to carry out robust reconstruction of the 3D large scale peculiar velocity through galaxy redshift surveys, in light of RSD. (1) We propose a mathematically unique and physically motivated decomposition of peculiar velocity into three eigencomponents: an irrotational component completely correlated with the underlying density field (${\mathbf{v}}_{\delta }$), an irrotational component uncorrelated with the density field (${\mathbf{v}}_S$), and a rotational (curl) component (${\mathbf{v}}_B$). The three components have different origins, different scale dependences, and different impacts on RSD. (2) This decomposition has the potential to simplify and improve the RSD modeling. (i) ${\mathbf{v}}_B$ damps the redshift space clustering. (ii) ${\mathbf{v}}_S$ causes both damping and enhancement to the redshift space power spectrum $P^s(k,u)$. Nevertheless, the leading order contribution to the enhancement has a $u^4$ directional dependence, distinctively different from the Kaiser formula. Here, $u\equiv k_z/k$, $k$ is the amplitude of the wave vector, and $k_z$ is the component along the line of sight. (iii) ${\mathbf{v}}_{\delta }$ is of the greatest importance for the RSD cosmology. We find that the induced redshift clustering shows a number of important deviations from the usual Kaiser formula. Even in the limit of ${\mathbf{v}}_S\to 0$ and ${\mathbf{v}}_B\to 0$, the leading order contribution $\propto (1+f\tilde{W}(k)u^2{)}^2$. It differs from the Kaiser formula by a window function $\tilde{W}(k)$. Nonlinear evolution generically drives $\tilde{W}(k)\le 1$. We hence identify a significant systematical error causing underestimation of the structure growth parameter $f$ by as much as $O(10\%)$ even at a relatively large scale $k=0.1h/\mathrm{Mpc}$. (iv) The velocity decomposition reveals the three origins of the “finger-of-God” (FOG) effect and suggests how to simplify and improve the modeling of FOG by treating the three components separately. (v) We derive a new formula for the redshift space power spectrum. Under the velocity decomposition scheme, all high order Gaussian corrections and non-Gaussian corrections of order ${\delta }^3$ can be taken into account without introducing extra model uncertainties. Here $\delta$ is the nonlinear overdensity. (3) The velocity decomposition clarifies issues in peculiar velocity reconstruction through 3D galaxy distribution. We discuss two possible ways to carry out the 3D ${\mathbf{v}}_{\delta }$ reconstruction. Both use the otherwise troublesome RSD in velocity reconstruction as a valuable source of information. Both have the advantage of rendering the reconstruction of a stochastic 3D field into the reconstruction of a deterministic window function $W^s(k,u)$ of limited degrees of freedom. Both can automatically and significantly alleviate the galaxy bias problem and, in the limit of a deterministic galaxy bias, completely overcome it. Part 1 of this series of works lays out the methodology. Companion papers Y. Zheng et al. (in preparation). will extensively evaluate its performance against N-body simulations.

In massive gravity, galileon, and braneworld explanations of cosmic acceleration, force modifications are screened by nonlinear derivative self-interactions of the scalar field mediating that force. Interactions between the field of a central body (“$A$”) and an orbiting body (“$B$”) imply that body $B$ does not move as a test body in the field of body $A$ if the orbit is smaller than the Vainshtein radius of body $B$. We find through numerical solutions of the joint field at the position of $B$ that the $A$-field Laplacian is nearly perfectly screened by the $B$ self-field, whereas first derivative or net forces are reduced in a manner that scales with the mass ratio of the bodies as $(M_B/M_A{)}^{3/5}$. The latter causes mass-dependent reductions in the universal perihelion precession rate due to the fifth force, with deviations for the Earth-Moon system at the $\sim 4\%$ level. In spite of universal coupling, which preserves the microscopic equivalence principle, the motion of macroscopic screened bodies depends on their mass providing in principle a means for testing the Vainshtein mechanism.