We present a Monte Carlo simulation-based partial wave analysis of the decay ${\mathrm{\Xi }}_c^{+}\to {\mathrm{\Xi }}^{-}{\pi }^{+}{\pi }^{+}$ by using the Feynman-Diagram-Calculation framework. The consistency of the input and output parameters implies the reliability of the partial wave analysis method. A robust method of the spin-parity determination of the ${\mathrm{\Xi }}^{*0}$ resonance is introduced. The rejection significance of the alternative spin-parity hypothesis over the favored hypothesis is strong for different spins, but weak for different parities based on the current integrated luminosity of the Belle experiment. Further data collection is needed to improve the sensitivity of parity determination in the future, e.g., Belle II experiment.

To shed light on the properties of states whose nature, internal structure, and spin-parity quantum numbers are not fully elucidated, we systematically study their electromagnetic properties. In light of this concept, we present a comprehensive analysis of the magnetic dipole moment of the $P_{cs}(4459)$ pentaquark within the context of QCD light cone sum rules, utilizing three distinct interpolating currents in the form of diquark-diquark-antiquark configurations that are likely to couple this pentaquark with $J^P={\frac{3}{2}}^{-}$ quantum numbers. The numerical analysis yielded the following results: ${\mu }_{J_{\mu }^1}=-0.60\pm 0.15{\mu }_N$, ${\mu }_{J_{\mu }^2}=1.60\pm 0.30{\mu }_N$, and ${\mu }_{J_{\mu }^3}=0.99\pm 0.20{\mu }_N$. The numerical results obtained have led to the conclusion that the magnetic dipole moments of the $P_{cs}(4459)$ state are capable of projecting its inner structure. As is seen, the different diquark-diquark-antiquark configurations of the $P_{cs}(4459)$ pentaquark state contain important information about its internal structure. Thus, this study will provide prominent data to investigate the inner structure of the $P_{cs}(4459)$ pentaquark state. We compared our results with other theoretical predictions that could be a useful complementary tool for interpreting the nature of the $P_{cs}(4459)$ state. A thorough examination reveals that the results obtained by employing disparate theoretical approaches and different internal structure models are not consistent with each other. It is recommended that further studies be conducted using alternative nonperturbative techniques to gain a more comprehensive understanding of the observed results.

We study the phenomenological impact of the preequilibrium glasma initial stage of heavy-ion collisions on heavy quark azimuthal correlations and spectra. Using our numerical solver, we simulate the transport of heavy quark test particles in an SU(3) glasma background field. The glasma field equations are formulated using classical real-time lattice gauge theory, and the heavy quark dynamics are described by classical transport equations numerically solved using the colored particle-in-cell method. For the first time, the effect of the glasma stage on the azimuthal correlations of $c\overline{c}$ and $b\overline{b}$ pairs is studied. The resulting azimuthal width ${\sigma }_{\mathrm{\Delta }\varphi }$ exhibits a large and quick decorrelation due to the strong glasma fields. Further, we evaluate how the $p_T$-broadening in the glasma affects heavy quark $p_T$-spectra, which are initialized according to the Fixed-Order Next-to-Leading Logarithm (FONLL) heavy quark production calculation. The nuclear modification factor $R_{AA}$ is extracted for $c$ and $b$ quarks in the glasma and additional nuclear PDF effects accounting for gluon shadowing are included.

The Weyl double copy (WDC) relation connects the Weyl tensor of the gravity theory and the field strength tensor of the Maxwell theory, which provides a concrete realization of the classical double copy. Although intensively investigated, the WDC is only limited in four-dimensional spacetime. In this Letter, we generalize the WDC relation to five-dimensional spacetime, which offers the first example of the WDC in higher dimensions. We show that a special class of five-dimensional type N vacuum solutions admits a special class of degenerate Maxwell field that squares to give the Weyl tensor. The five-dimensional WDC relation defines a scalar field that satisfies the source-free Klein-Gordon equation on the curved background. We further verify that for five-dimensional pp-wave solution and Kundt solutions, the Maxwell fields and the scalar fields also satisfy the Maxwell’s equations and the wave equation on five-dimensional Minkowski spacetime.

We compute the first nontrivial noncommutative correction to the Einstein-Hilbert Lagrangian, which arises from the double copy of noncommutative Yang-Mills theory (ncYM). We start by considering linear and quadratic $\theta$-corrections up to cubic order in fields in ncYM theory and in arbitrary $D$ dimensions. We compute the first nontrivial corrections to the three-points vertex operators and use them to construct a double copy theory of the form ncYM $\times$ ncYM. The resulting theory is given by a double geometrical formalism which includes noncommutative corrections to the perturbative cubic double field theory (DFT) formulation, where the star product of the theory is doubled in agreement with the doubling of the physical coordinates of the theory. Upon solving the level matching condition the noncommutative products are identified and they produced ${\theta }^2$-corrections to the cubic DFT action. We analyze the pure gravitational limit of this formulation considering $D=4$ and imposing the transverse-traceless gauge.

Equilibrium states of $\mathcal{N}=4$ supersymmetric Yang-Mills theory can be characterized by the temperature and three chemical potentials, corresponding to the $\mathrm{U}(1{)}^3$ subgroup of the $R$-symmetry group. We investigate the phase diagram of the theory at strong coupling in the grand canonical ensemble in flat space, using its holographic description via the five-dimensional supergravity solution of Behrndt et al. The bulk action includes the metric, three Abelian gauge fields, and two neutral scalar fields. The equilibrium state described by the charged black brane is always thermodynamically unstable at low temperature. Relativistic hydrodynamics with multiple conserved charges predicts that thermodynamic instability is accompanied by a dynamical instability, with the eigenvalues and eigenvectors of the corresponding Hessian playing a key role in identifying the unstable modes. We explicitly demonstrate this for three equal chemical potentials, finding unstable quasinormal modes that describe $R$-charge diffusion. Consequently, the low-temperature phase of $\mathcal{N}=4$ supersymmetric Yang-Mills theory with equal chemical potentials is not described by the AdS-Reissner-Nordström black brane.

It is well-established that compactifying type I string theory on a circle $S^{(1)}$ transforms the theory under T-duality into type I’ theory; the compactification of type IIA string theory on the orbifold ${\tilde{S}}^{(1)}/{\mathbb{Z}}_2$, where the ${\mathbb{Z}}_2$ action combines world sheet parity with spacetime reflection along the dual circle ${\tilde{S}}^{(1)}$. We propose that, upon compactification, the untwisted (twisted) sector of the type I effective action should map under the Buscher rules to the untwisted (twisted) sector of the type I’ effective action. This T-duality constraint offers significant insight into the determination of bosonic couplings in the effective action of type IIA theories, specifically those that remain after orbifold reduction, as well as in the untwisted sector of the type I effective action. However, its scope is limited and insufficient to fully determine the couplings within the twisted sectors of type I and type I’ theories. Within this framework, we demonstrate that the leading second-order derivative couplings in untwisted sector of type I and the second-order derivative couplings in type IIA theory are uniquely determined, except for the Chern-Simons term in type IIA, which is absent in the orbifold reduction.

The covariant, spin-dependent response tensor for an electric dipole-moment-polarized electron gas (statistical distribution of electrons and positrons) is calculated using the formalism of quantum plasmadynamics. A simultaneous eigenfunction of both the Dirac Hamiltonian and the electric moment spin operator is constructed. Expressions for the electric moment states and the corresponding vertex functions are derived. It is shown that when the distribution of momenta is isotropic, the spin-dependent response of an electric-moment-dependent quantum plasma is identically zero. The response is nonzero in the presence of a streaming motion perpendicular to the axis if the electron and positron distributions are different. The response has the same form as for a plasma with a nonzero, cross field current when $⟨p_i⟩\ne 0$. This quantum relativistic correction is used to identify the dispersion equation for an electric moment spin-polarized plasma with a streaming cold plasma background. In particular, the natural modes of an electric-moment-dependent quantum plasma exhibit elliptical polarization. This is in contrast to a magnetic-moment-dependent electron gas, which is gyrotropic, or a helicity-dependent electron gas, which is optically active. The different responses, due to quantum plasmas being spin-polarized by different relativistically acceptable spin operators, does not appear in other approaches to quantum plasma theory.

We study the effects of massive scalar-tensor theories on the internal properties, crystallization, and cooling process of white dwarf stars that might potentially solve observational tensions. We show that these modified gravity theories alter the inner structure of the star leading to sub-Chandrasekhar mass white dwarfs. This further results in a modification of Debye temperature, ion and electron specific heats. Finally, we find that the cooling process is significantly shortened in scalar-tensor theories leading to reduced cooling ages.

With the updated sensitivity of terrestrial gravitational-wave (GW) detectors in their fourth observing run, we expect a high rate of detection of binary black hole mergers. With this comes the hope that we will detect rarer classes of merger events. Compact binaries formed dynamically in dense stellar environments are likely to be detected with a residual eccentricity as they enter the sensitivity band of ground-based GW detectors. In this paper, we present a time-domain inspiral-merger-ringdowm (IMR) waveform model ESIGMAHM constructed within a framework we named ESIGMA for coalescing binaries of spinning black holes on moderately eccentric orbits [Phys. Rev. D 97, 024031 (2018).]. We now include the effect of black hole spins on the dynamics of eccentric binaries, as well as model sub-dominant waveform harmonics emitted by them. The inspiral evolution is described by a consistent combination of latest results from post-Newtonian theory, self-force, and black hole perturbation theory. We assume that these moderately eccentric binaries radiate away most of their orbital eccentricity before merger, and seamlessly connect the eccentric inspiral with a numerical relativity based surrogate waveform model NRSur7dq4 for mergers of spinning binaries on quasicircular orbits. We present two variants of ESIGMAHM: the inspiral-only version is named InspiralESIGMAHM, while the full IMR one is termed IMRESIGMAHM; or InspiralESIGMA and IMRESIGMA when only dominant modes are used. We validate ESIGMAHM against eccentric numerical relativity simulations, and also against contemporary effective-one-body and phenomenological models in the quasicircular limit. We find that ESIGMAHM achieves match values greater than 99% for quasicircular spin-aligned binaries with mass ratios up to 8, and above 97% for nonspinning and spinning eccentric systems with small or positively aligned spins. Using IMRESIGMA, we quantify the impact of orbital eccentricity on GW signals, showing that next-generation detectors can detect eccentric sources up to 10% louder than quasicircular ones. We also show that current templated LIGO-Virgo-KAGRA searches will lose more than 10% of optimal SNR for about 20% of all eccentric sources by using only quasicircular waveform templates. The same will result in a 25% loss in detection rate for eccentric sources with mass ratios $m_1/m_2\ge 4$. Our results highlight the need for including eccentricity and higher-order modes in GW source models and searches for asymmetric eccentric BBH signals.

We derive the scalar-tensor modification of the gravitational field of an ultrarelativistic particle beam and its effect on a test particle that is used as sensor. To do so, we solve the linearized scalar-tensor gravity field equations sourced by an energy-momentum tensor of a moving point particle. The geodesic equation and the geodesic deviation equation then predict the acceleration of the test particle as well as the momentum transfer due to a passing source. Comparing the momentum transfer predicted by general relativity and scalar tensor gravity, we find that there exists a relevant parameter regime where this difference increases significantly with the velocity of the source particle. Since ultrarelativistic particles are available at accelerators like the Large Hadron Collider, ultraprecise acceleration sensors in the vicinity of the particle beam could potentially detect deviations from general relativity or constrain modified gravity models.

Euclidean anti–de Sitter (AdS) wormholes provide a natural setup for studying the anti–de Sitter/conformal field theory (AdS/CFT) correspondence with multiple boundaries. However, from a bottom-up perspective, they cannot be embedded in the four-dimensional Einstein-AdS-Maxwell theory if these boundaries have positive curvature. Nevertheless, Maldacena and Maoz showed that this obstruction could be circumvented by introducing merons in the four-dimensional Einstein-AdS-Yang-Mills theory. In this work, we show that Euclidean-AdS wormholes also exist in the four-dimensional Einstein-AdS-Skyrme theory, whose matter sector possesses a nontrivial baryonic charge. We compute its free energy and show that it does not depend on the integration constants whatsoever, resembling topological solitons. Additionally, we obtain its holographic stress tensor and show that it vanishes, allowing us to interpret this configuration as a holographic Bogomol’nyi-Prasad-Sommerfield (BPS) state. Other topologically nontrivial ground states in Einstein-Skyrme theory are found, such as gravitational instantons, representing the homotopically inequivalent vacua of the theory. We find that they develop Hawking-Page phase transitions above a critical temperature. Some of these solutions are periodic in Euclidean time, representing the gravitational analog of calorons in Yang-Mills theory.

We present a semiclassical study of the mixmaster cosmology minimally coupled to a massive scalar field in the Hamiltonian formalism, with focus on three distinct scenarios: the classical cosmology coupled to the quantized scalar field and effective cosmology, with spacetime discreteness corrections, coupled to the classical scalar field and to the quantized scalar field. We find several results: (i) the effective cosmology undergoes several small bounces before expanding, with scalar field excitations rising through the bounce; (ii) anisotropies rise and fall as the universe undergoes a bounce, a feature that is enhanced with matter; (iii) Lyapunov exponents reveal that chaos is reduced in the effective systems compared to the classical case.

We study the correlation between a part of the gravitational field at the outer common dynamical horizon in the strong field regime, and the news of the gravitational radiation received from the system in the weak field regime, in the postmerger phase of quasicircular, nonspinning binary black hole mergers using numerical relativity simulations. We find that, as in the inspiral phase [V. Prasad, A. Gupta, S. Bose, B. Krishnan, and E. Schnetter, Phys. Rev. Lett. 125, 121101 (2020).], the shear of the outer common dynamical horizon formed late into the inspiral continues to be well correlated with the news of the outgoing gravitational radiation, even at early times. We show that the shear contains certain quasinormal frequencies, and information about the parameters of the remnant and the parent black holes, lending further concrete evidence to support the dynamical horizon correlation conjecture in all phases of binary black hole mergers.

We investigate cosmological vacuum amplification of gravitational waves in dynamical Chern-Simons gravity. We develop a comprehensive framework to compute graviton production induced by the parity violating Pontryagin coupling and study its imprint on the stochastic gravitational wave background energy power spectrum. We explore gravitational vacuum amplification in four concrete scenarios for the evolution of the Chern-Simons pseudoscalar. We show that a parity-violating contribution dominates over an initially flat spectrum when the velocity of the pseudoscalar quickly interpolates between two asymptotically constant values or when it is nonvanishing and constant through a finite period of time. This is also the case when we parametrize the pseudoscalar evolution by a perfect fluid with radiation- and dustlike equations of state for large enough values of its energy density. The resulting spectra are compared with the sensitivity curves of current and future gravitational wave observational searches.

We use Fisher information theory to forecast the bounds on the finite-size effects of astrophysical compact objects with next-generation gravitational wave detectors, including the ground-based Cosmic Explorer (CE) and Einstein Telescope (ET), as well as the space-based Laser Interferometer Space Antenna (LISA). Exploiting the worldline effective field theory formalism, we first characterize three types of quadrupole finite-size effects: the spin-induced quadrupole moments, the conservative tidal deformations, and the tidal heating. We then derive the corresponding contributions to the gravitational waveform phases for binary compact objects in aligned-spin quasicircular orbits. We separately estimate the constraints on these finite-size effects for black holes using the power spectral densities of the $\mathrm{CE}+\mathrm{ET}$ detector network and LISA observations. For the $\mathrm{CE}+\mathrm{ET}$ network, we find that the bounds on the mass-weighted spin-independent dissipation number ${\mathcal{H}}_0$ are of the order $\mathcal{O}(1)$, while the bounds on the mass-weighted tidal Love number $\tilde{\mathrm{\Lambda }}$ are of the order $\mathcal{O}(10)$. For high-spin binary black holes with dimensionless spin $\chi \simeq 0.8$, the bounds on the symmetric spin-induced quadrupole moment ${\kappa }_s$ are of the order $\mathcal{O}({10}^{-1})$. LISA observations of supermassive black hole mergers offer slightly tighter constraints on all three finite-size parameters. Additionally, we perform a Fisher analysis for a binary neutron star merger within the $\mathrm{CE}+\mathrm{ET}$ network. The bounds on the tidal parameter ${\mathcal{H}}_0$ and on $\tilde{\mathrm{\Lambda }}$ are around 2 orders of magnitude better than the current LIGO-Virgo-KAGRA bounds.

We derive new approximations for quintessence solutions that are simpler and an order of magnitude more accurate than anything available in the literature, which from an observational perspective makes numerical calculations superfluous. For example, our tracking quintessence approximation yields $\sim 0.1\%$ maximum relative errors of $H(z)/H_0$ and ${\mathrm{\Omega }}_{\mathrm{m}}(z)$ for the observationally viable inverse power law scalar field potentials, and similarly for viable thawing quintessence models using two slow-roll parameters. The approximations are trivially computed from the scalar field potential and as an application we give analytic expressions for the Chevallier-Polarski-Linder parameters calculated from an arbitrary scalar field potential for thawing and tracking quintessence models.

The $\mathrm{\Lambda }\mathrm{CDM}$ model has long served as a robust and predictive framework for cosmology, successfully explaining a wide range of observations, including the accelerated expansion of the Universe. However, discrepancies in cosmological parameter estimates and recent findings, such as those from DESI, hint at potential deviations from $\mathrm{\Lambda }\mathrm{CDM}$. Gravitational wave (GW) observations offer an independent method to probe the nature of dark energy, leveraging GWs from compact binary mergers as standard candles. In this study, we demonstrate that the integrated GW memory over cosmological distances encodes a unique imprint of the background spacetime. Unlike previous analyses, our approach captures nonlinear dependencies on cosmological quantities, resulting in an enhancement of the integrated GW memory by a factor of 100 for high-redshift sources which is well within the sensitivity range of next-generation detectors like Cosmic Explorer and the Einstein Telescope. We find that despite the diminishing strength of individual GWs at high redshifts, their cumulative effect leads to a significant amplification, akin to the integrated Sachs-Wolfe effect, offering a potential new avenue for cosmological studies. By examining a range of dark energy models, we reveal that GW memory is potentially highly sensitive to the underlying cosmological framework, making it a promising probe of dark energy. This novel approach presents the possibility of a fresh perspective to address persistent cosmological tensions, and the nature of dark energy.