General Relativity and Gravitation最新文献

We extend well-known results on the Newtonian limit of Lorentzian metrics to orthonormal frames. Concretely, we prove that, given a one-parameter family of Lorentzian metrics that in the Newtonian limit converges to a Galilei structure, any family of orthonormal frames for these metrics converges pointwise to a Galilei frame, assuming that the two obvious necessary conditions are satisfied: the spatial frame must not rotate indefinitely as the limit is approached, and the frame’s boost velocity with respect to some fixed reference observer needs to converge.

This investigation highlights an important application of complete geometric decoupling in constructing anisotropic, compact density-matter stars via a decoupled gravitational framework. In this context, the present study introduces an intriguing synthesis of two independent techniques, density-like constraints and the zero-complexity factor, to simultaneously derive the decoupler functions. By using this innovative relativistic scheme, we gain the ability to analytically control the anisotropies and complexity when modeling the dense-matter compact stars. We show that the complexity-free condition effectively captures the influence of anisotropic pressure inherent in compact dense-matter distributions, arising naturally from the chosen seed metric ansatz. Two distinct and physically viable anisotropic models satisfying all standard stability and energy conditions are obtained through the complete decoupling process. Our findings provide clear theoretical understanding of the coupling between known and standard gravity fields by demonstrating for the first time that the parameter responsible for deformation uniquely governs the direction of energy transfer between the seed sector and the decoupling source.

We investigate the cosmic inflation within a class of the scalar-tensor model with the scalar-dependent non-minimal kinetic couplings. The inflationary dynamical potential will be applied. Using the slow-roll approximation, we compute theoretical predictions for the key observables, like the spectral indexes (n_s), scalar-to-tensor ratio r and the running of the scalar spectral index (alpha _s) in terms of the free parameters of the model. Besides, we find the limitations of these parameters. In addition, these quantities will be compared with the latest observational data from the Planck data. Furthermore, we analyze the sensitivity of r, (n_s) and (alpha _s) in terms of the model’s free parameters.

Non-conservation of dark matter can lead to late-time cosmic acceleration. This mechanism is known as the matter creation theory and this replaces the need of dark energy and modified gravity theories. We consider a two-fluid system consisting of a cold dark matter and a second fluid with constant barotropic equation of state. We performed detailed investigations of such cosmologies using the powerful techniques of qualitative analysis of dynamical systems. Considering a wide variety of the creation rates, we examine the phase space analysis of the individual scenario. According to our analyses, these scenarios predict decelerating unstable dark matter (or second fluid) dominated critical points, accelerating attractors dominated either by dark matter or the second fluid, accelerating scaling attractors in which dark matter and the second fluid co-exist. The regime of late-time accelerating expansion can be classified as either quintessence, phantom or driven by a cosmological constant. This huge variety of critical points makes these scenarios phenomenologically rich, and naturally suggests that such scenarios can be viewed as viable and potential alternatives to the mainstream cosmological models.

We present a new methodology to explore the morphology of the High Frequency Feature (HFF), i.e., the dominant, rising-frequency GW emission from a proto-neutron star in core-collapse supernovae (CCSNe). We used a residual neural network (ResNet50) to perform multi-class classification of image samples constructed from time–frequency Morlet wavelet scalograms. We defined a three-class problem by categorizing the HFF slope as Steep, Moderate, or Low, according to physically informed ranges. The ResNet50 model was optimized with phenomenological waveforms injected into real noise from the LIGO-Virgo O3b observing run and then tested with numerically simulated CCSN waveforms embedded in the same real noise. At galactic distances of 1 kpc and 5 kpc with H1 and L1 data and 1 kpc with V1 data, we obtained highly accurate results (test accuracies from 0.8933 to 0.9867), which show the feasibility of our methodology. For further distances, we observed declines in test accuracy until 0.8000 with H1 and L1 data at 10 kpc and until 0.5933 with V1 data at 10 kpc, which we attribute to limitations in the input datasets. Our methodology is sufficiently general to enable early-stage characterization of the HFF in real interferometric data.

In our previous work [H. Zejli, Int. J. Mod. Phys. D 34, 2550052 (2025), arXiv:2508.00035], we introduced a (mathcal {P}mathcal {T})-symmetric wormhole model based on a bimetric geometry, capable of generating closed timelike curves (CTCs). In this paper, we extend the analysis to the null hypersurface at the throat of this modified Einstein-Rosen bridge, where two regular Eddington-Finkelstein metrics render the geometry traversable. Using the Barrabés-Israël formalism in Poisson’s reformulation, we evaluate the null shell’s surface stress-energy tensor (S^{alpha beta }) from the jump of the transverse curvature, revealing a violation of the null energy condition: a lightlike membrane of exotic matter with negative surface energy density and positive tangential pressure. This exotic fluid acts as a repulsive source stabilizing the throat, ensuring consistency with the Einstein field equations, including conservation laws on the shell. Beyond the local characterization, we outline potential observational signatures: (i) gravitational-wave echoes from the photon-sphere cavity; (ii) horizon-scale imaging with duplicated and through-throat photon rings, and non-Kerr asymmetries; (iii) quantum effects such as (mathcal{P}mathcal{T})-induced frequency pairing with possible QNM doublets and partial suppression of vacuum flux at the throat; and (iv) a relic cosmological population yielding an effective (Lambda _textrm{eff}) and seeding voids. Compared with timelike thin-shell constructions, our approach is based on a null junction interpreted as a lightlike membrane, combined with (mathcal{P}mathcal{T}) symmetry, providing a distinct route to traversability and clarifying the conditions under which CTCs can arise in a self-consistent framework.

We consider scalar perturbations of the Reissner–Nordström family and the Kerr family. We derive a characteristic expression of the radiation field, at any given fixed angle of future null infinity, and numerically show that its amplitude gets excited only in the extremal case. Our work, therefore, identifies an observational signature for extremal black holes. Moreover, we show that the source of the excitation is the extremal horizon instability and its magnitude is exactly equal to the conserved horizon charge.

We consider self-gravitating stationary configurations of a charged massive complex Proca field, also known as “charged Proca stars", in the particular case of spherical symmetry. We first present a general 3+1 decomposition of the Einstein–Maxwell–Proca system, starting from the action and field equations. We then restrict our system to the case of spherical symmetry and, after imposing a harmonic time dependence ansatz for the Proca field, we construct families of charged Proca stars for different values of the charge parameter q, and different values of the central Proca scalar potential (varphi ). In a similar way to the case of scalar boson stars, one can define a critical charge (q=q_c) that corresponds to the value for which the Coulomb repulsion of the charged Proca field exactly cancels their newtonian gravitational attraction. Just as in the case of boson stars studied in [1, 2], we find that supercritical solutions can exist for a limited range of charges above the critical value (q>q_c). We also consider the binding energy (E_B) for the different families of solutions, and find that gravitationally bound solutions such that (E_B<0) can only exist for subcritical charges such that (q<q_c), indicating that our supercritical solutions are probably dynamically unstable against perturbations.