This study proposes an automated defect detection system for large-scale fudge production, addressing the limitations of manual inspection, which is both labor-intensive and error-prone. Deep learning-based image recognition was employed to classify normal samples and four defect types using multiple object detection models, including SSD and YOLOv4/YOLOv5/YOLOv7/YOLOv8/YOLOv11. Instead of relying on a single model, the system integrates a multi-model strategy combining confidence-weighted voting, rule-based selection for specific defects, and Non-Maximum Suppression (NMS), enabling complementary strengths across models and improving robustness. The selected models were deployed in a real-time inspection system equipped with a flipping mechanism that allows each piece of fudge to be inspected on both sides, thereby expanding the coverage of defects. In evaluations using 1,000 real production samples, first-round accuracies were 47.5% (hole), 56.7% (leak), and 60.9% (white). After applying the flipping mechanism for a second inspection, accuracies increased to 75.8%, 83.6%, and 89.3%, respectively, with hole defects showing the largest improvement (28.3%). Our validation-learned fusion achieves 0.995 mAP@0.5 (on par with the best single model) and 0.944 mAP@0.5:0.95, outperforming YOLOv11 and YOLOv5 by + 0.2 and + 2.4 percentage points, respectively; gains are most evident for White defect and Hole defect. These results indicate that combining multi-model detection with dual-side inspection significantly enhances accuracy and enables the reliable screening of defects in real-time production environments.

There has been considerable effort to mimic analogue black holes and wormholes in solid state systems. Lattice realisations in particular present specific challenges. One of those is that event horizons in general have both white and black hole (grey hole) character, a feature guaranteed by the Nielsen-Ninomiya theorem. We here explore and extend the capability of superconducting circuit hardware to implement on-demand spacetime geometries on lattices, combining the nonreciprocity of gyrators with the non-linearity of Josephson junctions. We demonstrate the possibility of the metric sharply changing within a single lattice point, thus entering a regime where the modulation of system parameters is “trans-Planckian”, and the Hawking temperature ill-defined. Instead of regular Hawking radiation, we find an instability in the form of an exponential burst of charge and phase quantum fluctuations over short time scales – a robust signature even in the presence of an environment. Moreover, we present a loop-hole for the typical black/white hole ambiguity in lattice simulations: exceptional points in the dispersion relation allow for the creation of pure black (or white) hole horizons, at the expense of a radical change in the dynamics of the wormhole interior.

We study null geodesics that connect the two asymptotically flat regions of the maximally extended Kerr spacetime. These vortical geodesics traverse both horizons and pass through the ring singularity, linking the positive- <a:math xmlns:a="http://www.w3.org/1998/Math/MathML" display="inline"> <a:mi>r</a:mi> </a:math> exterior to the negative- <c:math xmlns:c="http://www.w3.org/1998/Math/MathML" display="inline"> <c:mi>r</c:mi> </c:math> asymptotic side. Using impact parameters, we identify a closed subset of parameter space, the inner throat, where the radial potential has no real roots, and photons exhibit no radial turning points. In this region, at most two constant-latitude geodesics exist, one of which is aligned with the principal null direction. We also identify the forbidden polar-angle band that limits the range of geodesics reaching an asymptotic observer. We solve the geodesic equations analytically and numerically in Eddington-Finkelstein-like coordinates, obtaining mutually consistent results that correct and extend previously available formulas. The resulting trajectories are used to construct simulated views for an observer in the negative- <e:math xmlns:e="http://www.w3.org/1998/Math/MathML" display="inline"> <e:mi>r</e:mi> </e:math> domain, revealing strong image distortion and inversion, with possible implications for analogous white hole configurations.

Abstract We prove that the black to white hole transition theorized in several papers can be described as a change in the topology of the event horizon. We also show, using the theory of cobordism due to Milnor and Wallace, how to obtain the full manifold containing the transition.

We present an asymptotically flat spherically symmetric non-singular metric that describes gravitational collapse and matter bounce with transient black hole and white hole regions. The metric provides a dynamical counterpart to proposed static non-singular black holes, and a phenomenological model for possible black hole to white hole transitions in quantum gravity.

In this work, we propose a dangerous journey – a journey through the strong singularity from one universe to another or from inside of a black hole to its ’inverse’ as a white hole. Such singularities are hidden in the Friedman and Schwarzschild solutions; we call them malicious singularities. The journey is made possible owing to two generalizations. The first generalization consists in considering spaces with differential structures on them (so-called ringed spaces) rather than the usual manifolds. This entails a generalization of the concept of smoothness, which allows us to think about a smooth passage through the singularity. The second generalization is related to the concept of curve. We show that if a kind of singularity is implanted in the set of curve’s parameters, along with an appropriate topology, in such a way that the structure of the set of parameters corresponds to the structure of the singular space-time, the curve can smoothly – in a generalized sense – pass through the singularity.

The Tsallis-Cirto non-extensive statistics with $$\delta = 2$$ describes the processes of splitting and merging of black holes and their thermodynamics [1, 2]. Here we consider a toy model, which matches this generalized statistics and extends it by providing the integer valued entropy of the black hole, SBH(N) = $$N(N - 1){\text{/}}2$$ . In this model the black hole consists of $$N$$ the so-called Planckons—objects with reduced Planck mass $${{m}_{{\text{P}}}} = 1{\text{/}}\sqrt {8\pi G} $$ – so that its mass is quantized, $$M = N{{m}_{{\text{P}}}}$$ . The entropy of each Planckon is zero, but the entropy of black hole with $$N$$ Planckons is provided by the $$N(N - 1){\text{/}}2$$ degrees of freedom—the correlations between the gravitationally attracted Planckons. This toy model can be extended to a charged Reissner-Nordström (RN) black hole, which consists of charged Planckons. Despite the charge, the statistical ensemble of Planckons remains the same, and the RN black hole with $$N$$ Planckons has the same entropy as the electrically neutral hole, $${{S}_{{{\text{RNBH}}}}}(N) = N(N - 1){\text{/}}2$$ . This is supported by the adiabatic process of transformation from the RN to Schwarzschild black hole by varying the fine structure constant. The adiabaticity is violated in the extreme limit, when the gravitational interaction between two Planckons is compensated by the repulsion between their electric charges, and the RN black hole loses stability. The white hole formed by the same $$N$$ Planckons has negative entropy, $${{S}_{{{\text{WH}}}}}(N) = - N(N - 1){\text{/}}2$$ .

Eccentric white dwarf-massive black hole binaries can potentially source some extreme x-ray transients, including tidal disruption events and the recently observed quasiperiodic x-ray eruptions at the galactic nuclei. Meanwhile, they are one of the target gravitational wave sources with extreme mass ratios for future millihertz gravitational wave missions. In this work, we focus on the tidal evolution and orbital dynamics of such binaries under the influence of the tidal backreaction and the dissipative effect from gravitational wave emission. We find that the latter can cause the dynamical tide to evolve chaotically after more than one orbital harmonics encounter the mode resonance through orbital decay. Different from the tidal-driven chaos, which only occurs for pericenter distances within around two times the tidal radius (${R}_{t}$), this gravitational wave-driven chaos can happen at much larger pericenter distances. The growth scales similarly to a diffusive process, in which the tidal energy grows linearly with time on average over a long duration. If the tidal energy eventually approaches the stellar binding energy, achievable when the pericenter distance is less than $4{R}_{t}$, it can cause mass ejection as the wave breaks due to nonlinear effects. We show that this can potentially lead to the repeating partial tidal disruptions observed at galactic centers. That means these disruptions can occur at a much larger pericenter distance than previous analytical estimates. Furthermore, if the system can evolve to a close pericenter distance of about 2.7${R}_{t}$, the white dwarf can further lose mass via tidal stripping at each pericenter passage. This provides a mechanism for producing the quasiperiodic eruptions. However, it requires at least a certain amount of angular momentum to escape the binary during the mass transfer process to match the observations, which we do not have a justification based on first-principle calculations.

This study has been undertaken to investigation of our universe actual location.Here the information about black hole and white hole and singularity and hy-pothesis of universe location.and here is the information about multiverse and the shortest distance of two universe.And dark energy dark matter.And here about how to research for scientists for founding our universe actual location.

Multidrug-resistant Klebsiella pneumoniae (MDR-KP) poses a significant clinical challenge due to limited therapeutic options and high mortality. This study investigated the antimicrobial efficacy of gamma-irradiation-synthesized gentamicin-conjugated silver nanoparticles (Gent-Ag NPs), copper oxide nanoparticles (CuO NPs), and bimetallic Ag-CuO NPs against three MDR-KP isolates in comparison with the gamma-irradiated gentamicin alone. Gent-Ag, Gent-CuO, and bimetallic Gent-Ag-CuO NPs were synthesized via gamma-radiation-induced reduction and characterized by different analytical methods to confirm their shape, size, surface morphology, particle size distribution, and crystallinity using HRTEM, SEM, DLS, and XRD, respectively. Comparative analysis demonstrated that Gent-Ag NPs exhibited superior antimicrobial activity, while Gent-CuO NPs showed diminished efficacy. SEM imaginganalysis showed that Gent-Ag-CuO NPs effectively damaged and weakened the bacterial surfaces. It should be noted that the complete lys of K. pneumoniae cells is depicted by the white holes seen inside the bacteria. These findings suggest potential therapeutic applications of Ag-based NPs against MDR-KP, warranting further validation with larger sample sizes.

Abstract Spatiotemporal moving interface consists of two media with different refractive indices separated by a boundary that propagates at a constant velocity. Although electromagnetic wave scatterings at the subluminal and superluminal interfaces have been well understood, how electromagnetic waves interact with the interluminal interface remains obstinate due to the breaking of phase matching and field continuity conditions at the moving boundary. Here, this problem is addressed by discretizing the moving interface into alternating spatial and temporal boundaries with larger scale than the incident wave packet. Consequently, the scattering event is discretized sequentially in a purely spatial or purely temporal boundary, thereby preserving both phase matching and field continuity conditions and enabling a closed‐form solution toward the interluminal scattering problem. The results reveal that the discretized interluminal boundary is analogous to the event horizons of black and white holes during the wave propagation, where transmitted or reflected waves become perpetually trapped at the discretized interface. These trapped waves undergo cascaded amplification and compression during propagation, resulting in a single forward‐propagating mode and an indefinite sequence of counter‐scattered modes, which can be utilized to achieve tunable and extreme field amplification and compression.

This paper considers non-singular black holes. It discusses the observation of particles falling onto ordinary and non-singular black holes from the perspective of a distant observer. It is demonstrated that, during a stage in the evolution of non-singular black holes, powerful energy fluxes can be emitted. Distant observers may interpret these fluxes as white holes.

This paper consists of two parts. In the first part, we attempt to find the intermolecular force of charged AdS black hole (BH). Starting from the fact that the equation of states of BH and the van der Waals (vdW) equation have the same compressibility factors , we determine the intermolecular force of BH. We find that this force can always be written as the sum of the topological force created by the topological charge, and the electrostatic force created by the conducting microsphere charged with the electric charge. This is the intermolecular force for all systems whose phase transition possesses the same compressibility factor . In part 2 we begin with the equation of state of white hole (WH) whose temperature is negative and find that its compressibility factor is equal to, and, at the same time, we establish the anti- vdW equation with compressibility factor . This is the main factor for us to determine the intermolecular force of WH. This force is composed of two terms. The first term is the repulsive force, created by the topological charge, and the second term exhibits the attractive electrostatic force, created by two quasi- Cooper pairs (similar to Cooper pairs in the superconductors) consisting of two charged spheric molecules with electric charge. The formation of quasi-Cooper pairs is by BH a quantum effect which was realized in the process of quantum tunneling from BH to WH. At high temperature, the quasi-Cooper pairs are broken, leading to the cancellation of the attractive force, and the repulsive force will push all molecules of WH further and further away. The behaviors of BH force and WH force are totally suppoted by the corresponding scalar curvatures of the thermodynamic geometry. Keywords: Intermolecular force, charged AdS black hole, white hole, quantum tunneling, topological force, phase transition.

It has been recently shown that regular black holes arise as the unique spherically symmetric solutions of broad families of generalizations of Einstein gravity involving infinite towers of higher-curvature corrections in D≥5 spacetime dimensions. In this paper we argue that such regular black holes arise as the byproduct of the gravitational collapse of pressureless dust stars. We show that, just like for Einstein gravity, the modified junction conditions for these models impose that the dust particles on the star surface follow geodesic trajectories on the corresponding black hole background. Generically, in these models the star collapses until it reaches a minimum size (and a maximum density) inside the inner horizon of the black hole it creates. Then, it bounces back and reappears through a white hole in a different universe, where it eventually reaches its original size and restarts the process. Along the way, we study Friedmann-Lemaître-Robertson-Walker (FLRW) cosmologies in the same theories that regularize black hole singularities. We find that the cosmological evolution is completely smooth, with the big bang and big crunch singularities predicted by Einstein gravity replaced by cosmological bounces.

This hypothesis presents a new perspective on the potential formation and instability of wormholes and white holes within a closed universe. Considering the universe as a spherical spacetime fabric, it suggests that extreme black hole gravitational warping may lead to temporary wormhole creation, whose instability explains the absence of observed white holes in nature.

In black hole thermodynamics, entropy is non-extensive. This entropy obeys the composition rule which coincides with the composition rule in the non-extensive Tsallis–Cirto $$\delta = 2$$ statistics. Here we extend this approach to the thermodynamics of white holes. The entropy of the white hole is negative as follows from the rate of macroscopic quantum tunneling from black hole to white hole. The white hole entropy is with the minus sign the entropy of the black hole with the same mass, S WH(M) = –S BH(M). This reflects the anti-symmetry with respect to time reversal, at which the shift vector in the Arnowitt–Deser–Misner formalism changes sign. This symmetry allows one to extend the Tsallis–Cirto entropy by adding a minus sign to the Tsallis–Cirto formula applied to white hole. As a result, the composition rule remains the same, with the only difference being that instead of entropy it contains the entropy modulus. The same non-extensive composition rule is obtained for the entropy of the Reissner–Nordström black hole. This entropy is formed by the positive entropy of the outer horizon and the negative entropy of the inner horizon. The model of the black hole formed by black hole atoms with Planck-scale mass is also extended to include the negative entropy of white holes.

We propose an analog quantum simulation for studying the collapse and bounce of a star from infinity. In this spacetime, which encompasses both a black hole and a white hole, we place a massless scalar field that propagates at the speed of light, which is modified by the curvature. We simulate this system using an SQUID array, in which we can alter the propagation of light using an external magnetic field. We consider both infalling and outfalling radiation, giving rise to two different scenarios: downstream and upstream radiation. We compute the magnetic flux profile required by the simulation in both cases and find out that the former is more experimentally suitable.

We consider the canonical quantisation of spherically symmetric spacetimes within unimodular gravity, leaving sign choices in the metric general enough to include both the interior and exterior Schwarzschild-(Anti-)de Sitter spacetime. In unimodular gravity the cosmological constant appears as an integration constant analogous to a total energy, and the quantum Wheeler-DeWitt equation takes the form of a Schrödinger equation in unimodular time. We discuss self-adjoint extensions of the Schrödinger-like Hamiltonian arising from the requirement of unitarity in unimodular time, and identify a physically motivated one-parameter family of extensions. For semiclassical states we are able to derive analytical expressions for expectation values of the metric, representing a quantum-corrected, nonsingular extension of the classical Schwarzschild-(A)dS geometry which describes a quantum transition between asymptotic black hole and white hole states. The sign of the self-adjoint extension parameter corresponds to the allowed sign of the black hole/white hole mass, and so it can be chosen to ensure that this mass is always positive. We also discuss tunnelling states which allow for a change in the sign of the mass, but which are not semiclassical in high-curvature regions. Our mechanism for singularity resolution and the explicit form of the quantum-corrected metric can be compared to other proposals for black holes in quantum gravity, and in the asymptotically AdS case can be contrasted with holographic arguments.

This paper presents the Horizon Model (HM) of cosmology, designed to resolve the cosmological constant problem by equating the vacuum energy density with that of the observable universe. Grounded in quantum information theory, HM proposes the first element of reality emerging from the Big Bang singularity as a Planck-sized qubit. The model views the Big Bang as the opening of a white hole, with spacetime and matter/energy emerging from the event horizon. Using the Schwarzschild solution and the Holographic Principle, HM calculates the number of vacuum qubits needed to equalize densities, and compares this to published estimates of the observable universe’s Shannon entropy (S). With this information, HM can calculate the state of the vacuum as a function of S. Results at S=1 (t=0) and S=1.46×10104 bits (t=now) are presented. At t=0, the radius of the event horizon is predicted to be ∼10-26 m in good agreement with the ad-hoc requirement of the current cosmic inflation paradigm. At t=now, HM predicts Hubble flow within 0.8σ of the Planck collaboration measurement and can resolve the Hubble tension with a small adjustment of the vacuum energy density. HM predictions of the vacuum pressure (∼10-10 Pa) are in good agreement with pressure measurements made on the lunar surface by NASA and the Chinese space program. Aligned with current research for spacetime emerging from surfaces, HM suggests new theoretical directions, potentially leading to a quantum theory of gravity.

We consider near-horizon collisions between two particles moving freely in the Schwarzschild metric in the region outside the horizon. One of them emerges from a white hole. We scrutinize when such a process can lead to the indefinitely large growth of the energy in the center of mass frame in the point of collision. We also trace how the kinematics of collision manifests itself in preserving the principle of kinematic censorship. According to this principle, the energy released in any event of collision, must remain finite although it can be made as large as one likes. Also, we find that particle decay near the singularity leads to unbounded release of energy independently of its initial value.