Pub Date : 2025-12-18DOI: 10.1016/j.aop.2025.170328
Anirudh Pradhan , K. Ghaderi , M. Zeyauddin
We study the optical properties of a new regular Gaussian black hole embedded in a cold isotropic non magnetized refractive plasma. The spacetime is sourced by a Gaussian matter distribution with smearing scale . Photon motion is analyzed for three plasma prescriptions: a uniform medium with constant plasma frequency, a singular isothermal sphere (SIS), and a radially decreasing model. Numerically we find that increasing enlarges both the photon sphere and the shadow, whereas stronger plasma reduces them through dispersion. In the weak field regime the bending angle increases with , while the magnification depends on the plasma profile: it is reduced as plasma strength grows and, for steep inhomogeneous profiles such as SIS, larger further lowers the net magnification due to core smoothing and refractive gradients. Mapping the shadow size to M87* and Sgr A* shows consistency with current Event Horizon Telescope (EHT) constraints for small and moderate plasma strength. These trends provide observational tests of quadratic spacetimes in dispersive media and motivate multi frequency analyses to disentangle geometric and environmental effects.
{"title":"A new regular R2 Gaussian black hole in refractive plasma: Observable signatures and EHT constraints","authors":"Anirudh Pradhan , K. Ghaderi , M. Zeyauddin","doi":"10.1016/j.aop.2025.170328","DOIUrl":"10.1016/j.aop.2025.170328","url":null,"abstract":"<div><div>We study the optical properties of a new regular <span><math><msup><mrow><mi>R</mi></mrow><mrow><mn>2</mn></mrow></msup></math></span> Gaussian black hole embedded in a cold isotropic non magnetized refractive plasma. The spacetime is sourced by a Gaussian matter distribution with smearing scale <span><math><mi>α</mi></math></span>. Photon motion is analyzed for three plasma prescriptions: a uniform medium with constant plasma frequency, a singular isothermal sphere (SIS), and a radially decreasing model. Numerically we find that increasing <span><math><mi>α</mi></math></span> enlarges both the photon sphere and the shadow, whereas stronger plasma reduces them through dispersion. In the weak field regime the bending angle increases with <span><math><mi>α</mi></math></span>, while the magnification depends on the plasma profile: it is reduced as plasma strength grows and, for steep inhomogeneous profiles such as SIS, larger <span><math><mi>α</mi></math></span> further lowers the net magnification due to core smoothing and refractive gradients. Mapping the shadow size to M87* and Sgr A* shows consistency with current Event Horizon Telescope (EHT) constraints for small <span><math><mi>α</mi></math></span> and moderate plasma strength. These trends provide observational tests of quadratic <span><math><mrow><mi>f</mi><mrow><mo>(</mo><mi>R</mi><mo>)</mo></mrow></mrow></math></span> spacetimes in dispersive media and motivate multi frequency analyses to disentangle geometric and environmental effects.</div></div>","PeriodicalId":8249,"journal":{"name":"Annals of Physics","volume":"485 ","pages":"Article 170328"},"PeriodicalIF":3.0,"publicationDate":"2025-12-18","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145797575","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Pub Date : 2025-12-17DOI: 10.1016/j.aop.2025.170319
Rounak Manna , Ujjal Debnath , Anirudh Pradhan
The main objective of this study is to inspect the dynamical characteristics of thin-shell wormholes originating from the Euler–Heisenberg anti-de Sitter (EHAdS) black hole. Within the framework of the Darmois–Israel formalism, this kind of geometric framework is produced by considering the cut-and-paste procedure to avoid the emergence of a singularity and to determine the location of the event horizon. Furthermore, we observe that the elements of stress energy inside the wormhole’s shell defy the weak- and null-energy requirements yet satisfy the criteria of strong energy. Next, we briefly review the gravitational properties (attractive or repulsive) of our wormhole solution. Next, we determine how much exotic substance is required overall to keep the throat of the wormhole open. Afterwards, we use the linearized radial perturbation to analyze the stability of the constructed wormhole structure through the assumption of three distinct variable equations of state (EoS), such as barotropic, phantom-like, and Chaplygin variable EoS. Our research reveals the presence of stable and unstable areas, which depend on how well certain parameters are chosen inside the metric spacetime and EoS. This analysis is further extended in a non-perturbative framework under different EoSs to explore stability beyond small perturbations. Finally, possible observational signatures are considered through the study of light deflection by thin-shell wormholes in EHAdS spacetime. Overall, the findings are highly intriguing and practically feasible in terms of the thin-shell wormhole stability problem.
{"title":"Stability of thin-shell wormholes constructed from Euler–Heisenberg AdS black holes","authors":"Rounak Manna , Ujjal Debnath , Anirudh Pradhan","doi":"10.1016/j.aop.2025.170319","DOIUrl":"10.1016/j.aop.2025.170319","url":null,"abstract":"<div><div>The main objective of this study is to inspect the dynamical characteristics of thin-shell wormholes originating from the Euler–Heisenberg anti-de Sitter (EHAdS) black hole. Within the framework of the Darmois–Israel formalism, this kind of geometric framework is produced by considering the cut-and-paste procedure to avoid the emergence of a singularity and to determine the location of the event horizon. Furthermore, we observe that the elements of stress energy inside the wormhole’s shell defy the weak- and null-energy requirements yet satisfy the criteria of strong energy. Next, we briefly review the gravitational properties (attractive or repulsive) of our wormhole solution. Next, we determine how much exotic substance is required overall to keep the throat of the wormhole open. Afterwards, we use the linearized radial perturbation to analyze the stability of the constructed wormhole structure through the assumption of three distinct variable equations of state (EoS), such as barotropic, phantom-like, and Chaplygin variable EoS. Our research reveals the presence of stable and unstable areas, which depend on how well certain parameters are chosen inside the metric spacetime and EoS. This analysis is further extended in a non-perturbative framework under different EoSs to explore stability beyond small perturbations. Finally, possible observational signatures are considered through the study of light deflection by thin-shell wormholes in EHAdS spacetime. Overall, the findings are highly intriguing and practically feasible in terms of the thin-shell wormhole stability problem.</div></div>","PeriodicalId":8249,"journal":{"name":"Annals of Physics","volume":"485 ","pages":"Article 170319"},"PeriodicalIF":3.0,"publicationDate":"2025-12-17","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145797574","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Pub Date : 2025-12-16DOI: 10.1016/j.aop.2025.170325
Toma Yoneya , Kazuya Fujimoto , Yuki Kawaguchi
The Monte Carlo trajectory sampling of stochastic differential equations based on the quasiprobability distribution functions, such as the Glauber–Sudarshan P, Wigner, and Husimi Q functions, enables us to investigate bosonic open quantum many-body dynamics described by the Gorini–Kossakowski–Sudarshan–Lindblad (GKSL) equation. In this method, the Monte Carlo samplings for the initial distribution and stochastic noises incorporate quantum fluctuations, and thus, we can go beyond the mean-field approximation. However, description using stochastic differential equations is possible only when the corresponding Fokker–Planck equation has a positive-semidefinite diffusion matrix. In this work, we analytically derive the stochastic differential equations for arbitrary Hamiltonian and jump operators based on the path-integral formula, independently of the derivation of the Fokker–Planck equation. In the course of the derivation, we formulate the path-integral representation of the GKSL equation by using the -ordered quasiprobability distribution function, which systematically describes the aforementioned quasiprobability distribution functions by changing the real parameter . The essential point of this derivation is that we employ the Hubbard–Stratonovich transformation in the path integral, and its application is not always feasible. We find that the feasible condition of the Hubbard–Stratonovich transformation is identical to the positive-semidefiniteness condition of the diffusion matrix in the Fokker–Planck equation. In the benchmark calculations, we confirm that the Monte Carlo simulations of the obtained stochastic differential equations well reproduce the exact dynamics of physical quantities and non-equal time correlation functions of numerically solvable models, including the Bose–Hubbard model. This work clarifies the applicability of the approximation and gives systematic and simplified procedures to obtain the stochastic differential equations to be numerically solved.
{"title":"Path-integral formulation of bosonic Markovian open quantum dynamics with Monte Carlo stochastic trajectories using the Glauber–Sudarshan P, Wigner, and Husimi Q functions and hybrids","authors":"Toma Yoneya , Kazuya Fujimoto , Yuki Kawaguchi","doi":"10.1016/j.aop.2025.170325","DOIUrl":"10.1016/j.aop.2025.170325","url":null,"abstract":"<div><div>The Monte Carlo trajectory sampling of stochastic differential equations based on the quasiprobability distribution functions, such as the Glauber–Sudarshan P, Wigner, and Husimi Q functions, enables us to investigate bosonic open quantum many-body dynamics described by the Gorini–Kossakowski–Sudarshan–Lindblad (GKSL) equation. In this method, the Monte Carlo samplings for the initial distribution and stochastic noises incorporate quantum fluctuations, and thus, we can go beyond the mean-field approximation. However, description using stochastic differential equations is possible only when the corresponding Fokker–Planck equation has a positive-semidefinite diffusion matrix. In this work, we analytically derive the stochastic differential equations for arbitrary Hamiltonian and jump operators based on the path-integral formula, independently of the derivation of the Fokker–Planck equation. In the course of the derivation, we formulate the path-integral representation of the GKSL equation by using the <span><math><mi>s</mi></math></span>-ordered quasiprobability distribution function, which systematically describes the aforementioned quasiprobability distribution functions by changing the real parameter <span><math><mi>s</mi></math></span>. The essential point of this derivation is that we employ the Hubbard–Stratonovich transformation in the path integral, and its application is not always feasible. We find that the feasible condition of the Hubbard–Stratonovich transformation is identical to the positive-semidefiniteness condition of the diffusion matrix in the Fokker–Planck equation. In the benchmark calculations, we confirm that the Monte Carlo simulations of the obtained stochastic differential equations well reproduce the exact dynamics of physical quantities and non-equal time correlation functions of numerically solvable models, including the Bose–Hubbard model. This work clarifies the applicability of the approximation and gives systematic and simplified procedures to obtain the stochastic differential equations to be numerically solved.</div></div>","PeriodicalId":8249,"journal":{"name":"Annals of Physics","volume":"485 ","pages":"Article 170325"},"PeriodicalIF":3.0,"publicationDate":"2025-12-16","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145836662","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Pub Date : 2025-12-16DOI: 10.1016/j.aop.2025.170326
Jesse Huhtala, Iiro Vilja
In quantum field theory, sharp momentum states have to be normalized to be in Fock space. We investigate two different normalization schemes: box normalization and wave packets. These methods are equivalent in flat spacetimes, but turn out to produce different results in curved spacetimes, specifically in those that break translation invariance. This means that scattering processes have to be defined in relation to the normalization scheme used, rather than being independent of it as is the case in flat spacetime. We prove this and provide an illustrative example.
{"title":"Normalizing Fock space states in static spacetimes","authors":"Jesse Huhtala, Iiro Vilja","doi":"10.1016/j.aop.2025.170326","DOIUrl":"10.1016/j.aop.2025.170326","url":null,"abstract":"<div><div>In quantum field theory, sharp momentum states have to be normalized to be in Fock space. We investigate two different normalization schemes: box normalization and wave packets. These methods are equivalent in flat spacetimes, but turn out to produce different results in curved spacetimes, specifically in those that break translation invariance. This means that scattering processes have to be defined in relation to the normalization scheme used, rather than being independent of it as is the case in flat spacetime. We prove this and provide an illustrative example.</div></div>","PeriodicalId":8249,"journal":{"name":"Annals of Physics","volume":"485 ","pages":"Article 170326"},"PeriodicalIF":3.0,"publicationDate":"2025-12-16","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145797571","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Pub Date : 2025-12-16DOI: 10.1016/j.aop.2025.170323
A.A. Araújo Filho , Iarley P. Lobo
A recent study (Touati and Zaim, 2023) examined the thermodynamic behavior of an axially symmetric black hole within a non–commutative framework that mimics the effect of an angular momentum. However, the analysis presents notable computational inconsistencies. In that analysis, the event horizon was miscalculated, and this error propagated through and compromised all subsequent results. In addition, an incorrect definition of surface gravity was used — the spherically symmetric case was invoked for an axially symmetric spacetime — rendering the thermodynamic results invalid. In other words, all the results presented in the paper require a thorough reexamination.
{"title":"Comment on “Thermodynamic properties of Schwarzschild black hole in non-commutative gauge theory of gravity”","authors":"A.A. Araújo Filho , Iarley P. Lobo","doi":"10.1016/j.aop.2025.170323","DOIUrl":"10.1016/j.aop.2025.170323","url":null,"abstract":"<div><div>A recent study (Touati and Zaim, 2023) examined the thermodynamic behavior of an axially symmetric black hole within a non–commutative framework that mimics the effect of an angular momentum. However, the analysis presents notable computational inconsistencies. In that analysis, the event horizon was miscalculated, and this error propagated through and compromised all subsequent results. In addition, an incorrect definition of surface gravity was used — the spherically symmetric case was invoked for an axially symmetric spacetime — rendering the thermodynamic results invalid. In other words, all the results presented in the paper require a thorough reexamination.</div></div>","PeriodicalId":8249,"journal":{"name":"Annals of Physics","volume":"485 ","pages":"Article 170323"},"PeriodicalIF":3.0,"publicationDate":"2025-12-16","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145797573","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Pub Date : 2025-12-15DOI: 10.1016/j.aop.2025.170324
Faizuddin Ahmed , Abdelmalek Bouzenada
In this study, we investigate the dynamics of photons and the propagation of electromagnetic waves in a three-dimensional static wormhole geometry threaded by disclinations. Our primary focus is on photon trajectories and how they are influenced by key geometric parameters, including the wormhole throat radius, the curvature radius, and the disclinations parameter. We demonstrate that these parameters significantly affect the path of photons traversing the wormhole background. We find that the effective potential governing photon motion asymptotically approaches a constant value near the wormhole throat, forming a repulsive barrier that restricts inward propagation unless the photon possesses energy above a critical threshold. Furthermore, we analyze the wave-optical properties by solving the scalar Helmholtz wave equation in this wormhole background. Employing a suitable wave function ansatz, we transform the equation into a Schrödinger-like form, which allows us to identify the effective potential governing wave propagation. From this formulation, we derive a spatially and frequency-dependent effective refractive index. Our results show that the geometrical parameters-particularly the throat radius, the curvature radius, and the disclinations parameter have a substantial impact on the refractive index and overall wave-optical behavior of the system.
{"title":"Null geodesic and Helmholtz wave equation in (1+2)-dimensional static wormhole with disclinations","authors":"Faizuddin Ahmed , Abdelmalek Bouzenada","doi":"10.1016/j.aop.2025.170324","DOIUrl":"10.1016/j.aop.2025.170324","url":null,"abstract":"<div><div>In this study, we investigate the dynamics of photons and the propagation of electromagnetic waves in a three-dimensional static wormhole geometry threaded by disclinations. Our primary focus is on photon trajectories and how they are influenced by key geometric parameters, including the wormhole throat radius, the curvature radius, and the disclinations parameter. We demonstrate that these parameters significantly affect the path of photons traversing the wormhole background. We find that the effective potential governing photon motion asymptotically approaches a constant value near the wormhole throat, forming a repulsive barrier that restricts inward propagation unless the photon possesses energy above a critical threshold. Furthermore, we analyze the wave-optical properties by solving the scalar Helmholtz wave equation in this wormhole background. Employing a suitable wave function ansatz, we transform the equation into a Schrödinger-like form, which allows us to identify the effective potential governing wave propagation. From this formulation, we derive a spatially and frequency-dependent effective refractive index. Our results show that the geometrical parameters-particularly the throat radius, the curvature radius, and the disclinations parameter have a substantial impact on the refractive index and overall wave-optical behavior of the system.</div></div>","PeriodicalId":8249,"journal":{"name":"Annals of Physics","volume":"485 ","pages":"Article 170324"},"PeriodicalIF":3.0,"publicationDate":"2025-12-15","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145797570","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
The supermultiplet model, based on the reduction chain , is revisited through the lens of commutants within universal enveloping algebras of Lie algebras. From this analysis, a collection of twenty polynomials up to degree nine emerges from the commutant associated with the subalgebra. This study is conducted in the Poisson (commutative) framework using the Lie-Poisson bracket associated with the dual of the Lie algebra under consideration. As the main result, we obtain the polynomial Poisson algebra generated by these twenty linearly independent and indecomposable polynomials, with five elements being central. This incorporates polynomial expansions up to degree seventeen in the Lie algebra generators. We further discuss additional algebraic relations among these polynomials, explicitly detailing some of the lower-order ones. As a byproduct of these results, we also show that the recently introduced ‘grading method’ turns out to be essential for deriving the Poisson bracket relations when the degree of the expansions becomes so high that standard approaches are no longer applicable due to computational limitations. These findings represent a further step toward the systematic exploration of polynomial algebras relevant to nuclear models.
{"title":"Polynomial algebra from the Lie algebra reduction chain su(4)⊃su(2)×su(2): The supermultiplet model","authors":"Rutwig Campoamor-Stursberg , Danilo Latini , Ian Marquette , Junze Zhang , Yao-Zhong Zhang","doi":"10.1016/j.aop.2025.170322","DOIUrl":"10.1016/j.aop.2025.170322","url":null,"abstract":"<div><div>The supermultiplet model, based on the reduction chain <span><math><mrow><mi>su</mi><mrow><mo>(</mo><mn>4</mn><mo>)</mo></mrow><mo>⊃</mo><mi>su</mi><mrow><mo>(</mo><mn>2</mn><mo>)</mo></mrow><mo>×</mo><mi>su</mi><mrow><mo>(</mo><mn>2</mn><mo>)</mo></mrow></mrow></math></span>, is revisited through the lens of commutants within universal enveloping algebras of Lie algebras. From this analysis, a collection of twenty polynomials up to degree nine emerges from the commutant associated with the <span><math><mrow><mi>su</mi><mrow><mo>(</mo><mn>2</mn><mo>)</mo></mrow><mo>×</mo><mi>su</mi><mrow><mo>(</mo><mn>2</mn><mo>)</mo></mrow></mrow></math></span> subalgebra. This study is conducted in the Poisson (commutative) framework using the Lie-Poisson bracket associated with the dual of the Lie algebra under consideration. As the main result, we obtain the polynomial Poisson algebra generated by these twenty linearly independent and indecomposable polynomials, with five elements being central. This incorporates polynomial expansions up to degree seventeen in the Lie algebra generators. We further discuss additional algebraic relations among these polynomials, explicitly detailing some of the lower-order ones. As a byproduct of these results, we also show that the recently introduced ‘grading method’ turns out to be essential for deriving the Poisson bracket relations when the degree of the expansions becomes so high that standard approaches are no longer applicable due to computational limitations. These findings represent a further step toward the systematic exploration of polynomial algebras relevant to nuclear models.</div></div>","PeriodicalId":8249,"journal":{"name":"Annals of Physics","volume":"485 ","pages":"Article 170322"},"PeriodicalIF":3.0,"publicationDate":"2025-12-15","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145836663","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
In this study, we investigate the stability of the Einstein Static Universe within gravity under homogeneous anisotropic perturbations in both scale factors and matter. The perturbed field equations are derived using a linear equation of state, and two specific models are analyzed. The Arctan model, , yields bounded curvature and smooth transitions across regimes, while the Logarithmic model, , incorporates quantum-motivated corrections. For each model, stability conditions are obtained and stability regions are mapped in parameter space. Our analysis shows that both models admit stable Einstein Static Universe solutions within certain parameter ranges, in contrast with the instability predicted by General Relativity.
{"title":"Cosmic evolution and stability of the Einstein Static Universe in modified gravity models","authors":"Sana Saleem , Jawahir Waqqas , Tooba Tariq , S.A. Mardan","doi":"10.1016/j.aop.2025.170321","DOIUrl":"10.1016/j.aop.2025.170321","url":null,"abstract":"<div><div>In this study, we investigate the stability of the Einstein Static Universe within <span><math><mrow><mi>f</mi><mrow><mo>(</mo><mi>R</mi><mo>)</mo></mrow></mrow></math></span> gravity under homogeneous anisotropic perturbations in both scale factors and matter. The perturbed field equations are derived using a linear equation of state, and two specific models are analyzed. The Arctan model, <span><math><mrow><mi>f</mi><mrow><mo>(</mo><mi>R</mi><mo>)</mo></mrow><mo>=</mo><mi>λ</mi><mo>arctan</mo><mrow><mo>(</mo><mi>R</mi><mo>)</mo></mrow></mrow></math></span>, yields bounded curvature and smooth transitions across regimes, while the Logarithmic model, <span><math><mrow><mi>f</mi><mrow><mo>(</mo><mi>R</mi><mo>)</mo></mrow><mo>=</mo><mi>β</mi><mo>ln</mo><mrow><mo>(</mo><mi>R</mi><mo>)</mo></mrow><mo>+</mo><mi>R</mi></mrow></math></span>, incorporates quantum-motivated corrections. For each model, stability conditions are obtained and stability regions are mapped in parameter space. Our analysis shows that both models admit stable Einstein Static Universe solutions within certain parameter ranges, in contrast with the instability predicted by General Relativity.</div></div>","PeriodicalId":8249,"journal":{"name":"Annals of Physics","volume":"485 ","pages":"Article 170321"},"PeriodicalIF":3.0,"publicationDate":"2025-12-12","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145797572","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Pub Date : 2025-12-12DOI: 10.1016/j.aop.2025.170316
L.C.N. Santos , H. Aounallah , L.G. Barbosa
In this work, we investigate the behavior of scalar bosons governed by the Klein–Gordon equation in a spacetime modified by both a cosmic string and a global monopole, under the framework of gravity’s rainbow. Two interaction types are considered: a Klein–Gordon oscillator and a Coulomb-like potential. The presence of topological defects introduces effective angular momentum modifications, while the rainbow functions and incorporate an energy dependence into the spacetime geometry. Analytical and numerical solutions are obtained for the bound states, and the resulting energy spectra are analyzed for different choices of rainbow functions. The results demonstrate that both the topological parameters , and the rainbow parameter significantly influence the energy levels, introducing shifts and asymmetries that are sensitive to the functional form of the rainbow modifications.
{"title":"Scalar bosons in the context of gravity’s rainbow in the double defect spacetime","authors":"L.C.N. Santos , H. Aounallah , L.G. Barbosa","doi":"10.1016/j.aop.2025.170316","DOIUrl":"10.1016/j.aop.2025.170316","url":null,"abstract":"<div><div>In this work, we investigate the behavior of scalar bosons governed by the Klein–Gordon equation in a spacetime modified by both a cosmic string and a global monopole, under the framework of gravity’s rainbow. Two interaction types are considered: a Klein–Gordon oscillator and a Coulomb-like potential. The presence of topological defects introduces effective angular momentum modifications, while the rainbow functions <span><math><mrow><mi>f</mi><mrow><mo>(</mo><mi>x</mi><mo>)</mo></mrow></mrow></math></span> and <span><math><mrow><mi>g</mi><mrow><mo>(</mo><mi>x</mi><mo>)</mo></mrow></mrow></math></span> incorporate an energy dependence into the spacetime geometry. Analytical and numerical solutions are obtained for the bound states, and the resulting energy spectra are analyzed for different choices of rainbow functions. The results demonstrate that both the topological parameters <span><math><mi>α</mi></math></span>, <span><math><mi>β</mi></math></span> and the rainbow parameter <span><math><mi>ξ</mi></math></span> significantly influence the energy levels, introducing shifts and asymmetries that are sensitive to the functional form of the rainbow modifications.</div></div>","PeriodicalId":8249,"journal":{"name":"Annals of Physics","volume":"485 ","pages":"Article 170316"},"PeriodicalIF":3.0,"publicationDate":"2025-12-12","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145747819","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Pub Date : 2025-12-10DOI: 10.1016/j.aop.2025.170320
Adnan Malik , Aimen Rauf , P.K. Sahoo , Wenbin Lin , Fatemah Mofarreh
This study investigates cosmological dynamics in modified gravity, where spacetime geometry is governed by the non-metricity scalar . Using Friedmann–Robertson–Walker spacetime, we derive exact cosmological solutions for six distinct epochs: dark energy-dominated, dust-dominated, sub-relativistic, radiation-dominated, ultra-relativistic, and stiff fluid phases. Employing a power-law approach, we analyze the universe’s evolutionary dynamics, identifying parameter ranges that satisfy energy conditions for viable bouncing cosmologies. We further examine three specific bouncing scenarios — symmetric bounce, superbounce, and oscillatory cosmology — within the framework, assessing their mathematical consistency and physical implications. Our results demonstrate how gravity can simultaneously address singularity avoidance, describe multi-phase cosmic evolution, and provide alternatives to standard cosmological paradigms while maintaining fundamental energy conditions. The findings highlight the theory’s potential to unify diverse cosmological phenomena through geometric modifications of gravity.
{"title":"Dark energy cosmological solutions in f(Q) modified gravity","authors":"Adnan Malik , Aimen Rauf , P.K. Sahoo , Wenbin Lin , Fatemah Mofarreh","doi":"10.1016/j.aop.2025.170320","DOIUrl":"10.1016/j.aop.2025.170320","url":null,"abstract":"<div><div>This study investigates cosmological dynamics in modified <span><math><mrow><mi>f</mi><mrow><mo>(</mo><mi>Q</mi><mo>)</mo></mrow></mrow></math></span> gravity, where spacetime geometry is governed by the non-metricity scalar <span><math><mi>Q</mi></math></span>. Using Friedmann–Robertson–Walker spacetime, we derive exact cosmological solutions for six distinct epochs: dark energy-dominated, dust-dominated, sub-relativistic, radiation-dominated, ultra-relativistic, and stiff fluid phases. Employing a power-law approach, we analyze the universe’s evolutionary dynamics, identifying parameter ranges that satisfy energy conditions for viable bouncing cosmologies. We further examine three specific bouncing scenarios — symmetric bounce, superbounce, and oscillatory cosmology — within the <span><math><mrow><mi>f</mi><mrow><mo>(</mo><mi>Q</mi><mo>)</mo></mrow></mrow></math></span> framework, assessing their mathematical consistency and physical implications. Our results demonstrate how <span><math><mrow><mi>f</mi><mrow><mo>(</mo><mi>Q</mi><mo>)</mo></mrow></mrow></math></span> gravity can simultaneously address singularity avoidance, describe multi-phase cosmic evolution, and provide alternatives to standard cosmological paradigms while maintaining fundamental energy conditions. The findings highlight the theory’s potential to unify diverse cosmological phenomena through geometric modifications of gravity.</div></div>","PeriodicalId":8249,"journal":{"name":"Annals of Physics","volume":"485 ","pages":"Article 170320"},"PeriodicalIF":3.0,"publicationDate":"2025-12-10","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145748920","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
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