This work presents a unified treatment of Nojiri–Odintsov holographic dark energy, encompassing its Ricci–Gauss–Bonnet realization and a second-order approximation as a particular case of the generalized framework. By incorporating higher-order curvature corrections from the Gauss–Bonnet invariant and the Ricci scalar, we construct an extended HDE model and study the evolution of the equation-of-state parameter in both interacting and non-interacting scenarios. The analysis reveals possible quintessence-to-phantom transitions, with observational validation from cosmic chronometer and Planck 2018 datasets. The outcomes indicate the role of higher-curvature corrections provide a viable description of late-time cosmic acceleration. Finally, within the Ricci–Gauss–Bonnet and Nojiri–Odintsov holographic frameworks, we find that the reconstructed exhibits the DESI-preferred quintessence–phantom crossing, although the Hubble tension between Planck and SH0ES determinations of remains unresolved.
{"title":"Second-order approximation of Nojiri–Odintsov infrared cutoff through heuristic expansion: A refined framework for holographic dark energy dynamics with Ricci–Gauss–Bonnet form","authors":"Aziza Altaibayeva , Assem Assetkhan , Surajit Chattopadhyay","doi":"10.1016/j.aop.2025.170220","DOIUrl":"10.1016/j.aop.2025.170220","url":null,"abstract":"<div><div>This work presents a unified treatment of Nojiri–Odintsov holographic dark energy, encompassing its Ricci–Gauss–Bonnet realization and a second-order approximation as a particular case of the generalized framework. By incorporating higher-order curvature corrections from the Gauss–Bonnet invariant and the Ricci scalar, we construct an extended HDE model and study the evolution of the equation-of-state parameter in both interacting and non-interacting scenarios. The analysis reveals possible quintessence-to-phantom transitions, with observational validation from cosmic chronometer and <em>Planck</em> 2018 datasets. The outcomes indicate the role of higher-curvature corrections provide a viable description of late-time cosmic acceleration. Finally, within the Ricci–Gauss–Bonnet and Nojiri–Odintsov holographic frameworks, we find that the reconstructed <span><math><mrow><msub><mrow><mi>w</mi></mrow><mrow><mi>tot</mi></mrow></msub><mrow><mo>(</mo><mi>z</mi><mo>)</mo></mrow></mrow></math></span> exhibits the DESI-preferred quintessence–phantom crossing, although the Hubble tension between <em>Planck</em> and SH0ES determinations of <span><math><msub><mrow><mi>H</mi></mrow><mrow><mn>0</mn></mrow></msub></math></span> remains unresolved.</div></div>","PeriodicalId":8249,"journal":{"name":"Annals of Physics","volume":"482 ","pages":"Article 170220"},"PeriodicalIF":3.0,"publicationDate":"2025-09-22","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145155363","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 : 2025-09-19DOI: 10.1016/j.aop.2025.170235
Shagun Kaushal , Sourav Bhattacharya
We investigate the entanglement generation or harvesting between two identical, comoving Unruh–DeWitt detectors in the cosmological de Sitter spacetime. The detectors are assumed to be unentangled initially. They are individually coupled to a complex scalar field, which eventually leads to coupling between themselves. Two kinds of complex scalar fields are investigated here — conformally invariant and massless minimally coupled. By tracing out the degrees of freedom corresponding to the scalar, we construct the reduced density matrix for the two detectors, whose eigenvalues characterise transition probabilities between the energy levels of the detectors. We have computed the negativity, quantifying the degree of entanglement generated at late times between the two detectors. The similarities and differences of these results between the aforementioned two kinds of scalar fields have been discussed. We also compare our results with the existing result of the real scalar field, and point out the qualitative differences. In particular, we emphasise that entanglement harvesting is more resilient in scenarios involving complex fields and nonlinear couplings.
{"title":"Entanglement generation between Unruh–DeWitt detectors in the de Sitter spacetime — Analysis with complex scalar fields","authors":"Shagun Kaushal , Sourav Bhattacharya","doi":"10.1016/j.aop.2025.170235","DOIUrl":"10.1016/j.aop.2025.170235","url":null,"abstract":"<div><div>We investigate the entanglement generation or harvesting between two identical, comoving Unruh–DeWitt detectors in the cosmological de Sitter spacetime. The detectors are assumed to be unentangled initially. They are individually coupled to a complex scalar field, which eventually leads to coupling between themselves. Two kinds of complex scalar fields are investigated here — conformally invariant and massless minimally coupled. By tracing out the degrees of freedom corresponding to the scalar, we construct the reduced density matrix for the two detectors, whose eigenvalues characterise transition probabilities between the energy levels of the detectors. We have computed the negativity, quantifying the degree of entanglement generated at late times between the two detectors. The similarities and differences of these results between the aforementioned two kinds of scalar fields have been discussed. We also compare our results with the existing result of the real scalar field, and point out the qualitative differences. In particular, we emphasise that entanglement harvesting is more resilient in scenarios involving complex fields and nonlinear couplings.</div></div>","PeriodicalId":8249,"journal":{"name":"Annals of Physics","volume":"482 ","pages":"Article 170235"},"PeriodicalIF":3.0,"publicationDate":"2025-09-19","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145099782","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 : 2025-09-18DOI: 10.1016/j.aop.2025.170236
S.L. Lyakhovich, N.A. Sinelnikov
We consider a classical field theory whose equations of motion follow from the least action principle, but the class of admissible trajectories is restricted by differential equations. The key element of the proposed construction is the complete gauge symmetry of these additional equations. The unfree variation of the trajectories reduces to the infinitesimal gauge symmetry transformation of the equations restricting the trajectories. We explicitly derive the equations that follow from the requirement that this gauge variation of the action vanishes. The system of equations for conditional extrema is not a Lagrangian system as such, but it admits an equivalent Hamiltonian formulation with a non-canonical Poisson bracket. The bracket is degenerate, in general. Alternatively, the equations restricting the dynamics could be added to the action with Lagrange multipliers with unrestricted variation of the original variables. In this case, we would arrive at the Lagrangian equations for the original variables involving Lagrange multipliers and for Lagrange multipliers themselves. In general, these two methods are not equivalent because the multipliers can bring extra degrees of freedom compared to the case of equations derived by unfree variation of the action. We illustrate the general method with two examples. The first example is a particle in a central field with varying trajectories restricted by the equation of conservation of angular momentum. The phase space acquires one more dimension, and there is an extra conserved quantity which is responsible for the precession of trajectories. corresponds to the trajectories of usual Lagrangian dynamics. The second example is linearized gravity with the Einstein–Hilbert action, and the class of varying fields is restricted by the linearized Nordström equation. This conditional extrema problem is shown to lead to the linearized Cotton gravity equations.
{"title":"Gauge symmetry and partially Lagrangian systems","authors":"S.L. Lyakhovich, N.A. Sinelnikov","doi":"10.1016/j.aop.2025.170236","DOIUrl":"10.1016/j.aop.2025.170236","url":null,"abstract":"<div><div>We consider a classical field theory whose equations of motion follow from the least action principle, but the class of admissible trajectories is restricted by differential equations. The key element of the proposed construction is the complete gauge symmetry of these additional equations. The unfree variation of the trajectories reduces to the infinitesimal gauge symmetry transformation of the equations restricting the trajectories. We explicitly derive the equations that follow from the requirement that this gauge variation of the action vanishes. The system of equations for conditional extrema is not a Lagrangian system as such, but it admits an equivalent Hamiltonian formulation with a non-canonical Poisson bracket. The bracket is degenerate, in general. Alternatively, the equations restricting the dynamics could be added to the action with Lagrange multipliers with unrestricted variation of the original variables. In this case, we would arrive at the Lagrangian equations for the original variables involving Lagrange multipliers and for Lagrange multipliers themselves. In general, these two methods are not equivalent because the multipliers can bring extra degrees of freedom compared to the case of equations derived by unfree variation of the action. We illustrate the general method with two examples. The first example is a particle in a central field with varying trajectories restricted by the equation of conservation of angular momentum. The phase space acquires one more dimension, and there is an extra conserved quantity <span><math><mi>K</mi></math></span> which is responsible for the precession of trajectories. <span><math><mrow><mi>K</mi><mo>=</mo><mn>0</mn></mrow></math></span> corresponds to the trajectories of usual Lagrangian dynamics. The second example is linearized gravity with the Einstein–Hilbert action, and the class of varying fields is restricted by the linearized Nordström equation. This conditional extrema problem is shown to lead to the linearized Cotton gravity equations.</div></div>","PeriodicalId":8249,"journal":{"name":"Annals of Physics","volume":"482 ","pages":"Article 170236"},"PeriodicalIF":3.0,"publicationDate":"2025-09-18","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145155364","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 : 2025-09-18DOI: 10.1016/j.aop.2025.170230
Madhukrishna Chakraborty , Subenoy Chakraborty
The paper deals with the modified Raychaudhuri equation (RE) and convergence of a congruence of time-like geodesics in anisotropic background. The analysis has been compared and contrasted with the isotropic case. Presence of anisotropy in early universe and its effect in the initial big-bang singularity has been discussed using the Raychaudhuri equation corresponding to shear () and expansion (). Further, the Harmonic oscillator form of the RE has been invoked and effect of anisotropy in convergence has been discussed. Additionally, the effect of anisotropy in determining cosmological dynamics has also been presented using the analytic solution of RE and a justification to Cosmic No Hair conjecture has been given in light of the present analysis. Finally, quantum gravitational aspects by formulating a Wheeler-DeWitt equation based on the anisotropic Raychaudhuri framework has been explored which offers a probabilistic criterion for singularity avoidance and quantum corrections to the cosmic evolution.
{"title":"Anisotropic modifications of Gravitational dynamics: Implications for singularity and Cosmic No-Hair theorem via Raychaudhuri equation","authors":"Madhukrishna Chakraborty , Subenoy Chakraborty","doi":"10.1016/j.aop.2025.170230","DOIUrl":"10.1016/j.aop.2025.170230","url":null,"abstract":"<div><div>The paper deals with the modified Raychaudhuri equation (RE) and convergence of a congruence of time-like geodesics in anisotropic background. The analysis has been compared and contrasted with the isotropic case. Presence of anisotropy in early universe and its effect in the initial big-bang singularity has been discussed using the Raychaudhuri equation corresponding to shear (<span><math><mi>σ</mi></math></span>) and expansion (<span><math><mi>Θ</mi></math></span>). Further, the Harmonic oscillator form of the RE has been invoked and effect of anisotropy in convergence has been discussed. Additionally, the effect of anisotropy in determining cosmological dynamics has also been presented using the analytic solution of RE and a justification to Cosmic No Hair conjecture has been given in light of the present analysis. Finally, quantum gravitational aspects by formulating a Wheeler-DeWitt equation based on the anisotropic Raychaudhuri framework has been explored which offers a probabilistic criterion for singularity avoidance and quantum corrections to the cosmic evolution.</div></div>","PeriodicalId":8249,"journal":{"name":"Annals of Physics","volume":"482 ","pages":"Article 170230"},"PeriodicalIF":3.0,"publicationDate":"2025-09-18","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145099716","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 : 2025-09-18DOI: 10.1016/j.aop.2025.170234
Byron P. Brassel , Sumeekha Singh , Sunil D. Maharaj
We study pressure models in higher dimensional general relativity and Einstein-Gauss–Bonnet (EGB) gravity in a spherically symmetric spacetime. In EGB gravity, we show that the dynamics of the model are governed by an Abel differential equation of the second kind. A general first integral is possible for all values of the spatial curvature, equation of state parameter and spacetime dimension. We further show that an explicit solution is possible for the cosmic scale factor in EGB gravity for the dark energy equation of state. We further demonstrate that for the dark energy equation of state, an anti-de Sitter-Gauss–Bonnet universe is possible, which is not necessarily the case in general relativity. It is also shown that the effective pressure of the Gauss–Bonnet universe contains the higher order curvature corrections and remains, like the general relativity case, negative for all dimensions. The Hawking temperature of the dark Gauss–Bonnet universe is found and is positive and constant for all spatial curvature, and depends critically on the spacetime dimension.
{"title":"Dark equation of state for the Gauss–Bonnet universe","authors":"Byron P. Brassel , Sumeekha Singh , Sunil D. Maharaj","doi":"10.1016/j.aop.2025.170234","DOIUrl":"10.1016/j.aop.2025.170234","url":null,"abstract":"<div><div>We study pressure models in higher dimensional general relativity and Einstein-Gauss–Bonnet (EGB) gravity in a spherically symmetric spacetime. In EGB gravity, we show that the dynamics of the model are governed by an Abel differential equation of the second kind. A general first integral is possible for all values of the spatial curvature, equation of state parameter and spacetime dimension. We further show that an explicit solution is possible for the cosmic scale factor in EGB gravity for the dark energy equation of state. We further demonstrate that for the dark energy equation of state, an anti-de Sitter-Gauss–Bonnet universe is possible, which is not necessarily the case in general relativity. It is also shown that the effective pressure of the Gauss–Bonnet universe contains the higher order curvature corrections and remains, like the general relativity case, negative for all dimensions. The Hawking temperature of the dark Gauss–Bonnet universe is found and is positive and constant for all spatial curvature, and depends critically on the spacetime dimension.</div></div>","PeriodicalId":8249,"journal":{"name":"Annals of Physics","volume":"482 ","pages":"Article 170234"},"PeriodicalIF":3.0,"publicationDate":"2025-09-18","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145118304","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 : 2025-09-18DOI: 10.1016/j.aop.2025.170229
D. Kileba Matondo , T.P. Mafa , S.D. Maharaj
We analyse matter distributions which are anisotropic and satisfy a generalised equation of state in an electromagnetic field. The generalised equation of state reduces to the standard polytrope and quark matter for suitable choices of parameters. New classes of exact solutions to the Einstein–Maxwell system are found for particular choices of the polytropic index. Known exact solutions are regained as special cases. The nonzero electric field has a significant effect on the behaviour of the model and affects the gravitational dynamics. The requirements for a physically acceptable relativistic compact object are satisfied.
{"title":"Charged anisotropic model with generalised polytropic equation of state","authors":"D. Kileba Matondo , T.P. Mafa , S.D. Maharaj","doi":"10.1016/j.aop.2025.170229","DOIUrl":"10.1016/j.aop.2025.170229","url":null,"abstract":"<div><div>We analyse matter distributions which are anisotropic and satisfy a generalised equation of state in an electromagnetic field. The generalised equation of state reduces to the standard polytrope and quark matter for suitable choices of parameters. New classes of exact solutions to the Einstein–Maxwell system are found for particular choices of the polytropic index. Known exact solutions are regained as special cases. The nonzero electric field has a significant effect on the behaviour of the model and affects the gravitational dynamics. The requirements for a physically acceptable relativistic compact object are satisfied.</div></div>","PeriodicalId":8249,"journal":{"name":"Annals of Physics","volume":"482 ","pages":"Article 170229"},"PeriodicalIF":3.0,"publicationDate":"2025-09-18","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145118227","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 : 2025-09-18DOI: 10.1016/j.aop.2025.170231
Manosh T. Manoharan
Cohen, Kaplan, and Nelson’s influential paper established that the UV–IR cut-offs cannot be arbitrarily chosen but are constrained by the relation . Here, we revisit the formulation of the CKN entropy bound and compare it with other bounds. The specific characteristics of each bound are shown to depend on the underlying scaling of entropy. Notably, employing a non-extensive scaling with the von Neumann entropy definition yields a more stringent constraint, , where is the Bekenstein–Hawking entropy. We also clarify distinctions between the IR cut-offs used in these frameworks. Moving to the causal entropy bound, we demonstrate that it categorises the CKN bound as matter-like, the von Neumann bound as radiation-like, and the Bekenstein bound as black hole-like systems when saturated. Emphasising cosmological implications, we confirm the consistency between the bounds and the first laws of horizon thermodynamics. We then analyse the shortcomings in standard Holographic Dark Energy (HDE) models, highlighting the challenges in constructing HDE using . Specifically, using the Hubble function in HDE definitions introduces circular logic, causing dark energy to mimic the second dominant component rather than behaving as matter. We further illustrate that the potential for other IR cut-offs, like the future event horizon in an FLRW background or those involving derivatives of the Hubble function, to explain late-time acceleration stems from an integration constant that cannot be trivially set to zero. In brief, the CKN relation does not assign an arbitrary cosmological constant; it explains why its value is small.
{"title":"Entropy bounds and holographic dark energy: Conflicts and consensus","authors":"Manosh T. Manoharan","doi":"10.1016/j.aop.2025.170231","DOIUrl":"10.1016/j.aop.2025.170231","url":null,"abstract":"<div><div>Cohen, Kaplan, and Nelson’s influential paper established that the UV–IR cut-offs cannot be arbitrarily chosen but are constrained by the relation <span><math><mrow><msup><mrow><mi>Λ</mi></mrow><mrow><mn>2</mn></mrow></msup><mi>L</mi><mo>≲</mo><msub><mrow><mi>M</mi></mrow><mrow><mi>p</mi></mrow></msub></mrow></math></span>. Here, we revisit the formulation of the CKN entropy bound and compare it with other bounds. The specific characteristics of each bound are shown to depend on the underlying scaling of entropy. Notably, employing a non-extensive scaling with the von Neumann entropy definition yields a more stringent constraint, <span><math><mrow><msub><mrow><mi>S</mi></mrow><mrow><mtext>max</mtext></mrow></msub><mo>≈</mo><msqrt><mrow><msub><mrow><mi>S</mi></mrow><mrow><mtext>BH</mtext></mrow></msub></mrow></msqrt></mrow></math></span>, where <span><math><msub><mrow><mi>S</mi></mrow><mrow><mtext>BH</mtext></mrow></msub></math></span> is the Bekenstein–Hawking entropy. We also clarify distinctions between the IR cut-offs used in these frameworks. Moving to the causal entropy bound, we demonstrate that it categorises the CKN bound as matter-like, the von Neumann bound as radiation-like, and the Bekenstein bound as black hole-like systems when saturated. Emphasising cosmological implications, we confirm the consistency between the bounds and the first laws of horizon thermodynamics. We then analyse the shortcomings in standard Holographic Dark Energy (HDE) models, highlighting the challenges in constructing HDE using <span><math><mrow><msup><mrow><mi>Λ</mi></mrow><mrow><mn>2</mn></mrow></msup><mi>L</mi><mo>≲</mo><msub><mrow><mi>M</mi></mrow><mrow><mi>p</mi></mrow></msub></mrow></math></span>. Specifically, using the Hubble function in HDE definitions introduces circular logic, causing dark energy to mimic the second dominant component rather than behaving as matter. We further illustrate that the potential for other IR cut-offs, like the future event horizon in an FLRW background or those involving derivatives of the Hubble function, to explain late-time acceleration stems from an integration constant that cannot be trivially set to zero. In brief, the CKN relation does not assign an arbitrary cosmological constant; it explains why its value is small.</div></div>","PeriodicalId":8249,"journal":{"name":"Annals of Physics","volume":"482 ","pages":"Article 170231"},"PeriodicalIF":3.0,"publicationDate":"2025-09-18","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145099717","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 : 2025-09-17DOI: 10.1016/j.aop.2025.170227
Yuan Xiang, Rui Guo
In this paper, we consider wave breaking problem for the photon fluid propagating along a stationary medium with its profile characterized by a cubic root shape with account of third-order dispersion and self-steepening effects. Using the finite-band integral method and averaging conservation laws, we derive the periodic solution and the corresponding Whitham equation, respectively. Based on Whitham modulation theory, the dispersive shock wave (DSW) can be approximately represented as a modulated periodic solution with correct phase shift. The motion laws of the DSW at the soliton edge and small-amplitude edge can be analyzed separately. Furthermore, utilizing time reversibility, wave-breaking phenomena and wave structures are explored across distinct parameter spaces of and in the optical field. Additionally, the impacts of the third-order dispersion and self-steepening effects — both governed by — on the evolution of wave structures are examined.
{"title":"The general cubic wave breaking problem for the photon fluid: Third-order dispersion and self-steepening effects","authors":"Yuan Xiang, Rui Guo","doi":"10.1016/j.aop.2025.170227","DOIUrl":"10.1016/j.aop.2025.170227","url":null,"abstract":"<div><div>In this paper, we consider wave breaking problem for the photon fluid propagating along a stationary medium with its profile characterized by a cubic root shape with account of third-order dispersion and self-steepening effects. Using the finite-band integral method and averaging conservation laws, we derive the periodic solution and the corresponding Whitham equation, respectively. Based on Whitham modulation theory, the dispersive shock wave (DSW) can be approximately represented as a modulated periodic solution with correct phase shift. The motion laws of the DSW at the soliton edge and small-amplitude edge can be analyzed separately. Furthermore, utilizing time reversibility, wave-breaking phenomena and wave structures are explored across distinct parameter spaces of <span><math><mi>α</mi></math></span> and <span><math><mi>β</mi></math></span> in the optical field. Additionally, the impacts of the third-order dispersion and self-steepening effects — both governed by <span><math><mi>β</mi></math></span> — on the evolution of wave structures are examined.</div></div>","PeriodicalId":8249,"journal":{"name":"Annals of Physics","volume":"482 ","pages":"Article 170227"},"PeriodicalIF":3.0,"publicationDate":"2025-09-17","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145099715","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 : 2025-09-15DOI: 10.1016/j.aop.2025.170226
Said Lantigua , Jonas Maziero
This paper develops a geometrodynamic extension of Bohmian mechanics to describe quantum tunneling through a potential barrier, treating particle trajectories as geodesics in an Alcubierre-type spacetime. The model provides analytical expressions for the quantum potential, particle dynamics, and tunneling time, explicitly linked to the underlying spacetime geometry. For narrow barriers, the tunneling time depends on the barrier width, while for sufficiently wide barriers, it saturates to a constant value—recovering the Hartman effect. This behavior arises from a geometric self-regulation mechanism, where the quantum potential dynamically adjusts the spacetime distortion to maintain a fixed tunneling time, consistent with relativistic causality despite effective superluminal propagation. The results establish a direct connection between quantum tunneling and spacetime geometry, offering a unified framework to interpret the Hartman effect. This approach naturally incorporates relativistic constraints while suggesting that similar geometric mechanisms may underlie other quantum phenomena, such as topological phases in condensed matter systems.
{"title":"Hartman effect from a geometrodynamic extension of Bohmian mechanics","authors":"Said Lantigua , Jonas Maziero","doi":"10.1016/j.aop.2025.170226","DOIUrl":"10.1016/j.aop.2025.170226","url":null,"abstract":"<div><div>This paper develops a geometrodynamic extension of Bohmian mechanics to describe quantum tunneling through a potential barrier, treating particle trajectories as geodesics in an Alcubierre-type spacetime. The model provides analytical expressions for the quantum potential, particle dynamics, and tunneling time, explicitly linked to the underlying spacetime geometry. For narrow barriers, the tunneling time depends on the barrier width, while for sufficiently wide barriers, it saturates to a constant value—recovering the Hartman effect. This behavior arises from a geometric self-regulation mechanism, where the quantum potential dynamically adjusts the spacetime distortion to maintain a fixed tunneling time, consistent with relativistic causality despite effective superluminal propagation. The results establish a direct connection between quantum tunneling and spacetime geometry, offering a unified framework to interpret the Hartman effect. This approach naturally incorporates relativistic constraints while suggesting that similar geometric mechanisms may underlie other quantum phenomena, such as topological phases in condensed matter systems.</div></div>","PeriodicalId":8249,"journal":{"name":"Annals of Physics","volume":"482 ","pages":"Article 170226"},"PeriodicalIF":3.0,"publicationDate":"2025-09-15","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145217181","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 : 2025-09-14DOI: 10.1016/j.aop.2025.170225
Meng-Dong Zhu , Yu-Hao Wang , Shi-Pu Gu , Xing-Fu Wang , Lan Zhou , Yu-Bo Sheng
Multipartite high-dimensional entanglement offers a larger space for storing and processing quantum information and is the crucial resource in future high-capacity and high-security quantum networks. The high-efficiency generation of multipartite high-dimensional entanglement is of central importance for its application. In the paper, we propose a recyclable generation protocol for the four-photon three-dimensional spatial-path Greenberger–Horne–Zeilinger (GHZ) state with linear optical elements and practical “on-off” photon detectors. Our protocol is feasible under current experimental conditions, and the generated three-dimensional GHZ state can be preserved for applications. When the generation protocol fails, the output state may evolve into the auxiliary state for the next generation round. In this way, our protocol can effectively save precious EPR resources. With the increase of repeating number, our protocol will have a prominent advantage in saving precious entanglement resources. Our protocol can provide effective guidance for the experimental preparation of the three-dimensional spatial-path GHZ state, and has important application in future multipartite high-dimensional quantum networks.
{"title":"Efficient recyclable generation protocol for high-dimensional spatial-path GHZ states","authors":"Meng-Dong Zhu , Yu-Hao Wang , Shi-Pu Gu , Xing-Fu Wang , Lan Zhou , Yu-Bo Sheng","doi":"10.1016/j.aop.2025.170225","DOIUrl":"10.1016/j.aop.2025.170225","url":null,"abstract":"<div><div>Multipartite high-dimensional entanglement offers a larger space for storing and processing quantum information and is the crucial resource in future high-capacity and high-security quantum networks. The high-efficiency generation of multipartite high-dimensional entanglement is of central importance for its application. In the paper, we propose a recyclable generation protocol for the four-photon three-dimensional spatial-path Greenberger–Horne–Zeilinger (GHZ) state with linear optical elements and practical “on-off” photon detectors. Our protocol is feasible under current experimental conditions, and the generated three-dimensional GHZ state can be preserved for applications. When the generation protocol fails, the output state may evolve into the auxiliary state for the next generation round. In this way, our protocol can effectively save precious EPR resources. With the increase of repeating number, our protocol will have a prominent advantage in saving precious entanglement resources. Our protocol can provide effective guidance for the experimental preparation of the three-dimensional spatial-path GHZ state, and has important application in future multipartite high-dimensional quantum networks.</div></div>","PeriodicalId":8249,"journal":{"name":"Annals of Physics","volume":"482 ","pages":"Article 170225"},"PeriodicalIF":3.0,"publicationDate":"2025-09-14","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145099713","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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