In the framework of gravity, where gravity emerges from non-metricity , we explore the cosmological implications of its non-minimal coupling to matter. Inspired by the recent success of Chaplygin gas models in explaining dark energy, we consider a background fluid composed of baryonic matter, radiation, and a family of Chaplygin gas variants namely Generalized Chaplygin Gas (GCG), Modified Chaplygin Gas (MCG), and Variable Chaplygin Gas (VCG). We constrain these models with three recent observational datasets: Observational Hubble Data (OHD), Baryonic Acoustic Oscillation (BAO) measurements, and Quasi-Stellar Objects (QSO) data. For the QSO dataset, we propose an analytical expression for errors in comoving distance to circumvent the reliance on Monte Carlo simulations. Using kinematic diagnostics such as the deceleration and jerk parameters and Om diagnostic, we assess deviations of the proposed models from CDM. Our joint analysis of the three datasets reveals that the transition redshift from a decelerated to an accelerated expansion of the universe for the GCG, MCG and VCG models is , and respectively, indicating a departure from CDM.
{"title":"Observational constraints on Chaplygin gas models in non-minimally coupled power law f(Q) gravity with quasars","authors":"Nakul Aggarwal , Ali Pourmand , Fatimah Shojai , Harish Parthasarathy","doi":"10.1016/j.aop.2025.170266","DOIUrl":"10.1016/j.aop.2025.170266","url":null,"abstract":"<div><div>In the framework of <span><math><mrow><mi>f</mi><mrow><mo>(</mo><mi>Q</mi><mo>)</mo></mrow></mrow></math></span> gravity, where gravity emerges from non-metricity <span><math><mi>Q</mi></math></span>, we explore the cosmological implications of its non-minimal coupling to matter. Inspired by the recent success of Chaplygin gas models in explaining dark energy, we consider a background fluid composed of baryonic matter, radiation, and a family of Chaplygin gas variants namely Generalized Chaplygin Gas (GCG), Modified Chaplygin Gas (MCG), and Variable Chaplygin Gas (VCG). We constrain these models with three recent observational datasets: Observational Hubble Data (OHD), Baryonic Acoustic Oscillation (BAO) measurements, and Quasi-Stellar Objects (QSO) data. For the QSO dataset, we propose an analytical expression for errors in comoving distance to circumvent the reliance on Monte Carlo simulations. Using kinematic diagnostics such as the deceleration and jerk parameters and Om diagnostic, we assess deviations of the proposed models from <span><math><mi>Λ</mi></math></span>CDM. Our joint analysis of the three datasets reveals that the transition redshift from a decelerated to an accelerated expansion of the universe for the GCG, MCG and VCG models is <span><math><mrow><mn>0</mn><mo>.</mo><mn>62</mn><msubsup><mrow><mn>0</mn></mrow><mrow><mo>−</mo><mn>0</mn><mo>.</mo><mn>017</mn></mrow><mrow><mo>+</mo><mn>0</mn><mo>.</mo><mn>018</mn></mrow></msubsup></mrow></math></span>, <span><math><mrow><mn>0</mn><mo>.</mo><mn>53</mn><msubsup><mrow><mn>7</mn></mrow><mrow><mo>−</mo><mn>0</mn><mo>.</mo><mn>017</mn></mrow><mrow><mo>+</mo><mn>0</mn><mo>.</mo><mn>017</mn></mrow></msubsup></mrow></math></span> and <span><math><mrow><mn>0</mn><mo>.</mo><mn>47</mn><msubsup><mrow><mn>0</mn></mrow><mrow><mo>−</mo><mn>0</mn><mo>.</mo><mn>012</mn></mrow><mrow><mo>+</mo><mn>0</mn><mo>.</mo><mn>012</mn></mrow></msubsup></mrow></math></span> respectively, indicating a departure from <span><math><mi>Λ</mi></math></span>CDM.</div></div>","PeriodicalId":8249,"journal":{"name":"Annals of Physics","volume":"483 ","pages":"Article 170266"},"PeriodicalIF":3.0,"publicationDate":"2025-12-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145360159","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 : 2025-12-01Epub Date: 2025-11-01DOI: 10.1016/j.aop.2025.170277
S. Habib Mazharimousavi
Motivated by developments in Loop Quantum Cosmology (LQC) and quantum-corrected black holes, we propose a cosmological black/white hole model in which a traveler can enter a black hole and emerge from a white hole without ever encountering a singularity. Our construction is based on the Reissner–Nordström (RN) black hole, which naturally possesses a timelike singularity. By employing the thin-shell wormhole (TSW) formalism, we demonstrate how the interior can be surgically modified to connect a black hole region to a white hole region. We analyze the junction conditions and identify the exotic surface matter required at the throat. Furthermore, we investigate the stability of the throat under linear mechanical perturbations and show that stability is achievable for throat radii smaller than a critical value. Our results illustrate, at a phenomenological level, the feasibility of constructing nonsingular black/white hole transitions, shedding light on possible quantum-gravity inspired alternatives to classical singularities.
{"title":"From black hole to white hole via thin-shell wormhole","authors":"S. Habib Mazharimousavi","doi":"10.1016/j.aop.2025.170277","DOIUrl":"10.1016/j.aop.2025.170277","url":null,"abstract":"<div><div>Motivated by developments in Loop Quantum Cosmology (LQC) and quantum-corrected black holes, we propose a cosmological black/white hole model in which a traveler can enter a black hole and emerge from a white hole without ever encountering a singularity. Our construction is based on the Reissner–Nordström (RN) black hole, which naturally possesses a timelike singularity. By employing the thin-shell wormhole (TSW) formalism, we demonstrate how the interior can be surgically modified to connect a black hole region to a white hole region. We analyze the junction conditions and identify the exotic surface matter required at the throat. Furthermore, we investigate the stability of the throat under linear mechanical perturbations and show that stability is achievable for throat radii smaller than a critical value. Our results illustrate, at a phenomenological level, the feasibility of constructing nonsingular black/white hole transitions, shedding light on possible quantum-gravity inspired alternatives to classical singularities.</div></div>","PeriodicalId":8249,"journal":{"name":"Annals of Physics","volume":"483 ","pages":"Article 170277"},"PeriodicalIF":3.0,"publicationDate":"2025-12-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145463423","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 : 2025-12-01Epub Date: 2025-10-10DOI: 10.1016/j.aop.2025.170245
Ratul Mandal , Ujjal Debnath , Anirudh Pradhan
In theoretical cosmology, symmetric teleparallel gravity or gravity based on nonmetricity tensor has become an interesting alternative to General relativity in recent years. The present research paper contains a rigorous dynamical system analysis of coincident gravity in the presence of a generalized DBI essence scalar field. We have considered two different models of coincident gravity, such as power law model and exponential model respectively, where are constant parameter and is the nonmetricity component. In this study, the generalized DBI essence scalar field acts as an additional dark energy component. After obtaining the field equation for the corresponding cosmological model, we employed several dynamical variables to form the dynamical system. The critical points of these dynamical systems are influenced by cosmological parameters and associated with particular epochs in the cosmological timeline. For different combinations of cosmological parameters, the critical points exhibit different cosmological eras, starting from the accelerated stiff matter era to late-time acceleration phenomena. The stability criteria of each critical point are studied by using linear stability theory, and the physical constraints on the cosmological parameters are also considered during this analysis. Furthermore, the current values of energy densities, deceleration parameters, and equation of state parameters obtained from the evolution diagram are compatible with observational data.
{"title":"Exploring the dynamics of coincident f(Q) gravity in the presence of DBI-essence scalar field","authors":"Ratul Mandal , Ujjal Debnath , Anirudh Pradhan","doi":"10.1016/j.aop.2025.170245","DOIUrl":"10.1016/j.aop.2025.170245","url":null,"abstract":"<div><div>In theoretical cosmology, symmetric teleparallel gravity or <span><math><mrow><mi>f</mi><mrow><mo>(</mo><mi>Q</mi><mo>)</mo></mrow></mrow></math></span> gravity based on nonmetricity tensor <span><math><mi>Q</mi></math></span> has become an interesting alternative to General relativity in recent years. The present research paper contains a rigorous dynamical system analysis of coincident <span><math><mrow><mi>f</mi><mrow><mo>(</mo><mi>Q</mi><mo>)</mo></mrow></mrow></math></span> gravity in the presence of a generalized DBI essence scalar field. We have considered two different models of coincident <span><math><mrow><mi>f</mi><mrow><mo>(</mo><mi>Q</mi><mo>)</mo></mrow></mrow></math></span> gravity, such as power law model <span><math><mrow><mi>f</mi><mrow><mo>(</mo><mi>Q</mi><mo>)</mo></mrow><mo>=</mo><mi>Q</mi><mo>+</mo><mi>n</mi><msup><mrow><mi>Q</mi></mrow><mrow><mi>m</mi></mrow></msup></mrow></math></span> and exponential model <span><math><mrow><mi>f</mi><mrow><mo>(</mo><mi>Q</mi><mo>)</mo></mrow><mo>=</mo><mi>Q</mi><msup><mrow><mi>e</mi></mrow><mrow><mfrac><mrow><mi>β</mi><msub><mrow><mi>Q</mi></mrow><mrow><mn>0</mn></mrow></msub></mrow><mrow><mi>Q</mi></mrow></mfrac></mrow></msup></mrow></math></span> respectively, where <span><math><mrow><mi>n</mi><mo>,</mo><mi>m</mi><mo>,</mo><mi>β</mi></mrow></math></span> are constant parameter and <span><math><mi>Q</mi></math></span> is the nonmetricity component. In this study, the generalized DBI essence scalar field acts as an additional dark energy component. After obtaining the field equation for the corresponding cosmological model, we employed several dynamical variables to form the dynamical system. The critical points of these dynamical systems are influenced by cosmological parameters and associated with particular epochs in the cosmological timeline. For different combinations of cosmological parameters, the critical points exhibit different cosmological eras, starting from the accelerated stiff matter era to late-time acceleration phenomena. The stability criteria of each critical point are studied by using linear stability theory, and the physical constraints on the cosmological parameters are also considered during this analysis. Furthermore, the current values of energy densities, deceleration parameters, and equation of state parameters obtained from the evolution diagram are compatible with observational data.</div></div>","PeriodicalId":8249,"journal":{"name":"Annals of Physics","volume":"483 ","pages":"Article 170245"},"PeriodicalIF":3.0,"publicationDate":"2025-12-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145322984","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 : 2025-12-01Epub Date: 2025-10-21DOI: 10.1016/j.aop.2025.170271
Cristiano Rosa , Sergio Giardino
Within this article one finds the statement of the Klein–Gordon problem within the real Hilbert space formalism (HS) in terms of complex wave functions, and in terms of quaternionic wave functions as well. The complex formulation comprises hermitian and non-hermitian cases, while the quaternionic solutions additionally set in motion self-interacting particles. The non-hermitian cases comprise non-conservative processes, while the self-interaction physically implies the increase of the effective mass of the particle, an effect that cannot be reproduced using a complex wave function. The obtained autonomous particle solutions, as well as the Klein problem agree to the previously discovered self-interacting non-relativistic particle, and thus reinforce HS as viable and consistent way to explore open problems in quantum mechanics. Also important, the negative energy problem that plagues the usual formalism is eliminated within this approach.
{"title":"Klein–Gordon equation within the real Hilbert space formalism","authors":"Cristiano Rosa , Sergio Giardino","doi":"10.1016/j.aop.2025.170271","DOIUrl":"10.1016/j.aop.2025.170271","url":null,"abstract":"<div><div>Within this article one finds the statement of the Klein–Gordon problem within the real Hilbert space formalism (<span><math><mi>R</mi></math></span>HS) in terms of complex wave functions, and in terms of quaternionic wave functions as well. The complex formulation comprises hermitian and non-hermitian cases, while the quaternionic solutions additionally set in motion self-interacting particles. The non-hermitian cases comprise non-conservative processes, while the self-interaction physically implies the increase of the effective mass of the particle, an effect that cannot be reproduced using a complex wave function. The obtained autonomous particle solutions, as well as the Klein problem agree to the previously discovered self-interacting non-relativistic particle, and thus reinforce <span><math><mi>R</mi></math></span>HS as viable and consistent way to explore open problems in quantum mechanics. Also important, the negative energy problem that plagues the usual formalism is eliminated within this approach.</div></div>","PeriodicalId":8249,"journal":{"name":"Annals of Physics","volume":"483 ","pages":"Article 170271"},"PeriodicalIF":3.0,"publicationDate":"2025-12-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145413806","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 theory of gravity, gravitational effect arises from non-metricity which controls how measurements of time and distance evolve over space–time. If a clock or a ruler is moved around in a space–time with nonzero , it would change the size or the ticking rate even if curvature and torsion are zero. This change comes purely from how the metric varies, not from bending (curvature) or twisting (torsion). Four models of theory of gravity are chosen
: , , and .
Equation of continuity and Friedmann equations are modified for these theories. Phase portraits are drawn with proper marking towards the fixed points. Physical interpretation of every such critical points along with center manifold analysis is pursued. Cosmological perspectives to obtain such critical points are presented for each model.
{"title":"Critical points and their cosmological interpretations for some f(Q) gravity theory models","authors":"Subhajit Pal , Atanu Mukherjee , Ritabrata Biswas , Farook Rahaman","doi":"10.1016/j.aop.2025.170272","DOIUrl":"10.1016/j.aop.2025.170272","url":null,"abstract":"<div><div>In <span><math><mrow><mi>f</mi><mrow><mo>(</mo><mi>Q</mi><mo>)</mo></mrow></mrow></math></span> theory of gravity, gravitational effect arises from non-metricity which controls how measurements of time and distance evolve over space–time. If a clock or a ruler is moved around in a space–time with nonzero <span><math><mi>Q</mi></math></span>, it would change the size or the ticking rate even if curvature and torsion are zero. This change comes purely from how the metric varies, not from bending (curvature) or twisting (torsion). Four models of <span><math><mrow><mi>f</mi><mrow><mo>(</mo><mi>Q</mi><mo>)</mo></mrow></mrow></math></span> theory of gravity are chosen</div><div>: <span><math><mrow><msup><mrow><mi>f</mi></mrow><mrow><mrow><mo>(</mo><mn>1</mn><mo>)</mo></mrow></mrow></msup><mrow><mo>(</mo><mi>Q</mi><mo>)</mo></mrow><mo>=</mo><mi>Q</mi><mo>+</mo><mi>m</mi><msup><mrow><mi>Q</mi></mrow><mrow><mi>n</mi></mrow></msup></mrow></math></span>, <span><math><mrow><msup><mrow><mi>f</mi></mrow><mrow><mrow><mo>(</mo><mn>2</mn><mo>)</mo></mrow></mrow></msup><mrow><mo>(</mo><mi>Q</mi><mo>)</mo></mrow><mo>=</mo><mi>Q</mi><msup><mrow><mi>e</mi></mrow><mrow><mfrac><mrow><mi>λ</mi></mrow><mrow><mi>Q</mi></mrow></mfrac></mrow></msup></mrow></math></span>, <span><math><mrow><msup><mrow><mi>f</mi></mrow><mrow><mrow><mo>(</mo><mn>3</mn><mo>)</mo></mrow></mrow></msup><mrow><mo>(</mo><mi>Q</mi><mo>)</mo></mrow><mo>=</mo><mi>Q</mi><mo>+</mo><mi>α</mi><msup><mrow><mi>Q</mi></mrow><mrow><mn>2</mn></mrow></msup><mo>+</mo><mi>v</mi><msup><mrow><mi>Q</mi></mrow><mrow><mn>2</mn></mrow></msup><mo>log</mo><mi>Q</mi></mrow></math></span> and <span><math><mrow><msup><mrow><mi>f</mi></mrow><mrow><mrow><mo>(</mo><mn>4</mn><mo>)</mo></mrow></mrow></msup><mrow><mo>(</mo><mi>Q</mi><mo>)</mo></mrow><mo>=</mo><mi>Q</mi><mo>+</mo><mi>n</mi><msub><mrow><mi>Q</mi></mrow><mrow><mn>0</mn></mrow></msub><mfenced><mrow><msqrt><mrow><mfrac><mrow><mi>Q</mi></mrow><mrow><mi>λ</mi></mrow></mfrac></mrow></msqrt></mrow></mfenced><mo>log</mo><mfenced><mrow><mfrac><mrow><mi>λ</mi><msub><mrow><mi>Q</mi></mrow><mrow><mn>0</mn></mrow></msub></mrow><mrow><mi>Q</mi></mrow></mfrac></mrow></mfenced></mrow></math></span>.</div><div>Equation of continuity and Friedmann equations are modified for these theories. Phase portraits are drawn with proper marking towards the fixed points. Physical interpretation of every such critical points along with center manifold analysis is pursued. Cosmological perspectives to obtain such critical points are presented for each model.</div></div>","PeriodicalId":8249,"journal":{"name":"Annals of Physics","volume":"483 ","pages":"Article 170272"},"PeriodicalIF":3.0,"publicationDate":"2025-12-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145413808","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 explore the impact of the interacting parameter on dark matter in a model resulting from a parametrization of dark energy density. To ensure a model-independent approach, we treat as a free parameter, avoiding assumptions about the physics of the early Universe or specific recombination models. This approach allows late-time cosmological observations to directly constrain along with other parameters. Using recent measurements from the Dark Energy Spectroscopic Instrument (DESI) Year 1, cosmic chronometers (CC) and Pantheon supernova (SNe Ia) data, we uncover a significant effect of the interacting parameter on dark matter. Our analysis reveals that while non-interacting models attribute 68.2% of the cosmic energy density to dark energy, interacting models increase this share to 73.4%. To further probe these differences, we evaluate the evolution of the deceleration parameter for each model, contrasting them against the CDM paradigm and observational data from CC and SNe Ia measurements. Finally, we apply various statistical metrics to rigorously assess the performance of these models.
{"title":"Dark sector interactions: Probing the Hubble parameter and the sound horizon","authors":"Ritika Nagpal , S.K.J. Pacif , Farruh Atamurotov , Rasmikanta Pati","doi":"10.1016/j.aop.2025.170249","DOIUrl":"10.1016/j.aop.2025.170249","url":null,"abstract":"<div><div>In this study, we explore the impact of the interacting parameter on dark matter in a model resulting from a parametrization of dark energy density. To ensure a model-independent approach, we treat <span><math><msub><mrow><mi>r</mi></mrow><mrow><mi>d</mi></mrow></msub></math></span> as a free parameter, avoiding assumptions about the physics of the early Universe or specific recombination models. This approach allows late-time cosmological observations to directly constrain <span><math><msub><mrow><mi>r</mi></mrow><mrow><mi>d</mi></mrow></msub></math></span> along with other parameters. Using recent measurements from the Dark Energy Spectroscopic Instrument (DESI) Year 1, cosmic chronometers (CC) and Pantheon<span><math><msup><mrow></mrow><mrow><mo>+</mo></mrow></msup></math></span> supernova (SNe Ia) data, we uncover a significant effect of the interacting parameter on dark matter. Our analysis reveals that while non-interacting models attribute 68.2% of the cosmic energy density to dark energy, interacting models increase this share to 73.4%. To further probe these differences, we evaluate the evolution of the deceleration parameter for each model, contrasting them against the <span><math><mi>Λ</mi></math></span>CDM paradigm and observational data from CC and SNe Ia measurements. Finally, we apply various statistical metrics to rigorously assess the performance of these models.</div></div>","PeriodicalId":8249,"journal":{"name":"Annals of Physics","volume":"483 ","pages":"Article 170249"},"PeriodicalIF":3.0,"publicationDate":"2025-12-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145360157","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}
This study investigates the effects of Hawking radiation on tripartite quantum coherence and tripartite entropy uncertainty measurement in the context of a Schwarzschild black hole. Two main cases are examined, each encompassing three distinct scenarios: one involving only accessible modes (particles outside the event horizon), another involving only inaccessible modes (antiparticles inside the event horizon), and a third involving both accessible and inaccessible modes. Results show that in scenarios with accessible modes, tripartite quantum coherence decreases monotonically with increasing Hawking temperature, while tripartite entropy uncertainty measurement rises. Conversely, when inaccessible modes are present, Hawking radiation generates quantum coherence and reduces entropy uncertainty measurement. This suggests that quantum coherence and measurement uncertainty can be transmitted or distributed across different regions of spacetime, even across the event horizon of a black hole, indicating an interconnection of quantum properties despite the horizon’s role as a boundary.
{"title":"The effect of Hawking radiation on tripartite entropic uncertainty and tripartite Quantum coherence in Schwarzschild spacetime","authors":"Wajid Joyia , Asif Ilyas , Mahtab A. Khan , Nahaa Eid Alsubaie , Amaria Javed","doi":"10.1016/j.aop.2025.170269","DOIUrl":"10.1016/j.aop.2025.170269","url":null,"abstract":"<div><div>This study investigates the effects of Hawking radiation on tripartite quantum coherence and tripartite entropy uncertainty measurement in the context of a Schwarzschild black hole. Two main cases are examined, each encompassing three distinct scenarios: one involving only accessible modes (particles outside the event horizon), another involving only inaccessible modes (antiparticles inside the event horizon), and a third involving both accessible and inaccessible modes. Results show that in scenarios with accessible modes, tripartite quantum coherence decreases monotonically with increasing Hawking temperature, while tripartite entropy uncertainty measurement rises. Conversely, when inaccessible modes are present, Hawking radiation generates quantum coherence and reduces entropy uncertainty measurement. This suggests that quantum coherence and measurement uncertainty can be transmitted or distributed across different regions of spacetime, even across the event horizon of a black hole, indicating an interconnection of quantum properties despite the horizon’s role as a boundary.</div></div>","PeriodicalId":8249,"journal":{"name":"Annals of Physics","volume":"483 ","pages":"Article 170269"},"PeriodicalIF":3.0,"publicationDate":"2025-12-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145463424","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 : 2025-12-01Epub Date: 2025-10-11DOI: 10.1016/j.aop.2025.170247
Jiadu Lin, Qing-Dong Jiang
We study the ponderomotive potential of a bosonic Josephson junction periodically modulated by a high-frequency electromagnetic field. Within the small population difference approximation, the ponderomotive drive induces the well-known Kapitza pendulum effect, stabilizing a -phase mode. We discuss the parameter dependence of the dynamical transition from macroscopic quantum self-trapping to -Josephson oscillations. Furthermore, we examine the situation where the small population difference approximation fails. In this case, an essential momentum-shortening effect emerges, leading to a stabilized -phase mode under certain conditions. By mapping this to a classical pendulum scenario, we highlight the uniqueness and limitations of the -phase mode in bosonic Josephson junctions.
{"title":"Engineering ponderomotive potential for realizing π and π/2 Bosonic Josephson junctions","authors":"Jiadu Lin, Qing-Dong Jiang","doi":"10.1016/j.aop.2025.170247","DOIUrl":"10.1016/j.aop.2025.170247","url":null,"abstract":"<div><div>We study the ponderomotive potential of a bosonic Josephson junction periodically modulated by a high-frequency electromagnetic field. Within the small population difference approximation, the ponderomotive drive induces the well-known Kapitza pendulum effect, stabilizing a <span><math><mi>π</mi></math></span>-phase mode. We discuss the parameter dependence of the dynamical transition from macroscopic quantum self-trapping to <span><math><mi>π</mi></math></span>-Josephson oscillations. Furthermore, we examine the situation where the small population difference approximation fails. In this case, an essential momentum-shortening effect emerges, leading to a stabilized <span><math><mrow><mi>π</mi><mo>/</mo><mn>2</mn></mrow></math></span>-phase mode under certain conditions. By mapping this to a classical pendulum scenario, we highlight the uniqueness and limitations of the <span><math><mrow><mi>π</mi><mo>/</mo><mn>2</mn></mrow></math></span>-phase mode in bosonic Josephson junctions.</div></div>","PeriodicalId":8249,"journal":{"name":"Annals of Physics","volume":"483 ","pages":"Article 170247"},"PeriodicalIF":3.0,"publicationDate":"2025-12-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145322986","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 : 2025-12-01Epub Date: 2025-10-11DOI: 10.1016/j.aop.2025.170258
J. Aldair Pantoja-González, D. Vanessa Castro-Luna, Alberto Escalante
A detailed Hamilton–Jacobi analysis for linearized gravity is developed. The model is constructed by rewriting linearized gravity in terms of a parameter and new variables. The set of all hamiltonians is identified successfully, and the fundamental differential is established. The non-involutive hamiltonians are eliminated, and the Hamilton–Jacobi generalized brackets are calculated. Such brackets are used to report the characteristic equations, and the counting of the number of degrees of freedom is performed. We fixed the gauge to indicate an intimate closeness between the model under study and linearized gravity.
{"title":"Characteristic equations of linearized λR gravity","authors":"J. Aldair Pantoja-González, D. Vanessa Castro-Luna, Alberto Escalante","doi":"10.1016/j.aop.2025.170258","DOIUrl":"10.1016/j.aop.2025.170258","url":null,"abstract":"<div><div>A detailed Hamilton–Jacobi analysis for linearized <span><math><mrow><mi>λ</mi><mi>R</mi></mrow></math></span> gravity is developed. The model is constructed by rewriting linearized gravity in terms of a parameter <span><math><mi>λ</mi></math></span> and new variables. The set of all hamiltonians is identified successfully, and the fundamental differential is established. The non-involutive hamiltonians are eliminated, and the Hamilton–Jacobi generalized brackets are calculated. Such brackets are used to report the characteristic equations, and the counting of the number of degrees of freedom is performed. We fixed the gauge to indicate an intimate closeness between the model under study and linearized gravity.</div></div>","PeriodicalId":8249,"journal":{"name":"Annals of Physics","volume":"483 ","pages":"Article 170258"},"PeriodicalIF":3.0,"publicationDate":"2025-12-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145322985","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 paper, we construct an isotropic cosmological model in the theory of gravity in the frame of a flat FLRW spacetime, with the non-metricity tensor and the trace of the energy–momentum tensor. The gravity function is taken to be a quadratic equation, , where and are the arbitrary constants. We constrain the model parameters arising while solving the deceleration parameter as an integration constant together with the present value of the Hubble parameter using the Hubble datasets (OHD), the of 1048 data points, and the joint datasets (OHD + ). The universe model transitions from an early deceleration state to an acceleration in late times. This model also provides the ekpyrotic phase of the universe on the redshift . In this model, the Big Bang is described as a collision of branes, and thus, the Big Bang is not the beginning of time. Before the Big Bang, there is an ekpyrotic phase with the equation of state . In late times, the undeviating Hubble measurements reduce the tension in the reconstructed function. Additionally, we study various physical parameters of the model. Finally, our model describes a quintessence dark energy model at later times.
{"title":"Cosmic reverberations on a constrained f(Q,T)-model of the Universe","authors":"Akanksha Singh , Shaily , J.K. Singh , Ertan Güdekli","doi":"10.1016/j.aop.2025.170274","DOIUrl":"10.1016/j.aop.2025.170274","url":null,"abstract":"<div><div>In this paper, we construct an isotropic cosmological model in the <span><math><mrow><mi>f</mi><mrow><mo>(</mo><mi>Q</mi><mo>,</mo><mi>T</mi><mo>)</mo></mrow></mrow></math></span> theory of gravity in the frame of a flat FLRW spacetime, with <span><math><mi>Q</mi></math></span> the non-metricity tensor and <span><math><mi>T</mi></math></span> the trace of the energy–momentum tensor. The gravity function is taken to be a quadratic equation, <span><math><mrow><mi>f</mi><mrow><mo>(</mo><mi>Q</mi><mo>,</mo><mi>T</mi><mo>)</mo></mrow><mo>=</mo><mi>ζ</mi><msup><mrow><mi>Q</mi></mrow><mrow><mn>2</mn></mrow></msup><mo>+</mo><mi>γ</mi><mi>T</mi></mrow></math></span>, where <span><math><mrow><mi>ζ</mi><mo><</mo><mn>0</mn></mrow></math></span> and <span><math><mi>γ</mi></math></span> are the arbitrary constants. We constrain the model parameters <span><math><mi>α</mi></math></span> arising while solving the deceleration parameter <span><math><mi>q</mi></math></span> as an integration constant together with the present value of the Hubble parameter <span><math><msub><mrow><mi>H</mi></mrow><mrow><mn>0</mn></mrow></msub></math></span> using the Hubble datasets (OHD), the <span><math><mrow><mi>P</mi><mi>a</mi><mi>n</mi><mi>t</mi><mi>h</mi><mi>e</mi><mi>o</mi><mi>n</mi></mrow></math></span> of 1048 data points, and the joint datasets (OHD + <span><math><mrow><mi>P</mi><mi>a</mi><mi>n</mi><mi>t</mi><mi>h</mi><mi>e</mi><mi>o</mi><mi>n</mi></mrow></math></span>). The universe model transitions from an early deceleration state to an acceleration in late times. This model also provides the ekpyrotic phase of the universe on the redshift <span><math><mrow><mi>z</mi><mo>></mo><mn>12</mn><mo>.</mo><mn>32</mn></mrow></math></span>. In this model, the Big Bang is described as a collision of branes, and thus, the Big Bang is not the beginning of time. Before the Big Bang, there is an ekpyrotic phase with the equation of state <span><math><mrow><mi>ω</mi><mo>></mo><mo>></mo><mn>1</mn></mrow></math></span>. In late times, the undeviating Hubble measurements reduce the <span><math><msub><mrow><mi>H</mi></mrow><mrow><mn>0</mn></mrow></msub></math></span> tension in the reconstructed <span><math><mrow><mi>f</mi><mrow><mo>(</mo><mi>Q</mi><mo>,</mo><mi>T</mi><mo>)</mo></mrow></mrow></math></span> function. Additionally, we study various physical parameters of the model. Finally, our model describes a quintessence dark energy model at later times.</div></div>","PeriodicalId":8249,"journal":{"name":"Annals of Physics","volume":"483 ","pages":"Article 170274"},"PeriodicalIF":3.0,"publicationDate":"2025-12-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145413807","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}
扫码关注我们
求助内容：
应助结果提醒方式：
京公网安备 11010802042870号