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":"2025-10-23","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}
Pub Date : 2025-10-23DOI: 10.1016/j.aop.2025.170264
A.E. Bernardini , W. de Paula , R. da Rocha
Heavy-light-flavor meson resonances with charm, in the and families, and charmonium-like states, in the and families, are explored and discussed in the AdS/QCD model with four quark flavors. The differential configurational entropy is computed and analyzed for these four charmed meson families, also combining 4-flavor AdS/QCD to experimental data for the , , , and meson families. It makes it possible to predict the mass spectrum of unexplored heavier charmed meson resonances and to identify further charmed meson states reported in PDG.
{"title":"Spectroscopy of charmonium-like mesons, heavy-light mesons with charm, AdS/QCD, and configurational entropy","authors":"A.E. Bernardini , W. de Paula , R. da Rocha","doi":"10.1016/j.aop.2025.170264","DOIUrl":"10.1016/j.aop.2025.170264","url":null,"abstract":"<div><div>Heavy-light-flavor meson resonances with charm, in the <span><math><msup><mrow><mi>D</mi></mrow><mrow><mn>0</mn></mrow></msup></math></span> and <span><math><msup><mrow><mi>D</mi></mrow><mrow><mo>∗</mo></mrow></msup></math></span> families, and charmonium-like states, in the <span><math><msub><mrow><mi>η</mi></mrow><mrow><mi>c</mi></mrow></msub></math></span> and <span><math><msub><mrow><mi>χ</mi></mrow><mrow><mi>c</mi><mn>1</mn></mrow></msub></math></span> families, are explored and discussed in the AdS/QCD model with four quark flavors. The differential configurational entropy is computed and analyzed for these four charmed meson families, also combining 4-flavor AdS/QCD to experimental data for the <span><math><msup><mrow><mi>D</mi></mrow><mrow><mn>0</mn></mrow></msup></math></span>, <span><math><msup><mrow><mi>D</mi></mrow><mrow><mo>∗</mo></mrow></msup></math></span>, <span><math><msub><mrow><mi>η</mi></mrow><mrow><mi>c</mi></mrow></msub></math></span>, and <span><math><msub><mrow><mi>χ</mi></mrow><mrow><mi>c</mi><mn>1</mn></mrow></msub></math></span> meson families. It makes it possible to predict the mass spectrum of unexplored heavier charmed meson resonances and to identify further charmed meson states reported in PDG.</div></div>","PeriodicalId":8249,"journal":{"name":"Annals of Physics","volume":"483 ","pages":"Article 170264"},"PeriodicalIF":3.0,"publicationDate":"2025-10-23","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145413872","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 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":"2025-10-21","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 : 2025-10-21DOI: 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":"2025-10-21","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 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":"2025-10-21","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}
Pub Date : 2025-10-21DOI: 10.1016/j.aop.2025.170275
Archana Dixit , Manish Yadav , Anirudh Pradhan , M.S. Barak
In this work, we investigate a cosmological scenario with a time-dependent cosmological constant (t) within the spatially flat Friedmann–Lemaître–Robertson–Walker (FLRW) framework. Here we study a power-law CDM model characterized by a dynamic cosmological constant expressed as a function of the Hubble parameter and its derivative Using recent observational datasets (DESI BAO, OHD, and PP&SH0ES), we constrain the model’s free parameters and analyze their impact on key cosmological quantities. A Markov chain Monte Carlo (MCMC) analysis of the best-fit value of km/s/Mpc from PP&SH0ES analysis only, which substantially alleviates the existing tension between early and late-time determinations of the Hubble constant, reducing it to . The reconstructed diagnostic exhibits a negative slope, indicating a dynamic dark energy behavior with quintessence-like characteristics (). These results suggest that the proposed model provides a viable alternative to the standard CDM paradigm to explain the late-time acceleration of the universe. Our findings show that this model alleviates the Hubble tension more effectively than the standard CDM. The model also demonstrates compatibility with late-time Hubble parameter observations and offers a compelling framework to address the limitations of CDM.
在这项工作中，我们在空间平坦的friedman - lema - robert - walker （FLRW）框架中研究了具有时间依赖的宇宙学常数Λ(t)的宇宙学场景。本文研究了一个幂律Λ(t)CDM模型，其特征是动力学宇宙常数表示为哈勃参数的函数及其导数Λ(t) =α（Ḣ+H2）+ Λ H2+4π ρη。利用最近的观测数据集（DESI BAO， OHD和pp&&； SH0ES），我们约束了模型的自由参数（H0,α,λ,η），并分析了它们对关键宇宙学量的影响。马尔可夫链蒙特卡罗(密度)的最佳价值分析H0 = 71.9±0.23 km / s / Mpc PP& SH0ES分析,这大大减轻现有的早期和后期数据决定的哈勃常数之间的紧张关系,减少∼1.5σ。重构的Om诊断曲线呈现负斜率，表明暗能量的动态行为具有类似精粹的特征（ω>−1）。这些结果表明，提出的Λ(t)模型提供了一个可行的替代标准ΛCDM范式来解释宇宙的后期加速。我们的发现表明，这个模型比标准模型更有效地缓解了哈勃张力ΛCDM。该模型还证明了与后期哈勃参数观测的兼容性，并提供了一个令人信服的框架来解决ΛCDM的局限性。
{"title":"Beyond ΛCDM: Exploring a dynamical cosmological constant framework consistent with late-time observations","authors":"Archana Dixit , Manish Yadav , Anirudh Pradhan , M.S. Barak","doi":"10.1016/j.aop.2025.170275","DOIUrl":"10.1016/j.aop.2025.170275","url":null,"abstract":"<div><div>In this work, we investigate a cosmological scenario with a time-dependent cosmological constant <span><math><mi>Λ</mi></math></span>(t) within the spatially flat Friedmann–Lemaître–Robertson–Walker (FLRW) framework. Here we study a power-law <span><math><mrow><mi>Λ</mi><mrow><mo>(</mo><mi>t</mi><mo>)</mo></mrow></mrow></math></span>CDM model characterized by a dynamic cosmological constant expressed as a function of the Hubble parameter and its derivative <span><math><mrow><mi>Λ</mi><mrow><mo>(</mo><mi>t</mi><mo>)</mo></mrow></mrow></math></span> <span><math><mrow><mo>=</mo><mi>α</mi><mrow><mo>(</mo><mover><mrow><mi>H</mi></mrow><mrow><mo>̇</mo></mrow></mover><mo>+</mo><msup><mrow><mi>H</mi></mrow><mrow><mn>2</mn></mrow></msup><mo>)</mo></mrow><mo>+</mo><mi>λ</mi><msup><mrow><mi>H</mi></mrow><mrow><mn>2</mn></mrow></msup><mo>+</mo><mn>4</mn><mi>π</mi><mi>G</mi><mi>ρ</mi><mi>η</mi><mo>.</mo></mrow></math></span> Using recent observational datasets (DESI BAO, OHD, and PP&SH0ES), we constrain the model’s free parameters <span><math><mrow><mo>(</mo><msub><mrow><mi>H</mi></mrow><mrow><mn>0</mn></mrow></msub><mo>,</mo><mi>α</mi><mo>,</mo><mi>λ</mi><mo>,</mo><mi>η</mi><mo>)</mo></mrow></math></span> and analyze their impact on key cosmological quantities. A Markov chain Monte Carlo (MCMC) analysis of the best-fit value of <span><math><mrow><msub><mrow><mi>H</mi></mrow><mrow><mn>0</mn></mrow></msub><mo>=</mo><mn>71</mn><mo>.</mo><mn>9</mn><mo>±</mo><mn>0</mn><mo>.</mo><mn>23</mn></mrow></math></span> km/s/Mpc from PP&SH0ES analysis only, which substantially alleviates the existing tension between early and late-time determinations of the Hubble constant, reducing it to <span><math><mrow><mo>∼</mo><mn>1</mn><mo>.</mo><mn>5</mn><mi>σ</mi></mrow></math></span>. The reconstructed <span><math><mrow><mi>O</mi><mi>m</mi></mrow></math></span> diagnostic exhibits a negative slope, indicating a dynamic dark energy behavior with quintessence-like characteristics (<span><math><mrow><mi>ω</mi><mo>></mo><mo>−</mo><mn>1</mn></mrow></math></span>). These results suggest that the proposed <span><math><mrow><mi>Λ</mi><mrow><mo>(</mo><mi>t</mi><mo>)</mo></mrow></mrow></math></span> model provides a viable alternative to the standard <span><math><mi>Λ</mi></math></span>CDM paradigm to explain the late-time acceleration of the universe. Our findings show that this model alleviates the Hubble tension more effectively than the standard <span><math><mi>Λ</mi></math></span>CDM. The model also demonstrates compatibility with late-time Hubble parameter observations and offers a compelling framework to address the limitations of <span><math><mi>Λ</mi></math></span>CDM.</div></div>","PeriodicalId":8249,"journal":{"name":"Annals of Physics","volume":"483 ","pages":"Article 170275"},"PeriodicalIF":3.0,"publicationDate":"2025-10-21","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145360156","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 : 2025-10-21DOI: 10.1016/j.aop.2025.170265
Azadeh Faridi , Reza Asgari
We investigate both intrinsic and extrinsic orbital Hall effects (OHE) in bilayer transition metal dichalcogenides (TMDs) in the presence of short-range disorder using quantum kinetic theory. Bilayer TMDs provide an ideal platform to study the effects of inversion symmetry breaking on transport properties due to their unique structural and electronic characteristics. While bilayer TMDs are naturally inversion symmetric, applying a finite gate voltage to create a bias between the layers effectively breaks this symmetry. Our findings reveal that slightly away from the band edges, the extrinsic OHE eventually becomes the dominant contribution in both inversion-symmetric and asymmetric cases, with its prominence increasing significantly as a function of Fermi energy. Furthermore, we demonstrate that breaking inversion symmetry greatly enhances the extrinsic OHE. This enhancement arises from the fundamentally distinct behavior of orbital angular momentum (OAM) in centrosymmetric systems, where intraband components vanish due to symmetry constraints. As a result, in centrosymmetric systems, only the off-diagonal components of the density matrix contribute to the extrinsic OHE. In contrast, in noncentrosymmetric systems, both diagonal and off-diagonal components play a role. Our study suggests that in experimentally relevant highly doped systems, the OHE becomes predominantly extrinsic in both centrosymmetric and noncentrosymmetric although the contribution is much more pronounced in the latter. Importantly, we infer that even a weakly breaking of inversion symmetry can lead to a dramatic enhancement of the OHE, a finding with significant implications for experimental investigations.
{"title":"Comparing the extrinsic orbital Hall effect in centrosymmetric and noncentrosymmetric systems: Insights from bilayer transition metal dichalcogenides","authors":"Azadeh Faridi , Reza Asgari","doi":"10.1016/j.aop.2025.170265","DOIUrl":"10.1016/j.aop.2025.170265","url":null,"abstract":"<div><div>We investigate both intrinsic and extrinsic orbital Hall effects (OHE) in bilayer transition metal dichalcogenides (TMDs) in the presence of short-range disorder using quantum kinetic theory. Bilayer TMDs provide an ideal platform to study the effects of inversion symmetry breaking on transport properties due to their unique structural and electronic characteristics. While bilayer TMDs are naturally inversion symmetric, applying a finite gate voltage to create a bias between the layers effectively breaks this symmetry. Our findings reveal that slightly away from the band edges, the extrinsic OHE eventually becomes the dominant contribution in both inversion-symmetric and asymmetric cases, with its prominence increasing significantly as a function of Fermi energy. Furthermore, we demonstrate that breaking inversion symmetry greatly enhances the extrinsic OHE. This enhancement arises from the fundamentally distinct behavior of orbital angular momentum (OAM) in centrosymmetric systems, where intraband components vanish due to symmetry constraints. As a result, in centrosymmetric systems, only the off-diagonal components of the density matrix contribute to the extrinsic OHE. In contrast, in noncentrosymmetric systems, both diagonal and off-diagonal components play a role. Our study suggests that in experimentally relevant highly doped systems, the OHE becomes predominantly extrinsic in both centrosymmetric and noncentrosymmetric although the contribution is much more pronounced in the latter. Importantly, we infer that even a weakly breaking of inversion symmetry can lead to a dramatic enhancement of the OHE, a finding with significant implications for experimental investigations.</div></div>","PeriodicalId":8249,"journal":{"name":"Annals of Physics","volume":"483 ","pages":"Article 170265"},"PeriodicalIF":3.0,"publicationDate":"2025-10-21","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145360161","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 : 2025-10-20DOI: 10.1016/j.aop.2025.170268
Mohamed Amazioug , Mohammed Daoud
The extraction of work from quantum systems is critical in quantum thermodynamics. In the case of homodyne/heterodyne measurement in de Sitter space (dS), we demonstrate that it is possible to achieve entanglement through extracted work in bi- and tripartite Gaussian states. We show that the entanglement detected by extracted work is in good agreement with that quantified by logarithmic negativity. The results indicate that the influence of de Sitter space curvature results in a distribution of quantum entanglement between modes in different open charts. Particularly, we show that the quantum entanglement of the initially correlated state persists up to infinite curvature.
{"title":"Extracting work as a witness of entanglement in de Sitter spacetime","authors":"Mohamed Amazioug , Mohammed Daoud","doi":"10.1016/j.aop.2025.170268","DOIUrl":"10.1016/j.aop.2025.170268","url":null,"abstract":"<div><div>The extraction of work from quantum systems is critical in quantum thermodynamics. In the case of homodyne/heterodyne measurement in de Sitter space (dS), we demonstrate that it is possible to achieve entanglement through extracted work in bi- and tripartite Gaussian states. We show that the entanglement detected by extracted work is in good agreement with that quantified by logarithmic negativity. The results indicate that the influence of de Sitter space curvature results in a distribution of quantum entanglement between modes in different open charts. Particularly, we show that the quantum entanglement of the initially correlated state persists up to infinite curvature.</div></div>","PeriodicalId":8249,"journal":{"name":"Annals of Physics","volume":"483 ","pages":"Article 170268"},"PeriodicalIF":3.0,"publicationDate":"2025-10-20","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145360160","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 : 2025-10-16DOI: 10.1016/j.aop.2025.170242
Muhamad Ashraf Azman, Siti Najihah Ramlay
This work investigates compact stellar models composed of a mixture of ordinary matter and dark energy within the Tolman IV spacetime, assuming an isotropic matter distribution and a linear equation of state (EoS) for the ordinary matter. The dark energy component is modeled via a negative-pressure fluid obeying , and is confined entirely within the star. We focus on identifying the maximum proportion of DE-like matter that can be tolerated by neutron star data while maintaining physical viability. Using observational constraints, we show that up to approximately 11% of the total energy density may consist of DE-like matter, with ordinary matter remaining dominant across the stellar interior. All resulting configurations satisfy energy conditions, causality, and equilibrium without invoking anisotropic forces or exotic gravity theories. Although we adopt a simplified linear EoS, the model provides a minimal framework to test the astrophysical compatibility of dark energy in compact objects, and suggests that DE-like components can be physically admissible at small fractions in admixed star models.
{"title":"Modeling dark-energy admixed stars in Tolman IV spacetime","authors":"Muhamad Ashraf Azman, Siti Najihah Ramlay","doi":"10.1016/j.aop.2025.170242","DOIUrl":"10.1016/j.aop.2025.170242","url":null,"abstract":"<div><div>This work investigates compact stellar models composed of a mixture of ordinary matter and dark energy within the Tolman IV spacetime, assuming an isotropic matter distribution and a linear equation of state (EoS) for the ordinary matter. The dark energy component is modeled via a negative-pressure fluid obeying <span><math><mrow><msub><mrow><mi>p</mi></mrow><mrow><mi>d</mi><mi>e</mi></mrow></msub><mo>=</mo><mo>−</mo><msub><mrow><mi>ρ</mi></mrow><mrow><mi>d</mi><mi>e</mi></mrow></msub></mrow></math></span>, and is confined entirely within the star. We focus on identifying the maximum proportion of DE-like matter that can be tolerated by neutron star data while maintaining physical viability. Using observational constraints, we show that up to approximately 11% of the total energy density may consist of DE-like matter, with ordinary matter remaining dominant across the stellar interior. All resulting configurations satisfy energy conditions, causality, and equilibrium without invoking anisotropic forces or exotic gravity theories. Although we adopt a simplified linear EoS, the model provides a minimal framework to test the astrophysical compatibility of dark energy in compact objects, and suggests that DE-like components can be physically admissible at small fractions in admixed star models.</div></div>","PeriodicalId":8249,"journal":{"name":"Annals of Physics","volume":"483 ","pages":"Article 170242"},"PeriodicalIF":3.0,"publicationDate":"2025-10-16","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145360158","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 : 2025-10-14DOI: 10.1016/j.aop.2025.170263
A.I. Milstein , I.S. Terekhov
The scattering of a nonrelativistic electron on a narrow solenoid of finite length is considered. In this case, the magnetic field outside the solenoid is not zero. Using the eikonal approximation, the differential and total cross sections of the process are found. It is shown that the total cross section is finite, in contrast to the case of scattering on an infinitely long solenoid (Aharonov-Bohm effect). An asymmetry in the scattering cross section is also found, which can be observed in an experiment.
{"title":"Skew scattering and the Aharonov-Bohm effect","authors":"A.I. Milstein , I.S. Terekhov","doi":"10.1016/j.aop.2025.170263","DOIUrl":"10.1016/j.aop.2025.170263","url":null,"abstract":"<div><div>The scattering of a nonrelativistic electron on a narrow solenoid of finite length is considered. In this case, the magnetic field outside the solenoid is not zero. Using the eikonal approximation, the differential and total cross sections of the process are found. It is shown that the total cross section is finite, in contrast to the case of scattering on an infinitely long solenoid (Aharonov-Bohm effect). An asymmetry in the scattering cross section is also found, which can be observed in an experiment.</div></div>","PeriodicalId":8249,"journal":{"name":"Annals of Physics","volume":"483 ","pages":"Article 170263"},"PeriodicalIF":3.0,"publicationDate":"2025-10-14","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145322987","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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