Pub Date : 2026-01-21DOI: 10.1016/j.aop.2026.170355
Simon Friederich, Mritunjay Tyagi
The Kochen–Specker theorem shows that it is impossible to assign sharp values to all dynamical variables in quantum mechanics in such a way that the algebraic relations among the values of dynamical variables whose self-adjoint operators commute are the same as those among the operators themselves. We point out that, for quantum theories obtained by quantizing some classical theory, this condition –Kochen–Specker non-contextuality – is implausible from the start because quantization usually changes algebraic relations. We explain why this is so, using the formalism of deformation quantization and its conception of star products, and we illustrate the relevance of this point using various examples of dynamical variables quantized via Weyl quantization and coherent state quantization. Our observations suggest that the relevance of the Kochen–Specker theorem to the question of whether one can assign sharp values to all dynamical variables is rather limited.
{"title":"Kochen–Specker non-contextuality through the lens of quantization","authors":"Simon Friederich, Mritunjay Tyagi","doi":"10.1016/j.aop.2026.170355","DOIUrl":"10.1016/j.aop.2026.170355","url":null,"abstract":"<div><div>The Kochen–Specker theorem shows that it is impossible to assign sharp values to all dynamical variables in quantum mechanics in such a way that the algebraic relations among the values of dynamical variables whose self-adjoint operators commute are the same as those among the operators themselves. We point out that, for quantum theories obtained by <em>quantizing</em> some classical theory, this condition –<em>Kochen–Specker non-contextuality</em> – is implausible from the start because quantization usually changes algebraic relations. We explain why this is so, using the formalism of deformation quantization and its conception of <em>star products</em>, and we illustrate the relevance of this point using various examples of dynamical variables quantized via Weyl quantization and coherent state quantization. Our observations suggest that the relevance of the Kochen–Specker theorem to the question of whether one can assign sharp values to all dynamical variables is rather limited.</div></div>","PeriodicalId":8249,"journal":{"name":"Annals of Physics","volume":"487 ","pages":"Article 170355"},"PeriodicalIF":3.0,"publicationDate":"2026-01-21","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"146025671","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
The Abelian super Stueckelberg model (ASSM) in the Wess–Zumino (WZ) gauge is revisited, and the actual set of supersymmetric (SUSY) transformation is derived. In particular, we verified that the SUSY transformation of the super Stueckelberg sector compensates the gauge fixing condition imposed on the vector superfield, leading to a mix between the field components of both sectors. We also discuss the possibility to construct an extension of the ASSM with infinite self interacting terms
{"title":"Revisiting the Abelian N=1 super Stueckelberg model","authors":"M.A.L. Capri , D.R. Granado , I.F. Justo , L.S.S. Mendes","doi":"10.1016/j.aop.2026.170354","DOIUrl":"10.1016/j.aop.2026.170354","url":null,"abstract":"<div><div>The Abelian super Stueckelberg model (ASSM) in the Wess–Zumino (WZ) gauge is revisited, and the actual set of supersymmetric (SUSY) transformation is derived. In particular, we verified that the SUSY transformation of the super Stueckelberg sector compensates the gauge fixing condition imposed on the vector superfield, leading to a mix between the field components of both sectors. We also discuss the possibility to construct an extension of the ASSM with infinite self interacting terms</div></div>","PeriodicalId":8249,"journal":{"name":"Annals of Physics","volume":"487 ","pages":"Article 170354"},"PeriodicalIF":3.0,"publicationDate":"2026-01-21","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"146037353","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}
With the non-metricity scalar as the functional argument, several gravity models are found to be proposed which are perfectly able to mimic the late-time accelerated expansion as pointed out by the type Ia supernovae observations. Temperature fluctuation differences for two celestial hemispheres, Hubble tension, voids, dipole modulation, anisotropic inflation, etc. motivates us to think beyond the CDM model and the cosmological principle. Bianchi-I model portrays an anisotropic universe imposing shear. model also enables us to produce early inflation to late de Sitter universe without the requirement of CDM. Ambiguities regarding fine-tuning or coincidences can be avoided alongwith. So, this article finds different stationary points of cosmic evolution with models habilitating in Bianchi-I anisotropic universe. Depending on models’ nature, fixed points with different categories are found. Perturbations are followed wherever are applicable. While pursuing cosmological implications towards these fixed points, some are found to be formed only for the consideration of gravity and Bianchi-I both. Besides different prediction towards early inflation to late-time expansion which are available in existing literature of dynamical system studies, occurrences of ultra slow roll inflation is predicted. For particular model, shear is predicted to decay leaving behind a constant valued residue. This models a universe that gradually turns more homogeneous. In some other models, depending on initial conditions, a final isotropic leftover is marked as the future fate of anisotropic world. More than one stable points are marked for special cases and are cosmologically interpreted.
{"title":"Stability analysis of four f(Q) gravity models: A cosmological review in the background of Bianchi-I anisotropy","authors":"Subhajit Pal , Atanu Mukherjee , Ritabrata Biswas , Farook Rahaman","doi":"10.1016/j.aop.2026.170351","DOIUrl":"10.1016/j.aop.2026.170351","url":null,"abstract":"<div><div>With the non-metricity scalar <span><math><mi>Q</mi></math></span> as the functional argument, several <span><math><mrow><mi>f</mi><mrow><mo>(</mo><mi>Q</mi><mo>)</mo></mrow></mrow></math></span> gravity models are found to be proposed which are perfectly able to mimic the late-time accelerated expansion as pointed out by the type Ia supernovae observations. Temperature fluctuation differences for two celestial hemispheres, Hubble tension, voids, dipole modulation, anisotropic inflation, etc. motivates us to think beyond the <span><math><mi>Λ</mi></math></span>CDM model and the cosmological principle. Bianchi-I model portrays an anisotropic universe imposing shear. <span><math><mrow><mi>f</mi><mrow><mo>(</mo><mi>Q</mi><mo>)</mo></mrow></mrow></math></span> model also enables us to produce early inflation to late de Sitter universe without the requirement of <span><math><mi>Λ</mi></math></span>CDM. Ambiguities regarding fine-tuning or coincidences can be avoided alongwith. So, this article finds different stationary points of cosmic evolution with <span><math><mrow><mi>f</mi><mrow><mo>(</mo><mi>Q</mi><mo>)</mo></mrow></mrow></math></span> models habilitating in Bianchi-I anisotropic universe. Depending on models’ nature, fixed points with different categories are found. Perturbations are followed wherever are applicable. While pursuing cosmological implications towards these fixed points, some are found to be formed only for the consideration of <span><math><mrow><mi>f</mi><mrow><mo>(</mo><mi>Q</mi><mo>)</mo></mrow></mrow></math></span> gravity and Bianchi-I both. Besides different prediction towards early inflation to late-time expansion which are available in existing literature of dynamical system studies, occurrences of ultra slow roll inflation is predicted. For particular <span><math><mrow><mi>f</mi><mrow><mo>(</mo><mi>Q</mi><mo>)</mo></mrow></mrow></math></span> model, shear is predicted to decay leaving behind a constant valued residue. This models a universe that gradually turns more homogeneous. In some other models, depending on initial conditions, a final isotropic leftover is marked as the future fate of anisotropic world. More than one stable points are marked for special cases and are cosmologically interpreted.</div></div>","PeriodicalId":8249,"journal":{"name":"Annals of Physics","volume":"487 ","pages":"Article 170351"},"PeriodicalIF":3.0,"publicationDate":"2026-01-21","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"146006639","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 : 2026-01-20DOI: 10.1016/j.aop.2026.170347
H. Aruna Kumara , Chaitra Chooda Chalavadi , V. Venkatesha
The study investigates the possibility of wormhole solutions with dark matter profiles in the context of gravity. Its primary focus is to understand how dark matter influences the formation of traversable wormholes in galactic halos. The analysis considers different dark matter models, such as Moradpour density profile and Sofue’s exponential density profile in linear gravity. Under this model, the density profiles generate shape functions that satisfy all essential conditions for wormhole geometries. The violation of null energy conditions observed in these cases confirms that dark matter can support the existence of wormholes within galactic halos. In addition, the analysis focuses on important features of wormholes, namely the complexity factor, anisotropy, volume integral quantifier, and their embedding diagrams. The findings suggest that solutions based on various dark-matter profiles in extended symmetric teleparallel gravity are feasible and consistent.
{"title":"Exploring wormhole solutions supported by dark matter density profiles in f(Q,T) gravity","authors":"H. Aruna Kumara , Chaitra Chooda Chalavadi , V. Venkatesha","doi":"10.1016/j.aop.2026.170347","DOIUrl":"10.1016/j.aop.2026.170347","url":null,"abstract":"<div><div>The study investigates the possibility of wormhole solutions with dark matter profiles in the context of <span><math><mrow><mi>f</mi><mrow><mo>(</mo><mi>Q</mi><mo>,</mo><mi>T</mi><mo>)</mo></mrow></mrow></math></span> gravity. Its primary focus is to understand how dark matter influences the formation of traversable wormholes in galactic halos. The analysis considers different dark matter models, such as Moradpour density profile and Sofue’s exponential density profile in linear <span><math><mrow><mi>f</mi><mrow><mo>(</mo><mi>Q</mi><mo>,</mo><mi>T</mi><mo>)</mo></mrow></mrow></math></span> gravity. Under this model, the density profiles generate shape functions that satisfy all essential conditions for wormhole geometries. The violation of null energy conditions observed in these cases confirms that dark matter can support the existence of wormholes within galactic halos. In addition, the analysis focuses on important features of wormholes, namely the complexity factor, anisotropy, volume integral quantifier, and their embedding diagrams. The findings suggest that solutions based on various dark-matter profiles in extended symmetric teleparallel gravity are feasible and consistent.</div></div>","PeriodicalId":8249,"journal":{"name":"Annals of Physics","volume":"487 ","pages":"Article 170347"},"PeriodicalIF":3.0,"publicationDate":"2026-01-20","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"146037354","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 : 2026-01-17DOI: 10.1016/j.aop.2026.170352
Erfan Bayenat , Babak Vakili
We develop and analyze a two-oscillator model for black hole evaporation in which an effective geometric degree of freedom and a representative Hawking radiation mode are described by coupled harmonic oscillators with opposite signs in their free Hamiltonians. The normal-mode structure is obtained analytically and the corresponding modal amplitudes determine the pattern of energy exchange between the two sectors. To bridge the discrete and semiclassical pictures, we introduce smooth envelope functions that provide a continuous effective description along the geometric variable. Numerical simulations in a truncated Fock space show that the two oscillators exchange quanta in an approximately out-of-phase manner, consistent with an effective conservation of . The reduced entropy exhibits periodic growth, indicating entanglement generation. These results demonstrate that even a minimal two-mode framework can capture key qualitative features of energy transfer and information flow during evaporation.
我们建立并分析了一个黑洞蒸发的双振子模型，在该模型中，有效的几何自由度和具有代表性的霍金辐射模式由自由哈密顿量中具有相反符号的耦合谐振子来描述。解析得到了正模态结构，相应的模态振幅决定了两扇区之间能量交换的模式。为了连接离散和半经典图像，我们引入平滑包络函数，它沿着几何变量提供连续有效的描述。截断Fock空间中的数值模拟表明，两个振子以近似非相的方式交换量子，符合< nx > - < ny >的有效守恒。约简熵Sx(t)呈现周期性增长，表明纠缠产生。这些结果表明，即使是最小的双模框架也可以捕获蒸发过程中能量传递和信息流的关键定性特征。
{"title":"A two-mode model for black hole evaporation and information flow","authors":"Erfan Bayenat , Babak Vakili","doi":"10.1016/j.aop.2026.170352","DOIUrl":"10.1016/j.aop.2026.170352","url":null,"abstract":"<div><div>We develop and analyze a two-oscillator model for black hole evaporation in which an effective geometric degree of freedom and a representative Hawking radiation mode are described by coupled harmonic oscillators with opposite signs in their free Hamiltonians. The normal-mode structure is obtained analytically and the corresponding modal amplitudes determine the pattern of energy exchange between the two sectors. To bridge the discrete and semiclassical pictures, we introduce smooth envelope functions that provide a continuous effective description along the geometric variable. Numerical simulations in a truncated Fock space show that the two oscillators exchange quanta in an approximately out-of-phase manner, consistent with an effective conservation of <span><math><mrow><mrow><mo>〈</mo><msub><mrow><mi>n</mi></mrow><mrow><mi>x</mi></mrow></msub><mo>〉</mo></mrow><mo>−</mo><mrow><mo>〈</mo><msub><mrow><mi>n</mi></mrow><mrow><mi>y</mi></mrow></msub><mo>〉</mo></mrow></mrow></math></span>. The reduced entropy <span><math><mrow><msub><mrow><mi>S</mi></mrow><mrow><mi>x</mi></mrow></msub><mrow><mo>(</mo><mi>t</mi><mo>)</mo></mrow></mrow></math></span> exhibits periodic growth, indicating entanglement generation. These results demonstrate that even a minimal two-mode framework can capture key qualitative features of energy transfer and information flow during evaporation.</div></div>","PeriodicalId":8249,"journal":{"name":"Annals of Physics","volume":"488 ","pages":"Article 170352"},"PeriodicalIF":3.0,"publicationDate":"2026-01-17","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"146098725","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 : 2026-01-16DOI: 10.1016/j.aop.2026.170349
W.M. Seif , A.S. Hashem
Tidal deformability measures how NS can comfortably deform as a response to an applied tidal field. We use updated constraints on the mass, radius, and tidal deformability of neutron star (NS) objects and pulsars to examine nuclear equations of state (EOS) based on realistic finite-range M3Y nucleon–nucleon interaction, which have been successfully used to describe low- and high-dense nuclear matter (NM). We then employ these EOSs to examine the impact of tidal deformability and compactness of NSs on their structure. We found that the EOSs from CDM3Y-230 to CDM3Y-330 characterized with the saturation incompressibility together yield more limited ranges of tidal deformability and radius for NS objects than their observational inferred ranges. For light NS (), both and decreases upon decreasing the NS mass, which enhances its tidal deformability. The stiffness of the NS core matter has shown a minor effect on the tidal deformability of such NS (). An opposite behavior is obtained as an increase in the tidal Love number but a decrease in the more effective compactness of NS (), upon increasing (decreasing) the stiffness of the employed EOS (its mass). This appears as enhanced tidal deformability indicated at a larger radius for NS of stiffer NM and for the lighter NS above . Unified description of some correlations between tidal deformability, tidal Love number, and NS compactness is provided independent of the details of the considered EOS.
{"title":"Tidal deformability and compactness of neutron stars and massive pulsars from semi-microscopic equations of state","authors":"W.M. Seif , A.S. Hashem","doi":"10.1016/j.aop.2026.170349","DOIUrl":"10.1016/j.aop.2026.170349","url":null,"abstract":"<div><div>Tidal deformability measures how NS can comfortably deform as a response to an applied tidal field. We use updated constraints on the mass, radius, and tidal deformability of neutron star (NS) objects and pulsars to examine nuclear equations of state (EOS) based on realistic finite-range M3Y nucleon–nucleon interaction, which have been successfully used to describe low- and high-dense nuclear matter (NM). We then employ these EOSs to examine the impact of tidal deformability and compactness of NSs on their structure. We found that the EOSs from CDM3Y-230 to CDM3Y-330 characterized with the saturation incompressibility <span><math><mrow><msub><mrow><mi>K</mi></mrow><mrow><mn>0</mn></mrow></msub><mo>=</mo><mn>230</mn><mo>−</mo><mn>330</mn><mspace></mspace><mi>MeV</mi></mrow></math></span> together yield more limited ranges of tidal deformability and radius for NS objects than their observational inferred ranges. For light NS (<span><math><mrow><mi>M</mi><mo><</mo><msub><mrow><mtext>M</mtext></mrow><mrow><mo>⊙</mo></mrow></msub></mrow></math></span>), both <span><math><msub><mrow><mi>k</mi></mrow><mrow><mn>2</mn></mrow></msub></math></span> and <span><math><mi>C</mi></math></span> decreases upon decreasing the NS mass, which enhances its tidal deformability. The stiffness of the NS core matter has shown a minor effect on the tidal deformability of such NS (<span><math><mrow><mi>M</mi><mo><</mo><msub><mrow><mtext>M</mtext></mrow><mrow><mo>⊙</mo></mrow></msub></mrow></math></span>). An opposite behavior is obtained as an increase in the tidal Love number but a decrease in the more effective compactness of NS (<span><math><mrow><mi>M</mi><mo>></mo><msub><mrow><mtext>M</mtext></mrow><mrow><mo>⊙</mo></mrow></msub></mrow></math></span>), upon increasing (decreasing) the stiffness of the employed EOS (its mass). This appears as enhanced tidal deformability indicated at a larger radius for NS of stiffer NM and for the lighter NS above <span><math><msub><mrow><mtext>M</mtext></mrow><mrow><mo>⊙</mo></mrow></msub></math></span>. Unified description of some correlations between tidal deformability, tidal Love number, and NS compactness is provided independent of the details of the considered EOS.</div></div>","PeriodicalId":8249,"journal":{"name":"Annals of Physics","volume":"486 ","pages":"Article 170349"},"PeriodicalIF":3.0,"publicationDate":"2026-01-16","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"146034388","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 : 2026-01-12DOI: 10.1016/j.aop.2026.170350
Orhan Donmez , Sardor Murodov , Javlon Rayimbaev
<div><div>Testing the Kerr spacetime solution of general relativity (GR) has increasingly become a requirement with the recent observations of black hole shadows and gravitational waves. In this context, we examine the physical properties of the shock cone formed by Bondi–Hoyle–Lyttleton (BHL) accretion around a black hole or a naked singularity using the Johannsen–Psaltis (JP) metric, and compare them with those of the Kerr metric solution. We demonstrate how these properties vary with the metric’s deviation parameter (<span><math><mi>η</mi></math></span>). We find that when <span><math><mrow><mi>a</mi><mo>/</mo><mi>M</mi><mo>=</mo><mn>0</mn><mo>.</mo><mn>9</mn></mrow></math></span> and a black hole is formed for <span><math><mrow><mi>η</mi><mo><</mo><mn>0</mn></mrow></math></span>, as the deviation parameter decreases, the opening angle of the resulting cone becomes smaller, leading to a shift of the resulting quasi-periodic oscillations (QPOs) from low to high frequencies. On the other hand, for <span><math><mrow><mi>η</mi><mo>></mo><mn>0</mn></mrow></math></span>, it is observed that the shock cone forms around the naked singularity at small values of <span><math><mi>η</mi></math></span>. Furthermore, at large <span><math><mi>η</mi></math></span> values, the cone evolves into a torus-like structure under the influence of the strong gravitational field. In the case of <span><math><mrow><mrow><mo>|</mo><mi>η</mi><mo>|</mo></mrow><mo>∼</mo><mn>8</mn></mrow></math></span>, perfect harmonicity is observed, along with possible resonances such as the 3:2 ratio, consistent with observations. Additionally, for the case of a slowly rotating black hole (<span><math><mrow><mi>a</mi><mo>/</mo><mi>M</mi><mo>=</mo><mn>0</mn><mo>.</mo><mn>4</mn></mrow></math></span>), a behavior resembling the bending of the shock cone due to the curvature of spacetime in the presence of a strong gravitational field is also observed at large <span><math><mi>η</mi></math></span> values, similar to what is observed when the spin parameter of the Kerr black hole is <span><math><mrow><mi>a</mi><mo>/</mo><mi>M</mi><mo>≥</mo><mn>0</mn><mo>.</mo><mn>9</mn></mrow></math></span>. Finally, we have calculated fundamental frequencies to investigate QPOs around rotating JP black holes. We use Markov Chain Monte Carlo (MCMC) analyses to obtain constrained values for the black hole mass, spacetime deformation, and QPO orbits around black hole candidates at the center of the Milky Way and M82 galaxies, and microquasars XTE J1550, GRO J1655-40,& GRS 1915-105, using QPO data observed in them. Overall, the JP metric with moderate deviation (<span><math><mrow><mrow><mo>|</mo><mi>η</mi><mo>|</mo></mrow><mo>≈</mo><mn>8</mn></mrow></math></span>) is more consistent with the observed QPO frequencies and resonance structures than the pure Kerr metric, suggesting that small deviations from Kerr spacetime may more accurately describe strong field gravity around astrophysical black holes.</di
随着近年来对黑洞阴影和引力波的观测，检验广义相对论（GR）的克尔时空解日益成为一种需求。在这种情况下，我们使用Johannsen-Psaltis （JP）度规研究了黑洞或裸奇点周围Bondi-Hoyle-Lyttleton （BHL）吸积形成的激波锥的物理性质，并将其与Kerr度规解的物理性质进行了比较。我们演示了这些性质如何随度量的偏差参数（η）而变化。我们发现，当a/M=0.9, η<；0形成黑洞时，随着偏差参数的减小，产生的锥开口角变小，导致产生的准周期振荡（QPOs）由低频向高频偏移。另一方面，当η>；0时，在较小的η值处，激波锥在裸奇点周围形成。当η值较大时，锥体在强引力场作用下演化为环面结构。在|η| ~ 8的情况下，观测到完美的谐波，以及可能的共振，如3:2的比例，与观测结果一致。此外，对于缓慢旋转的黑洞（a/M=0.4），在大η值下也观察到类似于激波锥由于时空曲率在强引力场下的弯曲行为，类似于克尔黑洞自旋参数为a/M≥0.9时观察到的现象。最后，我们计算了基频来研究旋转JP黑洞周围的qpo。利用观测到的QPO数据，利用Markov Chain Monte Carlo （MCMC）分析方法，获得了银河系和M82星系中心候选黑洞以及微类星体XTE J1550、GRO J1655-40和GRS 15% -105周围的黑洞质量、时空变形和QPO轨道的约束值。总体而言，中等偏差（|η|≈8）的JP度规比纯Kerr度规更符合观测到的QPO频率和共振结构，这表明与Kerr时空的小偏差可能更准确地描述天体物理黑洞周围的强场引力。
{"title":"Testing strong gravitational field using the Johannsen–Psaltis metric: Bondi–Hoyle–Lyttleton accretion model and QPO studies","authors":"Orhan Donmez , Sardor Murodov , Javlon Rayimbaev","doi":"10.1016/j.aop.2026.170350","DOIUrl":"10.1016/j.aop.2026.170350","url":null,"abstract":"<div><div>Testing the Kerr spacetime solution of general relativity (GR) has increasingly become a requirement with the recent observations of black hole shadows and gravitational waves. In this context, we examine the physical properties of the shock cone formed by Bondi–Hoyle–Lyttleton (BHL) accretion around a black hole or a naked singularity using the Johannsen–Psaltis (JP) metric, and compare them with those of the Kerr metric solution. We demonstrate how these properties vary with the metric’s deviation parameter (<span><math><mi>η</mi></math></span>). We find that when <span><math><mrow><mi>a</mi><mo>/</mo><mi>M</mi><mo>=</mo><mn>0</mn><mo>.</mo><mn>9</mn></mrow></math></span> and a black hole is formed for <span><math><mrow><mi>η</mi><mo><</mo><mn>0</mn></mrow></math></span>, as the deviation parameter decreases, the opening angle of the resulting cone becomes smaller, leading to a shift of the resulting quasi-periodic oscillations (QPOs) from low to high frequencies. On the other hand, for <span><math><mrow><mi>η</mi><mo>></mo><mn>0</mn></mrow></math></span>, it is observed that the shock cone forms around the naked singularity at small values of <span><math><mi>η</mi></math></span>. Furthermore, at large <span><math><mi>η</mi></math></span> values, the cone evolves into a torus-like structure under the influence of the strong gravitational field. In the case of <span><math><mrow><mrow><mo>|</mo><mi>η</mi><mo>|</mo></mrow><mo>∼</mo><mn>8</mn></mrow></math></span>, perfect harmonicity is observed, along with possible resonances such as the 3:2 ratio, consistent with observations. Additionally, for the case of a slowly rotating black hole (<span><math><mrow><mi>a</mi><mo>/</mo><mi>M</mi><mo>=</mo><mn>0</mn><mo>.</mo><mn>4</mn></mrow></math></span>), a behavior resembling the bending of the shock cone due to the curvature of spacetime in the presence of a strong gravitational field is also observed at large <span><math><mi>η</mi></math></span> values, similar to what is observed when the spin parameter of the Kerr black hole is <span><math><mrow><mi>a</mi><mo>/</mo><mi>M</mi><mo>≥</mo><mn>0</mn><mo>.</mo><mn>9</mn></mrow></math></span>. Finally, we have calculated fundamental frequencies to investigate QPOs around rotating JP black holes. We use Markov Chain Monte Carlo (MCMC) analyses to obtain constrained values for the black hole mass, spacetime deformation, and QPO orbits around black hole candidates at the center of the Milky Way and M82 galaxies, and microquasars XTE J1550, GRO J1655-40,& GRS 1915-105, using QPO data observed in them. Overall, the JP metric with moderate deviation (<span><math><mrow><mrow><mo>|</mo><mi>η</mi><mo>|</mo></mrow><mo>≈</mo><mn>8</mn></mrow></math></span>) is more consistent with the observed QPO frequencies and resonance structures than the pure Kerr metric, suggesting that small deviations from Kerr spacetime may more accurately describe strong field gravity around astrophysical black holes.</di","PeriodicalId":8249,"journal":{"name":"Annals of Physics","volume":"486 ","pages":"Article 170350"},"PeriodicalIF":3.0,"publicationDate":"2026-01-12","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145973931","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 : 2026-01-10DOI: 10.1016/j.aop.2026.170344
Dongyang Yu
The Lipkin–Meshkov–Glick (LMG) model is paradigmatic for studying quantum phase transitions in equilibrium or non-equilibrium systems and entanglement dynamics in a variety of disciplines. A generic LMG model typically incorporates dual nonlinear interactions. While the classical dynamics of the single-nonlinear-interaction LMG model is well understood through Jacobi elliptic functions, the dual-interaction case remains unexplored owing to analytical challenges. By constructing an auxiliary function that maps the dynamics to the complex plane of Jacobi elliptic functions, we derive the exact solutions of the classical dynamics for the dual-interaction LMG model. Based on the exact solutions, we provide the classical dynamical phase diagram of the LMG model with dual nonlinear interactions, and find out the non-logarithmic behavior of dynamical criticality that is absent in the case of single nonlinear interaction. Our results establish a benchmark for analyzing the quantum dynamical phase transitions and many-body entanglement dynamics of finite-size LMG models with dual nonlinear interactions.
{"title":"Exact solutions and dynamical phase transitions in the Lipkin–Meshkov–Glick model with dual nonlinear interactions","authors":"Dongyang Yu","doi":"10.1016/j.aop.2026.170344","DOIUrl":"10.1016/j.aop.2026.170344","url":null,"abstract":"<div><div>The Lipkin–Meshkov–Glick (LMG) model is paradigmatic for studying quantum phase transitions in equilibrium or non-equilibrium systems and entanglement dynamics in a variety of disciplines. A generic LMG model typically incorporates dual nonlinear interactions. While the classical dynamics of the single-nonlinear-interaction LMG model is well understood through Jacobi elliptic functions, the dual-interaction case remains unexplored owing to analytical challenges. By constructing an auxiliary function that maps the dynamics to the complex plane of Jacobi elliptic functions, we derive the exact solutions of the classical dynamics for the dual-interaction LMG model. Based on the exact solutions, we provide the classical dynamical phase diagram of the LMG model with dual nonlinear interactions, and find out the non-logarithmic behavior of dynamical criticality that is absent in the case of single nonlinear interaction. Our results establish a benchmark for analyzing the quantum dynamical phase transitions and many-body entanglement dynamics of finite-size LMG models with dual nonlinear interactions.</div></div>","PeriodicalId":8249,"journal":{"name":"Annals of Physics","volume":"486 ","pages":"Article 170344"},"PeriodicalIF":3.0,"publicationDate":"2026-01-10","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145973989","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}
We explore the strong-field effects of a screened dark-sector interaction by embedding a Yukawa-type scalar field in Scalar–Tensor–Vector Gravity (MOG) and constructing a static, spherically symmetric black hole solution. Building on this geometry, we develop a consistent thermodynamic description and obtain analytic expressions for the Hawking temperature, entropy, and heat capacity. The resulting phase structure identifies parameter windows where the black hole is locally stable and loci where instabilities or transitions may occur. We then study equatorial geodesics and circular motion, deriving the effective potential, the specific energy and angular momentum at circular orbits, and the innermost stable circular orbits (ISCOs). The Yukawa screening scale and coupling, in conjunction with the MOG parameter, yield systematic shifts in the ISCO radius and binding energy relative to general relativity and the unscreened MOG. Finally, we evaluated the center-of-mass energy for two-particle collisions near the event horizon. We show how screened interactions alter the attainable collision energy spectra, particularly the near-horizon enhancement. Thermodynamic, orbital, and collisional analyses provide insight into deviations induced by the Yukawa field. We discuss how these effects can be leveraged as observables to test screened dark-sector interactions and the viability of MOG in astrophysical black-hole systems.
{"title":"Yukawa black holes in modified gravity: From thermodynamics to particle collisions","authors":"Isomiddin Nishonov , Bekzod Rahmatov , Saeed Ullah Khan , Muhammad Zahid , Javlon Rayimbaev , Inomjon Ibragimov , Erkaboy Davletov","doi":"10.1016/j.aop.2025.170332","DOIUrl":"10.1016/j.aop.2025.170332","url":null,"abstract":"<div><div>We explore the strong-field effects of a screened dark-sector interaction by embedding a Yukawa-type scalar field in Scalar–Tensor–Vector Gravity (MOG) and constructing a static, spherically symmetric black hole solution. Building on this geometry, we develop a consistent thermodynamic description and obtain analytic expressions for the Hawking temperature, entropy, and heat capacity. The resulting phase structure identifies parameter windows where the black hole is locally stable and loci where instabilities or transitions may occur. We then study equatorial geodesics and circular motion, deriving the effective potential, the specific energy and angular momentum at circular orbits, and the innermost stable circular orbits (ISCOs). The Yukawa screening scale and coupling, in conjunction with the MOG parameter, yield systematic shifts in the ISCO radius and binding energy relative to general relativity and the unscreened MOG. Finally, we evaluated the center-of-mass energy for two-particle collisions near the event horizon. We show how screened interactions alter the attainable collision energy spectra, particularly the near-horizon enhancement. Thermodynamic, orbital, and collisional analyses provide insight into deviations induced by the Yukawa field. We discuss how these effects can be leveraged as observables to test screened dark-sector interactions and the viability of MOG in astrophysical black-hole systems.</div></div>","PeriodicalId":8249,"journal":{"name":"Annals of Physics","volume":"486 ","pages":"Article 170332"},"PeriodicalIF":3.0,"publicationDate":"2026-01-08","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145922858","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 : 2026-01-08DOI: 10.1016/j.aop.2026.170348
Rachid El Aitouni , Aotmane En Naciri , Clarence Cortes , David Laroze , Ahmed Jellal
We study how fermions in molybdenum disulfide MoS interact with a laser field and a static potential barrier, focusing on the transmission probability. Our aim is to understand and control photon-assisted quantum transport in this two-dimensional material under external driving. We use the Floquet approximation to describe the wave functions in the three regions of the system. By applying continuity conditions at the boundaries, we obtain a set of equations involving an infinite number of Floquet modes. We explicitly determine transmissions involving the central band and the first sidebands . As for higher-order bands, we use the transfer matrix approach together with current density to compute the associated transmissions. Our results reveal that the transmission probability oscillates for both spin-up and spin-down electrons. The oscillations of spin-down electrons occur over nearly twice the period of spin-up electrons. Among all bands, the central one consistently shows the highest transmission. We also find that stronger laser fields and wider barriers both lead to reduced transmission. Moreover, laser irradiation enables controllable channeling and filtering of transmission bands by tuning the laser intensity and system parameters. This highlights the potential of laser-driven MoS structures for highly sensitive electromagnetic sensors and advanced optoelectronic devices.
{"title":"Floquet-driven tunneling control in monolayer MoS2","authors":"Rachid El Aitouni , Aotmane En Naciri , Clarence Cortes , David Laroze , Ahmed Jellal","doi":"10.1016/j.aop.2026.170348","DOIUrl":"10.1016/j.aop.2026.170348","url":null,"abstract":"<div><div>We study how fermions in molybdenum disulfide MoS<span><math><msub><mrow></mrow><mrow><mn>2</mn></mrow></msub></math></span> interact with a laser field and a static potential barrier, focusing on the transmission probability. Our aim is to understand and control photon-assisted quantum transport in this two-dimensional material under external driving. We use the Floquet approximation to describe the wave functions in the three regions of the system. By applying continuity conditions at the boundaries, we obtain a set of equations involving an infinite number of Floquet modes. We explicitly determine transmissions involving the central band <span><math><mi>E</mi></math></span> and the first sidebands <span><math><mrow><mi>E</mi><mo>±</mo><mo>ħ</mo><mi>ω</mi></mrow></math></span>. As for higher-order bands, we use the transfer matrix approach together with current density to compute the associated transmissions. Our results reveal that the transmission probability oscillates for both spin-up and spin-down electrons. The oscillations of spin-down electrons occur over nearly twice the period of spin-up electrons. Among all bands, the central one consistently shows the highest transmission. We also find that stronger laser fields and wider barriers both lead to reduced transmission. Moreover, laser irradiation enables controllable channeling and filtering of transmission bands by tuning the laser intensity and system parameters. This highlights the potential of laser-driven MoS<span><math><msub><mrow></mrow><mrow><mn>2</mn></mrow></msub></math></span> structures for highly sensitive electromagnetic sensors and advanced optoelectronic devices.</div></div>","PeriodicalId":8249,"journal":{"name":"Annals of Physics","volume":"486 ","pages":"Article 170348"},"PeriodicalIF":3.0,"publicationDate":"2026-01-08","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145922874","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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