Pub Date : 2026-03-01Epub 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":"2026-03-01","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 : 2026-03-01Epub 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":"2026-03-01","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 : 2026-03-01Epub Date: 2025-12-30DOI: 10.1016/j.aop.2025.170327
Harshit Sharma, Udaysinh T. Bhosale
We study an -spin Floquet model with infinite-range Ising interactions and derive the general formula to calculate the single-qubit reduced density matrix and its linear entropy and entanglement entropy for any and . For systems up to 10 qubits, we analytically obtain the eigensystem, entanglement measures, and time-averaged linear entropy for arbitrary initial states and special values of and . For a special class of initial states and specific values of , the model was studied in earlier work. Here, we generalize those results to arbitrary initial states. We numerically find that the average concurrence decreases with , implying multipartite nature of entanglement. We numerically show that for both single-qubit and half-bipartitaion cases , when indicating non-integrability. Whereas for and , it deviates from 1, indicating integrability. In integrable cases, depth in entanglement grows with partition size. Possible experimental realizations are discussed.
{"title":"Exact solvability of entanglement for arbitrary initial state in an infinite-range Floquet system","authors":"Harshit Sharma, Udaysinh T. Bhosale","doi":"10.1016/j.aop.2025.170327","DOIUrl":"10.1016/j.aop.2025.170327","url":null,"abstract":"<div><div>We study an <span><math><mi>N</mi></math></span>-spin Floquet model with infinite-range Ising interactions and derive the general formula to calculate the single-qubit reduced density matrix and its linear entropy and entanglement entropy for any <span><math><mrow><mi>N</mi><mo>,</mo><mi>J</mi></mrow></math></span> and <span><math><mi>τ</mi></math></span>. For systems up to 10 qubits, we analytically obtain the eigensystem, entanglement measures, and time-averaged linear entropy for arbitrary initial states <span><math><mrow><mo>|</mo><msub><mrow><mi>θ</mi></mrow><mrow><mn>0</mn></mrow></msub><mo>,</mo><msub><mrow><mi>ϕ</mi></mrow><mrow><mn>0</mn></mrow></msub><mo>〉</mo></mrow></math></span> and special values of <span><math><mi>J</mi></math></span> and <span><math><mrow><mi>τ</mi><mo>=</mo><mi>π</mi><mo>/</mo><mn>4</mn></mrow></math></span>. For a special class of initial states and specific values of <span><math><mi>J</mi></math></span>, the model was studied in earlier work. Here, we generalize those results to arbitrary initial states. We numerically find that the average concurrence decreases with <span><math><mi>N</mi></math></span>, implying multipartite nature of entanglement. We numerically show that for both single-qubit and half-bipartitaion cases <span><math><mrow><mrow><mo>〈</mo><msub><mrow><mi>S</mi></mrow><mrow><mi>V</mi><mi>N</mi></mrow></msub><mo>〉</mo></mrow><mo>/</mo><msub><mrow><mi>S</mi></mrow><mrow><mi>M</mi><mi>a</mi><mi>x</mi></mrow></msub><mo>→</mo><mn>1</mn></mrow></math></span>, when <span><math><mrow><mi>J</mi><mo>≠</mo><mn>1</mn><mo>,</mo><mn>1</mn><mo>/</mo><mn>2</mn></mrow></math></span> indicating non-integrability. Whereas for <span><math><mrow><mi>J</mi><mo>=</mo><mn>1</mn></mrow></math></span> and <span><math><mrow><mn>1</mn><mo>/</mo><mn>2</mn></mrow></math></span>, it deviates from 1, indicating integrability. In integrable cases, depth in entanglement grows with partition size. Possible experimental realizations are discussed.</div></div>","PeriodicalId":8249,"journal":{"name":"Annals of Physics","volume":"486 ","pages":"Article 170327"},"PeriodicalIF":3.0,"publicationDate":"2026-03-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145883113","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 : 2026-03-01Epub Date: 2026-01-07DOI: 10.1016/j.aop.2026.170345
Alexey E. Rastegin
Kirkwood–Dirac quasiprobabilities are currently the subject of active studies. Such quasiprobabilities often give more convenient descriptions of measurement statistics. It is an alternative to the Wigner function. Methods of quantum information science use generalized measurements. Overcomplete sets of states are inevitable for these purposes. Here, complex projective two-designs are of certain interest. They include symmetric informationally complete measurements and complete sets of mutually unbiased bases. This study examines Kirkwood–Dirac quasiprobabilities for induced quantum measurements. It estimates norms and anti-norms of the matrices consisting of quasiprobabilities. Entropic uncertainty relations appear for unravelings of the corresponding quantum channels. Qubit examples of projective designs show the usefulness of the presented inequalities.
{"title":"Kirkwood–Dirac quasiprobabilities for measurements assigned to a projective two-design","authors":"Alexey E. Rastegin","doi":"10.1016/j.aop.2026.170345","DOIUrl":"10.1016/j.aop.2026.170345","url":null,"abstract":"<div><div>Kirkwood–Dirac quasiprobabilities are currently the subject of active studies. Such quasiprobabilities often give more convenient descriptions of measurement statistics. It is an alternative to the Wigner function. Methods of quantum information science use generalized measurements. Overcomplete sets of states are inevitable for these purposes. Here, complex projective two-designs are of certain interest. They include symmetric informationally complete measurements and complete sets of mutually unbiased bases. This study examines Kirkwood–Dirac quasiprobabilities for induced quantum measurements. It estimates norms and anti-norms of the matrices consisting of quasiprobabilities. Entropic uncertainty relations appear for unravelings of the corresponding quantum channels. Qubit examples of projective designs show the usefulness of the presented inequalities.</div></div>","PeriodicalId":8249,"journal":{"name":"Annals of Physics","volume":"486 ","pages":"Article 170345"},"PeriodicalIF":3.0,"publicationDate":"2026-03-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145922859","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 : 2026-03-01Epub Date: 2026-01-03DOI: 10.1016/j.aop.2026.170342
Valery Shchesnovich
Solvable bosonic models provide a fundamental framework for describing light propagation in nonlinear media, including optical down-conversion processes that generate squeezed states of light and their higher-order generalizations. In quantum optics a central objective is to determine the time evolution of a given initial state. Exact analytic solution to the state-evolution problem is presented, applicable to a broad class of solvable bosonic models and arbitrary initial states. Moreover, the characteristic equation governing the energy spectrum is derived and the eigenstates are found in the form of continued fractions and as the principal minors of the associated Jacobi matrix. The results provide a solid analytical framework for discussion of exactly solvable bosonic models.
{"title":"Exact state evolution and energy spectrum in solvable bosonic models","authors":"Valery Shchesnovich","doi":"10.1016/j.aop.2026.170342","DOIUrl":"10.1016/j.aop.2026.170342","url":null,"abstract":"<div><div>Solvable bosonic models provide a fundamental framework for describing light propagation in nonlinear media, including optical down-conversion processes that generate squeezed states of light and their higher-order generalizations. In quantum optics a central objective is to determine the time evolution of a given initial state. Exact analytic solution to the state-evolution problem is presented, applicable to a broad class of solvable bosonic models and arbitrary initial states. Moreover, the characteristic equation governing the energy spectrum is derived and the eigenstates are found in the form of continued fractions and as the principal minors of the associated Jacobi matrix. The results provide a solid analytical framework for discussion of exactly solvable bosonic models.</div></div>","PeriodicalId":8249,"journal":{"name":"Annals of Physics","volume":"486 ","pages":"Article 170342"},"PeriodicalIF":3.0,"publicationDate":"2026-03-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145922860","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":"2026-03-01","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 : 2026-03-01Epub 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":"2026-03-01","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}
Pub Date : 2026-02-01Epub Date: 2025-12-16DOI: 10.1016/j.aop.2025.170325
Toma Yoneya , Kazuya Fujimoto , Yuki Kawaguchi
The Monte Carlo trajectory sampling of stochastic differential equations based on the quasiprobability distribution functions, such as the Glauber–Sudarshan P, Wigner, and Husimi Q functions, enables us to investigate bosonic open quantum many-body dynamics described by the Gorini–Kossakowski–Sudarshan–Lindblad (GKSL) equation. In this method, the Monte Carlo samplings for the initial distribution and stochastic noises incorporate quantum fluctuations, and thus, we can go beyond the mean-field approximation. However, description using stochastic differential equations is possible only when the corresponding Fokker–Planck equation has a positive-semidefinite diffusion matrix. In this work, we analytically derive the stochastic differential equations for arbitrary Hamiltonian and jump operators based on the path-integral formula, independently of the derivation of the Fokker–Planck equation. In the course of the derivation, we formulate the path-integral representation of the GKSL equation by using the -ordered quasiprobability distribution function, which systematically describes the aforementioned quasiprobability distribution functions by changing the real parameter . The essential point of this derivation is that we employ the Hubbard–Stratonovich transformation in the path integral, and its application is not always feasible. We find that the feasible condition of the Hubbard–Stratonovich transformation is identical to the positive-semidefiniteness condition of the diffusion matrix in the Fokker–Planck equation. In the benchmark calculations, we confirm that the Monte Carlo simulations of the obtained stochastic differential equations well reproduce the exact dynamics of physical quantities and non-equal time correlation functions of numerically solvable models, including the Bose–Hubbard model. This work clarifies the applicability of the approximation and gives systematic and simplified procedures to obtain the stochastic differential equations to be numerically solved.
{"title":"Path-integral formulation of bosonic Markovian open quantum dynamics with Monte Carlo stochastic trajectories using the Glauber–Sudarshan P, Wigner, and Husimi Q functions and hybrids","authors":"Toma Yoneya , Kazuya Fujimoto , Yuki Kawaguchi","doi":"10.1016/j.aop.2025.170325","DOIUrl":"10.1016/j.aop.2025.170325","url":null,"abstract":"<div><div>The Monte Carlo trajectory sampling of stochastic differential equations based on the quasiprobability distribution functions, such as the Glauber–Sudarshan P, Wigner, and Husimi Q functions, enables us to investigate bosonic open quantum many-body dynamics described by the Gorini–Kossakowski–Sudarshan–Lindblad (GKSL) equation. In this method, the Monte Carlo samplings for the initial distribution and stochastic noises incorporate quantum fluctuations, and thus, we can go beyond the mean-field approximation. However, description using stochastic differential equations is possible only when the corresponding Fokker–Planck equation has a positive-semidefinite diffusion matrix. In this work, we analytically derive the stochastic differential equations for arbitrary Hamiltonian and jump operators based on the path-integral formula, independently of the derivation of the Fokker–Planck equation. In the course of the derivation, we formulate the path-integral representation of the GKSL equation by using the <span><math><mi>s</mi></math></span>-ordered quasiprobability distribution function, which systematically describes the aforementioned quasiprobability distribution functions by changing the real parameter <span><math><mi>s</mi></math></span>. The essential point of this derivation is that we employ the Hubbard–Stratonovich transformation in the path integral, and its application is not always feasible. We find that the feasible condition of the Hubbard–Stratonovich transformation is identical to the positive-semidefiniteness condition of the diffusion matrix in the Fokker–Planck equation. In the benchmark calculations, we confirm that the Monte Carlo simulations of the obtained stochastic differential equations well reproduce the exact dynamics of physical quantities and non-equal time correlation functions of numerically solvable models, including the Bose–Hubbard model. This work clarifies the applicability of the approximation and gives systematic and simplified procedures to obtain the stochastic differential equations to be numerically solved.</div></div>","PeriodicalId":8249,"journal":{"name":"Annals of Physics","volume":"485 ","pages":"Article 170325"},"PeriodicalIF":3.0,"publicationDate":"2026-02-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145836662","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Pub Date : 2026-02-01Epub Date: 2025-12-01DOI: 10.1016/j.aop.2025.170303
Sergiu I. Vacaru
Modified gravity theories (MGTs) have long been studied as alternatives to general relativity (GR) and the standard CDM cosmological model. For example, exponential models often yield better fits to observational data, suggesting that CDM may be inadequate. In this work, we argue that the gravitational and accelerating cosmology paradigm can remain close to GR and CDM if one considers broader classes of off-diagonal cosmological solutions of the Einstein equations. These solutions are constructed using the anholonomic frame and connection deformation method (AFCDM), which enables the decoupling and integration of nonlinear systems in nonholonomic dyadic variables with connection distortions. The resulting off-diagonal Einstein manifolds and cosmological models are characterized by nonholonomic constraints, nonlinear symmetries, and effective cosmological constants. Such structures allow one to approximate cosmological effects, mimic features of MGTs, and describe gravitational polarization, local anisotropies, and dark energy and dark matter phenomena within GR. We further show that these models can be endowed with relativistic versions of Perelman’s thermodynamic variables for geometric flows, which we compute in general form for accelerating cosmology.
{"title":"Off-diagonal solutions in Einstein gravity modeling f(R) gravity and dynamical dark energy vs ΛCDM cosmology","authors":"Sergiu I. Vacaru","doi":"10.1016/j.aop.2025.170303","DOIUrl":"10.1016/j.aop.2025.170303","url":null,"abstract":"<div><div>Modified gravity theories (MGTs) have long been studied as alternatives to general relativity (GR) and the standard <span><math><mi>Λ</mi></math></span>CDM cosmological model. For example, exponential <span><math><mrow><mi>f</mi><mrow><mo>(</mo><mi>R</mi><mo>)</mo></mrow></mrow></math></span> models often yield better fits to observational data, suggesting that <span><math><mi>Λ</mi></math></span>CDM may be inadequate. In this work, we argue that the gravitational and accelerating cosmology paradigm can remain close to GR and <span><math><mi>Λ</mi></math></span>CDM if one considers broader classes of off-diagonal cosmological solutions of the Einstein equations. These solutions are constructed using the anholonomic frame and connection deformation method (AFCDM), which enables the decoupling and integration of nonlinear systems in nonholonomic dyadic variables with connection distortions. The resulting off-diagonal Einstein manifolds and cosmological models are characterized by nonholonomic constraints, nonlinear symmetries, and effective cosmological constants. Such structures allow one to approximate cosmological effects, mimic features of MGTs, and describe gravitational polarization, local anisotropies, and dark energy and dark matter phenomena within GR. We further show that these models can be endowed with relativistic versions of Perelman’s thermodynamic variables for geometric flows, which we compute in general form for accelerating cosmology.</div></div>","PeriodicalId":8249,"journal":{"name":"Annals of Physics","volume":"485 ","pages":"Article 170303"},"PeriodicalIF":3.0,"publicationDate":"2026-02-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145692356","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 : 2026-02-01Epub Date: 2025-11-28DOI: 10.1016/j.aop.2025.170301
Rui Zhu
The pseudospin-3/2 Dirac–Weyl system is the kind of system bearing the quasiparticle band structure of two cones with different apex angles and their reversed replica touching at the apex, whose properties can be described by the pseudospin-3/2 Dirac equation. In this work, we analytically solved the pseudospin-3/2 Dirac equation and investigated the electronic transport properties in the double-barrier modulated two-dimensional system. The probability current density operator is explicitly derived from the time-dependent pseudospin-3/2 Dirac equation, which paves way for investigation of the electronic transport properties of general pseudospin- Dirac–Weyl systems with an integer or half integer larger than 1. As a result of the double-cone band structure, the pseudospin-3/2 system has two incident channels for a single incident energy and incident angle pair. Similar to its counterparts of pseudospin-1/2 and pseudospin-1 Dirac–Weyl systems, the Klein tunneling and resonant tunneling effects in the transmission probability are numerically observed for incidence coming from both Dirac cones in the double-barrier-modulated pseudospin-3/2 system. In contrast to its pseudospin-1/2 and -1 counterparts, the Klein tunneling and resonant tunneling effects are differentiated into double-channel and single-channel incidences, corresponding to different regimes in the - dispersion plane. Without a flat band, the super Klein tunneling effect of the pseudospin-1 Dirac–Weyl system does not occur in the pseudospin-3/2 system. Using the numerically obtained probability current density, the zero-temperature conductivity, shot noise, and Fano factor are calculated. As a combined result of double-channel incidence, Klein tunneling, and resonant tunneling, in comparison with its pseudospin-1/2 (graphene) and pseudospin-1 counterparts, the conductivity and shot noise in the pseudospin-3/2 double-barrier structure is enhanced. A Fano factor between 0.4 and 0.5 close to the Dirac point is observed.
{"title":"Transport properties of the pseudospin-3/2 Dirac–Weyl fermions in the double-barrier-modulated two-dimensional system","authors":"Rui Zhu","doi":"10.1016/j.aop.2025.170301","DOIUrl":"10.1016/j.aop.2025.170301","url":null,"abstract":"<div><div>The pseudospin-3/2 Dirac–Weyl system is the kind of system bearing the quasiparticle band structure of two cones with different apex angles and their reversed replica touching at the apex, whose properties can be described by the pseudospin-3/2 Dirac equation. In this work, we analytically solved the pseudospin-3/2 Dirac equation and investigated the electronic transport properties in the double-barrier modulated two-dimensional system. The probability current density operator is explicitly derived from the time-dependent pseudospin-3/2 Dirac equation, which paves way for investigation of the electronic transport properties of general pseudospin-<span><math><mi>s</mi></math></span> Dirac–Weyl systems with <span><math><mi>s</mi></math></span> an integer or half integer larger than 1. As a result of the double-cone band structure, the pseudospin-3/2 system has two incident channels for a single incident energy and incident angle pair. Similar to its counterparts of pseudospin-1/2 and pseudospin-1 Dirac–Weyl systems, the Klein tunneling and resonant tunneling effects in the transmission probability are numerically observed for incidence coming from both Dirac cones in the double-barrier-modulated pseudospin-3/2 system. In contrast to its pseudospin-1/2 and -1 counterparts, the Klein tunneling and resonant tunneling effects are differentiated into double-channel and single-channel incidences, corresponding to different regimes in the <span><math><mi>E</mi></math></span>-<span><math><msub><mrow><mi>k</mi></mrow><mrow><mi>y</mi></mrow></msub></math></span> dispersion plane. Without a flat band, the super Klein tunneling effect of the pseudospin-1 Dirac–Weyl system does not occur in the pseudospin-3/2 system. Using the numerically obtained probability current density, the zero-temperature conductivity, shot noise, and Fano factor are calculated. As a combined result of double-channel incidence, Klein tunneling, and resonant tunneling, in comparison with its pseudospin-1/2 (graphene) and pseudospin-1 counterparts, the conductivity and shot noise in the pseudospin-3/2 double-barrier structure is enhanced. A Fano factor between 0.4 and 0.5 close to the Dirac point <span><math><mrow><msub><mrow><mi>E</mi></mrow><mrow><mi>F</mi></mrow></msub><mo>=</mo><msub><mrow><mi>V</mi></mrow><mrow><mn>0</mn></mrow></msub></mrow></math></span> is observed.</div></div>","PeriodicalId":8249,"journal":{"name":"Annals of Physics","volume":"485 ","pages":"Article 170301"},"PeriodicalIF":3.0,"publicationDate":"2026-02-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145692411","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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