Annals of Physics最新文献

{"title":"Analyzing the effect of higher dimensions on the black hole silhouette, deflection angles, and PINN approximated quasinormal modes","authors":"Nikko John Leo S. Lobos ,&nbsp;Anele M. Ncube ,&nbsp;Reggie C. Pantig ,&nbsp;Alan S. Cornell","doi":"10.1016/j.aop.2024.169906","DOIUrl":"10.1016/j.aop.2024.169906","url":null,"abstract":"<div><div>This study investigates the effects of higher dimensions on the observable properties of Schwarzschild-Tangherlini black holes, focusing on the photonsphere, shadow radius, deflection angles, and quasinormal modes (QNMs). By extending classical methods with Physics-Informed Neural Networks (PINNs), the research examines how increasing dimensionality alters these properties, causing shadow size reduction, weaker deflection angles, and shifts in QNM frequencies. The findings suggest that as black holes increase in dimensionality, their gravitational influence diminishes, particularly affecting light deflection and the stability of photon orbits. Through both weak and strong deflection analyses, this study indicates the need for ultrasensitive technology to detect these higher-dimensional signatures. Remarks on the observational data constraints currently favor four-dimensional spacetime; however, the exploration of additional dimensions remains vital in advancing models of quantum gravity. This work provides a theoretical framework for understanding black hole behavior in higher dimensions, potentially informing future astrophysical observations.</div></div>","PeriodicalId":8249,"journal":{"name":"Annals of Physics","volume":"473 ","pages":"Article 169906"},"PeriodicalIF":3.0,"publicationDate":"2025-02-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143098963","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}

{"title":"Emergent universe in f(Q) gravity theories","authors":"Hamid Shabani ,&nbsp;Avik De ,&nbsp;Tee-How Loo","doi":"10.1016/j.aop.2024.169900","DOIUrl":"10.1016/j.aop.2024.169900","url":null,"abstract":"<div><div>One resolution of the ancient cosmic singularity, i.e., the Big Bang Singularity (BBS), is to assume an inflationary stage preceded by a long enough static state in which the universe and its physical properties would oscillate around certain equilibrium points. The early period is referred to as the Einstein Static (ES) Universe phase, which characterizes a static phase with positive spatial curvature. A stable Einstein static state can serve as a substitute for BBS, followed by an inflationary period known as the Emergent Scenario. The initial need has not been fulfilled within the context of General Relativity, prompting the investigation of modified theories of gravity. The current research aims to find such a solution within the framework of symmetric teleparallel gravity, specifically in the trendy <span><math><mrow><mi>f</mi><mrow><mo>(</mo><mi>Q</mi><mo>)</mo></mrow></mrow></math></span> theories. An analysis has been conducted to investigate stable solutions for both positively and negatively curved spatial FRW universes, in the presence of a perfect fluid, by utilizing various torsion-free and curvature-free affine connections. Additionally, we propose a method to facilitate an exit from a stable ES to a subsequent inflationary phase. We demonstrate that <span><math><mrow><mi>f</mi><mrow><mo>(</mo><mi>Q</mi><mo>)</mo></mrow></mrow></math></span> gravity theories have the ability to accurately depict the emergence of the universe.</div></div>","PeriodicalId":8249,"journal":{"name":"Annals of Physics","volume":"473 ","pages":"Article 169900"},"PeriodicalIF":3.0,"publicationDate":"2025-02-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143099308","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}

{"title":"Weyl cohomology and the conformal anomaly in the presence of torsion","authors":"Gregorio Paci,&nbsp;Omar Zanusso","doi":"10.1016/j.aop.2024.169877","DOIUrl":"10.1016/j.aop.2024.169877","url":null,"abstract":"<div><div>Using cohomological methods, we identify both trivial and nontrivial contributions to the conformal anomaly in the presence of vectorial torsion in <span><math><mrow><mi>d</mi><mo>=</mo><mn>2</mn><mo>,</mo><mn>4</mn></mrow></math></span> dimensions. In both cases, our analysis considers two scenarios: one in which the torsion vector transforms in an affine way, i.e., it is a gauge potential for Weyl transformations, and the other in which it is invariant under the Weyl group. An important outcome for the former case in both <span><math><mrow><mi>d</mi><mo>=</mo><mn>2</mn><mo>,</mo><mn>4</mn></mrow></math></span> is the presence of anomalies of a “mixed” nature in relation to the classification of Deser and Schwimmer. For invariant torsion in <span><math><mrow><mi>d</mi><mo>=</mo><mn>4</mn></mrow></math></span>, we also find a new type of anomaly which we dub <span><math><mi>Ψ</mi></math></span>-anomaly. Taking these results into account, we integrate the different anomalies to obtain renormalized anomalous effective actions. Thereafter, we recast such actions in the covariant nonlocal and local forms, the latter being easier to work with. Along the way, we pause to comment on the physical usefulness of these effective actions, in particular to obtain renormalized energy–momentum tensors and thermodynamics of <span><math><mrow><mn>2</mn><mi>d</mi></mrow></math></span> black holes.</div></div>","PeriodicalId":8249,"journal":{"name":"Annals of Physics","volume":"473 ","pages":"Article 169877"},"PeriodicalIF":3.0,"publicationDate":"2025-02-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143150177","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"OA","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Investigating quantum criticality through charged scalar fields near the BTZ black hole horizon","authors":"Abdullah Guvendi ,&nbsp;Omar Mustafa","doi":"10.1016/j.aop.2024.169897","DOIUrl":"10.1016/j.aop.2024.169897","url":null,"abstract":"<div><div>We examine a charged scalar field with a position-dependent mass <span><math><mrow><mi>m</mi><mrow><mo>(</mo><mi>ρ</mi><mo>)</mo></mrow><mo>=</mo><msub><mrow><mi>m</mi></mrow><mrow><mn>0</mn></mrow></msub><mo>+</mo><mi>S</mi><mrow><mo>(</mo><mi>ρ</mi><mo>)</mo></mrow></mrow></math></span>, where <span><math><mrow><mi>S</mi><mrow><mo>(</mo><mi>ρ</mi><mo>)</mo></mrow></mrow></math></span> represents a Lorentz scalar potential, near a BTZ black hole in the presence of an external magnetic field. By deriving the Klein–Gordon equation for this setup, we explore two scenarios: (i) a mass-modified scalar field with <span><math><mrow><mi>m</mi><mrow><mo>(</mo><mi>ρ</mi><mo>)</mo></mrow><mo>=</mo><msub><mrow><mi>m</mi></mrow><mrow><mn>0</mn></mrow></msub><mo>−</mo><mi>a</mi><mo>/</mo><mi>ρ</mi></mrow></math></span> (an exactly solvable case), and (ii) a scenario involving both mass modification and an external magnetic field (conditionally exactly solvable). We identify quantum critical points (QCPs) associated with the coupling constant <span><math><mi>a</mi></math></span>. In the first scenario, for massless charged scalar fields, critical points occur at <span><math><mrow><mi>a</mi><mo>=</mo><mi>n</mi><mo>+</mo><mn>1</mn><mo>/</mo><mn>2</mn></mrow></math></span> for all radial quantum numbers <span><math><mrow><mi>n</mi><mo>≥</mo><mn>0</mn></mrow></math></span> and magnetic quantum numbers <span><math><mrow><mrow><mo>|</mo><mi>m</mi><mo>|</mo></mrow><mo>≥</mo><mn>0</mn></mrow></math></span>. In the second scenario, these critical points shift to <span><math><mrow><mi>a</mi><mo>=</mo><mi>n</mi><mo>+</mo><mn>3</mn><mo>/</mo><mn>2</mn></mrow></math></span> for <span><math><mrow><mi>n</mi><mo>≥</mo><mn>0</mn></mrow></math></span> and <span><math><mrow><mrow><mo>|</mo><mi>m</mi><mo>|</mo></mrow><mo>&gt;</mo><mn>0</mn></mrow></math></span>, with the case <span><math><mrow><mi>m</mi><mo>=</mo><mn>0</mn></mrow></math></span> excluded. For massive scalar fields, QCPs emerge at <span><math><mrow><mi>a</mi><mo>=</mo><mrow><mo>(</mo><mi>n</mi><mo>+</mo><mn>1</mn><mo>/</mo><mn>2</mn><mo>)</mo></mrow><mo>/</mo><mn>2</mn></mrow></math></span>, leading to non-propagating fields at zero frequency. At these QCPs, the field frequencies drop to zero, marking transitions from stable oscillatory modes to non-propagating states. Below the critical points, the system exhibits instability, characterized by negative imaginary frequencies that suggest rapid decay and high dissipation. Above the critical points, the modes stabilize and propagate, indicating a transition to a superconducting-like phase, where dissipation vanishes and stable excitations dominate.</div></div>","PeriodicalId":8249,"journal":{"name":"Annals of Physics","volume":"473 ","pages":"Article 169897"},"PeriodicalIF":3.0,"publicationDate":"2025-02-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143149609","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}

{"title":"Gravitational lensing and image distortion by Buchdahl inspired metric in R2 gravity","authors":"Shafia Maryam ,&nbsp;Mubasher Jamil ,&nbsp;Mustapha Azreg-Aïnou ,&nbsp;Zoe C.S. Chan","doi":"10.1016/j.aop.2024.169911","DOIUrl":"10.1016/j.aop.2024.169911","url":null,"abstract":"<div><div>We investigate gravitational lensing by <em>special</em> Buchdahl inspired metric with the Buchdahl parameter <span><math><mover><mrow><mi>k</mi></mrow><mrow><mo>̃</mo></mrow></mover></math></span>. In strong deflection limit, we derive the deflection angle analytically for the light rays that diverge as photons approach the photon sphere. These are then used in order to compute the angular image positions modeling supermassive black holes, Sgr A* and M87* as lenses. The Einstein rings for the outermost relativistic images are also depicted here alongside observational constraints on <span><math><mover><mrow><mi>k</mi></mrow><mrow><mo>̃</mo></mrow></mover></math></span> by the Einstein radius and lens mass. Constraints on <span><math><mover><mrow><mi>k</mi></mrow><mrow><mo>̃</mo></mrow></mover></math></span> are obtained modeling black holes (Sgr A* and M87*) and Canarias Einstein ring. In weak deflection limit, the analytic expression of deflection angle of the subject asymptotically flat metric in <span><math><msup><mrow><mi>R</mi></mrow><mrow><mn>2</mn></mrow></msup></math></span> gravity is determined using the Gauss Bonnet theorem. Considering M87* as a lens, weak deflection angle is used to study the image magnification and image distortion for primary and secondary images. It is shown that image distortion satisfies the hypothesis of Virbhadra. Moreover, it is seen that our general expression of deflection angle reduces, as a special case, to the deflection angle of Schwarzschild metric in both weak and strong deflection limits.</div></div>","PeriodicalId":8249,"journal":{"name":"Annals of Physics","volume":"473 ","pages":"Article 169911"},"PeriodicalIF":3.0,"publicationDate":"2025-02-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143098529","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}

{"title":"Yang–Mills extension of the Loop Quantum Gravity-corrected Maxwell equations","authors":"G.L.L.W. Levy,&nbsp;J.A. Helayël-Neto","doi":"10.1016/j.aop.2024.169892","DOIUrl":"10.1016/j.aop.2024.169892","url":null,"abstract":"<div><div>In this paper, we endeavor to build up a non-Abelian formulation to describe the self-interactions of massless vector bosons in the context of Loop Quantum Gravity (LQG). To accomplish this task, we start off from the modified Maxwell equations with the inclusion of LQG corrections and its corresponding local <span><math><mrow><mi>U</mi><mrow><mo>(</mo><mn>1</mn><mo>)</mo></mrow></mrow></math></span> gauge invariance. LQG effects in the electromagnetic interactions have significant importance, as they might be adopted to describe the flight time of cosmic photons coming from very high-energy explosions in the Universe, such as events of Gamma-Ray Bursts (GRBs). These photons have energy-dependent speeds, indicating that the velocity of light in the vacuum is not constant. To carry out the extension from the Abelian to the non-Abelian scenario, we shall follow the so-called Noether current procedure, which consists in recurrently introducing self-interactions into an initially free action for vector bosons by coupling the latter to the conserved currents of a global symmetry present in the action of departure. In the end of the non-Abelianization process, the initial global symmetry naturally becomes local. Once the Yang–Mills system includes LQG correction terms, it becomes possible to analyze how quantum-gravity induced contributions show up in both the electroweak and the QCD sectors of the Standard Model, providing a set-up for phenomenological investigations that may bring about new elements to discuss Physics beyond the Standard-Model.</div></div>","PeriodicalId":8249,"journal":{"name":"Annals of Physics","volume":"473 ","pages":"Article 169892"},"PeriodicalIF":3.0,"publicationDate":"2025-02-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143099311","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}

{"title":"Inflation in a scalar-vector gravity theory","authors":"Manuel Gonzalez-Espinoza ,&nbsp;Ramón Herrera","doi":"10.1016/j.aop.2024.169876","DOIUrl":"10.1016/j.aop.2024.169876","url":null,"abstract":"<div><div>We study the possibility that inflation is driven by a scalar field together with a vector field minimally coupled to gravity. By assuming an effective potential that incorporates both fields into the action, we explore two distinct scenarios: one where the fields interact and another where they do not. In this context, we find different analytical solutions to the background scalar-vector fields dynamics during the inflationary scenario considering the slow-roll approximation. Besides, general conditions required for these models of two fields to be realizable are determined and discussed. From the cosmological perturbations, we consider a local field rotation, and then we determine these perturbations (scalar and tensor) during inflation, and we also utilize recent cosmological observations for constraining the parameter-space in these scalar-vector inflationary models.</div></div>","PeriodicalId":8249,"journal":{"name":"Annals of Physics","volume":"473 ","pages":"Article 169876"},"PeriodicalIF":3.0,"publicationDate":"2025-02-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143099316","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}

{"title":"New canonical analysis for consistent extension of λR gravity","authors":"Alberto Escalante,&nbsp;P. Fernando Ocaña-García","doi":"10.1016/j.aop.2024.169916","DOIUrl":"10.1016/j.aop.2024.169916","url":null,"abstract":"<div><div>The canonical analysis of the <span><math><mrow><mi>λ</mi><mi>R</mi></mrow></math></span> model extended with the term due to Blas, Pujolas, and Sibiryakov <span><math><mrow><mo>[</mo><mi>B</mi><mi>P</mi><mi>S</mi><mo>]</mo></mrow></math></span> is performed. The analysis is developed for any value of <span><math><mi>λ</mi></math></span>, but particular attention is paid to the point <span><math><mrow><mi>λ</mi><mo>=</mo><mfrac><mrow><mn>1</mn></mrow><mrow><mn>3</mn></mrow></mfrac></mrow></math></span> because of the closeness with linearized General Relativity [GR]. Then, we add the higher-order conformal term, the so-called Cotton-square term, to study the constraint structure of what constitutes an example of kinetic-conformal Horava’s gravity. At the conformal point, an extra second-class constraint appears; this does not arise at other values of <span><math><mi>λ</mi></math></span>. Then, the Dirac brackets are constructed, and we will observe that the <span><math><mrow><mi>λ</mi><mi>R</mi></mrow></math></span>-Cotton-square model shares the same number of degrees of freedom with linearized <span><math><mrow><mi>G</mi><mi>R</mi></mrow></math></span>.</div></div>","PeriodicalId":8249,"journal":{"name":"Annals of Physics","volume":"473 ","pages":"Article 169916"},"PeriodicalIF":3.0,"publicationDate":"2025-02-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143098528","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"OA","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Quasi-local mass on rigid or round spheres in Kerr spacetime","authors":"Jacek Jezierski,&nbsp;Tomasz Smołka","doi":"10.1016/j.aop.2024.169905","DOIUrl":"10.1016/j.aop.2024.169905","url":null,"abstract":"<div><div>We introduce and analyze quasi-local mass using Hamiltonian methods. It is based on multipole decomposition for surfaces that are topological spheres. Based on the above model, tests were performed for Kerr spacetime for two arbitrary choices of surfaces: rigid spheres and round spheres. The model predicts upper and lower bounds on the total mass.</div></div>","PeriodicalId":8249,"journal":{"name":"Annals of Physics","volume":"473 ","pages":"Article 169905"},"PeriodicalIF":3.0,"publicationDate":"2025-02-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143098530","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}

{"title":"Aharonov–Bohm effect in an attractive inverse-square potential","authors":"J. Carvalho Veloso,&nbsp;K. Bakke","doi":"10.1016/j.aop.2024.169902","DOIUrl":"10.1016/j.aop.2024.169902","url":null,"abstract":"<div><div>We search for the Aharonov-Bohm effect for bound states when a point charge is confined to an attractive inverse-square potential. Then, we extend our discussion to the persistent currents and the revival times. In another perspective, we discuss the case in which the centrifugal term is the dominant term. In this case, we confine the point charge to two cylindrical surfaces with impenetrable potential walls and obtain the energy levels. We also discuss the Aharonov–Bohm effect for bound states and persistent currents. Finally, we calculate the revival times.</div></div>","PeriodicalId":8249,"journal":{"name":"Annals of Physics","volume":"473 ","pages":"Article 169902"},"PeriodicalIF":3.0,"publicationDate":"2025-02-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143098965","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}