Gravitation and Cosmology最新文献_第6页

Scalar Fields for Bianchi-I Model in (boldsymbol{f(R,T)}) Theory of Gravity $$boldsymbol{f(R,T)}$$ 引力理论中比安奇-I 模型的标量场

IF 1.2 4区物理与天体物理

Gravitation and Cosmology Pub Date : 2024-05-21 DOI: 10.1134/S0202289324700117

Yasemin Kabaoğlu, Can Aktaş

引用次数: 0

Shadows and Photon Rings of Binary Black Holes 双黑洞的阴影和光子环

IF 1.2 4区物理与天体物理

Gravitation and Cosmology Pub Date : 2024-05-21 DOI: 10.1134/S0202289324700063

S. V. Chernov

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Arions Generation by Magnetodipole Waves of Pulsars and Magnetars in a Constant Magnetic Field 恒定磁场中脉冲星和磁星的磁偶极子波产生的氩离子

IF 1.2 4区物理与天体物理

Gravitation and Cosmology Pub Date : 2024-05-21 DOI: 10.1134/S0202289324700051

V. I. Denisov, G. A. Dantsev, V. I. Priclonsky, I. P. Denisova, O. N. Gavrish

{"title":"Arions Generation by Magnetodipole Waves of Pulsars and Magnetars in a Constant Magnetic Field","authors":"V. I. Denisov, G. A. Dantsev, V. I. Priclonsky, I. P. Denisova, O. N. Gavrish","doi":"10.1134/S0202289324700051","DOIUrl":"10.1134/S0202289324700051","url":null,"abstract":"The influence of the gravitational fields of pulsars and magnetars on the emission of arions (strictly massless pseudoscalar Goldstone particles) during propagation of magnetodipole waves in a constant magnetic field has been evaluated. The solution of the equation was obtained, and the flux of arions emitted by magnetodipole waves during their propagation in a constant magnetic field was found. It has been shown that the amplitude of a created arion wave at a distance from the source of magnetodipole radiation of a pulsar or magnetar, ((rtoinfty)), in the considered case tends to a constant value. The intensity of arion emission in a solid angle element and the amount of arion energy (overline{I}), emitted in all directions per unit time grow quadratically with increasing distance traveled by the magnetodipole radiation of a pulsar or magnetar in a constant magnetic field. Such growth of the energy is due to the fact that the constant magnetic field is defined in the whole space. In reality, the galactic and intergalactic magnetic fields can exist in this form only in finite regions of space, outside which the force lines of their induction vector are curved. Therefore, it is possible to apply these results only in a region of space for which (rleq L_{textrm{coh}}<infty), where (L_{textrm{coh}}) is the coherence length, the distance at which the force lines of the induction vector can be considered to be straight. An estimate for the value of the coupling constant of photons with arions is obtained.","PeriodicalId":583,"journal":{"name":"Gravitation and Cosmology","volume":"30 2","pages":"160 - 164"},"PeriodicalIF":1.2,"publicationDate":"2024-05-21","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141115529","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"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}

引用次数: 0

Formation of Supermassive Nuclei of Black Holes in the Early Universe by the Mechanism of Scalar-Gravitational Instability. II. Evolution of Localized Spherical Perturbations({}^{mathbf{1}}) 早期宇宙中黑洞超大质量核的形成：标量-引力不稳定性机制。II.局部球形扰动的演变 ${}^{mathbf{1}}$$

IF 1.2 4区物理与天体物理

Gravitation and Cosmology Pub Date : 2024-04-04 DOI: 10.1134/S0202289324010067

Yu. G. Ignat’ev

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On the Accelerated Expansion of the Universe 论宇宙的加速膨胀

IF 1.2 4区物理与天体物理

Gravitation and Cosmology Pub Date : 2024-04-04 DOI: 10.1134/S0202289324010080

Naman Kumar

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Noncanonical Domain Wall as a Unified Model of Dark Energy and Dark Matter: I. Cosmic Dynamics 作为暗能量和暗物质统一模型的非规范域壁：I. 宇宙动力学

IF 1.2 4区物理与天体物理

Gravitation and Cosmology Pub Date : 2024-04-04 DOI: 10.1134/S0202289324010092

Fargiza A. M. Mulki, Hesti Wulandari, Taufiq Hidayat

{"title":"Noncanonical Domain Wall as a Unified Model of Dark Energy and Dark Matter: I. Cosmic Dynamics","authors":"Fargiza A. M. Mulki, Hesti Wulandari, Taufiq Hidayat","doi":"10.1134/S0202289324010092","DOIUrl":"10.1134/S0202289324010092","url":null,"abstract":"We propose noncanonical domain walls as a new dark energy model inspired by Grand Unified theories (GUTs). We investigate the cosmic dynamics and discover that the domain walls act as either dark energy or dark matter at different times, depending on the velocity (v) in the observer’s comoving frame. We find a single stable solution to the dynamics, i.e., only freezing ((v=0)) noncanonical domain walls can enter the phantom zone without having to experience ghost field instability. This means that the solution has the equation of state (EoS) (w_{textrm{dw}}<-1) without having to possess negative kinetic energy. These domain walls give rise to a late-time cosmic acceleration starting from (zapprox 0.24), resulting in (w_{textrm{dw}}=-1.5) and (w_{textrm{eff}}=-1.03) today. We learn that the EoS of the noncanonical domain walls is independent from the potential form. We also investigate the perturbation dynamics following the model. Our simulations show that, compared to (Lambda)CDM, the amplitude of the dark matter power spectrum in the noncanonical domain wall model is lower, while the CMB power spectrum is shifted slightly to lower (l) multipoles. The proposed model gives a smaller (sigma_{8}) as compared to that of (Lambda)CDM.","PeriodicalId":583,"journal":{"name":"Gravitation and Cosmology","volume":"30 1","pages":"89 - 106"},"PeriodicalIF":1.2,"publicationDate":"2024-04-04","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"140575690","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"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}

引用次数: 0

Quantum Schwarzschild Black Hole Optical Aspects 量子 Schwarzschild 黑洞光学方面

IF 1.2 4区物理与天体物理

Gravitation and Cosmology Pub Date : 2024-04-04 DOI: 10.1134/S0202289324010043

Anas El Balali

{"title":"Quantum Schwarzschild Black Hole Optical Aspects","authors":"Anas El Balali","doi":"10.1134/S0202289324010043","DOIUrl":"10.1134/S0202289324010043","url":null,"abstract":"We investigate the optical behavior of a quantum Schwarzschild black hole with a space-time solution including a parameter (lambda) that encodes its discretization. Specifically, we derive the effective potential of this solution. In particular, we study circular orbits around the quantum black hole. Indeed, we find that the effective potential is characterized by a minimum and a maximum yielding double photon spheres denoted by (r_{p_{1}}) and (r_{p_{2}}). Then, we analyze the double shadow behavior as a function of the parameter (lambda), where we show that it controls the shadow circular size. An inspection of the Innermost Stable Circular Orbits (ISCO) shows that the radius (r_{textrm{ISCO}}) increases as a function of (lambda). Besides, we find that this radius is equal to (6M) for an angular momentum (L=2sqrt{3}) independently of (lambda). A numerical analysis shows that the photon sphere of radius (r_{p_{1}}) generates a shadow with a radius larger than (r_{textrm{ISCO}}). Thus, a truncation of the effective potential is imposed to exclude such behavior. Finally, the (lambda)-effect is inspected depending on the deflection angle of such a black hole, showing that it increases when higher values of the parameter (lambda) are considered. However, such an increase is limited by an upper bound given by ({6M}/{b}).","PeriodicalId":583,"journal":{"name":"Gravitation and Cosmology","volume":"30 1","pages":"71 - 84"},"PeriodicalIF":1.2,"publicationDate":"2024-04-04","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"140575703","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"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}

引用次数: 0

On Particle Collisions in the Vicinity of Charged Black Holes 带电黑洞附近的粒子碰撞

IF 1.2 4区物理与天体物理

Gravitation and Cosmology Pub Date : 2024-04-04 DOI: 10.1134/S0202289324010109

Timur Pryadilin, Daniil Zhitov, Vitalii Vertogradov

{"title":"On Particle Collisions in the Vicinity of Charged Black Holes","authors":"Timur Pryadilin, Daniil Zhitov, Vitalii Vertogradov","doi":"10.1134/S0202289324010109","DOIUrl":"10.1134/S0202289324010109","url":null,"abstract":"The process of particle collision in the vicinity of black holes is known to generate unbounded energies in the center-of-mass frame (the Bañados–Silk–West (BSW) effect) under specific conditions. We consider this process in the charged black hole metrics, namely, the Reissner–Nordström (RN) and Majumdar–Papapetrou (MP) metrics. We consider energy extraction from a Bardeen regular black hole due to the BSW effect. As in the RN case, we show that there is no restriction on energy extraction, but for real charged particles this effect is negligible. We derive necessary and sufficient conditions for this process. The conditions for the BSW effect in RN and MP metrics are shown to be identical, which is explained by the asymptotic equivalence of the two metrics near the horizons. Energy extraction in the RN metric is discussed. It is shown that if two real particles collide while falling onto a black hole, they are extremely unlikely to generate an ultra-massive particle. For the case of head-on collisions, we derive an upper bound on the extracted mass, which depends on the lapse function of the metric at the point of collision.","PeriodicalId":583,"journal":{"name":"Gravitation and Cosmology","volume":"30 1","pages":"48 - 56"},"PeriodicalIF":1.2,"publicationDate":"2024-04-04","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"140575500","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"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}

引用次数: 0

Cosmography of (boldsymbol{f(R,T)}) Gravity $$boldsymbol{f(R,T)}$$ 引力宇宙学

IF 1.2 4区物理与天体物理

Gravitation and Cosmology Pub Date : 2024-04-04 DOI: 10.1134/S0202289324010055

I. S. Farias, P. H. R. S. Moraes

{"title":"Cosmography of (boldsymbol{f(R,T)}) Gravity","authors":"I. S. Farias, P. H. R. S. Moraes","doi":"10.1134/S0202289324010055","DOIUrl":"10.1134/S0202289324010055","url":null,"abstract":"Currently, in order to explain the accelerated expansion phase of the Universe, several alternative approaches have been proposed, among which the most common are dark energy models and alternative theories of gravity. Although these approaches rest on very different physical aspects, it has been shown that both can be in agreement with the data in the current status of cosmological observations, thus leading to an enormous degeneration among these models. Therefore, until evidence of higher experimental accuracy is available, more conservative model-independent approaches are a useful tool for breaking this degenerated cosmological models picture. Cosmography as a kinematic study of the Universe is the most popular candidate in this regard. In this paper, we show how to construct the cosmographic equations for the (f(R,T)) theory of gravity within a conservative scenario of this theory, where (R) is the Ricci curvature scalar, and (T) is the trace of the energy-moment tensor. Such equations relate the (f(R,T)) function and its derivatives at current time (t_{0}) to the cosmographic parameters (q_{0}), (j_{0}), and (s_{0}). In addition, we show how these equations can be written within different dark energy scenarios, thus helping to discriminate among them. We also show how different (f(R,T)) gravity models can be constrained using these cosmographic equations.","PeriodicalId":583,"journal":{"name":"Gravitation and Cosmology","volume":"30 1","pages":"28 - 39"},"PeriodicalIF":1.2,"publicationDate":"2024-04-04","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"140575488","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"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}

引用次数: 0

The Extended Einstein–Maxwell-Aether-Axion Theory: Effective Metric as an Instrument of the Aetheric Control over the Axion Dynamics 扩展的爱因斯坦-麦克斯韦-乙太-轴子理论：作为乙太控制轴子动力学工具的有效度量

IF 1.2 4区物理与天体物理

Gravitation and Cosmology Pub Date : 2024-04-04 DOI: 10.1134/S020228932401002X

A. B. Balakin, A. F. Shakirzyanov

{"title":"The Extended Einstein–Maxwell-Aether-Axion Theory: Effective Metric as an Instrument of the Aetheric Control over the Axion Dynamics","authors":"A. B. Balakin, A. F. Shakirzyanov","doi":"10.1134/S020228932401002X","DOIUrl":"10.1134/S020228932401002X","url":null,"abstract":"In the framework of the Einstein–Maxwell-aether-axion theory, we consider a self-consistent model based on the concept of two-level control, which is carried out by the dynamic aether over the behavior of an axionically active electrodynamic system. The Lagrangian of this model contains two guiding functions, which depend on four differential invariants of the aether velocity: the scalar of expansion of the aether flow, the square of the acceleration four-vector, the squares of the shear and vorticity tensors. The guiding function of the first type is an element of the effective aetheric metric; this effective metric is involved in the formulation of kinetic terms for the vector, pseudoscalar and electromagnetic fields and predetermines features of their evolution. The guiding function of the second type is associated with the distribution of axions and describes its vacuum average value; basically, this function appears in the potential of the axion field and predetermines the position and depth of its minima. The self-consistent set of coupled master equations of the model is derived. An example of a static spherically symmetric system is considered as an application.","PeriodicalId":583,"journal":{"name":"Gravitation and Cosmology","volume":"30 1","pages":"57 - 67"},"PeriodicalIF":1.2,"publicationDate":"2024-04-04","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"140602840","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"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}

引用次数: 0