General Relativity and Gravitation最新文献

{"title":"Exploring the possibility of interacting quintessence model as an alternative to the (Lambda )CDM model","authors":"Nandan Roy","doi":"10.1007/s10714-023-03160-1","DOIUrl":"10.1007/s10714-023-03160-1","url":null,"abstract":"<div><p>This study examines interacting quintessence dark energy models and their observational constraints for a general parameterization of the quintessence potential, which encompasses a broad range of popular potentials. Four different forms of interactions are considered. The analysis is done by expressing the system as a set of autonomous equations for each interaction. The Bayesian Model Comparison has been used to compare these models with the standard Lambda Cold Dark Matter (<span>(Lambda )</span>CDM) model. Our analysis shows positive and moderate evidence for the interacting models over the <span>(Lambda )</span>CDM model. We also report the status of the Hubble tension for these models, even though there is an increment in the best-fit value of the Hubble parameters, these models can not resolve the Hubble tension.</p></div>","PeriodicalId":578,"journal":{"name":"General Relativity and Gravitation","volume":"55 10","pages":""},"PeriodicalIF":2.8,"publicationDate":"2023-10-15","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"71511236","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}

{"title":"The quasi-Keplerian motion in regular Bardeen spacetime","authors":"Jie Li,&nbsp;Bo Yang,&nbsp;Yu Wang,&nbsp;Wenbin Lin","doi":"10.1007/s10714-023-03166-9","DOIUrl":"10.1007/s10714-023-03166-9","url":null,"abstract":"<div><p>We present the second post-Newtonian solution for the quasi-Keplerian motion of a test particle in the gravitational field of Bardeen black hole. This solution is formulated in terms of energy and angular momentum of the particle, as well as the black hole’s magnetic charge. The leading effects of the magnetic charge on the test particle’s orbit and motion including perihelion precession are displayed explicitly. In particular, it is shown that the magnetic charge does not have effects on the orbital period when the second post-Newtonian order is considered.\u0000</p></div>","PeriodicalId":578,"journal":{"name":"General Relativity and Gravitation","volume":"55 10","pages":""},"PeriodicalIF":2.8,"publicationDate":"2023-10-14","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"71511235","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}

{"title":"Properties of Melvin–Taub–NUT spacetime with Manko–Ruiz parameter","authors":"Haryanto M. Siahaan,&nbsp;B. J. Bansawang,&nbsp;Tasrief Surungan,&nbsp;Paulus C. Tjiang","doi":"10.1007/s10714-023-03165-w","DOIUrl":"10.1007/s10714-023-03165-w","url":null,"abstract":"<div><p>In this study, we present a novel solution in Einstein–Maxwell theory that represents the magnetized Taub–NUT spacetime incorporating the Manko–Ruiz parameter. We investigate various aspects of this spacetime, including its curvature, closed timelike curve, and electromagnetic fields. Additionally, we explore the phenomenon of Hawking radiation within this magnetized spacetime by employing the tunneling picture. Our findings shed light on the unique characteristics and physical implications of the magnetized Taub–NUT spacetime with the Manko–Ruiz parameter.</p></div>","PeriodicalId":578,"journal":{"name":"General Relativity and Gravitation","volume":"55 10","pages":""},"PeriodicalIF":2.8,"publicationDate":"2023-10-13","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"71511234","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}

{"title":"Correction to: Formalism for stochastic perturbations and analysis in relativistic stars","authors":"Seema Satin","doi":"10.1007/s10714-023-03164-x","DOIUrl":"10.1007/s10714-023-03164-x","url":null,"abstract":"","PeriodicalId":578,"journal":{"name":"General Relativity and Gravitation","volume":"55 10","pages":""},"PeriodicalIF":2.8,"publicationDate":"2023-10-13","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"134878330","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}

{"title":"Qualitative stability analysis of cosmological models in (f(T,phi )) gravity","authors":"Amit Samaddar,&nbsp;S. Surendra Singh","doi":"10.1007/s10714-023-03163-y","DOIUrl":"10.1007/s10714-023-03163-y","url":null,"abstract":"<div><p>Using the dynamical system approach, we investigated the stability condition of two considered models in <span>(f(T,phi ))</span> gravity where <i>T</i> is the torsion scalar of teleparallel gravity and <span>(phi )</span> is a canonical scalar field. In this context, we are concerned with the phenomenology of the class of models with non-linear coupling to gravity and exponential potential. We assume the forms of G(T) as (i) <i>G</i>(<i>T</i>) = <span>(alpha T+frac{beta }{T})</span> and (ii) <i>G</i>(<i>T</i>) = <span>(zeta T)</span> ln<span>((psi T))</span>, where <span>(alpha )</span>, <span>(beta )</span>, <span>(zeta )</span> and <span>(psi )</span> be the free parameters and <i>G</i>(<i>T</i>) is the function of <i>T</i>. We evaluated the equilibrium points for these models and examine the stability behaviors. For Model I, we found four stable critical points while for Model II, we found three stable critical points. The stable critical points represent the attractors with accelerated expansion. The phase plots for these systems are examined and discussed the physical interpretation. We illustrate all the cosmological parameters such as <span>(Omega _{m})</span>, <span>(Omega _{phi })</span>, <i>q</i> and <span>(omega _{Tot})</span> at each fixed points and compare the parameters with observational values. In both Model I and Model II, we found <span>(Omega _{de}=1)</span> which represents the dark energy dominant Universe. Further, we assume hybrid scale factor to develop our model and this model produces a transition phase from deceleration to the acceleration. We transform all the parameters in redshift and examine the behavior of these parameters. From the Figures, it is observed that <span>(q=- 1)</span> represents the accelerating stage of the Universe and EoS parameter <span>(omega =-1)</span> represents the <span>(Lambda )</span>CDM model. For Model I, we get <span>(omega _{0}=- 0.992)</span> and for Model II, we get <span>(omega _{0}=- 0.883)</span> which is comparable to the observational data. The energy conditions are examined in terms of redshift while strong energy condition is violated for both models which shows the accelerated expansion evolution of present universe. We also find the statefinder parameters <span>({r,s})</span> in terms of <i>z</i> and discuss the nature of <span>(r-s)</span> and <span>(r-q)</span> plane. For both models, <span>(r=1, s=0)</span> and <span>(r=1, q=- 1)</span> represent the <span>(Lambda )</span>CDM model. We observed that our <span>(f(T,phi ))</span> models are stable and it is in accordance with the observational data.\u0000</p></div>","PeriodicalId":578,"journal":{"name":"General Relativity and Gravitation","volume":"55 10","pages":""},"PeriodicalIF":2.8,"publicationDate":"2023-10-10","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"71511230","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}

{"title":"On some phase equilibrium features of charged black holes in flat spacetime via Rényi statistics","authors":"F. Barzi,&nbsp;H. El Moumni,&nbsp;K. Masmar","doi":"10.1007/s10714-023-03158-9","DOIUrl":"10.1007/s10714-023-03158-9","url":null,"abstract":"<div><p>Motivated by the nonextensive nature of entropy in the gravitational context and the Gauge/Gravity duality, black hole thermodynamics has been attracting intense emphasis in the literature. Along the present work, we investigate some features of the phase structure and critical phenomena of the 4-dimensional charged black holes in asymptotically flat spacetime within the formalism of Rényi statistics. First, we explore the extended phase space via the Rényi statistics approach. Concretely, based on the modified version of the Smarr formula, we recall the equal-area law to remove the oscillatory non-physical region in the <span>(P_R-V)</span> and <span>(T_R-S_R)</span> planes. Then, the coexistence curves are determined, as well as the latent heat of phase change. Moreover, we prove that the critical exponent describing the behavior of the order parameter near the critical point is <span>(frac{1}{2})</span>, which is consistent with Landau’s theory of continuous phase transition. Lastly, we apply the Hamiltonian approach to Rényi thermodynamics which provides a new and solid mathematical basis for the extension of phase space and puts more insight into an expected and profound possible connection between the nonextensivity Rényi parameter <span>(lambda )</span> and the cosmological constant <span>( Lambda )</span>.\u0000</p></div>","PeriodicalId":578,"journal":{"name":"General Relativity and Gravitation","volume":"55 10","pages":""},"PeriodicalIF":2.8,"publicationDate":"2023-10-10","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"71511232","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}

{"title":"Optical behaviors of black holes in Starobinsky–Bel–Robinson gravity","authors":"A. Belhaj,&nbsp;H. Belmahi,&nbsp;M. Benali,&nbsp;Y. Hassouni,&nbsp;M. B. Sedra","doi":"10.1007/s10714-023-03159-8","DOIUrl":"10.1007/s10714-023-03159-8","url":null,"abstract":"<div><p>Inspired by M-theory scenarios, we investigate optical properties of black holes in the Starobinsky–Bel–Robinsion gravity. Precisely, we study the shadows and the deflection angle of light rays by this class of black holes in such a novel gravity. First, we approach the shadows of the Schwarzschild-type solutions. As expected, we find perfect circular shadows where the size decreases with a stringy gravity parameter denoted by <span>(beta )</span>. We reveal that this parameter is constrained by the shadow existence. Combining the Newman–Janis algorithm and the Hamilton–Jacobi mechanism, we examine the shadow behaviors of the rotating solutions in terms of one-dimensional real curves. Precisely, we obtain various sizes and shapes depending on the rotating parameter and the stringy gravity parameter <i>a</i> and <span>(beta )</span>, respectively. To examine the shadow geometric deformations, we study the astronomical observables and the energy emission rate. As envisaged, we show that <i>a</i> and <span>(beta )</span> have an impact on such shadow behaviors. For specific values of <i>a</i>, we remark that the obtained shadow shapes share certain similarities with the ones of the Kerr black holes in the plasma backgrounds. Using the Event Horizon Telescope observational data, we provide predictions for the stringy gravity parameter <span>(beta )</span> which could play a relevant role in the M-theory compactifications. After that, we discuss the behaviors of the light rays near to such four dimensional black holes by calculating the deflection angle in terms of a required moduli space. \u0000</p></div>","PeriodicalId":578,"journal":{"name":"General Relativity and Gravitation","volume":"55 10","pages":""},"PeriodicalIF":2.8,"publicationDate":"2023-10-10","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"71511233","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}

{"title":"Charged black string bounce and its field source","authors":"A. Lima,&nbsp;G. Alencar,&nbsp;R. N. Costa Filho,&nbsp;R. R. Landim","doi":"10.1007/s10714-023-03156-x","DOIUrl":"10.1007/s10714-023-03156-x","url":null,"abstract":"<div><p>This work builds upon the previous article (Lima in Symmetry 15:150, 2023) and explores the solution of the charged black string introduced in Lemos (Phys Rev 54:3840-3853, 1996). The black bounce regularization method, based on the Simpson-Visser solution, is employed by transforming the radial variable using <span>(rrightarrow sqrt{r^2+a^2})</span>. The regular charged black string metric is defined, and the properties of event horizons, surface gravity, and Hawking temperature are investigated. The behavior of curvature quantities, including curvature invariants and tensors, is examined to verify the absence of singularities when <span>(ane 0)</span>. The Einstein equation for the energy-momentum tensor is solved, and the null energy condition is analyzed for the obtained solution. The sources of this solution are evaluated, combining a scalar field with nonlinear electrodynamics. However, unlike other works, an electric field is considered instead of a magnetic field. Finally, the study calculates the possibility of stable or unstable circular orbits for massive and massless particles.</p></div>","PeriodicalId":578,"journal":{"name":"General Relativity and Gravitation","volume":"55 10","pages":""},"PeriodicalIF":2.8,"publicationDate":"2023-10-04","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"71511231","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}

{"title":"Particle creation and bulk viscosity in Bianchi-I universe in Saez–Ballester theory with different deceleration parameters","authors":"Chayanika Chetia,&nbsp;Mrinnoy M. Gohain,&nbsp;Kalyan Bhuyan","doi":"10.1007/s10714-023-03155-y","DOIUrl":"10.1007/s10714-023-03155-y","url":null,"abstract":"<div><p>In Saez–Ballester gravitational theory, we studied the role of particle creation and bulk viscosity in the evolution of a spatially homogeneous and anisotropic Bianchi type I universe. We treated particle creation and bulk viscosity as two distinct irreversible processes, and we modified the energy momentum tensor to account for viscous and particle creation pressures. We employed constant and variable deceleration parameters to obtain average scale factor solutions for the Bianchi type I model. The use of constant deceleration parameter resulted in two unique scale factor solutions that led to singular and non-singular natures of the universe with power-law and exponential laws, respectively. Furthermore, the variable deceleration parameter yielded a de Sitter like solution representing a non-singular universe. We also explored the temporal evolution of the bulk viscosity coefficient in Eckart’s theory, truncated theory, and full causal theory for all three models.</p></div>","PeriodicalId":578,"journal":{"name":"General Relativity and Gravitation","volume":"55 10","pages":""},"PeriodicalIF":2.8,"publicationDate":"2023-10-03","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"71511229","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}

{"title":"Hawking temperature of black holes with multiple horizons","authors":"Chiranjeeb Singha,&nbsp;Pritam Nanda,&nbsp;Pabitra Tripathy","doi":"10.1007/s10714-023-03154-z","DOIUrl":"10.1007/s10714-023-03154-z","url":null,"abstract":"<div><p>There are several well-established methods for computing thermodynamics in single-horizon spacetimes. However, understanding thermodynamics becomes particularly important when dealing with spacetimes with multiple horizons. Multiple horizons raise questions about the existence of a global temperature for such spacetimes. Recent studies highlight the significant role played by the contribution of all the horizons in determining Hawking’s temperature. Here we explore the Hawking temperature of a rotating and charged black hole in four spacetime dimensions and a rotating BTZ black hole. We also find that each horizon of those black holes contributes to the Hawking temperature. The effective Hawking temperature for a four-dimensional rotating and charged black hole depends only on its mass. This temperature is the same as the Hawking temperature of a Schwarzschild’s black hole. In contrast, the effective Hawking temperature depends on the black hole’s mass and angular momentum for a rotating BTZ hole.\u0000</p></div>","PeriodicalId":578,"journal":{"name":"General Relativity and Gravitation","volume":"55 10","pages":""},"PeriodicalIF":2.8,"publicationDate":"2023-09-28","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"41083445","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}