Applications of the Schwarzschild–Finsler–Randers model

Kapsabelis, E.; Triantafyllopoulos, A.; Basilakos, Spyros; Stavrinos, P. C.

doi:10.1140/epjc/s10052-021-09790-6

Cited by 12 publications

(8 citation statements)

References 59 publications

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“…( 4) and A γ (x) is a covector which expresses a deviation from general relativity, with |A γ (x)| 1, i.e., we assume that the deviation is small. In this work, we continue the investigation of the Schwarzschild-Finsler-Randers spacetime (SFR) which has been studied in previous works by a subset of the present authors [1,2].…”

Section: Introductionmentioning

confidence: 79%

“…1a, we can see that the radial component in the SFR model takes lower values compared to the GR one which remains constant. This difference between the r-components of SFR and GR can be interpreted as the increase of the radius of the photonsphere due to the one-form A γ as we have shown in [2]. This leads the orbit of the photon to fall inside the event horizon because the initial distance r 0 = 3 and energy are not sufficient to allow circular orbits of the photonsphere.…”

Section: Remarkmentioning

confidence: 92%

“…In this article, we investigated the analytic form of the geodesics of the model SFR which was introduced in previous works [1,2]. A dynamical analysis was presented based on the energy and angular momentum of a particle along of geodesics (null or timelike) of the SFR spacetime.…”

Section: Conclusion and Future Challengesmentioning

confidence: 99%

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Schwarzschild–Finsler–Randers spacetime: geodesics, dynamical analysis and deflection angle

2022

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In this work, we extend the study of Schwarzschi ld–Finsler–Randers (SFR) spacetime previously investigated by a subset of the present authors (Triantafyllopoulos et al. in Eur Phys J C 80(12):1200, 2020; Kapsabelis et al. in Eur Phys J C 81(11):990, 2021). We will examine the dynamical analysis of geodesics which provides the derivation of the energy and the angular momentum of a particle moving along a geodesic of SFR spacetime. This study allows us to compare our model with the corresponding of general relativity (GR). In addition, the effective potential of SFR model is examined and it is compared with the effective potential of GR. The phase portraits generated by these effective potentials are also compared. Finally we deal with the derivation of the deflection angle of the SFR spacetime and we find that there is a small perturbation from the deflection angle of GR. We also derive an interesting relation between the deflection angles of the SFR model and the corresponding result in the work of Shapiro et al. (Phys Rev Lett 92(12):121101, 2004). These small differences are attributed to the anisotropic metric structure of the model and especially to a Randers term which provides a small deviation from GR.

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Section: Introductionmentioning

confidence: 79%

Section: Remarkmentioning

confidence: 92%

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Schwarzschild–Finsler–Randers spacetime: geodesics, dynamical analysis and deflection angle

2022

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“…These equations have also been given in a different form in [5,[34][35][36][37][38][39][40]. In this article, as an additional motivation, we investigate the form of the equation of geodesics deviation, the Raychaudhuri equation in a Schwarzshild-Finsler-Randers (SFR) space adapted on the Lorentz tangent bundle of spacetime, thus extending the investigation on the SFR framework we have given in previous works [17,41,42]. Some physical consequences are also given in this article.…”

Section: Introductionmentioning

confidence: 83%

Raychaudhuri Equations, Tidal Forces, and the Weak-Field Limit in Schwarzshild–Finsler–Randers Spacetime

Triantafyllopoulos,

Kapsabelis,

Stavrinos

2024

Universe

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In this article, we study the form of the deviation of geodesics (tidal forces) and the Raychaudhuri equation in a Schwarzschild–Finsler–Randers (SFR) spacetime which has been investigated in previous papers. This model is obtained by considering the structure of a Lorentz tangent bundle of spacetime and, in particular, the kind of the curvatures in generalized metric spaces where there is more than one curvature tensor, such as Finsler-like spacetimes. In these cases, the concept of the Raychaudhuri equation is extended with extra terms and degrees of freedom from the dependence on internal variables such as the velocity or an anisotropic vector field. Additionally, we investigate some consequences of the weak-field limit on the spacetime under consideration and study the Newtonian limit equations which include a generalization of the Poisson equation.

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“…However, Randers geometry is a typical example of a Finsler geometry, with F (x, y) = a ij (x)dx i dx j 1/2 +A k (x)y k , where A k (x) is an arbitrary vector field. Recently, Randers geometry was extensively applied in the study of various gravitational phenomena in [17][18][19][20][21][22][23][24]. Finsler geometry has also important applications in the geometric description of quantum mechanics [25][26][27][28].…”

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confidence: 99%

Cosmological tests of the osculating Barthel–Kropina dark energy model

et al. 2023

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We further investigate the dark energy model based on the Finsler geometry inspired osculating Barthel–Kropina cosmology. The Barthel–Kropina cosmological approach is based on the introduction of a Barthel connection in an osculating Finsler geometry, with the connection having the property that it is the Levi-Civita connection of a Riemannian metric. From the generalized Friedmann equations of the Barthel–Kropina model, obtained by assuming that the background Riemannian metric is of the Friedmann–Lemaitre–Robertson–Walker type, an effective geometric dark energy component can be generated, with the effective, geometric type pressure, satisfying a linear barotropic type equation of state. The cosmological tests, and comparisons with observational data of this dark energy model are considered in detail. To constrain the Barthel–Kropina model parameters, and the parameter of the equation of state, we use 57 Hubble data points, and the Pantheon Supernovae Type Ia data sample. The st statistical analysis is performed by using Markov Chain Monte Carlo (MCMC) simulations. A detailed comparison with the standard $$\Lambda $$ Λ CDM model is also performed, with the Akaike information criterion (AIC), and the Bayesian information criterion (BIC) used as the two model selection tools. The statefinder diagnostics consisting of jerk and snap parameters, and the Om(z) diagnostics are also considered for the comparative study of the Barthel–Kropina and $$\Lambda $$ Λ CDM cosmologies. Our results indicate that the Barthel–Kropina dark energy model gives a good description of the observational data, and thus it can be considered a viable alternative of the $$\Lambda $$ Λ CDM model.

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Applications of the Schwarzschild–Finsler–Randers model

Cited by 12 publications

References 59 publications

Schwarzschild–Finsler–Randers spacetime: geodesics, dynamical analysis and deflection angle

Schwarzschild–Finsler–Randers spacetime: geodesics, dynamical analysis and deflection angle

Raychaudhuri Equations, Tidal Forces, and the Weak-Field Limit in Schwarzshild–Finsler–Randers Spacetime

Cosmological tests of the osculating Barthel–Kropina dark energy model

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