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

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

doi:10.1140/epjc/s10052-022-11081-7

Cited by 10 publications

(6 citation statements)

References 68 publications

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“…Our results are As a general result, we have put forward the study of MDRs by their effects on a kinetic gas under the assumption of spherical symmetry and symmetry under time translation. Applying this result to further MDRs, in particular those derived from quantum gravity theories mentioned in the introduction, or other modifications of the Schwarzschild metric [79][80][81], establishes a window towards quantum gravity phenomenology through the observation of gas dynamics in the vicinity of massive, compact objects, such as neutron stars and black holes. As a particular result, we have found these effects for a κ-Poincaré MDR.…”

Section: Discussionmentioning

confidence: 85%

Kinetic gases in static spherically symmetric modified dispersion relations

Hohmann

2023

Class. Quantum Grav.

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We study the dynamics of a collisionless kinetic gas in the most general static, spherically symmetric dispersion relation. For a static, spherically symmetric kinetic gas, we derive the most general solution to these dynamics, and find that any solution is given by a one-particle distribution function which depends on three variables. For two particular solutions, describing a shell of monoenergetic orbiting particles and a purely radial inflow, we calculate the particle density as a function of the radial coordinate. As a particular example, we study aκ-Poincaré modification of the Schwarzschild metric dispersion relation and derive its influence on the particle density. Our results provide a possible route towards quantum gravity phenomenology via the observation of matter dynamics in the vicinity of massive compact objects.

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Section: Discussionmentioning

confidence: 85%

Kinetic gases in static spherically symmetric modified dispersion relations

Hohmann

2023

Class. Quantum Grav.

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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: 84%

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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“…Therefore, they investigated the perturbation in the features of the classical Schwarzschild space-time. Recently, the geodesics (time-like or null) on the Schwarzschild-Finsler-Randers space-time are investigated in [71], and the deviation from GR is demonstrated graphically. Additionally, the phase portraits and the effective potential of the model induced by them are analyzed and analogized with GR.…”

Section: Geodesics Of Finsler Space-timementioning

confidence: 99%

Black hole solutions with constant Ricci scalar in a model of Finsler gravity

Nekouee,

Narasimhamurthy,

Pacif

2024

J. Cosmol. Astropart. Phys.

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Ricci scalar being zero is equivalent to the vacuum field equation in Finsler space-time. The Schwarzschild metric can be concluded from the field equation's solution if the space-time conserves spherical symmetry. This research aims to investigate Finslerian Schwarzschild-de Sitter space-time. Recent studies based on Finslerian space-time geometric models are becoming more prevalent because the local anisotropic structure of space-time influences the gravitational field and gives rise to modified cosmological relations. We suggest a gravitational field equation with a non-zero cosmological constant in Finslerian geometry and apprehend that the presented Finslerian gravitational field equation corresponds to the non-zero Ricci scalar. In Finsler geometry, the peer of spherical symmetry is the Finslerian sphere. Assuming space-time to conserve the “Finslerian sphere” symmetry, the counterpart of the Riemannian sphere (Finslerian sphere) must have a constant flag curvature (λ). It is demonstrated that the Finslerian covariant derivative of the geometric part of the gravitational field equation is preserved under a condition using the Chern connection. According to the string theory, string clouds can be defined as a pool of strings made due to symmetry breaking in the universe's early stages. We find that for λ ≠ 1, this solution resembles a black hole surrounded by a cloud of strings. Furthermore, we investigate null and time-like geodesics for λ = 1. In this regard, the photon geodesics are obtained that are the closest paths to the photon sphere of the first photons visible at the black hole shadow limit. Also, circular orbit conditions are obtained for the effective potential.

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

Cited by 10 publications

References 68 publications

Kinetic gases in static spherically symmetric modified dispersion relations

Kinetic gases in static spherically symmetric modified dispersion relations

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

Black hole solutions with constant Ricci scalar in a model of Finsler gravity

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