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Geodesics in the field of a perturbed black hole: where appears chaos?
Polcar, Lukáš ; Semerák, Oldřich (advisor) ; Suková, Petra (referee)
It is widely known that the motion around Schwarzshild black hole is completely integrable. However, after adding a disc or a ring one of the symmetries of the system is broken and the motion may become chaotic for some values of parameters. The aim of this thesis is to identify where appears chaos in static, axially symmetric spacetime by using the geometrical method based on the geodesic deviation equation. Is it possible to predict chaotic behaviour in general relativity solely from local geometrical properties of spacetime, without explicitly solving the geodesic equation? Powered by TCPDF (www.tcpdf.org)
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Weyl metrics and their generalizations: classical and quantum viewpoint
Polcar, Lukáš ; Svítek, Otakar (advisor) ; Ledvinka, Tomáš (referee) ; Pound, Adam (referee)
In this thesis, we study two distinct topics both connected to stationary axially sym- metric spacetimes. The first is a study of an exact solution sourced by phantom scalar field. This solution can be derived from the well-known Curzon-Chazy metric and has several unusual features. It is a spherically symmetric wormhole which is however not symmetric with respect to its throat, it possesses a non-scalar curvature singularity and functions as a one-directional time machine. The energy content of the spacetime is ex- amined and various other properties are discussed. The remaining parts are dedicated to extreme mass ratio inspirals in two stationary axially symmetric spacetimes, perturbed Schwarzschild and Kerr. The canonical perturbation theory was used to transform the respective geodesic Hamiltonian to action-angle coordinates allowing us to evolve flux- driven inspirals in both spacetimes. 1
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Geodesic chaos in a perturbed Schwarzschild field
Polcar, Lukáš ; Semerák, Oldřich (advisor) ; Kopáček, Ondřej (referee)
We study the dynamics of time-like geodesics in the field of black holes perturbed by a circular ring or disc, restricting to static and axisymmetric class of space-times. Two analytical methods are tested which do not require solving the equations of motion: (i) the so-called geometric criterion of chaos based on eigenvalues of the Riemann tensor, and (ii) the method of Melnikov which detects the chaotic layer arising by break-up of a homoclinic orbit. Predictions of both methods are compared with numerical results in order to learn how accurate and reliable they are.
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Geodesic chaos in a perturbed Schwarzschild field
Polcar, Lukáš ; Semerák, Oldřich (advisor) ; Kopáček, Ondřej (referee)
We study the dynamics of time-like geodesics in the field of black holes perturbed by a circular ring or disc, restricting to static and axisymmetric class of space-times. Two analytical methods are tested which do not require solving the equations of motion: (i) the so-called geometric criterion of chaos based on eigenvalues of the Riemann tensor, and (ii) the method of Melnikov which detects the chaotic layer arising by break-up of a homoclinic orbit. Predictions of both methods are compared with numerical results in order to learn how accurate and reliable they are.
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Geodesics in the field of a perturbed black hole: where appears chaos?
Polcar, Lukáš ; Semerák, Oldřich (advisor) ; Suková, Petra (referee)
It is widely known that the motion around Schwarzshild black hole is completely integrable. However, after adding a disc or a ring one of the symmetries of the system is broken and the motion may become chaotic for some values of parameters. The aim of this thesis is to identify where appears chaos in static, axially symmetric spacetime by using the geometrical method based on the geodesic deviation equation. Is it possible to predict chaotic behaviour in general relativity solely from local geometrical properties of spacetime, without explicitly solving the geodesic equation? Powered by TCPDF (www.tcpdf.org)
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