Abstract
We investigate the dynamical behavior of a scalar field non-minimally coupled to Einstein’s tensor and Ricci scalar in geometries of asymptotically de Sitter spacetimes. We show that the quasinormal modes remain unaffected if the scalar field is massless and the black hole is electrically chargeless. In the massive case, the coupling of both parameters produces a region of instability in the spacetime determined by the geometry and field parameters. In the Schwarzschild case, every solution for the equations of motion with ell >0 has a range of values of the coupling constant that produces unstable modes. The case ell =0 is the most unstable one, with a threshold value for stability in the coupling. For the charged black hole, the existence of a range of instability in eta is strongly related to geometry parameters presenting a region of stability independent of the chosen parameter.
Highlights
The evolution of probe fields in black hole backgrounds has long been a very active field of research in theoretical physics [1–3, and references therein]
Probe field profiles in the time domain present a discrete set of complex frequencies called quasinormal frequencies (QNFs) that can provide valuable information about the structure of spacetime
The set of quasinormal mode (QNM)’s carry specific information about the signature of the geometry and its interaction with fields, since it depends on the parameters that define the metric
Summary
The evolution of probe fields in black hole backgrounds has long been a very active field of research in theoretical physics [1–3, and references therein]. The presence of a scalar field coupled to curvature terms in Einstein–Hilbert action allows for a suitable solution for the inflation exit, and in general has a de Sitter spacetime as the attractor for later times, as should be expected. For a particular choice of couplings, it is still possible to achieve second order equations: when the Lagrangian derivative terms are placed as Einstein tensor coupled to scalar field components [40]. This choice turns the NMDC into a more suitable (simple) form, as it makes unnecessary to fine tune the scalar field potential.
Sign-in/Register to view highlights & summary Talk to us
Join us for a 30 min session where you can share your feedback and ask us any queries you have
Schedule a callDisclaimer: All third-party content on this website/platform is and will remain the property of their respective owners and is provided on "as is" basis without any warranties, express or implied. Use of third-party content does not indicate any affiliation, sponsorship with or endorsement by them. Any references to third-party content is to identify the corresponding services and shall be considered fair use under The CopyrightLaw.
