Orbital resonances in Kerr - de Sitter black holes


  • Lemuel Gavin G. Saret ⋅ PH National Institute of Physics, University of the Philippines Diliman
  • Michael Francis Ian G. Vega II ⋅ PH National Institute of Physics, University of the Philippines Diliman


The inspiral of a stellar mass compact object (1 − 100 M) into a supermassive black hole (106 – 109 M) in the center of galaxies are the primary generators of gravitational waves, much to the interest of current ground-based and future space-based detectors. When accurately modelled, these extreme mass ratio inspirals serve as tests for the validity of the general theory of relativity. In this paper, we determine the location of low-ordered resonances in Kerr-de Sitter black holes and study how they are affected by changes in the cosmological constant. Resonant orbits are geodesics for which the ratio of the radial and longitudinal frequencies follow the form, ωrθ = n/m, where n,m are integers. Evolving through low-ordered resonances (small n+m value) causes jumps in the evolution of the orbital parameters which could produce phase shifts in the respective gravitational wave emission. Since typically an inspiral passes through multiple low-ordered resonances, probing the location of these resonances can help in improving current templates in gravitational wave analysis. We find that for a Kerr-de Sitter black hole (Λ > 0), the locations of the orbital resonances are shifted to larger semi-latus rectum values and lower eccentricities as the cosmological constant is increased.



Article ID



Gravitational Physics and Astrophysics



How to Cite

LGG Saret and MFIG Vega, Orbital resonances in Kerr - de Sitter black holes, Proceedings of the Samahang Pisika ng Pilipinas 42, SPP-2024-2E-03 (2024). URL: https://proceedings.spp-online.org/article/view/SPP-2024-2E-03.