2021/03/20 by Vasilisa Nikiforova
Mathematics · Physics and Astronomy · #Astrophysical Phenomena and Observations #Black Holes and Theoretical Physics #Black hole (networking) #Circular symmetry #Classical mechanics #General relativity #Geometry #Gravitation #Gravitational singularity #Inverse #Kerr metric #Mathematical physics #Mathematics #Physics #Pulsars and Gravitational Waves Research #Quantum mechanics #Schwarzschild geodesics #Schwarzschild metric #Schwarzschild radius #Torsion (gastropod) #gr-qc #hep-th
paper · pdf · doi:10.1103/physrevd.104.024032
published as Phys. Rev. D 104, 024032 (2021) · 15 pages, 2 figures, 1 Mathematica notebook as ancillary file
arxiv created 2021/03/20 · openalex created_date 2021/03/29 · openalex publication_date 2021/07/13 · arxiv updated 2021/07/21 · openalex updated_date 2026/08/05
Time-dependent spherically symmetric perturbations of Schwarzschild black holes are studied within torsion bigravity, i.e., within generalized Einstein-Cartan theories where the dynamical torsion carries massive spin-2 excitation. We reduce linearized perturbations to a Zerilli-like equation. The structure of the potential entering the latter Zerilli-like equation has two important consequences. First, in order to avoid the presence of singularities in generic perturbations, one must restrict the range (or inverse mass) of the spin-2 excitation to be (essentially) smaller than the radius of the considered black hole. Second, we then show that the Schwarzschild black hole is linearly stable against spherically symmetric perturbations.