2020/07/16 by Vasilisa Nikiforova, Thibault Damour · 6 citations
Mathematics · Physics and Astronomy · #Black Holes and Theoretical Physics #Black hole (networking) #Classical mechanics #Cosmology and Gravitation Theories #General relativity #Gravitation #Gravitational collapse #Infinitesimal #Mathematical analysis #Mathematical physics #Mathematics #Physics #Pulsars and Gravitational Waves Research #Schwarzschild metric #Schwarzschild radius #Theoretical physics #Torsion (gastropod) #White hole #gr-qc
paper · pdf · doi:10.1103/physrevd.102.084027
published in Physical review. D/Physical review. D. 102(8) (American Physical Society) · 19 pages, 3 figures
arxiv created 2020/07/16 · openalex publication_date 2020/10/12 · arxiv updated 2020/10/21 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
We study spherically symmetric black hole solutions in a four-parameter Einstein-Cartan-type class of theories, called ``torsion bigravity.'' These theories offer a geometric framework (with a metric and an independent torsionfull connection) for a modification of Einstein's theory that has the same spectrum as bimetric gravity models. In addition to an Einsteinlike massless spin-2 excitation, there is a massive spin-2 one (of range \ensuremathκ^\ensuremath-1) coming from the torsion sector, rather than from a second metric. We prove the existence of three broad classes of spherically symmetric black hole solutions in torsion bigravity. First, the Schwarzschild solution defines an asymptotically-flat torsionless black hole for all values of the parameters. [And we prove that one cannot deform a Schwarzschild solution, at the linearized level, by adding an infinitesimal torsion hair.] Second, when considering finite values of the range, we find that there exist non asymptotically flat torsion-hairy black holes in a large domain of parameter space. Third, we find that, in the limit of infinite range, there exists a two-parameter family of asymptotically flat torsion-hairy black holes. The latter black hole solutions give an interesting example of non-Einsteinian (but still purely geometric) black hole structures which might be astrophysically relevant when considering a range of cosmological size.