2013/04/30 by Mikhail S. Volkov, Mikhail S Volkov · 92 citations
Physics and Astronomy · #Black Holes and Theoretical Physics #Black hole (networking) #Class (philosophy) #Cosmology and Gravitation Theories #General relativity #Gravitation #Graviton #Massive gravity #Pulsars and Gravitational Waves Research #Term (time) #gr-qc #hep-th
paper · pdf · doi:10.1088/0264-9381/30/18/184009
published in Classical and Quantum Gravity 30(18), 184009 (IOP Publishing) · The version published in the focus issue of Classical and Quantum Gravity
openalex publication_date 2013/09/06 · arxiv created 2013/11/06 · arxiv updated 2015/06/15 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/08
We present a survey of the known cosmological and black hole solutions in ghost-free bigravity and massive gravity theories. These can be divided into three classes. First, there are solutions with proportional metrics, which are the same as in General Relativity with a cosmological term, which can be positive, negative or zero. Secondly, for spherically symmetric systems, there are solutions with non-bidiagonal metrics. The g -metric fulfils Einstein equations with a positive cosmological term and a matter source, while the f -metric is anti-de Sitter. The third class contains solutions with bidiagonal metrics, and these can be quite complex. The time-dependent solutions describe homogeneous (isotropic or anisotropic) cosmologies which show a late-time self-acceleration or other types of behavior. The static solutions describe black holes with a massive graviton hair, and also globally regular lumps of energy. None of these are asymptotically flat. Including a matter source gives rise to asymptotically flat solutions which exhibit the Vainshtein mechanism of recovery of General Relativity in a finite region.