2021/12/10 by Vítor Cardoso, Vitor Cardoso, Caio F. B. Macedo +4
Physics and Astronomy · #Astrophysics #Binary black hole #Binary number #Black Holes and Theoretical Physics #Black hole (networking) #Classical mechanics #Compact space #Cosmology and Gravitation Theories #General relativity #Gravitational wave #Numerical relativity #Physics #Pulsars and Gravitational Waves Research #Pure mathematics #Quantum mechanics #Spacetime #Stars #Theoretical physics #gr-qc
paper · pdf · doi:10.1088/1361-6382/ac41e7
22 pages, 11 figures. Accepted for publication in CQG
arxiv created 2021/12/10 · openalex publication_date 2021/12/10 · arxiv updated 2022/02/02 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/06
Abstract Black holes are thought to describe the geometry of massive, dark compact objects in the Universe. To further support and quantify this long-held belief requires knowledge of possible, if exotic alternatives. Here, we wish to understand how compact can self-gravitating solutions be. We discuss theories with a well-posed initial value problem, consisting in either a single self-interacting scalar, vector or both. We focus on spherically symmetric solutions, investigating the influence of self-interacting potentials into the compactness of the solutions, in particular those that allow for flat-spacetime solutions. We are able to connect such stars to hairy black hole solutions, which emerge as a zero-mass black hole. We show that such stars can have light rings, but their compactness is never parametrically close to that of black holes. The challenge of finding black hole mimickers to investigate full numerical-relativity binary setups remains open.