HAL CCSD
Boundary conditions for stationary black holes: Application to Kerr, Martínez-Troncoso-Zanelli, and hairy black holes
Grandclément, Philippe
Nicoules, Jordan
Laboratoire Univers et Théories (LUTH (UMR_8102)) ; Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris ; Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)
International audience
Physical Review D
insu-03713228
https://insu.hal.science/insu-03713228
https://insu.hal.science/insu-03713228
Physical Review D, 2022, 105, ⟨10.1103/PhysRevD.105.104011⟩
ARXIV: 2203.09341
info:eu-repo/semantics/altIdentifier/arxiv/2203.09341
BIBCODE: 2022PhRvD.105j4011G
DOI: 10.1103/PhysRevD.105.104011
info:eu-repo/semantics/altIdentifier/doi/10.1103/PhysRevD.105.104011
en
General Relativity and Quantum Cosmology
High Energy Physics - Theory
[SDU]Sciences of the Universe [physics]
info:eu-repo/semantics/article
Journal articles
This work proposes a set of equations that can be used to numerically compute spacetimes containing a stationary black hole. The formalism is based on the 3 +1 decomposition of General Relativity with maximal slicing and spatial harmonic gauge. The presence of the black hole is enforced using the notion of apparent horizon in equilibrium. This setting leads to the main result of this paper: a set of boundary conditions describing the horizon and that must be used when solving the 3 +1 equations. Those conditions lead to a choice of coordinates that is regular even on the horizon itself. The whole procedure is validated with three different examples chosen to illustrate the great versatility of the method. First, the single rotating black holes are recovered up to very high values of the Kerr parameter. Second, nonrotating black holes coupled to a real scalar field, in the presence of a negative cosmological constant (the so-called Martinez-Troncoso-Zanelli black holes), are obtained. Last, black holes with complex scalar hairs are computed. Eventually, prospects for future work, in particular in contexts where stationarity is only approximate, are discussed.
2022