The stability of Kerr-de Sitter black holes | Vidéo | Carmin.tv

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The stability of Kerr-de Sitter black holes

Apparaît dans la collection : Resonances: geometric scattering and dynamics / Résonances : scattering géométrique et dynamique

In this lecture I will discuss Kerr-de Sitter black holes, which are rotating black holes in a universe with a positive cosmological constant, i.e. they are explicit solutions (in 3+1 dimensions) of Einstein's equations of general relativity. They are parameterized by their mass and angular momentum. I will discuss the geometry of these black holes, and then talk about the stability question for these black holes in the initial value formulation. Namely, appropriately interpreted, Einstein's equations can be thought of as quasilinear wave equations, and then the question is if perturbations of the initial data produce solutions which are close to, and indeed asymptotic to, a Kerr-de Sitter black hole, typically with a different mass and angular momentum. In this talk, I will emphasize geometric aspects of the stability problem, in particular showing that Kerr-de Sitter black holes with small angular momentum are stable in this sense.

Informations sur la vidéo

Date de captation 14/03/2017
Date de publication 23/03/2017
Institut CIRM
Licence CC BY NC ND
Langue Anglais
Audience Chercheurs
Réalisateur(s) Guillaume Hennenfent
Format MP4

Données de citation

DOI 10.24350/CIRM.V.19142603
Citer cette vidéo Hintz, Peter (14/03/2017). The stability of Kerr-de Sitter black holes. CIRM. Audiovisual resource. DOI: 10.24350/CIRM.V.19142603
URL https://dx.doi.org/10.24350/CIRM.V.19142603

Domaine(s)

Bibliographie

Hintz, P., & Vasy, A. (2016). The global non-linear stability of the Kerr-de Sitter family of black holes. <arXiv:1606.04014> - https://arxiv.org/abs/1606.04014

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