2007/02/28 by Catherine Williams, Catherine M. Williams · 1 citation
Mathematics · Physics and Astronomy · #Black Holes and Theoretical Physics #Cosmology and Gravitation Theories #Pulsars and Gravitational Waves Research #gr-qc #math.DG
paper · pdf · doi:10.1007/s00023-008-0385-5
published as AnnalesHenriPoincare9:1029-1067,2008 · 43 pages, 7 figures. Updated to agree with published version; Theorem 1 strengthened slightly, minor issues fixed
openalex publication_date 2008/09/25 · arxiv created 2009/01/14 · arxiv updated 2009/12/01 · openalex created_date 2025/10/10 · openalex updated_date 2026/07/29
We give conditions on a general stress-energy tensor Tαβ in a spherically symmetric black hole spacetime which are sufficient to guarantee that the black hole will contain a (spherically symmetric) marginally trapped tube which is eventually achronal, connected, and asymptotic to the event horizon. Price law decay per se is not required for this asymptotic result, and in this general setting, such decay only implies that the marginally trapped tube has finite length with respect to the induced metric. We do, however, impose a smallness condition (B1) which one may obtain in practice by imposing decay on the Tvv component of the stress-energy tensor. We give two applications of the theorem to self-gravitating Higgs field spacetimes, one using weak Price law decay, the other certain strong smallness and monotonicity assumptions.