1997/12/18 by M. A. Abramowicz, V. Karas, Abramowicz, M. A. +3 · 1 citation
Physics and Astronomy · #Astrophysical Phenomena and Observations #Astrophysics (astro-ph) #Black Holes and Theoretical Physics #FOS: Physical sciences #Pulsars and Gravitational Waves Research #astro-ph
paper · pdf · doi:10.48550/arxiv.astro-ph/9712245
Research Note in Astronomy & Astrophysics; 4 pages and 2 figures; also available at http://otokar.troja.mff.cuni.cz/user/karas/au_www/karas/papers.htm
arxiv created 1997/12/18 · openalex publication_date 1997/12/18 · arxiv updated 2009/12/01 · openalex created_date 2025/10/10 · openalex updated_date 2026/07/28
We further investigate the runaway instability of relativistic tori around black holes assuming a power law distribution of the specific angular momentum. We neglect the self-gravity of the torus; thus the gravitational field of the system is determined by the central rotating black hole alone (the Kerr geometry). We find that for any positive (i.e. consistent with the local Rayleigh stability condition) power law index of the angular momentum distribution, the tori are always runaway stable for a sufficiently large spin of the black hole. However, before concluding that some (astrophysically realistic) tori could indeed be runaway stable, one should include, in full general relativity, the destabilizing effect of self-gravity.