2017/03/27 by G. Compère, Geoffrey Compère, R. Oliveri +1
Physics and Astronomy · #Accretion (finance) #Accretion disc #Astronomy #Astrophysical Phenomena and Observations #Astrophysics #Black hole (networking) #Galaxies: Formation, Evolution, Phenomena #Physics #Pulsars and Gravitational Waves Research #astro-ph.HE #gr-qc #hep-th
paper · pdf · doi:10.1093/mnras/stx748
published as Mon Not R Astron Soc (2017) 468 (4): 4351-4361 · 13 pages, 6 figures; v2 matches published version in MNRAS; v3: typos fixed, results unchanged
openalex created_date 2017/03/16 · openalex publication_date 2017/03/27 · arxiv created 2017/10/28 · arxiv updated 2017/10/31 · openalex updated_date 2026/08/05
Near-maximally spinning black holes display conformal symmetry in their near-horizon region, which is therefore the locus of critical phenomena. In this paper, we revisit the Novikov–Thorne accretion thin disc model and find a new self-similar radiation-dominated solution in the extremely high spin regime. Motivated by the self-consistency of the model, we require that matter flows at the sound speed at the innermost stable circular orbit (ISCO). We observe that, when the disc pressure is dominated by radiation at the ISCO, which occurs for the best-fitting Novikov–Thorne model of GRS 1915+105, the Shakura–Sunyaev viscosity parameter can be expressed in terms of the spin, mass accretion rate and radiative efficiency. We quantitatively describe how the exact thin disc solution approaches the self-similar solution in the vicinity of the ISCO and for increasing spins.