Modelling general-relativistic disk in OJ 287
arXiv:1903.07955 · doi:10.1093/mnras/stz1058
Abstract
We model self-gravitating disks in Keplerian motion around the primary black hole, in the binary black hole system OJ 287 with a torus, employing a consistently general-relativistic approach. They satisfy geometric and/or mass density requirements found by Sillanpaa, Valtonen, Lehto and their coworkers. It is plausible that essential observational features of OJ 287 can be obtained via the general-relativistic description of the Bondi-Hoyle-Lyttleton transits through these tori, within the framework of radiation hydrodynamics.
arXiv comment7 pages, 7 figures
References in corpus (9)
- A massive binary black-hole system in OJ287 and a test of general relativity
- A Review of Bondi--Hoyle--Lyttleton Accretion
- Authenticating the Presence of a Relativistic Massive Black Hole Binary in OJ 287 Using its General Relativity Centenary Flare: Improved Orbital Parameters
- General relativistic radiation hydrodynamics of accretion flows. I: Bondi-Hoyle accretion
- Precursor flares in OJ 287
- Black hole accretion disc impacts
- Self-gravitating axially symmetric disks in general-relativistic rotation
- General-relativistic rotation laws in rotating fluid bodies
- General-relativistic rotation: self-gravitating fluid tori in motion around black holes