2018/03/01 by Patryk Mach, Michał Piróg, José A. Font +1 · 8 citations
Physics and Astronomy · #Accretion (finance) #Angular momentum #Astrophysical Phenomena and Observations #Astrophysics and Cosmic Phenomena #Flow (mathematics) #Horizon #Inviscid flow #Momentum (technical analysis) #Pulsars and Gravitational Waves Research #Schwarzschild metric #Schwarzschild radius #Specific relative angular momentum #gr-qc
paper · pdf · doi:10.1088/1361-6382/aab333
published in Classical and Quantum Gravity 35(9), 095005 (IOP Publishing) · 28 pages, 17 figures, to appear in Class. Quantum Grav
openalex publication_date 2018/03/01 · arxiv created 2018/03/11 · arxiv updated 2018/03/13 · openalex created_date 2018/03/29 · openalex updated_date 2026/08/05
Abstract We investigate relativistic low angular momentum accretion of inviscid perfect fluid onto a Schwarzschild black hole. The simulations are performed with a general-relativistic, high-resolution (second-order), shock-capturing, hydrodynamical numerical code. We use horizon-penetrating Eddington–Finkelstein coordinates to remove inaccuracies in regions of strong gravity near the black hole horizon and show the expected convergence of the code with the Michel solution and stationary Fishbone–Moncrief toroids. We recover, in the framework of relativistic hydrodynamics, the qualitative behavior known from previous Newtonian studies that used a Bondi background flow in a pseudo-relativistic gravitational potential with a latitude-dependent angular momentum at the outer boundary. Our models exhibit characteristic ‘turbulent’ behavior and the attained accretion rates are lower than those of the Bondi–Michel radial flow. For sufficiently low values of the asymptotic sound speed, geometrically thick tori form in the equatorial plane surrounding the black hole horizon while accretion takes place mainly through the poles.