Relativistic Bondi–Hoyle–LYttleton accretion onto a rotating black hole: density gradients
In this work, for the first time, we present a numerical study of Bondi–Hoyle accretion with density gradients in the fully relativistic regime. In this context, we consider the accretion onto a Kerr black hole (BH) of a supersonic ideal gas with density gradients perpendicular to the relative motion. The parameters of interest in this study are the Mach number, M, the spin of the BH, a, and the density-gradient parameter of the gas, ϵ{sub ρ}. We show that, unlike in the Newtonian case, all of the studied cases, especially those with a density gradient, approach a stationary flow pattern. To illustrate that the system reaches a steady state, we calculate the mass and angular momentum accretion rates on a spherical surface almost located at the event horizon. In the particular case of M=1, ϵ{sub ρ} = 0.5, and BH spin a = 0.5, we observe a disk-like configuration surrounding the BH. Finally, we present the gas morphology and some of its properties.
- OSTI ID:
- 22872428
- Journal Information:
- Astrophysical Journal, Supplement Series, Vol. 219, Issue 2; Other Information: Country of input: International Atomic Energy Agency (IAEA); ISSN 0067-0049
- Country of Publication:
- United States
- Language:
- English
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