This video shows the evolution of a simulated accretion disc around a rotating black hole (BH). This is 3D renderings of our simulation. Brighter colors indicate a greater density of the gas. This simulation was performed using the code PHANTOM SPH on the Unitech INDACO platform provided by "Università degli Studi di Milano". Data is visualized using SPLASH.
The simulated disc is thin (i.e. its thickness 'H' is much smaller than its distance 'R' from the BH) and in the diffusive hydrodynamical regime (i.e. the Shakura & Sunyaev 1973 viscosity parameter 'α' is greater than the aspect ratio 'H/R' of the disc). In this disc α=0.03.
The video shows that the initially flat and 30° inclined disc quickly starts to show alignment of its inner regions, as expected by Bardeen & Petterson 1975. Notice how the disc warps and twists differently depending on distance from the central body. Such differences are strong enough to break the disc into two sections. After a full precession, the inner ring of gas reconnects with the outer disc. This kind of reconnection has never been witnessed before in an accretion disc simulation. Further simulations are required to verify our results.
PHANTOM homepage:
[ Ссылка ]
SPLASH homepage:
[ Ссылка ]
Unitech homepage:
[ Ссылка ]
References:
- Shakura & Sunyaev 1973: [ Ссылка ]
-Bardeen & Petterson 1975: [ Ссылка ]
