Accretion into Black Holes - KD models
(from SF0 3D)
This page contains links to the various mpegs that were produced using the GRMHD code to study the accretion of magnetized gas into black holes via the Magneto-rotational Instability (MRI).
Initial torus configuration is the general relativistic version near-Keplerian torus of Hawley (2000) that was subsequently studied by Hawley and Krolik (2001, 2002) in a pseudo-Newtonian potential. Initial magnetic field configuration is poloidal loops, with beta=100 in all but one model, where beta=200 (see Table 1 in preprint for more information on model parameters). We designate these the KD models because of the properties of their initial angular momentum distribution.
The movies linked in the left margin show animations at ~30 frames per orbit, following 10 orbits (at pressure maximum) of the evolution of a magnetized torus orbiting a black hole. The 3D views are animations of gas density (linear scale - red maximum, blue minimum). The 2D views are scaled logarithmically, over 4 decades from the initial density maximum.
NOTE: These are direct animations in the Boyer-Lindquist coordinate system. Fully ray-traced images are "in the works". Also note that these mpegs are compressed from several GB of data... loss of image quality is inevitable.
KD0 - Torus and Schwarzschild Black Hole
The movies linked in the marging are: 1) 3D view of the density in the inner region of the accretion flow (triangular patterns at inner edge are an artifact), and 2) a view of a 2D poloidal slice of density for the inner region of the flow.
The movies linked in the marging are: 1) 3D view of the density in the inner region of the accretion flow (triangular patterns at inner edge are an artifact), 2) a full view of a 2D poloidal slice of density, 3) a view of a 2D poloidal slice of density in the inner region, and 4) a view of a 2D equatorial slice of density in the inner region.