Guest
Here we show a transverse density contour of a thin H/R= accretion disc (red) around a spinning black hole (white dot in the middle) in a general relativistic MHD simulation. The inner parts of the accretion disc align with the black hole, also called Bardeen-Petterson alignment. Later on in the movie the disc forms a low density highly turbulent inner disc coupled to a high density weakly turbulent outer disc. Could this inner disc be the precursor of a thick accretion disc? Furthermore, against the standard expectation, a highly relativistic jet is launched (the outflow in the dark blue regions). Why is this happening and why don't we see this jet in 'real' observations? Read our paper: This research was made possible by running my GRMHD code H-AMR with full adaptive mesh refinement (AMR) ability on 300 NVIDIA K20X GPUs and constitutes the highest effective resolution GRMHD simulation ever performed. Note: There is a 'jump' around rg/c because the plane of the
