Numerical simulations of black hole accretion flows

Understand

We model the structure and evolution of black hole accretion disks, and their neighboring regions, using numerical simulations.

• The numerics is governed by the equations of general relativistic magneto-hydrodynamics (GRMHD).
• In particular, such disks and outflows can be found at the base of very energetic ultra-relativistic jets produced by cosmic explosions, so called gamma-ray bursts (GRBs).
• Another, more persistent type of the jet phenomena, are blazars, emitted from the centers of galaxies.