Current Status of Simulations

Abstract

As the title suggests, the purpose of this chapter is to review the current status of numerical simulations of black hole accretion disks. This chapter focuses exclusively on global simulations of the accretion process within a few tens of gravitational radii of the black hole. Most of the simulations discussed are performed using general relativistic magnetohydrodynamic (MHD) schemes, although some mention is made of Newtonian radiation MHD simulations and smoothed particle hydrodynamics. The goal is to convey some of the exciting work that has been going on in the past few years and provide some speculation on future directions.

The Size, Shape, and Scattering of Sagittarius A* at 86 GHz: First VLBI with ALMA

“…They are believed to be the origin of the most energetically efficient and powerful processes in the Universe, and yet we are far from fully grasping how these processes are launched and maintained (e.g., Boccardi et al 2017;Padovani et al 2017). Several theories have been put forward to explain accretion and jet launching mechanisms of SMBHs, but observational evidence to discriminate among theoretical models remains scarce (e.g., Yuan & Narayan 2014;Fragile 2014).…”