Numerical simulations of astrophysical jets from randomly perturbed Keplerian disks
Instituto Astronômico e Geofísico, Universidade de São Paulo, Av. Miguel Stéfano 4200, 04301-904 São Paulo, Brazil
Corresponding author: B. F. Vitorino, email@example.com
Accepted: 26 November 2001
We study the outflows from randomly perturbed Keplerian accretion disks. In the velocity field of the gas at the surface of the disk, we introduce a random perturbation proportional to ra, where r is the radial distance and a is a fixed parameter in the simulation (with values of , -1, , 0, or 1). In the simulations, the disk is a fixed boundary from which the gas is ejected with continuous and random velocities added together. The continuous ejection velocity is taken to be a thousandth of that of the local Keplerian disk; the maximum value of the random velocity is 10 times the continuous velocity. We observe the formation of periodic structures along the outflow axis. The distance of the axial separation between the structures is found to be about 11 times the innermost radius of the accretion disk. For a negative radial slope a, the structures are well defined and situated near the jet axis, whereas for a positive slope, decollimation of the jet occurs.
Key words: ISM: jets and outflows / galaxies: jets / accretion, accretion disks / magnetohydrodynamics (MHD)
© ESO, 2002