Numerical Simulations of Astrophysical Jets from Keplerian Disks with Periodic Ejection

Details Numerical Simulations of Astrophysical Jets from Keplerian Disks with Periodic Ejection Numerical Simulations of Astrophysical Jets from Keplerian Disks with Periodic Ejection

2003-04-22

arxiv.org/abs/astro-ph/0304395v1

Astrophys.J. 592 (2003) 332-346

Astronomy and Astrophysics

Astrophysics

27 pages, 11 figures (by e-mail to braulo@astro.iag.usp.br), accepted for publication in ApJ

Scientific paper

10.1086/375558

We present 2.5-dimensional time-dependent simulations of nonrelativistic and nonradiative outflows from sinusoidally perturbed Keplerian accretion disks. A sinusoidal perturbation is introduced in the velocity of the gas ejected from the surface of the disk into a cold corona. In the simulations, the disk is a fixed boundary from which the gas is ejected with a pulsed velocity. The maximum value of this velocity is taken to be a thousandth of the local Keplerian disk velocity. It was found that for large periods, the structures in the jet tend to fragment into smaller substructures. For small values of the period, the structures tend to dissipate, while for medium values of the period, they tend to persist.

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