A numerical simulation of the young stellar outflow DG Tauri B

Abstract

A series of axisymmetric, radiatively cooling variable jets was modeled with the ZEUS3D hydrodynamic code, revealing features commonly seen in outflows from Young Stellar Objects. The jet known as DG Tau B, discovered in 1983 by Mundt and Fried, was used to determine the parameters for the jet to be modeled. A molecular outflow surrounding the jet is also modeled in the simulations. New subroutines were written and implemented in order to model DG Tau B, believed to be a radiatively cooling jet possibly undergoing variability in jet velocity. Comparison to the observations in optical and radio wavelengths of DG Tau B shows a notable correspondence to the morphological and emission features in the atomic and molecular components of the simulated outflow.