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High resolution observations of Young Stellar Object (YSO) jets show them tobe composed of many small-scale knots or clumps. In this paper we reportresults of 3-D numerical simulations designed to study how such clumps interactand create morphologies and kinematic patterns seen in emission lineobservations. Our simulations focus on clump scale dynamics by imposingvelocity differences between spherical, over-dense regions which then lead tothe formation of bow shocks as faster clumps overtake slower material. We showthat much of the spatial structure apparent in emission line images of jetsarises from the dynamics and interactions of these bow shocks. Our simulationsshow a variety of time-dependent features, including bright knots associatedwith Mach stems where the shocks intersect, a "frothy" emission structure thatarises from the presence of the Non-linear Thin Shell Instability (NTSI) alongthe surfaces of the bow shocks, and the merging and fragmentation of clumps.Our simulations use a new non-equilibrium cooling method to produce syntheticemission maps in H$\alpha$ and [S II]. These are directly compared withmulti-epoch Hubble Space Telescope (HST) observations of Herbig-Haro (HH) jets.We find excellent agreement between features seen in the simulations and theobservations in terms of both proper motion and morphologies. Thus we concludethat YSO jets may be dominated by heterogeneous structures and thatinteractions between these structures and the shocks they produce can accountfor many details of YSO jet evolution.

The Shock Dynamics of Heterogeneous YSO Jets: 3-D Simulations Meet Multi-Epoch Observations