Interacting Jets from Binary Protostars

TL;DR

This study models binary protostellar jets to understand their morphology and interactions, revealing how magnetic fields and orbital motion influence jet collimation and observable features.

Contribution

It introduces detailed 3D MHD simulations of binary jets, including a case study of L1551 IRS 5, to explain observed jet interactions and morphologies.

Findings

Jets interfere and can merge or be engulfed

Magnetic fields aid in jet collimation and refocusing

Orbital motion has negligible effect on jet dynamics

Abstract

We investigate potential models that could explain why multiple proto-stellar systems predominantly show single jets. During their formation, stars most frequently produce energetic outflows and jets. However, binary jets have only been observed in a very small number of systems. We model numerically 3D binary jets for various outflow parameters. We also model the propagation of jets from a specific source, namely L1551 IRS 5, known to have two jets, using recent observations as constraints for simulations with a new MHD code. We examine their morphology and dynamics, and produce synthetic emission maps. We find that the two jets interfere up to the stage where one of them is almost destroyed or engulfed into the second one. We are able to reproduce some of the observational features of L1551 such as the bending of the secondary jet. While the effects of orbital motion are negligible over the jets dynamical timeline, their interaction has significant impact on their morphology. If the jets are not strictly parallel, as in most observed cases, we show that the magnetic field can help the collimation and refocusing of both of the two jets.