Two-component jet simulations: I. Topological stability of analytical MHD outflow solutions

TL;DR

This paper investigates the topological stability of two analytical MHD outflow solutions, representing stellar and disk-wind components, through time-dependent simulations to understand their behavior and robustness in astrophysical jet models.

Contribution

It systematically examines the stability and behavior of two prototypical two-component jet models using numerical simulations, extending analytical solutions to all space.

Findings

Radially self-similar solutions reach a steady state with preserved properties.

Singularity removal leads to shock formation at the fast magnetosonic surface.

Stability of meridionally self-similar models depends on base heating processes.

Abstract

Observations of collimated outflows in young stellar objects indicate that several features of the jets can be understood by adopting the picture of a two-component outflow, wherein a central stellar component around the jet axis is surrounded by an extended disk-wind. The precise contribution of each component may depend on the intrinsic physical properties of the YSO-disk system as well as its evolutionary stage. In this context, the present article starts a systematic investigation of two-component jet models via time-dependent simulations of two prototypical and complementary analytical solutions, each closely related to the properties of stellar-outflows and disk-winds. These models describe a meridionally and a radially self-similar exact solution of the steady-state, ideal hydromagnetic equations, respectively. By using the PLUTO code to carry out the simulations, the study focuses on the topological stability of each of the two analytical solutions, which are successfully extended to all space by removing their singularities. In addition, their behavior and robustness over several physical and numerical modifications is extensively examined. It is found that radially self-similar solutions (disk-winds) always reach a final steady-state while maintaining all their well-defined properties. The different ways to replace the singular part of the solution around the symmetry axis, being a first approximation towards a two-component outflow, lead to the appearance of a shock at the super-fast domain corresponding to the fast magnetosonic separatrix surface. Conversely, the asymptotic configuration and the stability of meridionally self-similar models (stellar-winds) is related to the heating processes at the base of the wind.