# Magnetized Gas Collimation of Interstellar Outflow Scaled by Laser-produced Plasma

## TL;DR

This study demonstrates how magnetic fields and gas density influence plasma outflow shapes in laboratory experiments, providing insights into astrophysical jet formation and a scalable model for unresolved cosmic regions.

## Contribution

It introduces a laboratory analog using laser-produced plasma and magnetic fields to simulate and analyze astrophysical outflow collimation mechanisms.

## Key findings

- Magnetic field strength and gas density significantly affect outflow morphology.
- The experimental results align with observed structures in protostars and planetary nebulae.
- A scalable framework is developed for modeling astrophysical jet structures in laboratory settings.

## Abstract

Young stellar objects/planetary nebula outflow anisotropies usually involve wind-wind interactions and magnetic collimation, but detailed structures of wind and magnetic fields inside collimation region remain undetermined. We numerically investigated its laboratory counterpart, based on poloidal field collimation in magnetocentrifugal launching model. Our analog consist of fast wind: Aluminum plasma generated by laser and magnetized ambient: molecular Helium and B=5-60 Tesla embedded field. Elevating magnetic field strength or decreasing gas density can alter expansion morphology, from sphere to prolonged cavity and ultimately to collimated jet. Outflow patterns can be quantitatively predicted based on the knowledge of its surroundings through a set of external Mach numbers. We conclude that such mixed gas and magnetic field dynamics are consistent with astronomical observations of protostars and planetary nebulae in certain evolution stages, and here provide a scalable framework allowing fitting of flow-field structures in astronomical unresolved regions by assuming their possible geometries on a repeatable laboratory platform.