Resistive MHD Simulations of Star-Disk-Jet System

TL;DR

This paper uses resistive MHD simulations to study star-disk-jet interactions, revealing outflows can form at certain distances from the star but not very close to it, providing insights into protostellar outflow origins.

Contribution

It introduces resistive MHD simulations with ZEUS347 to explore outflow formation in star-disk systems, highlighting where outflows can and cannot occur.

Findings

Outflows do not form very close to the star in simulations.

Quasi-stationary funnel flows are observed onto the star.

Outflows may occur at tens of stellar radii above the star.

Abstract

Stellar magnetosphere and accretion disk interact, and a result should be outflow launched from the innermost vicinity of a protostellar object. We simulated physical conditions in this region by resistive MHD simulations. Outflows resembling the observed ones do not happen in the closest vicinity, except for quasi-stationary funnel flows onto the star, but could occur at few tens of stellar radii above the star. Numerical simulations we performed using our resistive version of ZEUS-3D code, ZEUS347.