Modeling YSO Jets in 3D. II. Accretion-fed, Star-anchored Poynting Jets in the Low-density Polar Cavity Powered by Disk–Magnetosphere Interaction

Abstract The origin of the jets in young stellar objects (YSOs) remains a subject of active investigation. We present a 3D MHD simulation of the jet launching in YSOs, focusing on the interaction between the stellar magnetosphere and the accretion disk. In our model, a fast low-density bipolar jet is powered by disk–magnetosphere interaction and launched through the polar cavity that is mass-loaded from the disk rather than the star. Specifically, outflows are driven by toroidal magnetic pressure generated along “two-legged” field lines, anchored at a magnetically dominated stellar footpoint and a mass-dominated point on the (magnetically elevated) disk surface via a cyclic “load–fire–reload” process: in the “load” stage, the differential rotation between the stellar and disk footpoints generates toroidal magnetic pressure; in the “fire” stage, vertical gradients in the toroidal field accelerate plasma and transport the Poynting flux into the polar cavity; and in the “reload” stage, magnetic reconnection allows the cycle to repeat, reforming “two-legged” field lines. These field lines are not required to be fully reset to a dipolar loop configuration; it is only required that the disk end be shallowly embedded in the (elevated) disk surface. This rapid asynchronous process produces a continuous large-scale outflow. The resulting magnetically dominated (Poynting) jet, accelerated by magnetic pressure within the low-density polar cavity, is distinct from the denser, slower disk wind launched through the classic magnetic tower mechanism. Comparison with a disk-only model shows that the rotating stellar magnetosphere promotes bipolar jet launching by shaping a magnetic geometry favorable to symmetric outflows.