Magnetic launching and collimation of jets from the disk-magnetosphere boundary: 2.5D MHD simulations

TL;DR

This study employs 2.5D MHD simulations to explore how jets are launched and collimated from the disk-magnetosphere boundary of accreting magnetized stars, revealing magnetic acceleration and collimation mechanisms.

Contribution

It provides detailed simulation-based insights into jet launching and collimation processes, including velocity profiles and magnetic forces, applicable to various magnetized stellar objects.

Findings

Matter flows into jets from the inner accretion disk edge.

Jets are magnetically accelerated and collimated along magnetic field lines.

Jet velocities range from 30 km/s to over 260 km/s depending on the stellar environment.

Abstract

We use axisymmetric magnetohydrodynamic (MHD) simulations to investigate the launching and collimation of jets emerging from the disk-magnetosphere boundary of accreting magnetized stars. Our analysis shows that the matter flows into the jet from the inner edge of the accretion disk. It is magnetically accelerated along field lines extending up from the disk and simultaneously collimated by the magnetic pinch force. In the reference run which we use for analysis, the matter in the jet crosses the Alfv\'en surface a few R_* above the disk and the fast magnetosonic surface ~13 R_* above the disk. At larger distances, the magnetic pressure is a few times smaller than the total matter pressure but the magnetic force continues to accelerate and collimate the jet. In steady state, we observe a matter ejection-to-accretion ratio of ~0.2. Across different simulation runs, we measure a range of half-opening angles between {\Theta} \approx 4{\deg} and 20{\deg} at the top of the simulation region, depending on the degree of magnetization in the outflow. We consider the case of stars undergoing epochs of high accretion (such as EXors, FUORs, and CTTSs) where the stellar magnetosphere is strongly compressed by the incoming accretion disk. For a typical EXor (mass 0.8 M_sun, radius 2 R_sun) accreting at ~10^-5 M_sun/yr, we measure poloidal velocities in the jet ranging from 30 km/s on the outer edge of the jet to more than 260 km/s on the inner edge. In general, the models can be applied to a variety of magnetized stars--white dwarfs, neutron stars, and brown dwarfs--which exhibit periods of high accretion.