Magnetic outflows from turbulent accretion disks: I. Vertical structure & secular evolution

TL;DR

This paper uses 3D ideal-MHD simulations to analyze the vertical structure and long-term evolution of magnetized accretion disks, revealing how magnetic fields influence jet formation, turbulence, and disk restructuring.

Contribution

It provides the first detailed quantitative analysis of the secular evolution and vertical structure of magnetized accretion disks through global 3D simulations.

Findings

Weak magnetic fields produce small jets and subsonic accretion speeds.

Strong magnetization leads to inner accretion-ejection regions with steady magnetic fields.

Disk structure significantly differs from hydrostatic models, showing inward magnetic dragging and radial readjustment.

Abstract

Astrophysical disks are likely embedded in an ambient vertical magnetic field. This ambient field is known to drive magneto-rotational turbulence in the disk bulk but is also responsible for the launching of magnetized outflows at the origin of astrophysical jets. The vertical structure and long-term (secular) evolution of such a system lack quantitative predictions. It is nevertheless this secular evolution that is proposed to explain time variability in many accreting systems such as X-ray binaries. We compute and analyze global 3D ideal-MHD simulations of an accretion disk threaded by a large-scale magnetic field. We evaluate the role of the turbulent terms in the equilibrium of the system. We then compute the transport of mass, angular momentum, and magnetic fields in the disk to characterize its secular evolution. We perform a parameter survey to characterize the influence of disk properties on secular transport. We find that weakly magnetized disks drive jets that carry away a small fraction of the disk angular momentum. The mass-weighted accretion speed remains subsonic although, there is always an upper turbulent atmospheric region where transonic accretion takes place. We show that a strongly magnetized version of the magneto-rotational instability drives this turbulence. The disk structure is drastically different from the conventional hydrostatic picture. The magnetic field is always dragged inwards in the disk, at a velocity that increases with the disk magnetization. Beyond a threshold on the latter, the disk undergoes a profound radial readjustment. It leads to the formation of an inner accretion-ejection region with a supersonic mass-weighted accretion speed and where the magnetic field distribution becomes steady, near equipartition with the thermal pressure. This inner structure shares many properties with the Jet Emitting Disk model described by Ferreira (1997).