Advection of Magnetic Fields in Accretion Disks: Not So Difficult After All

TL;DR

This paper demonstrates that large-scale magnetic fields can be efficiently advected inward in accretion disks due to surface layer properties, challenging previous beliefs and supporting jet formation models.

Contribution

It reveals that weak magnetic fields are advected inward in turbulent accretion disks through surface layers, supported by 3D simulations, impacting jet formation theories.

Findings

Inward advection of magnetic fields is facilitated by surface layers.

Weak fields of a few percent of equipartition can generate strong turbulence.

Results support the feasibility of large-scale magnetic fields in inner disks.

Abstract

We show that a large-scale, weak magnetic field threading a turbulent accretion disk tends to be advected inward, contrary to previous suggestions that it will be stopped by outward diffusion. The efficient inward transport is a consequence of the diffuse, magnetically-dominated surface layers of the disk, where the turbulence is suppressed and the conductivity is very high. This structure arises naturally in three-dimensional simulations of magnetorotationally unstable disks, and we demonstrate here that it can easily support inward advection and compression of a weak field. The advected field is anchored in the surface layer but penetrates the main body of the disk, where it can generate strong turbulence and produce values of alpha (i.e., the turbulent stress) large enough to match observational constraints; typical values of the vertical magnetic field merely need to reach a few percent of equipartition for this to occur. Overall, these results have important implications for models of jet formation which require strong, large-scale magnetic fields to exist over a region of the inner accretion disk.