Stability of accretion discs threaded by a strong magnetic field

Abstract

We study the stability of poloidal magnetic fields anchored in a thin accretion disc. The two-dimensional hydrodynamics in the disc plane is followed by a grid-based numerical simulation including the vertically integrated magnetic forces. The 3--dimensional magnetic field outside the disc is calculated in a potential field approximation from the magnetic flux density distribution in the disc. For uniformly rotating discs we confirm numerically the existence of the interchange instability as predicted by Spruit, Stehle & Papaloizou (1995). In agreement with predictions from the shearing sheet model, discs with Keplerian rotation are found to be stabilized by the shear, as long as the contribution of magnetic forces to support against gravity is small. When this support becomes significant, we find a global instability which transports angular momentum outward and allows mass to accrete inward. The instability takes the form of a $m=1$ rotating `crescent', reminiscent of the purely hydrodynamic nonlinear instability previously found in pressure-supported discs. A model where the initial surface mass density $\Sigma (r)$ and $B_{\mathrm{z}}(r)$ decrease with radius as power laws shows transient mass accretion during about 6 orbital periods, and settles into a state with surface density and field strength decreasing approximately exponentially with radius. We argue that this instability is likely to be the main angular momentum transport mechanism in discs with a poloidal magnetic field sufficiently strong to suppress magnetic turbulence. It may be especially relevant in jet-producing discs.

MNRAS in press. 9 postscript figures included in text, 4 jpeg images included separately

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