Saturation of the magnetorotational instability and the origin of magnetically elevated accretion discs

Abstract

We propose that the strength of angular momentum transport in accretion discs threaded by net vertical magnetic field is determined by a self-regulation mechanism: the magnetorotational instability (MRI) grows until its own turbulent resistivity damps the fastest growing mode on the scale of the disc thickness. Given weak assumptions as to the structure of MRI-derived turbulence, supported by prior simulation evidence, the proposed mechanism reproduces the known scaling of the viscous $\alpha$-parameter, $\alpha \propto {\beta }_z^{-1/2}$. Here, ${\beta }_z=8\pi p_g/B_{z0}^2$ is the initial plasma $\beta$-parameter on the disc midplane, $B_{z0}$ is the net field, and $p_g$ is the midplane gas pressure. We generalize the argument to discs with strong suprathermal toroidal magnetic fields, where the MRI growth rate is modified from the weak-field limit. Additional sources of turbulence are required if such discs are to become magnetically elevated, with the increased scale heights near the midplane that are seen in simulations. We speculate that tearing modes, associated with current sheets broadened by the effective resistivity, are a possible source of enhanced turbulence in elevated discs.

arXiv comment9 pages, 2 figures, to be published in Monthly Notices of the Royal Astronomical Society. Replaces arXiv:2211.09261, eliminating section 2.2 and with moderate revisions and clarifications in sections 3.1, 3.3, 4.2 and 4.3

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• Energy Extraction from a Black Hole by a Strongly Magnetized Thin Accretion Disk
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• Helical and nonhelical large-scale dynamos in thin accretion discs
• Direct Collapse Accretion Disks Within Dark Matter Halos: Saturation of the Magnetorotational Instability and the Field Expulsion