Characterizing the mean-field dynamo in turbulent accretion disks

TL;DR

This study develops a comprehensive mean-field model for turbulent accretion disks by analyzing magnetorotational turbulence, characterizing dynamo coefficients, and predicting magnetic cycle periods based on shear and turbulence properties.

Contribution

It systematically characterizes the mean-field dynamo coefficients and their scale dependence in turbulent accretion disks, advancing the understanding of magnetic field evolution.

Findings

The dynamo { extalpha} effect scales linearly with shear rate.

Turbulent diffusion { exteta} also scales linearly with shear.

The scale-separation ratio of the dynamo is approximately ten.

Abstract

The formation and evolution of a wide class of astrophysical objects is governed by turbulent, magnetized accretion disks. Understanding their secular dynamics is of primary importance. Apart from enabling mass accretion via the transport of angular momentum, the turbulence affects the long-term evolution of the embedded magnetic flux, which in turn regulates the efficiency of the transport. In this paper, we take a comprehensive next step towards an effective mean-field model for turbulent astrophysical disks by systematically studying the key properties of magnetorotational turbulence in vertically-stratified, isothermal shearing boxes. This allows us to infer emergent properties of the ensuing chaotic flow as a function of the shear parameter as well as the amount of net-vertical flux. Using the test-field method, we furthermore characterize the mean-field dynamo coefficients that describe the long-term evolution of large-scale fields. We simultaneously infer the vertical shape and the spectral scale dependence of these closure coefficients, with the latter describing non-local contributions to the turbulent electromotive force. Based on this, we infer a scale-separation ratio of about ten for the large-scale dynamo. We finally determine scaling properties of the mean-field dynamo coefficients. The relevant component of the dynamo {\alpha} effect is found to scale linearly with the shear rate, as is the corresponding turbulent diffusion, {\eta}. Together, these scalings allow us to predict, in a quantitative manner, the cycle period of the well-known butterfly diagram. This lends new support to the importance of the {\alpha}{\Omega} mechanism in determining the evolution of large-scale magnetic fields in turbulent accretion disks.