Linear Stability Analysis of a Magnetic Rotating Disk with Ohmic Dissipation and Ambipolar Diffusion

TL;DR

This paper conducts a linear stability analysis of magnetized, rotating, self-gravitating sheets considering nonideal MHD effects, revealing how these factors influence gravitational instability scales relevant to protostellar disk formation.

Contribution

It introduces a comprehensive linear stability framework including Ohmic dissipation and ambipolar diffusion for rotating, magnetized sheets, extending previous models.

Findings

Identifies a preferred length scale and minimum timescale for gravitational instability.

Shows the maximum instability scale depends on nonideal MHD parameters.

Finds the preferred fragmentation mass range to be approximately 10-90 Jupiter masses.

Abstract

We perform a linear analysis of the stability of isothermal, rotating, magnetic, self-gravitating sheets that are weakly ionized. The magnetic field and rotation axis are perpendicular to the sheet. We include a self-consistent treatment of thermal pressure, gravitational, rotational, and magnetic (pressure and tension) forces together with two nonideal magnetohydrodynamic (MHD) effects (Ohmic dissipation and ambipolar diffusion) that are treated together for their influence on the properties of gravitational instability for a rotating sheet-like cloud or disk. Our results show that there is always a preferred length scale and associated minimum timescale for gravitational instability. We investigate their dependence on important dimensionless free parameters of the problem: the initial normalized mass-to-flux ratio $\mu_0$, the rotational Toomre parameter $Q$, the dimensionless Ohmic diffusivity $\tilde{\eta}_{\rm OD,0}$, and the dimensionless neutral-ion collision time $\tilde{\tau}_{\rm{ni,0}}$ that is a measure of the ambipolar diffusivity. One consequence of $\tilde{\eta}_{\rm OD,0}$ is that there is a maximum preferred lengthscale of instability that occurs in the transcritical ($\mu_0 \gtrsim 1$) regime, qualitatively similar to the effect of $\tilde{\tau}_{\rm{ni,0}}$, but with quantitative differences. The addition of rotation leads to a generalized Toomre criterion (that includes a magnetic dependence) and modified lengthscales and timescales for collapse. When nonideal MHD effects are also included, the Toomre criterion reverts back to the hydrodynamic value. We apply our results to protostellar disk properties in the early embedded phase and find that the preferred scale of instability can significantly exceed the thermal (Jeans) scale and the peak preferred fragmentation mass is likely to be $\sim 10- 90 \ M_{\rm Jup}$.