Simulations of the Poynting--Robertson Cosmic Battery in Resistive Accretion Disks

TL;DR

This paper presents 2.5D MHD simulations demonstrating how the Poynting--Robertson effect generates magnetic fields in accretion disks, leading to MRI-driven angular momentum transfer and episodic jet formation.

Contribution

It introduces a novel simulation of the PR-driven magnetic field generation and its role in disk evolution, including MRI activation and jet production.

Findings

Magnetic fields grow linearly without saturation in the inner disk.

MRI transfers angular momentum outward, forming a magnetized nuclear disk.

Episodic jet-like outflows occur when magnetic fields reach equipartition.

Abstract

We describe the results of numerical "2.5--dimensional" MHD simulations of an initially unmagnetized disk model orbiting a central point--mass and responding to the continual generation of poloidal magnetic field due to a secular source that emulates the Poynting--Robertson (PR) drag on electrons in the vicinity of a luminous stellar or compact accreting object. The fluid in the disk and in the surrounding hotter atmosphere has finite electrical conductivity and allows for the magnetic field to diffuse freely out of the areas where it is generated, while at the same time, the differential rotation of the disk twists the poloidal field and quickly induces a substantial toroidal--field component. The secular PR term has dual purpose in these simulations as the source of the magnetic field and the trigger of a magnetorotational instability (MRI) in the disk. The MRI is especially mild and does not destroy the disk because a small amount of resistivity dampens the instability efficiently. In simulations with moderate resistivities (diffusion timescales up to $\sim$16 local dynamical times) and after $\sim$100 orbits, the MRI has managed to transfer outward substantial amounts of angular momentum and the inner edge of the disk, along with azimuthal magnetic flux, has flowed toward the central point--mass where a new, magnetized, nuclear disk has formed. The toroidal field in this nuclear disk is amplified by differential rotation and it cannot be contained; when it approaches equipartition, it unwinds vertically and produces episodic jet--like outflows. The poloidal field in the inner region cannot diffuse back out if the characteristic diffusion time is of the order of or larger than the dynamical time; it continues to grow linearly in time undisturbed and without saturation, as the outer sections of many poloidal loops are being drawn radially outward.