2-D MHD Configurations for Accretion Disks Around Magnetized Stars

TL;DR

This paper explores the structure of accretion disks around magnetized stars, comparing traditional visco-resistive MHD models with plasma instabilities like ballooning modes caused by low resistivity.

Contribution

It introduces a comparison between standard MHD accretion models and plasma instabilities, highlighting the effects of low resistivity on disk morphology.

Findings

Standard MHD models describe steady accretion disk features.

Plasma instabilities can significantly alter disk structure.

Low resistivity triggers ballooning modes affecting accretion dynamics.

Abstract

We discuss basic features of steady accretion disk morphology around magnetized compact astrophysical objects. A comparison between the standard model of accretion based on visco-resistive MHD and the plasma instabilities, like ballooning modes, triggered by very low value of resistivity, is proposed.