The Impact of the Hall Effect on the Structure and Outflows of Magnetized Accretion Disks

Abstract

The structure and evolution of magnetic accretion disks are greatly affected by non-ideal MHD effects and the Hall effect is one of the special and key non-ideal MHD effects. In this work, we study the role of the Hall effect on the internal structure of magnetized outflow in both analytical analysis and numerical simulations of magnetized accretion disks. The fact that the physical problem is formulated in spherical coordinates (as opposed to an azimuthal coordinate) enables us to correctly represent the global behavior of disk winds and outflows in a fully physical manner. The analysis and the simulation approaches involve estimating partial differential equations that capture the intricate physics within the disk, including the role of the Hall term. These results show that the Hall effect breaks down the disk symmetry, and may significantly modify mass loss rates and the structure of outflows. Such results contribute to our understanding of the evolution of accretion disks, the birthplaces of stars and planet in the Universe.