Formulation of the solar surface dynamo

TL;DR

This paper presents a first-principles formulation of the solar surface dynamo, incorporating partial ionization and multifluid effects like Hall and ambipolar diffusion, to better understand magnetic field structures on the sun.

Contribution

It introduces a novel, first-principles approach to modeling the solar surface dynamo that includes non-ideal MHD effects such as partial ionization, Hall effect, and ambipolar diffusion.

Findings

Highlights the importance of non-ideal effects in solar dynamo modeling

Provides a theoretical framework for future simulations of the solar surface magnetic fields

Suggests modifications to standard dynamo models to include multifluid plasma effects

Abstract

The solar surface dynamo has become an active area of research in an attempt to understand the origin of a variety of magnetic field structures on the sun. The major modification that needs to be incorporated in the standard dynamo process is the inclusion of the partial ionization of the gas in the layers underlying and overlaying the photosphere along with the effects associated with the multifluid nature of the system. This not only changes the inertia carrying species but also substantially modifies the temporal and spatial evolution of the magnetic induction. The energy equation also carries the import of these non-ideal effects. The effects such as the Hall effect and the ambipolar diffusion take the dynamo study beyond the realm of the ideal magnetohydrodynamics. In this paper, a first principle formulation of the solar surface dynamo problem has been attempted.