Exploring the Origin and Dynamics of Solar Magnetic Fields

TL;DR

This paper investigates the origin, behavior, and effects of solar magnetic fields, combining theoretical modeling with observational data to understand their role in solar activity and phenomena like flares and coronal heating.

Contribution

It integrates magnetohydrodynamic dynamo theory with observational analysis to advance understanding of solar magnetic field generation and related solar phenomena.

Findings

Magnetic field generation modeled through dynamo theory

Insights into coronal heating mechanisms

Analysis of solar flare initiation processes

Abstract

The Sun is a magnetically active star and is the source of the solar wind, electromagnetic radiation and energetic particles which affect the heliosphere and the Earths atmosphere. The magnetic field of the Sun is responsible for most of the dynamic activity of the Sun. This thesis research seeks to understand solar magnetic field generation and the role that magnetic fields play in the dynamics of the solar atmosphere. Specifically, this thesis focuses on two themes: in the first part, we study the origin and behaviour of solar magnetic fields using magnetohydrodynamic dynamo theory and modelling, and in the second part, utilizing observations and data analysis we study two major problems in solar physics, namely, the coronal heating problem and initiation mechanisms of solar flares.