Solar Transients and Space Weather (STSW) Section

Introduction

About the Solar Transients and Space Weather Section

The Sun's ubiquitous magnetism is formed in the solar interior. Relentlessly, magnetic flux rises through the star's convective layers and pierces the photosphere at almost all spatial scales to mould the structures of the Sun's outer atmosphere. In addition, the blend of convective motion and magnetism provide an almost endless reservoir of energy to supply the solar corona and wind, as well as a host of impulsive events such as flares and coronal mass ejections (CMEs). HAO's Solar Transients and (the Origins of) Space Weather research section, or STSW, is dedicated to understanding the processes that establish the (magnetism-governed) flow of mass and energy through the outer atmosphere that give rise to the radiative and particulate output which bathes the solar system. We study these processes using a blend of observation, theory, and numerical simulation, developing cutting edge concepts in each area to understand the short-term variability of our relentless star.