Modelling the Global Solar Corona: Filament Chirality Observations and Surface Simulations

TL;DR

This study compares observed filament chirality patterns with advanced surface and coronal magnetic field simulations over six months, demonstrating a new technique that maintains magnetic field accuracy without resetting, enabling long-term solar magnetic studies.

Contribution

It introduces a novel simulation method that accurately models the solar surface magnetic field over extended periods without resetting, improving long-term coronal magnetic field modeling.

Findings

Large-scale surface magnetic field remains accurate over 6 months

Simulation technique captures filament chirality patterns effectively

Method enables long-term helicity and shear transport studies

Abstract

The hemispheric pattern of solar filaments is considered in the context of the global magnetic field of the solar corona. In recent work Mackay and van Ballegooijen have shown how, for a pair of interacting magnetic bipoles, the observed chirality pattern could be explained by the dominant range of bipole tilt angles and helicity in each hemisphere. This study aims to test this earlier result through a direct comparison between theory and observations, using newly-developed simulations of the actual surface and 3D coronal magnetic fields over a 6-month period, on a global scale. In this paper we consider two key components of the study; firstly the observations of filament chirality for the sample of 255 filaments, and secondly our new simulations of the large-scale surface magnetic field. Based on a flux-transport model, these will be used as the lower boundary condition for the future 3D coronal simulations. Our technique differs significantly from those of other authors, where the coronal field is either assumed to be purely potential, or has to be reset back to potential every 27 days in order that the photospheric field remain accurate. In our case we ensure accuracy by the insertion of newly-emerging bipolar active regions, based on observed photospheric synoptic magnetograms. The large-scale surface field is shown to remain accurate over the 6-month period, without any resetting. This new technique will enable future simulations to consider the long-term build-up and transport of helicity and shear in the coronal magnetic field, over many months or years.