Analysis of the Coronal Mass Ejections through Axial Field Direction of Solar Filaments and IMF Bz

TL;DR

This study extends previous research by analyzing solar filament axial field directions and IMF Bz data from 1996-2006, confirming the correlation between filament orientation and geomagnetic storm potential.

Contribution

It provides an extended analysis of filament axial fields and IMF Bz, validating earlier findings over a broader time period and dataset.

Findings

High correlation between filament axial field and Bz orientation persists from 1996-2006.

Filament magnetic field direction can be used to predict geomagnetic storm onset.

Extended dataset confirms previous correlation results.

Abstract

In the past, there have been many studies claiming that the effects of geomagnetic storms strongly depends on the orientation of the magnetic-cloud part of the Coronal Mass Ejections (CMEs). Aparna & Martens (2020), using Halo-CME data from 2007-2017, have shown that the magnetic field orientation of filaments at the location where CMEs originate can be effectively used for predicting the onset of geo-magnetic storms. The purpose of this study is to extend their survey by analyzing the halo-CME data for 1996-2006. The correlation of filament axial direction and their corresponding Bz signatures are used to form a more extensive reasoning for the claims presented by Aparna & Martens before. This study utilizes SOHO EIT 195 \r{A}, MDI magnetogram images, KSO and BBSO H$\alpha$ images for the time period, along with ACE data for inter-planetary magnetic field signatures. Correlating all these, we have found that the trend in Aparna & Martens' study of a high likelihood of the correlation between the axial field direction and Bz orientation, persists for the data between 1996-2006 as well.