Abstract
Abstract There have been a few previous studies claiming that the effects of geomagnetic storms strongly depend on the orientation of the magnetic cloud portion of coronal mass ejections (CMEs). Aparna & Martens, using halo-CME data from 2007 to 2017, showed that the magnetic field orientation of filaments at the location where CMEs originate on the Sun can be used to credibly predict the geoeffectiveness of the CMEs being studied. 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 on the solar surface and the corresponding Bz signatures at L1 are used to form a more extensive analysis for the results previously presented by Aparna & Martens. This study utilizes Solar and Heliospheric Observatory Extreme-ultraviolet Imaging Telescope 195 Å, Michelson Doppler Imager magnetogram images, and Kanzelhöhe Solar Observatory and Big Bear Solar Observatory Hα images for each particular time period, along with ACE data for interplanetary magnetic field signatures. Utilizing all these, we have found that the trend in Aparna & Martens’ study of a high likelihood of correlation between the axial field direction on the solar surface and Bz orientation persists for the data between 1996 and 2006, for which we find a match percentage of 65%.
Highlights
The correlation between the axial field direction of filaments and the Interplanetary Magnetic Field (IMF) Bz orientation of their corresponding Coronal Mass Ejections (CMEs) is of great importance to the astronomical community
This study provides more evidence for the correlation of axial field directions of solar filaments and the Bz orientation in the corresponding CMEs
With a set of 84 total CMEs determined in this analysis, a 63.09% match rate between the correlations of the filament axes and the Bz orientations was found
Summary
The correlation between the axial field direction of filaments and the Interplanetary Magnetic Field (IMF) Bz orientation of their corresponding Coronal Mass Ejections (CMEs) is of great importance to the astronomical community. Palmerio et al (2018)’s study focuses upon analyzing various features of the source region at the surface of the Sun to find the axial direction and using flux rope fittings at the L1 Lagrangian point between Sun and the Earth, and uses a subset of events from 2010-2015 Their analysis has given a match rate of 55% between the orientations at the sun and at Earth when considering a span of 45◦. Aparna & Martens (2020), hereafter AM20, considers all the halo-CMEs between 2007 and 2017 and analyze their corresponding filaments on the Sun to get the axial field direction to compare with the Bz component of the IMF near the Earth Their data-set is by far the largest and they classify ∼85% of the cases to have a match.
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