| Summary: | Halo Coronal Mass Ejections (HCMEs) are extreme solar events directly towards the Earth which expel an enormous amount of magnetic field and energetic plasma from the Sun. They are known to be geoeffective as they can generate geomagnetic storm and geomagnetic induced current upon their arrival. This study is aimed to investigate the kinematics of HCMEs and their relationships with geomagnetic storm intensity. The scope of this study includes all HCME events during minimum phase of solar cycle 25 (2020-2023) and this study focuses on the distribution of velocity and acceleration of flare and non-flare associated HCMEs. Data collection is made from SOHO LASCO Catalogue and SpaceWeatherLive that provide data of HCMEs properties and Kp-index of each relative geomagnetic storm. The outcomes show that a majority of non-flare HCMEs propagate below 1000 km/s and accelerate, while those accompanied by flares can travel further, exceeding 1000 km/s and they decelerate. HCMEs without flares that travel less than 1250 km/s are more likely to cause quiet storms and flare-associated HCMEs traveling at 500-2000 km/s generate more intense storms (above Kp4). Results of correlation analysis have demonstrated that Kp-index cannot be fully predicted based on velocity and acceleration as correlation coefficients are too weak for group of flare associated and non-flare associated HCMEs with R values of 0.059 and 0.27 respectively. As this study highlights the relationship of HCMEs with geomagnetic storm that have occurred, this acts as a reference to predict any possibilities of severe events that can be watched out. © 2024 Taylor's University. All rights reserved.
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