Abstract. The current work aims to explore the properties of geoeffective coronal mass ejections (CMEs) in solar cycle-24 (2009-2019). A total of 325 halo CMEs were discovered during our analysis, and 113 geoeffective events were chosen from them. Additionally, based on the speed of the CME, we divided the geoeffective events into two groups: CMEs with a speed of ≥ 1000 km/s and < 1000 km/s and we examined each group independently. Our analysis revealed that, for both groups of CMEs with a speed of &ge 1000 km/s and < 1000 km/s, the largest number of geoeffective events happened in the year 2012, whereas there were no geoeffective events occurrences in the year of solar minimum. Only one extremely strong storm having disturbance storm time index (Dst) -234 nT occurred during this solar cycle, and the majority of events are determined to be moderately geoeffective. The percentage of intense geoeffective events is higher for CMEs travelling at speeds greater than 1000 km/s than for those travelling at speeds less than 1000km/s. We discovered that the $Dst$ and CME speed for ≥ 1000 km/s and < 1000 km/s events had a correlation coefficient of 0.0069 and 0.063, respectively. We found that all halo CMEs in the multiple halo events are not responsible for producing the associated geomagnetic storms (GSs). The Geoeffective CMEs of speed ≥ 1000 km/s and < 1000 km/s occurred at low and moderate latitudes and are mainly disk events In addition, we discovered that M or X-class flares are responsible for most CMEs that have a speed of ≥ 1000 km/s, while M and C-class flares account for 28.3% and 26.86% of CMEs that have a speed of < 1000 km/s, respectively, and X and B-class flares for 5.97% and 20.89% of CMEs that have a speed of < 1000 km/s. Based on data analysis, we came to the conclusion that source areas and accompanying solar flares are significant factors for the strength of GSs, and that the mere speed of the halo CMEs is not a factor for the generation of GSs.

doi: https://doi.org/10.55318/bgjp.2025.52.2.131

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