Abstract
We researched the slow, normal, and fast coronal mass ejections (CMEs) associated with solar flares ( \({>}\) M5.0 X-ray class) from December 2019 to July 2023 (44 month period) in the early rising phase of solar cycle 25. This research aims to examine the features of slow, normal, and fast CMEs along with their associated Solar Flares, Type II Bursts, SEPs, and Geomagnetic Storms. This paper highlights CME-Flare pairs by grouping them based on speed and investigating their connection to DH type II bursts, solar energetic particle occurrences, and Dst indices. The locations of flares associated with the three types of CMEs, the number of events corresponding to different flare classes, as well as the flare rise times and durations, were thoroughly studied. During the study period, we analyzed the 57 CME events and the distribution of their angular widths. Using different electron density models, the start distance, end distance, drift rate, and shock speed were analyzed in detail. Solar energetic particles (SEPs) with intensities greater than 10 pfu, generated by shock waves and the geoeffectiveness of full halo CME, were discussed. In this statistical study, we conclude that the fast CMEs are associated with longer flare durations, and stronger geoeffectiveness compared to slow and normal CMEs. They are also significant drivers of type II radio bursts, SEP events, and geomagnetic storms.
