Overexpansion-dominated coronal mass ejection formation and induced radio bursts

Aims. Coronal Mass Ejections (CMEs) are the most fascinating explosion in solar system; however, their formation is still not fully understood. Methods. Here, we investigate a well-observed CME on 2021 May 07 that showed typical three-component structure and was continuously observed from 0 to 3 Rsun by combination of SDO/AIA (0--1.3 Rsun), PROBA2/SWAP (0--1.7 Rsun) MLSO/K-Cor (1.05--3 Rsun). Furthermore, compare morphological discrepancy between white-light bright core EUV blob. In end, explore origin various radio bursts closely related interaction overexpansion with nearby streamer. Results. An interesting finding height increases both leading front dominated during formation. The aspect ratios bubble core, quantifying overexpansion, found decrease as SO/STIX 4--10 keV GOES 1--8 A soft X-ray flux associated flare near peaks, indicating an important role reconnection first overexpansion. even takes place second although relatively weak, which compression streamer likely arises ideal MHD process. Moreover, blob be lower wider than may correspond bottom part growing rope. leads two type II bursts, one normally drifting stationary, speculated induced at different sources CME-driven shock front. bidirectional electrons evidenced series "C-shaped" III suggest interchange also involved