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

Overexpansion-dominated Coronal Mass Ejection Formation and Induced Radio Bursts