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Using high time cadence images from the STEREO EUVI, COR1 and COR2instruments, we derived detailed kinematics of the main acceleration stage fora sample of 95 CMEs in comparison with associated flares and filamenteruptions. We found that CMEs associated with flares reveal on averagesignificantly higher peak accelerations and lower acceleration phase durations,initiation heights and heights, at which they reach their peak velocities andpeak accelerations. This means that CMEs that are associated with flares arecharacterized by higher and more impulsive accelerations and originate fromlower in the corona where the magnetic field is stronger. For CMEs that areassociated with filament eruptions we found only for the CME peak accelerationsignificantly lower values than for events which were not associated withfilament eruptions. The flare rise time was found to be positively correlatedwith the CME acceleration duration, and negatively correlated with the CME peakacceleration. For the majority of the events the CME acceleration starts beforethe flare onset (for 75% of the events) and the CME accleration ends after theSXR peak time (for 77% of the events). In ~60% of the events, the timedifference between the peak time of the flare SXR flux derivative and the peaktime of the CME acceleration is smaller than \pm5 min, which hints at afeedback relationship between the CME acceleration and the energy release inthe associated flare due to magnetic reconnection.

Impulsive acceleration of coronal mass ejections: II. Relation to SXR flares and filament eruptions