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Multi-instrument observations of two filament eruptions on 24 February and 11May 2011 suggest the following updated scenario for eruptive flare, CME andshock wave evolution. An initial destabilization of a filament results instretching out of magnetic threads belonging to its body and rooted in thephotosphere along the inversion line. Their reconnection leads to i) heating ofparts of the filament or its environment, ii) initial development of the flarearcade cusp and ribbons, and iii) increasing similarity of the filament to acurved flux rope and its acceleration. Then the pre-eruption arcade envelopingthe filament gets involved in reconnection according to the standard model andcontinues to form the flare arcade and ribbons. The poloidal magnetic flux inthe curved rope developing from the filament progressively increases and forcesits toroidal expansion. This flux rope impulsively expands and produces an MHDdisturbance, which rapidly steepens into a shock. The shock passes through thearcade expanding above the filament and then freely propagates ahead of the CMElike a decelerating blast wave for some time. If the CME is slow, then theshock eventually decays. Otherwise, the frontal part of the shock changes intothe bow-shock regime. This was observed for the first time in the 24 February2011 event. When reconnection ceases, the flux rope relaxes and constitutes theCME core-cavity system. The expanding arcade develops into the CME frontalstructure. We also found that reconnection in the current sheet of a remotestreamer forced by the shock's passage results in a running flare-like processwithin the streamer responsible for a type II burst. The development of dimmingand various associated phenomena are discussed.

Responsibility of a Filament Eruption for the Initiation of a Flare, CME, and Blast Wave, and its Possible Transformation into a Bow Shock