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Episodic ejections of blobs (episodic jets) are widely observed in black holesources and usually associated with flares. In this paper, by performing andanalyzing three dimensional general relativity magnetohydrodynamical numericalsimulations of accretion flows, we investigate their physical mechanisms. Wefind that magnetic reconnection occurs in the accretion flow, likely due to theturbulent motion and differential rotation of the accretion flow, resulting inflares and formation of flux ropes. Flux ropes formed inside of 10-15gravitational radii are found to mainly stay within the accretion flow, whileflux ropes formed beyond this radius are ejected outward by magnetic forces andform the episodic jets. These results confirm the basic scenario proposed inYuan et al.(2009). Moreover, our simulations find that the predicted velocityof the ejected blobs is in good consistency with observations of Sgr A*, M81,and M87. The whole processes are found to occur quasi-periodically, with theperiod being the orbital time at the radius where the flux rope is formed. Thepredicted period of flares and ejections is consistent with those found fromthe light curves or image of Sgr A*, M87, and PKS 1510-089. The possibleapplications to protostellar accretion systems are discussed.

Formation of episodic jets and associated flares from black hole accretion systems