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We study the small scale magnetic reconnection above the radiativeinefficient accretion flow around massive black hole via 2Dmagnetohydrodynamics (MHD) numerical simulation, in order to model the blobformation and ejection from the accretion flow around Sgr A*. The connection ofboth the newly emerging magnetic field and the pre-existing magnetic field isinvestigated to check whether blobs could be driven in the environment of blackhole accretion disc. After the magnetic connection, both the velocity andtemperature of the plasma can be comparable to the inferred physical propertiesat the base of the observed blob ejection. For illustration, three small boxeswhich are located within 40 Schwarzschild radii from the central black hole arechosen as our simulation areas. At the beginning of the reconnections, thefluid is pulled toward the central black hole due to the gravitationalattraction and the current sheet produced by the reconnection is also pulledtoward the same direction, consequently, the resulting outflows move bothupwards and towards the symmetry axis of the central black hole. Eventually,huge blobs appear, which supports the catastrophe model of episodic jets\citep{2009MNRAS.395.2183Y}. It is also found that the closer to the black holethe magnetic connection happens, the higher the converting efficiency of themagnetic energy into the heat and kinetic energy. For these inner blobs, theyhave vortex structure due to the K-H instability, which happens along thecurrent sheet separating the fluids with different speed.

Blob formation and ejection from the radiative inefficient accretion flow around massive black hole