  We study the small scale magnetic reconnection above the radiative
inefficient accretion flow around massive black hole via 2D
magnetohydrodynamics (MHD) numerical simulation, in order to model the blob
formation and ejection from the accretion flow around Sgr A*. The connection of
both the newly emerging magnetic field and the pre-existing magnetic field is
investigated to check whether blobs could be driven in the environment of black
hole accretion disc. After the magnetic connection, both the velocity and
temperature of the plasma can be comparable to the inferred physical properties
at the base of the observed blob ejection. For illustration, three small boxes
which are located within 40 Schwarzschild radii from the central black hole are
chosen as our simulation areas. At the beginning of the reconnections, the
fluid is pulled toward the central black hole due to the gravitational
attraction and the current sheet produced by the reconnection is also pulled
toward the same direction, consequently, the resulting outflows move both
upwards 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 hole
the magnetic connection happens, the higher the converting efficiency of the
magnetic energy into the heat and kinetic energy. For these inner blobs, they
have vortex structure due to the K-H instability, which happens along the
current sheet separating the fluids with different speed.
