  We study two dimensional low angular momentum flow around the black hole
using the resistive magnetohydrodynamic module of PLUTO code. Simulations have
been performed for the flows with parameters of specific angular momentum,
specific energy, and magnetic field which may be expected for the flow around
Sgr A*. For flows with lower resistivity $\eta=10^{-6}$ and $0.01$, the
luminosity and the shock location on the equator vary quasi-periodically. The
power density spectra of luminosity variation show the peak frequencies which
correspond to the periods of $5 \times 10^5$, $1.4 \times 10^5$, and $5 \times
10^4$ seconds, respectively. These quasi-periodic oscillations (QPOs) occur due
to the interaction between the outer oscillating standing shock and the inner
weak shocks occurring at the innermost hot blob. While for cases with higher
resistivity $\eta=0.1$ and 1.0, the high resistivity considerably suppresses
the magnetic activity such as the MHD turbulence and the flows tend to be
steady and symmetric to the equator. The steady standing shock is formed more
outward compared with the hydrodynamical flow. The low angular momentum flow
model with the above flow parameters and with low resistivity has a possibility
for the explanation of the long-term flares with $\sim$ one per day and $\sim 5
- 10$ days of Sgr A* in the latest observations by Chandra, Swift, and
XMM-Newton monitoring of Sgr A*.
