  We examine time-dependent 2D relativistic radiation MHD flows to develop the
shock oscillation model for the long-term flares of Sgr A*. Adopting modified
flow parameters in addition to the previous studies, we confirm quasi-periodic
flares with periods of $\sim$ 5 and 10 days which are compatible with
observations by Chandra, Swift, and XMM-Newton monitoring of Sgr A*. Using a
simplified two-temperature model of ions and electrons, we find that the flare
due to synchrotron emission lags that of bremsstrahlung emission by 1 -- 2
hours which are qualitatively comparable to the time-lags of 1 -- 5 hours
reported in several simultaneous observations of radio and X-ray variability in
Sgr A*. The synchrotron emission is confined in a core region of 3 $R_{\rm g}$
size with the strong magnetic field, while the bremsstrahlung emission mainly
originates in a distant region of 10 -- 20 $R_{\rm g}$ behind the oscillating
shock, where $R_{\rm g}$ is the Schwarzschild radius. The time lag is estimated
as the transit time of the acoustic wave between the above two regions. The
time-averaged distribution of radiation shows a strong anisotropic nature along
the rotational axis but isotropic distribution in the radial direction. A
high-velocity jet with $\sim 0.6c$ along the rotational axis is intermittently
found in a narrow funnel region with a collimation angle $\sim 15^\circ$. The
shock oscillating model explains well the flaring rate and the time lag between
radio and X-ray emissions for the long-term flares of Sgr A*.
