  In the previous numerical study, we find the blob formation and ejection in
the presence of magnetic reconnection in the environment of the hot flow of the
accretion disk. Based on those encouraging results, in the present work, we
calculate the energy and the spectrum of the emission in the different bands
around Sgr A*. We assume the electrons in the magnetic reconnection region are
non-thermal and emits synchrotron radiation. The electrons in the other region
are thermal, which follows the thermal distribution, and the thermal electron
emission mechanism is thermal synchrotron radiation. During the whole process
of the magnetic evolution and reconnection, we find two peaks in the temporal
light curve in the recently observed Radio frequencies (230 GHz and 43 GHz) and
NIR wavelengths. Although, the light curve of the NIR band is most prominent in
a single peak. The first peak appears because of the blob in the plasma flow,
which is formed due to the magnetic reconnection. The second peak appears due
to the production of the non-thermal electrons with the evolution of the
magnetic flux. Both peaks reach luminosity more than 1026 erg/s for a single
plasmoid/blob. For the NIR band, the highest luminosity can reach more than
1028 erg/s. These luminosities can be high for the large simulation area and
the stronger magnetic field with the multiple blobs. We infer that the observed
flares are a group of magnetic reconnection phenomena, not a single one.
