  We employ a low angular momentum accretion-outflow scenario to model the
flares emanating out from the central region of Sgr A$^*$. The primary donor
for matter accreting onto the central SMBH of Sgr A$^*$ is assumed to be the WR
star ISR 13 E3. We analytically calculate the specific energy and angular
momentum density of stellar wind originating from ISR 13 E3 and study the
dynamics of that wind down to the very close vicinity of the central SMBH of
Sgr A$^*$. We show that on the way to the Galactic centre, such wind-fed
accretion may encounter standing shocks and such shock drives outflow from the
close vicinity of the SMBH. Matter content of such outflow is computed and it
is argued that such outflow is responsible for production of the Galactic
centre flares. We then self-consistently compute the luminosity ${\cal L}_j$
and the duration time scale $\tau$ of such flares, as a function of fundamental
accretion parameters. Our theoretical calculation of ${\cal L}_j$ and $\tau$
are in good agreement with observational results.
