  Sgr A* is an ideal target to study low-luminosity accreting systems. It has
been recently proposed that properties of the accretion flow around Sgr A* can
be probed through its interactions with the stellar wind of nearby massive
stars belonging to the S-cluster. When a star intercepts the accretion disk,
the ram and thermal pressures of the disk terminate the stellar wind leading to
the formation of a bow shock structure. Here, a semi-analytical model is
constructed which describes the geometry of the termination shock formed in the
wind. With the employment of numerical hydrodynamic simulations, this model is
both verified and extended to a region prone to Kelvin-Helmholtz instabilities.
Because the characteristic wind and stellar velocities are in $\sim10^{8}$ cm
s$^{-1}$ range, the shocked wind may produce detectable X-rays via thermal
bremsstrahlung emission. The application of this model to the pericenter
passage of S2, the brightest member of the S-cluster, shows that the shocked
wind produces roughly a month long X-ray flare with a peak luminosity of
$L\approx 4 \times 10^{33}$ erg s$^{-1}$ for a stellar mass-loss rate, disk
number density, and thermal pressure strength of $\dot{M}_{\rm w}= 10^{-7}
M_\odot\, {\rm yr}^{-1}$, $n_{\rm d} = 10^{5}$ cm$^{-3}$, and $\alpha=0.1$,
respectively. This peak luminosity is comparable to the quiescent X-ray
emission detected from Sgr A* and is within the detection capabilities of
current X-ray observatories. Its detection could constrain the density and
thickness of the disk at a distance of $\sim 3000$ gravitational radii from the
supermassive black hole.
