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 \sim 10 ^ { 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 } _ { w } = 10 ^ { -7 } M _ { \odot } { yr } ^ { -1 } , n _ { 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 .