  Sgr A* is thought to be the radiative manifestation of a ~3.6E6 Msun
supermassive black hole at the Galactic center. Its mm/sub-mm spectrum and its
flare emission at IR and X-ray wavelengths may be produced within the inner ten
Schwarzschild radii of a hot, magnetized Keplerian flow. The lightcurve
produced in this region may exhibit quasi-periodic variability. We present
ray-tracing simulations to determine the general-relativistically modulated
X-ray luminosity expected from plasma coupled magnetically to the rest of the
disk as it spirals inwards below the innermost stable circular orbit towards
the "stress edge" in the case of a Schwarzschild metric. The resulting
lightcurve exhibits a modulation similar to that observed during a recent X-ray
flare from Sgr A*.
