  PAPER WITHDRAWN.
  The recent detection of Sgr A* in the X-ray band, together with the radio
polarization measurements conducted over the past few years, offer the best
constraints yet for understanding the nature of the emitting gas within several
Schwarzschild radii ($r_S$) of this supermassive black hole candidate at the
Galactic Center. Earlier, we showed that the sub-mm radiation from this source
may be associated with thermal synchrotron emission from an inner Keplerian
region within the circularization radius of the accreting plasma. In this
paper, we extend this analysis in a very important way, by calculating the
implied high-energy emission of Sgr A* associated with the orbiting, hot,
magnetized gas. We find that for the accretion rate inferred from the fits to
the sub-mm data, the dominant contribution to Sgr A*'s X-ray flux is due to
self-Comptonization of the radio photons, rather than from bremsstrahlung. The
latter is a two-body process, which would produce significant X-ray emission
only at much higher accretion rates. This picture leads to the testable
prediction that the physical conditions within the inner $\sim5r_S$ are
variable on a time scale of order a year. In particular, the accretion rate
$\dot M$ appears to have changed by about 15% between the sub-mm measurements
in 1996 and 1999. Given that the radio and self-Comptonized fluxes are strongly
correlated in this picture, the upcoming second generation Chandra observations
of Sgr A* may provide the direct evidence required to test this model.
