  I review radiatively inefficient accretion flow models for the 2.6 million
solar mass black hole (BH) in the Galactic Center. I argue for a 'concordance
model' of Sgr A*: both theory and observations suggest that hot ambient gas
around the BH is accreted at a rate of order 10^{-8} solar masses/year, much
less than the canonical Bondi rate. I interpret Chandra observations of Sgr A*
in the context of such a model: (1) the extended 'quiescent' X-ray emission is
due to thermal bremsstrahlung from gas in the vicinity of the Bondi accretion
radius, and (2) the ~ ksec long X-ray flares are due to synchrotron or
Inverse-Compton emission by non-thermal electrons accelerated in the inner 10
Schwarzschild radii of the accretion flow.
