The Jet Model for Sgr A *

In this paper the jet model for the supermassive black hole candidate Sgr A* in the Center of the Galaxy is reviewed. The most recent model, with a reduced set of parameters, is able to account for all major radio properties of the source: size, structure, ux density, and spectrum. The model requires a minimum jet power of 10 39 erg/sec and in a symbiotic jet/disk system implies a minimum accretion rate of a few times 10 ?8 M /yr for a radio loud jet or 10 ?5 M /yr for a radio quiet jet. Low near-infrared limits on the Sgr A* ux then imply that the accretion ow onto the central black hole must be radiatively deecient, but most likely has a high viscosity. Within the jet model the high-frequency part of the Sgr A* spectrum is self-consistently explained as the nozzle of the outtow. In a symbiotic model this innermost region of the jet could possibly be identiied with the innermost region of an advection dominated accretion disk, a Bondi-Hoyle accretion ow, or any other type of underluminous accretion process. The compact nozzle region is of particular importance since it can be used as a background photon source against which the central black hole could be directly imaged with future mm-VLBI experiments.