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The vicinity of the supermassive black hole associated with the compact radiosource Sagittarius (Sgr) A* is believed to dominate the observed emission atwavelengths near and shorter than $\sim$ 1 millimeter. We show that a generalrelativistic accretion flow, heated via the plasma wave heating mechanism, isconsistent with the polarization and recent mm-VLBI observations of Sgr A* foran inclination angle of $\sim 45^\circ$, position angle of $\sim 140^\circ$,and spin $\lesssim 0.9$. Structure in visibilities produced by the black holeshadow can potentially be observed by 1.3 mm-VLBI on the existing Hawaii-CARMAand Hawaii-SMT baselines. We also consider eight additional potential mm-VLBIstations, including sites in Chile and New Zealand, finding that with these thebasic geometry of the emission region can be reliably estimated.

Testing the Accretion Flow with Plasma Wave Heating Mechanism for Sagittarius a* by the 1.3MM Vlbi Measurements